Discovery of new members of the nearby young stellar association in Cepheus
A. Klutsch A. Frasca P. Guillout D. Montes F. -X. Pineau N. Grosso B. Stelzer
astro-ph.SR astro-ph.GA





A. Klutsch 

klutsch@astro.uni-tuebingen.de


Institut für Astronomie und Astrophysik, Eberhard Karls Universität, Sand 1, D-72076 Tübingen, Germany
INAF-Osservatorio Astrofisico di Catania, via S. Sofia 78, I-95123 Catania, Italy
Observatoire Astronomique, Université de Strasbourg & CNRS, UMR 7550, 11 rue de l'Université, F-67000 Strasbourg, France
Departamento de Física de la Tierra y Astrofísica and IPARCOS-UCM (Instituto de Física de Partículas y del Cosmos de la UCM),
Facultad de Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90134 Palermo, Italy




Young field stars are hardly distinguishable from older ones because their space motion rapidly mixes them with the stellar population of the Galactic plane. Nevertheless, a careful target selection allows for young stars to be spotted throughout the sky.

We aim to identify additional sources associated with the four young comoving stars that we discovered towards the CO Cepheus void and to provide a comprehensive view of the Cepheus association. 

Based on multivariate analysis methods, we have built an extended sample of 193 young star candidates, which are the optical and infrared counterparts of ROSAT All-Sky Survey and XMM-Newton X-ray sources. From optical spectroscopic observations, we measured their radial velocity with the cross-correlation technique. We derived their atmospheric parameters and projected rotational velocity with the code ROTFIT. We applied the subtraction of inactive templates to measure the lithium equivalent width, from which we infer their lithium abundance and age. Finally, we studied their kinematics using the second Gaia data release.

Our sample is mainly composed of young or active stars and multiple systems. We identify two distinct populations of young stars that are spatially and kinematically separated. Those with an age between 100 and 300 Myr are mostly projected towards the Galactic plane. In contrast, 23 of the 37 sources younger than 30 Myr are located in the CO Cepheus void, and 21 of them belong to the stellar kinematic group that we previously reported in this sky area. We report a total of 32 bona fide members and nine candidates for this nearby (distance =157± 10 pc) young (age = 10–20 Myr) stellar association. According to the spatial distribution of its members, the original cluster is already dispersed and partially mixed with the local population of the Galactic plane.



Properties of the young stellar association in Cepheus
A. Klutsch et al.
Discovery of new members of the nearby young stellar association in Cepheus
Based on observations collected at the Isaac Newton Telescope (INT) operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias, the 2.2-m telescope of the German-Spanish Astronomical Centre, Calar Alto (Almería, Spain), operated by the Max-Planck-Institute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy, and the SOPHIE spectrograph on the 1.93-m telescope at Observatoire de Haute-Provence (CNRS), France (program 09A.PNPS.GUIL).
Tables <ref> and <ref>–<ref> are available at the CDS via anonymous FTP to 
		   cdsarc.u-strasbg.fr (130.79.128.5) or via 
		   http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/.

    A. Klutsch 1,2,4, A. Frasca2, P. Guillout3, D. Montes4,  F.-X. Pineau3, N. Grosso5 B. Stelzer 1,6
	    
    Received 29 November 2019 / Accepted 07 March 2020
========================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================================






§ INTRODUCTION



The “natural” birth sites of stars are young open clusters and star-forming regions (SFRs) which are often tightly associated with emission nebulae and molecular clouds <cit.>. However young stars are also found in wide regions around SFRs and also in the field, apparently unrelated to any of the known star-forming sites. Such populations of young stars are composed of both classical T Tauri stars (CTTSs) and weak-line T Tauri stars (WTTSs). There is evidence of different space distributions for CTTSs and WTTSs, the former  located near the cloud cores while the latter are spread all around the SFR <cit.>. Moreover, WTTSs are on average older than CTTSs and have already dissipated their accretion disks <cit.>. These young stars may form substructures that can be located up to tens of parsecs away from the SFR's core <cit.>. 

In the 1990s, various scenarios for explaining the presence of dispersed young stars were proposed. For those located in the outskirts of SFRs or in the space surrounding them, the simplest explanation was that they had drifted by thermal velocity dispersion of gas within star-forming sites. On the other hand, those far away from any conventional SFRs should have formed locally from cloudlets in turbulent giant molecular clouds <cit.>. However neither of these theories could explain the presence of T Tauri stars (TTSs) with high space velocity, the so-called “runaway” TTSs <cit.>. Their ejection could have occurred during the dynamical evolution of young multiple systems and come from close encounters with other members of their parent cloud <cit.>.

The picture of star formation in our Galaxy is still not well-defined and new important details are being added by the recent large spectroscopic surveys and astrometric space missions, such as Gaia. One of the most relevant results of the Gaia-ESO survey <cit.> is the discovery of two kinematically distinct populations (A and B) in the field of both the Gamma Velorum <cit.> and NGC 2547 <cit.> clusters. The properties of sources belonging to Gamma Velorum B and NGC 2547 B are fairly similar in terms of age and kinematics. Since these two clusters are close to each other (≈ 6 on the sky corresponding to about 40 pc at their distance) and both are in the field of the Vela OB2 association, the B populations of these two clusters might form an extended low-mass population in the Vela OB2 association. 

Over the past two decades, several nearby (30–150 pc) young (5–70 Myr) associations were identified, mostly in the southern hemisphere <cit.>. <cit.> found many of them and their members during the SACY survey. The use of a Bayesian analysis and, subsequently, the BANYAN Σ multivariate Bayesian algorithm contributed significantly to the continued identification of new members, mainly low-mass stars and brown dwarfs <cit.>. The first release of the Gaia mission <cit.> improved the astrometric accuracy for the Tycho sources. This has made it possible to search for new comoving stars <cit.>, as well as stellar kinematic groups and clusters <cit.>. Based on the very accurate astrometry from the second data release of the Gaia mission <cit.>, <cit.> discovered a considerable number of likely new members in these young associations.

However, it remains difficult to recognize the young stars without a circumstellar disk in the field among the Galactic plane stellar population. Neither their global photometric properties nor the presence of nearby gas differentiates them from older stars. An efficient methodology for identifying the young stars is through the use of large X-ray surveys because the stellar X-ray sources in the ROSAT catalog are mainly stars younger than 1 Gyr <cit.>. <cit.> showed that this stellar population can be used as a tracer of young local structures, like the late-type stellar population in the Gould Belt <cit.>. To this end, <cit.> cross-correlated the ROSAT All-Sky Survey (RASS) with the Tycho catalog building the first large dataset (≈ 14,000 objects) of late-type stellar X-ray sources, the so-called RasTyc sample. 

Spectroscopic surveys of northern RasTyc sources were performed by <cit.> and <cit.>. In Paper I, we identified five young field stars in the optically bright (V<9.5 mag) sample. Afterwards, BD+44 3670 and BD+45 598 were recognized as members of the Columba association <cit.> and of the β Pic moving group <cit.>, respectively. <cit.> noticed that an almost uniform spatial density of young stars in the optically bright RasTyc sample. At the same time, the spatial density in the northern hemisphere (Paper I) is about one order of magnitude lower, on average, than that in the southern hemisphere (the SACY survey). This is consistent with the significant asymmetry in the all-sky RasTyc map with respect to the Galactic plane, as reported by <cit.>, and is likely related to the structure of the Gould Belt. A higher fraction of young stars was found in the optically faint sample (Paper III). This may be due to the larger distances involved, on average, in the faint survey, which facilitated the detection of many more intrinsically brighter X-ray (more active and younger) sources when compared to the bright sample. A larger contribution from the Gould Belt, which is more distant in the northern hemisphere, can also explain these differences.

<cit.> analyzed the early spectroscopic observations of optically faint RasTyc sources. This led to the discovery of an over-density of stellar X-ray sources near the Cepheus-Cassiopeia complex. We refer the reader to the reviews on SFRs in the Cassiopeia and Cepheus constellations of <cit.> and <cit.>, respectively. Although this sky area is rich in CO molecular regions <cit.> and dark clouds <cit.>, <cit.> identified four comoving TTSs towards a region devoid of interstellar matter that is denoted as the fourth void in the Cepheus Flare region by <cit.>. Moreover, <cit.> had already reported the discovery of 16 WTTSs in this region. In Paper III, we found four other likely members of this group based on their spectral characteristics, position in the HR diagram, and kinematic properties. The group 38 in <cit.> and <cit.> is composed of seven stars all belonging to the young association analyzed in the present paper and formerly discovered by our group (; Paper II), which already included four of their seven stars; here, we extend the census of this young association.

The main aim of the present work is to identify other young stars surrounding the four comoving TTSs in Cepheus reported in Paper II, and to characterize their physical and kinematic properties, including the WTTSs provided by <cit.>. In Sect. <ref> we detail our procedure to build a sample of “young star candidates”, based on the data available in 2009, when it was created. We also describe our campaign of optical spectroscopic observations. Section <ref> presents our analytical methods and results thereof. In Sect. <ref> we mainly focus the discussion on the properties of the selected sources, on the spatial distribution and kinematics of the young stars belonging to the young association towards the CO Cepheus void, and on its reliability. Finally, we outline our conclusions and perspectives in Sect. <ref>. We present the extraction of spectra with a double Gaussian profile in Appendix <ref>. We also provide further information on multiple systems (Appendix <ref>), low-mass stars (Appendix <ref>), and a few specific targets (Appendix <ref>).




§ SAMPLE AND OBSERVATIONS





 §.§ Sample selection



The greatest difficulty in finding young stars in the field is the selection of a suitable sample of candidates. The best manner for identifying such a population is to excavate into an extensive and comprehensive sample of stellar X-ray sources, such as the RasTyc sample <cit.>. 

To this end, we picked out all counterparts of the X-ray sources by cross-matching the RASS catalog <cit.> with the Two Micron All-Sky Survey catalog <cit.> using a likelihood ratio approach and an original way to estimate the rate of spurious associations <cit.>. We discarded all the matches having an angular separation larger than 15 and a probability of identification less than 0.7. We then correlated the remaining sources with the Guide Star Catalog II <cit.>. We kept all the optical sources at an angular distance not exceeding 5 from 2MASS sources and 15 from RASS ones. 



We proceeded in a similar way for the XMM-Newton X-ray sources of the 2XMMi catalog <cit.>. This turned out to be quite inconclusive because we only selected three stars. However, we note that the source 1RXS 184257 <cit.>, which is a well-known young visual binary, is part of the selection. That makes us confident in the effectiveness of our approach, even for optically faint sources.

We then applied a multivariate analysis on these two X-ray selected datasets. A principal component analysis, which takes measurements errors <cit.> on 19 parameters into account, was used to build up linear combinations of flux ratios from X-ray to near-infrared (NIR) wavelength domain, X-ray hardness ratios, and color indexes. Applying a mean shift procedure on the three first principal components, we were able to disentangle the stellar population from the extragalactic component (galaxies and quasars) that also emits X-rays (Fig. <ref>). We followed the guidelines of <cit.> to identify the local maximum of the population of well-known young stars in this three-dimensional space. We therefore built a reliable learning sample composed of sources whose object type is either “young stellar object”, “T Tau-type star”, or “pre-main-sequence star” in the Simbad database. We finally labeled all the likely stellar X-ray sources located in the latter region as our young star candidates. The objects are distributed all over the sky. 

This work is focused on the identification of young stars towards the CO Cepheus void and its surroundings. Therefore, we selected all the young stars located in a 30-wide region encompassing the four comoving TTSs discovered in Paper II in that region and we then restricted our sample to the population of late-type (B–V > 0.5 mag) and faint (V > 9 mag) stars. Relying on the photometric distance estimate of the group (Paper II), we retain all the candidates within 170 pc of the Sun and with X-ray luminosity L_X⩾10^29 erg s^-1 <cit.>. This X-ray emission threshold picks the majority of 1 Myr-old stars with spectral type G and K <cit.>. The choice of these selection criteria and of this vast sky area allows us i) to look for additional bona fide members both in a restricted region around the Cepheus void and far away (i.e., to search for any runaway WTTSs), and ii) to characterize the population of stellar X-ray sources in an under-researched sky area. The 162 strongest stellar X-ray sources, which are also a priori the youngest stars selected, form our list of prime targets. 

The low-resolution spectroscopic survey by <cit.> includes 14 sources common to our sample, as well as one analyzed in Paper II (i.e., TYC 4500-1478-1). We decided to add the remaining 31 stars from <cit.> to our sample, which leads to a total of 193 candidates. Table <ref> lists their basic data, together with that of the eight young stars reported in Papers II and III (labeled as G1–G4 and F1–F4, respectively). 




 §.§ Photometric and astrometric data



The selection of young star candidates to be observed spectroscopically was performed before the launch of Gaia. At that time, only two of the 193 pre-selected candidates had reliable Hipparcos parallaxes, while 102 sources, which are included in the Tycho catalog <cit.>, had unreliable parallaxes and proper motions with a fair accuracy. We therefore needed multi-band photometric data (from optical to infrared wavelengths) to select the young star candidates with the multivariate analysis described in Sect. <ref>. However, meanwhile, the Gaia DR2 catalog reports very accurate parallaxes and proper motions for nearly all the sources investigated in the present paper, which allows us to study their kinematics and evolutionary status. 

Since we only selected stellar X-ray sources with a 2MASS counterpart, their photometry in the NIR wavelength domain is homogeneous. The J, H, and K_ s magnitudes of the targets are in the range 7–12 mag and have generally a high level of accuracy (in more than 96 % of cases). For seven sources, at least one of NIR magnitudes is an upper limit or a poor-quality value in the final release of 2MASS data.

We encountered difficulties with the homogenization of photometry in optical bands. Indeed, when we started our target selection, no catalog provided Johnson B and V magnitudes up to V=14.5 mag. The completeness of the Tycho-2 catalog <cit.> is to about 90 % for sources brighter than V ∼11.5 mag, although it also contains fainter stars. For the non-Tycho sources fainter than V=12 mag, only the photographic magnitudes were available and reliable. For the 102 sources with an entry in the Tycho-2 catalog, the V_T magnitude ranges from 9 to 13 mag (Fig. <ref>). We converted the B_T and V_T magnitudes into Johnson B and V magnitudes following the transformation given in the introduction of the Tycho-2 catalog: B = B_T - 0.24 (B_T - V_T) and V = V_T - 0.09 (B_T - V_T). 

For 79 of the remaining sources with both B_J and R_F photographic magnitudes in the USNO-B1.0 catalog <cit.>, we estimated the V magnitude using the formula proposed by <cit.>: V=B_J - 0.46 (B_J - R_F). We used the B_J and R_F magnitudes extracted from the second Palomar Observatory Sky Survey (POSS) scans in the IIIa-J and IIIa-F passbands, respectively. All these sources are fainter than V=11 mag. Additional magnitudes in the Johnson B band were retrieved either from the GSC II catalog or from the unpublished Yellow-Blue 6 catalog (YB6 – USNO). The latter is available through the NOMAD catalog <cit.>. 

In Table <ref>, we mainly list the B and V magnitudes in the Johnson-Cousins system (∼88 % and ∼94 % of sources). If one of these values are not available, we substitute them by the B_J or V photographic passbands taken from GSC II (Fig. <ref>). 



lllllccrcrcrrrcc
Main parameters of the young stars candidates available in 2009, when the sample was created.



1c#     1cX-ray name     1cIR name     GSC II  name     Other name     α (2000)      δ (2000)     1cB     Ref.     1cV     Ref.      1cJ     1cH     1cK_ s     B–V ^a     V–J ^b 

    1c1RXS     1c2MASS               (h m s)     ()     (mag)          (mag)         (mag)     (mag)     (mag)     (mag)     (mag) 



Continued. 


1c#     1cX-ray name     1cIR name     GSC II  name     Other name     α (2000)      δ (2000)     1cB     Ref.     1cV     Ref.      1cJ     1cH     1cK_ s     B–V ^a     V–J ^b  

    1c1RXS     1c2MASS               (h m s)     ()     (mag)          (mag)         (mag)     (mag)     (mag)     (mag)     (mag) 





    15lStars cross-identified with a source of the RASS catalogs:



1		   	J000221.0+552519	   	J00022092+5525145	   	NAHS000445	   		   	00 02 20.929	   	+55 25 14.55	   	13.58	   	G_J	   	12.64	   	G_V	   	9.828	   	9.056	   	8.859	   	(0.94)	   	(2.81)	

2	^	   	J000806.3+475659	   	J00080642+4757025	   	NAH9000368	   		   	00 08 06.428	   	+47 57 02.50	   	14.53	   	G_B	   	12.69	   	U	   	8.523	   	8.000	   	7.677	   	1.84	   	4.17	

3	^	   	J002158.0+491245	   	J00215781+4912379	   	NAH1000233	   	GJ 3030	   	00 21 57.815	   	+49 12 37.96	   	13.43	   	G_J	   	12.75	   	U	   	9.139	   	8.454	   	8.205	   	(1.14)	   	3.61	

4	 ^∗, ^⋆	   	J002827.8+785750	   	J00282798+7857426	   	NAG0000520	   	TYC 4500-730-1	   	00 28 27.987	   	+78 57 42.70	   	11.20	   	T	   	10.61	   	T	   	9.251	   	8.916	   	8.868	   	0.59	   	1.36	

5		   	J002854.1+502226	   	J00285391+5022330	   	NAIJ018308	   	GJ 3036	   	00 28 53.920	   	+50 22 33.02	   	14.09	   	G_J	   	13.16	   	U	   	8.847	   	8.289	   	7.991	   	[0.93]	   	4.32	

6	 ^∗, ^⋆, ^	   	J003904.2+791912 [This source is the companion to TYC 4500-1549-1, which turns out to be the brighter component of a visual binary reported by <cit.>. See Appendix <ref> for details.]	   	J00390355+7919191	   	NAG3000177	   		   	00 39 03.554	   	+79 19 19.11	   	14.66	   	G_J	   	13.46	   	G_V	   	10.479	   	9.837	   	9.627	   	(1.20)	   	(2.98)	

7	 ^∗, ^	   	J005300.8+682125	   	J00530041+6821225	   	NAZ0000392	   	GSC 04296-00542	   	00 53 00.419	   	+68 21 22.52	   	12.80	   	G_J	   	12.01	   	G_V	   	10.088	   	9.468	   	9.367	   	(0.79)	   	(1.92)	

8		   	J010112.8+570839	   	J01011345+5708444	   	NANY000113	   		   	01 01 13.458	   	+57 08 44.43	   	15.84	   	G_B	   	14.58	   	U	   	10.050	   	9.135	   	8.818	   	1.26	   	4.53	

9		   	J011319.6+585523	   	J01131976+5855224	   	NANP000198	   	NLTT 4027	   	01 13 19.767	   	+58 55 22.42	   	12.73	   	G_J	   	11.58	   	U	   	8.409	   	7.770	   	7.570	   	(1.46)	   	3.17	

10	^	   	J011415.5+715933	   	J01141803+7159271	   	NAD4000574	   	TYC 4305-1502-1	   	01 14 18.033	   	+71 59 27.12	   	12.15	   	T	   	11.43	   	T	   	10.132	   	9.611	   	9.484	   	0.73	   	1.30	

11	^	   	J011523.1+882923	   	J01153189+8829200	   	NA9T000196	   		   	01 15 31.890	   	+88 29 20.04	   	13.53	   	G_J	   	12.50	   	U	   	9.733	   	9.069	   	8.877	   	[1.03]	   	2.77	

12		   	J011740.0+582954	   	J01173999+5829508	   	NANP000382	   		   	01 17 39.996	   	+58 29 50.90	   	13.73	   	G_B	   	12.51	   	U	   	9.399	   	8.773	   	8.528	   	1.22	   	3.11	

13	 ^∗, ^	   	J012927.4+744448	   	J01292907+7444495	   	NACY000071	   	GSC 04309-00722	   	01 29 29.074	   	+74 44 49.51	   	14.01	   	G_J	   	13.40	   	U	   	10.641	   	10.066	   	9.925	   	(1.23)	   	2.76	

14		   	J013426.8+642651	   	J01342688+6426505	   	NAZ6000334	   		   	01 34 26.886	   	+64 26 50.54	   	14.55	   	G_J	   	12.38	   	G_V	   	9.301	   	8.772	   	8.517	   	(2.17)	   	(3.08)	

15		   	J015949.7+532301	   	J01595005+5323080	   	NBYW000158	   		   	01 59 50.055	   	+53 23 08.04	   	14.78	   	G_B	   	14.01	   	U	   	10.083	   	9.383	   	9.226	   	0.77	   	3.93	

16		   	J020434.1+675635	   	J02043300+6756308	   	NAZ8000167	   		   	02 04 33.006	   	+67 56 30.88	   	13.66	   	G_B	   	12.71	   	U	   	10.579	   	10.091	   	10.003	   	0.85	   	2.13	

17	 ^∗	   	J022036.3+774419	   	J02203711+7744132	   	NAGK000428	   	GSC 04499-02076	   	02 20 37.113	   	+77 44 13.20	   	13.98	   	G_B	   	12.60	   	U	   	9.619	   	8.969	   	8.811	   	1.38	   	2.98	

18	^	   	J023919.7+872828	   	J02391539+8728237	   	NAA7000100	   		   	02 39 15.392	   	+87 28 23.73	   	13.78	   	G_B	   	12.89	   	U	   	10.642	   	10.012	   	9.813	   	0.89	   	2.25	

19	^	   	J024324.6+695320	   	J02433138+6953362	   	NB0N000191	   	TYC 4316-2055-1	   	02 43 31.385	   	+69 53 36.22	   	11.83	   	T	   	11.08	   	T	   	9.716	   	9.285	   	9.249	   	0.75	   	1.36	

20	^	   	J025538.5+544706	   	J02553878+5447121	   	NAIO000292	   		   	02 55 38.782	   	+54 47 12.12	   	13.91	   	Y	   	13.08	   	Y	   	10.405	   	9.700	   	9.454	   	(0.83)	   	3.61	

21		   	J025620.0+614129	   	J02561984+6141223	   	NAWU000406	   	GSC 04048-00621	   	02 56 19.846	   	+61 41 22.37	   	14.89	   	G_B	   	14.04	   	U	   	9.741	   	9.170	   	8.927	   	0.85	   	4.30	

22		   	J030016.2+722537	   	J03001477+7225410	   	NB0J000073	   	TYC 4321-507-1	   	03 00 14.779	   	+72 25 41.02	   	11.32	   	T	   	10.71	   	T	   	8.872	   	8.358	   	8.287	   	0.61	   	1.84	

23	^	   	J030926.6+673238	   	J03092643+6732425	   	NB27000316	   		   	03 09 26.435	   	+67 32 42.51	   	15.03	   	G_B	   	13.00	   	U	   	9.572	   	8.986	   	8.767	   	2.03	   	3.43	

24		   	J031026.1+582608	   	J03102649+5826086	   	NAVB000247	   	GJ 3204 	   	03 10 26.490	   	+58 26 08.66	   	12.83	   	G_J	   	12.08	   	U	   	8.332	   	7.742	   	7.503	   	(1.27)	   	3.75	

25	^	   	J032802.3+642341	   	J03280189+6423409	   	NB1L000603	   		   	03 28 01.891	   	+64 23 41.00	   	13.30	   	G_B	   	12.19	   	U	   	9.753	   	9.259	   	9.054	   	1.11	   	2.44	

26		   	J034458.8+634439	   	J03445843+6344327	   	NB1E000050	   		   	03 44 58.433	   	+63 44 32.71	   	14.21	   	G_B	   	13.33	   	U	   	9.658	   	9.015	   	8.786	   	0.88	   	3.67	

27		   	J034857.2+785910	   	J03485943+7859114	   	NAGP000513	   		   	03 48 59.436	   	+78 59 11.44	   	13.49	   	G_B	   	12.97	   	U	   	10.196	   	9.689	   	9.508	   	0.52	   	2.78	

28	^	   	J040745.1+875030	   	J04073943+8750250	   	NAA5000047	   	BD+87 28	   	04 07 39.437	   	+87 50 25.00	   	11.51	   	T	   	10.72	   	T	   	9.253	   	8.865	   	8.762	   	0.79	   	1.47	

29		   	J041128.6+754422	   	J04112810+7544231	   	NAEJ000542	   		   	04 11 28.109	   	+75 44 23.17	   	13.72	   	G_B	   	12.60	   	U	   	9.464	   	8.804	   	8.608	   	1.12	   	3.13	

30		   	J041244.9+612123	   	J04124477+6121201	   	NASI000025	   		   	04 12 44.771	   	+61 21 20.17	   	15.94	   	G_B	   	14.37	   	U	   	9.995	   	9.417	   	9.183	   	1.57	   	4.37	

31		   	J041641.4+613848	   	J04164046+6138443	   	NATF000004	   		   	04 16 40.465	   	+61 38 44.39	   	14.69	   	G_B	   	13.62	   	U	   	10.615	   	10.02	   	9.827	   	1.07	   	3.00	

32	^	   	J043208.0+811627	   	J04321010+8116139	   	NAFQ000210	   	TYC 4522-713-1	   	04 32 10.108	   	+81 16 13.91	   	12.25	   	T	   	11.14	   	T	   	9.140	   	8.564	   	8.414	   	1.11	   	2.00	

33	^	   	J044912.7+773719	   	J04491531+7737122	   	NADY000313	   	TYC 4515-156-1	   	04 49 15.318	   	+77 37 12.23	   	11.72	   	T	   	10.92	   	T	   	9.520	   	9.148	   	9.030	   	0.81	   	1.40	

34		   	J045741.8+683548	   	J04574103+6835478	   	NAX6000074	   		   	04 57 41.031	   	+68 35 47.88	   	13.55	   	G_B	   	12.61	   	U	   	9.227	   	8.574	   	8.412	   	0.98	   	3.39	

35		   	J045808.2+790813	   	J04580667+7908072	   	NAFX000397	   		   	04 58 06.670	   	+79 08 07.30	   	14.15	   	G_J	   	12.88	   	U	   	9.657	   	9.000	   	8.830	   	(1.66)	   	3.22	

36		   	J050248.7+735215	   	J05024924+7352143	   	NAF0000068	   		   	05 02 49.245	   	+73 52 14.34	   	13.35	   	G_B	   	11.89	   	U	   	9.348	   	8.726	   	8.550	   	1.46	   	2.54	

37	^	   	J050642.4+745604	   	J05063831+7456010	   	NAF1000019	   	TYC 4354-433-1	   	05 06 38.314	   	+74 56 01.08	   	11.44	   	T	   	10.80	   	T	   	9.416	   	9.127	   	9.048	   	0.64	   	1.38	

38	^	   	J053459.0+652146	   	J05345873+6521435	   	NAQ7000082	   	StKM 1-570	   	05 34 58.736	   	+65 21 43.53	   	12.70	   	G_J	   	11.55	   	U	   	8.709	   	8.037	   	7.841	   	(1.42)	   	2.84	

39		   	J061330.8+820121	   	J06133128+8201270	   	N74P000117	   		   	06 13 31.287	   	+82 01 27.04	   	16.12	   	G_B	   	14.57	   	U	   	10.090	   	9.507	   	9.258	   	1.55	   	4.48	

40	^	   	J061946.4+771933	   	J06194548+7719330	   	N76R000372	   		   	06 19 45.489	   	+77 19 33.04	   	13.47	   	G_B	   	12.71	   	U	   	(10.245)	   	9.651	   	9.523	   	0.76	   	(2.46)	

41	^	   	J062558.2+822124	   	J06260175+8221277	   	N74T000027	   	BD+82 160	   	06 26 01.753	   	+82 21 27.76	   	11.51	   	T	   	10.78	   	T	   	9.277	   	8.874	   	8.771	   	0.73	   	1.50	

42		   	J063405.9+770040	   	J06340499+7700395	   	N773000344	   	TYC 4529-1687-1	   	06 34 04.991	   	+77 00 39.52	   	11.05	   	T	   	10.45	   	T	   	9.179	   	8.831	   	8.756	   	0.61	   	1.27	

43	^	   	J064241.4+880442	   	J06423375+8804441	   	N741000014	   	BD+88 28	   	06 42 33.754	   	+88 04 44.16	   	11.53	   	T	   	10.83	   	T	   	9.560	   	9.188	   	9.106	   	0.70	   	1.27	

44		   	J070350.7+831346	   	J07035520+8313387	   	N74Q000405	   	BD+83 171p	   	07 03 55.208	   	+83 13 38.78	   	11.39	   	T	   	10.79	   	T	   	9.510	   	9.249	   	9.150	   	0.60	   	1.28	

45		   	J071537.9+764648	   	J07153237+7647084	   	N76Z000045	   	TYC 4526-474-1	   	07 15 32.373	   	+76 47 08.40	   	11.26	   	T	   	10.65	   	T	   	9.594	   	9.318	   	9.216	   	0.61	   	1.06	

46	^	   	J071743.1+764416	   	J07174240+7644203	   	N76W000013	   	TYC 4526-646-1	   	07 17 42.401	   	+76 44 20.39	   	11.96	   	T	   	11.19	   	T	   	9.477	   	9.017	   	8.907	   	0.78	   	1.71	

47	^	   	J075427.0+780633	   	J07543054+7806452	   	N7AC000093	   	NR Cam	   	07 54 30.541	   	+78 06 45.23	   	11.74	   	T	   	10.98	   	T	   	9.399	   	8.954	   	8.870	   	0.76	   	1.58	

48		   	J075556.7+832310	   	J07555396+8323049	   	N74L003701	   	GJ 1101	   	07 55 53.968	   	+83 23 04.99	   	14.36	   	G_J	   	13.52	   	U	   	8.744	   	8.144	   	7.912	   	[0.84]	   	4.77	

49	^	   	J083407.4+791449	   	J08340581+7914458	   	N7B2000444	   	TYC 4543-837-1	   	08 34 05.814	   	+79 14 45.86	   	11.50	   	T	   	10.69	   	T	   	9.079	   	8.640	   	8.513	   	0.81	   	1.61	

50	^	   	J085353.7+870708	   	J08535198+8707127	   	N74F000137	   	BD+87 64	   	08 53 51.989	   	+87 07 12.72	   	11.61	   	T	   	10.99	   	T	   	9.129	   	8.766	   	8.619	   	0.63	   	1.86	

51		   	J092654.8+812751	   	J09265323+8127469	   	N79W000299	   		   	09 26 53.231	   	+81 27 46.90	   	13.36	   	G_B	   	12.30	   	U	   	9.616	   	8.943	   	8.826	   	1.06	   	2.68	

52		   	J093852.0+852625	   	J09385059+8526172	   	N75H000195	   	BD+86 136	   	09 38 50.597	   	+85 26 17.22	   	11.32	   	T	   	10.75	   	T	   	9.502	   	9.109	   	9.041	   	0.57	   	1.25	

53		   	J102225.9+752828	   	J10222618+7528312	   	N78Q000124	   	TYC 4542-1861-1	   	10 22 26.188	   	+75 28 31.29	   	11.95	   	T	   	11.18	   	T	   	9.443	   	8.931	   	8.815	   	0.76	   	1.74	

54		   	J112114.0+824715	   	J11211194+8247172	   	N752000249	   	FBS 1117-830	   	11 21 11.945	   	+82 47 17.22	   	16.04	   	G_B	   	14.03	   	U	   	10.263	   	9.645	   	9.418	   	2.01	   	3.77	

55	^	   	J113533.7+825920	   	J11353465+8259217	   	N753000234	   	TYC 4632-1171-1	   	11 35 34.655	   	+82 59 21.71	   	11.91	   	T	   	11.15	   	T	   	(8.939)	   	8.280	   	8.091	   	0.76	   	(2.21)	

56	^	   	J123048.8+832257	   	J12303982+8323081	   	N3YZ000121	   	TYC 4633-1518-1	   	12 30 39.826	   	+83 23 08.18	   	12.39	   	T	   	11.70	   	T	   	10.604	   	10.256	   	10.184	   	0.69	   	1.10	

57	^	   	J123205.6+841719	   	J12320278+8417191	   	N3YW000031	   		   	12 32 02.788	   	+84 17 19.14	   	13.31	   	G_B	   	12.35	   	U	   	9.975	   	9.319	   	9.162	   	0.96	   	2.38	

58		   	J125912.7+743529	   	J12591320+7435207	   	N41R000077	   	TYC 4407-145-1	   	12 59 13.208	   	+74 35 20.77	   	11.34	   	T	   	10.78	   	T	   	9.475	   	9.127	   	9.035	   	0.56	   	1.31	

59		   	J130433.9+882441	   	J13033881+8824072	   	N3Y9000244	   	TYC 4645-293-1	   	13 03 38.815	   	+88 24 07.23	   	12.11	   	T	   	11.48	   	T	   	10.501	   	10.268	   	10.197	   	0.64	   	0.98	

60		   	J134050.7+792553	   	J13405128+7925550	   	N44S000296	   		   	13 40 51.282	   	+79 25 55.01	   	12.83	   	G_B	   	11.88	   	U	   	9.519	   	8.919	   	8.776	   	0.95	   	2.36	

61		   	J135117.4+770307	   	J13511765+7703008	   	N40K000009	   		   	13 51 17.653	   	+77 03 00.81	   	14.54	   	G_B	   	13.43	   	U	   	10.287	   	9.653	   	9.496	   	1.11	   	3.14	

62		   	J135337.0+773708	   	J13533877+7737083	   	N450000288	   	NLTT 35712 ? 	   	13 53 38.772	   	+77 37 08.30	   	14.14	   	G_J	   	13.40	   	U	   	8.635	   	8.056	   	7.795	   	(1.42)	   	4.76	

63		   	J141447.2+680442	   	J14144719+6804420	   	N4PK000120	   	TYC 4403-57-1	   	14 14 47.196	   	+68 04 42.05	   	11.42	   	T	   	10.83	   	T	   	9.404	   	9.146	   	9.072	   	0.58	   	1.43	

64		   	J143642.7+613935	   	J14363900+6139519	   	N4KS000228	   		   	14 36 39.010	   	+61 39 51.93	   	12.82	   	G_B	   	12.19	   	U	   	9.882	   	9.388	   	9.250	   	0.63	   	2.31	

65		   	J145154.8+604616	   	J14515684+6046205	   	N4LA000311	   	TYC 4180-1135-1	   	14 51 56.842	   	+60 46 20.60	   	11.79	   	T	   	11.16	   	T	   	9.717	   	9.315	   	9.199	   	0.63	   	1.44	

66	^	   	J145228.8+714026	   	J14523175+7140132	   	N4OX000133	   	TYC 4413-1113-1	   	14 52 31.757	   	+71 40 13.20	   	11.81	   	T	   	11.22	   	T	   	9.720	   	9.381	   	9.274	   	0.60	   	1.50	

67		   	J150043.3+682234	   	J15004194+6822327	   	N4QK000131	   	TYC 4411-1400-1	   	15 00 41.946	   	+68 22 32.75	   	12.60	   	T	   	11.77	   	T	   	10.214	   	9.730	   	9.627	   	0.84	   	1.56	

68		   	J154457.5+793054	   	J15445657+7931016	   	N455000017	   	TYC 4563-1484-1	   	15 44 56.576	   	+79 31 01.63	   	11.87	   	T	   	11.26	   	T	   	10.007	   	9.546	   	9.438	   	0.62	   	1.25	

69	^	   	J154522.2+751500	   	J15452354+7514548	   	N431000294	   		   	15 45 23.546	   	+75 14 54.84	   	14.71	   	G_B	   	13.32	   	U	   	9.725	   	9.142	   	8.897	   	1.39	   	3.60	

70		   	J155547.5+684014	   	J15554725+6840138	   	N4MO000164	   		   	15 55 47.250	   	+68 40 13.86	   	13.70	   	G_B	   	11.94	   	U	   	8.593	   	7.962	   	7.752	   	1.76	   	3.35	

71		   	J160438.3+702212	   	J16043736+7022142	   	N4LX003834	   		   	16 04 37.363	   	+70 22 14.26	   	12.34	   	G_J	   	11.30	   	U	   	8.793	   	8.180	   	8.002	   	[1.04]	   	2.51	

72		   	J160820.6+700353	   	J16081945+7003468	   	N4MQ000416	   	TYC 4422-1970-1	   	16 08 19.455	   	+70 03 46.84	   	11.63	   	T	   	10.96	   	T	   	9.548	   	9.116	   	9.010	   	0.67	   	1.41	

73		   	J161939.9+765515	   	J16193872+7655165	   	N434000404	   		   	16 19 38.730	   	+76 55 16.58	   	13.82	   	G_B	   	12.59	   	U	   	9.357	   	8.719	   	8.511	   	1.23	   	3.24	

74		   	J162708.9+662620	   	J16270823+6626144	   	N4MK000366	   	TYC 4196-1624-1	   	16 27 08.233	   	+66 26 14.42	   	12.32	   	T	   	11.42	   	T	   	10.107	   	9.705	   	9.618	   	0.89	   	1.31	

75		   	J162939.7+620505	   	J16293983+6205131	   	N4HU000060	   	BD+62 1487	   	16 29 39.838	   	+62 05 13.14	   	11.53	   	T	   	10.84	   	T	   	8.906	   	8.454	   	8.310	   	0.69	   	1.93	

76	^	   	J163747.2+723937	   	J16374587+7239423	   	N42S000309	   	TYC 4426-221-1	   	16 37 45.880	   	+72 39 42.39	   	12.05	   	T	   	11.34	   	T	   	10.176	   	9.787	   	9.650	   	0.72	   	1.16	

77		   	J165315.4+701554	   	J16531433+7015596	   	N4LJ000266	   	TYC 4423-1336-1	   	16 53 14.334	   	+70 15 59.68	   	11.42	   	T	   	10.74	   	T	   	9.338	   	8.898	   	8.754	   	0.68	   	1.40	

78	^	   	J170526.8+743600	   	J17052388+7436042	   	N43J000280	   	TYC 4427-715-1	   	17 05 23.886	   	+74 36 04.28	   	11.61	   	T	   	10.93	   	T	   	9.713	   	9.357	   	9.285	   	0.68	   	1.22	

79	^	   	J171928.8+652227	   	J17192868+6522298	   	N4EF000088	   	TYC 4206-459-1	   	17 19 28.682	   	+65 22 29.81	   	12.15	   	T	   	11.40	   	T	   	10.034	   	9.602	   	9.516	   	0.75	   	1.37	

80		   	J173451.2+784419	   	J17345173+7844186	   	N440000010	   		   	17 34 51.734	   	+78 44 18.66	   	14.25	   	G_B	   	12.90	   	U	   	9.495	   	8.773	   	8.621	   	1.35	   	3.41	

81	^	   	J174104.6+842458	   	J17410836+8424552	   	N3ZO000437	   		   	17 41 08.370	   	+84 24 55.29	   	14.65	   	G_B	   	13.09	   	U	   	(10.386)	   	(9.859)	   	(9.466)	   	1.56	   	(2.71)	

82		   	J175140.9+730509	   	J17514141+7305112	   	N43C000018	   	TYC  4436-501-1	   	17 51 41.415	   	+73 05 11.24	   	11.41	   	T	   	10.84	   	T	   	9.736	   	9.419	   	9.340	   	0.57	   	1.10	

83		   	J175614.1+680707	   	J17561374+6807116	   	N41S000411	   		   	17 56 13.748	   	+68 07 11.65	   	13.77	   	G_B	   	13.19	   	U	   	10.481	   	9.888	   	9.775	   	0.58	   	2.71	

84	^	   	J175910.1+584300	   	J17591035+5842594	   	N4F5000235	   	TYC  3914-118-1	   	17 59 10.359	   	+58 42 59.49	   	11.63	   	T	   	11.01	   	T	   	9.465	   	9.073	   	8.981	   	0.63	   	1.55	

85		   	J180643.4+682200	   	J18064367+6822031	   	N0U8000324	   		   	18 06 43.679	   	+68 22 03.19	   	14.38	   	G_J	   	12.85	   	G_V	   	9.685	   	9.064	   	8.845	   	(1.47)	   	(3.17)	

86		   	J181048.9+701601	   	J18104997+7016100	   	N0UL000431	   	TYC 4433-597-1	   	18 10 49.975	   	+70 16 10.07	   	11.28	   	T	   	10.63	   	T	   	9.183	   	8.810	   	8.679	   	0.65	   	1.45	

87	^	   	J181610.9+585539	   	J18161159+5855420	   	N13Y000374	   	TYC 3916-1907-1	   	18 16 11.596	   	+58 55 42.10	   	11.24	   	T	   	10.57	   	T	   	8.945	   	8.498	   	8.383	   	0.67	   	1.63	

88		   	J183552.8+800536	   	J18355181+8005394	   	N0YQ000010	   	GJ 4068	   	18 35 51.818	   	+80 05 39.48	   	14.36	   	G_J	   	13.27	   	U	   	8.989	   	8.419	   	8.163	   	(1.32)	   	4.28	

89	^	   	J183627.4+715311	   	J18362702+7153157	   	N0UK000328	   	TYC 4438-627-1	   	18 36 27.025	   	+71 53 15.76	   	11.82	   	T	   	11.14	   	T	   	9.644	   	9.256	   	9.149	   	0.68	   	1.50	

90		   	J183810.6+682424	   	J18381041+6824221	   	N1HR000382	   		   	18 38 10.414	   	+68 24 22.14	   	14.99	   	G_B	   	14.41	   	U	   	11.847	   	11.285	   	11.144	   	0.58	   	2.56	

91	^	   	J184830.1+642330	   	J18482942+6423281	   	N14N000211	   	TYC 4223-399-1	   	18 48 29.427	   	+64 23 28.12	   	12.25	   	T	   	11.31	   	T	   	9.094	   	8.557	   	8.447	   	0.94	   	2.22	

92	^	   	J185131.1+584258	   	J18513099+5842579	   	N16J000101	   	TYC 3930-1709-1	   	18 51 30.991	   	+58 42 57.98	   	11.76	   	T	   	10.98	   	T	   	9.442	   	9.079	   	8.984	   	0.78	   	1.54	

93		   	J190445.7+700628	   	J19044518+7006293	   	N1HM000270	   	TYC 4435-516-1	   	19 04 45.189	   	+70 06 29.33	   	11.79	   	T	   	11.18	   	T	   	10.02	   	9.673	   	9.584	   	0.61	   	1.16	

94		   	J190921.0+562658	   	J19092137+5626548	   	N16E000589	   	TYC 3928-1195-1	   	19 09 21.372	   	+56 26 54.87	   	11.23	   	T	   	10.65	   	T	   	9.627	   	9.292	   	9.219	   	0.58	   	1.02	

95		   	J191412.4+615122	   	J19141236+6151223	   	N149000119	   		   	19 14 12.369	   	+61 51 22.39	   	14.21	   	G_B	   	12.94	   	U	   	10.701	   	10.097	   	9.932	   	1.28	   	2.24	

96		   	J191519.4+660830	   	J19151619+6608517	   	N1I0000495	   	TYC 4229-1836-1	   	19 15 16.198	   	+66 08 51.77	   	11.25	   	T	   	10.69	   	T	   	9.652	   	9.337	   	9.274	   	0.56	   	1.04	

97		   	J192104.3+561940	   	J19210447+5619420	   	N15Z000573	   	TYC 3929-1500-1	   	19 21 04.470	   	+56 19 42.09	   	11.45	   	T	   	10.85	   	T	   	9.692	   	9.402	   	9.346	   	0.60	   	1.16	

98		   	J192127.4+611208	   	J19212759+6112042	   	N15A000164	   		   	19 21 27.599	   	+61 12 04.27	   	13.26	   	G_B	   	12.45	   	U	   	10.39	   	9.901	   	9.739	   	0.81	   	2.06	

99		   	J192215.6+673918[The X-ray emission seems to be produced from the galaxy 2MASX 19221485+6739143. See Appendix <ref> for details.]	   	J19221289+6739053	   	N1IX000468	   	TYC 4444-1831-1	   	19 22 12.897	   	+67 39 05.34	   	12.37	   	T	   	11.67	   	T	   	9.510	   	8.924	   	8.825	   	0.70	   	2.16	

100	^	   	J193003.3+663021	   	J19300213+6630231	   	N1I2000502	   	HD 184481	   	19 30 02.135	   	+66 30 23.16	   	9.78	   	T	   	9.25	   	T	   	8.118	   	7.845	   	7.803	   	0.52	   	1.13	

101		   	J193026.5+580427	   	J19302663+5804352	   	N154000033	   	TYC 3929-592-1	   	19 30 26.637	   	+58 04 35.21	   	11.53	   	T	   	10.55	   	T	   	8.393	   	7.903	   	7.696	   	0.98	   	2.16	

102	^	   	J193124.1+672401	   	J19312400+6723567	   	N1IX000266	   	TYC  4242-151-1	   	19 31 24.007	   	+67 23 56.76	   	13.09	   	T	   	12.77	   	T	   	(10.367)	   	10.052	   	(9.827)	   	0.32	   	(2.40)	

103	^	   	J193141.7+641951	   	J19314063+6419520	   	N1HU000422	   	TYC 4238-1049-1	   	19 31 40.632	   	+64 19 52.02	   	11.01	   	T	   	10.37	   	T	   	8.831	   	8.434	   	8.349	   	0.63	   	1.54	

104		   	J193231.8+565905	   	J19323041+5659071	   	N12G000059	   	TYC 3929-1760-1	   	19 32 30.418	   	+56 59 07.20	   	12.29	   	T	   	11.62	   	T	   	9.295	   	8.765	   	8.630	   	0.67	   	2.33	

105	^	   	J193958.2+851032	   	J19400095+8510230	   	N0U3000120	   	TYC 4652-781-1	   	19 40 00.952	   	+85 10 23.03	   	12.24	   	T	   	11.44	   	T	   	10.009	   	9.542	   	9.460	   	0.80	   	1.43	

106		   	J194206.0+654655	   	J19420596+6546497	   	N1I7007118	   	TYC 4242-1123-1	   	19 42 05.966	   	+65 46 49.75	   	11.50	   	T	   	10.81	   	T	   	9.540	   	9.157	   	9.053	   	0.69	   	1.27	

107		   	J194616.6+701413	   	J19461559+7014135	   	N1J2000362	   		   	19 46 15.595	   	+70 14 13.58	   	14.71	   	G_B	   	13.22	   	U	   	10.224	   	9.585	   	9.402	   	1.49	   	2.99	

108		   	J195139.1+710122	   	J19513766+7101255	   	N1ID000252	   		   	19 51 37.660	   	+71 01 25.53	   	13.87	   	G_B	   	12.74	   	U	   	10.128	   	9.570	   	9.416	   	1.13	   	2.61	

109	^	   	J195542.3+663207	   	J19554228+6632051	   	N1HY000096	   	TYC 4243-473-1	   	19 55 42.283	   	+66 32 05.19	   	13.08	   	T	   	11.79	   	T	   	9.248	   	8.666	   	8.453	   	1.28	   	2.54	

110	^	   	J195758.2+664253	   	J19575836+6642514	   	N1HY000042	   	TYC 4243-597-1	   	19 57 58.365	   	+66 42 51.46	   	11.14	   	T	   	10.22	   	T	   	8.806	   	8.402	   	8.281	   	0.92	   	1.41	

111		   	J200110.8+743025	   	J20011185+7430305	   	N0V3000572	   		   	20 01 11.856	   	+74 30 30.57	   	15.61	   	G_B	   	14.08	   	U	   	10.821	   	10.145	   	9.957	   	1.53	   	3.26	

112		   	J200245.4+592015	   	J20024462+5920162	   	N124000775	   	TYC 3948-1516-1	   	20 02 44.627	   	+59 20 16.27	   	11.57	   	T	   	10.69	   	T	   	8.792	   	8.312	   	8.185	   	0.88	   	1.90	

113		   	J200348.4+642542	   	J20034781+6425471	   	N1JN000198	   	TYC 4240-978-1	   	20 03 47.812	   	+64 25 47.12	   	12.49	   	T	   	11.29	   	T	   	8.267	   	7.659	   	7.486	   	1.20	   	3.02	

114	 ^∗	   	J201424.6+660521	   	J20142610+6605199	   	N1JT000259	   	TYC 4244-322-1	   	20 14 26.110	   	+66 05 19.95	   	12.25	   	T	   	11.58	   	T	   	9.688	   	9.150	   	9.033	   	0.67	   	1.89	

115	 ^∗	   	J202513.8+733638	   	J20251540+7336332	   	N0UQ000374	   	TYC 4459-83-1	   	20 25 15.402	   	+73 36 33.26	   	11.51	   	T	   	10.69	   	T	   	9.128	   	8.731	   	8.639	   	0.82	   	1.56	

116		   	J203549.9+594930	   	J20354953+5949379	   	N1F8000090	   		   	20 35 49.539	   	+59 49 37.95	   	13.75	   	G_B	   	12.37	   	U	   	9.883	   	9.386	   	9.249	   	1.38	   	2.48	

117		   	J203638.5+553811	   	J20363836+5538141	   	N11P000076	   		   	20 36 38.364	   	+55 38 14.14	   	13.59	   	G_J	   	12.28	   	G_V	   	9.978	   	9.362	   	9.177	   	(1.31)	   	(2.30)	

118	 ^∗	   	J203813.1+692413	   	J20381376+6924127	   	N1JB000834	   	GSC 04451-00172	   	20 38 13.769	   	+69 24 12.78	   	14.11	   	G_B	   	13.42	   	U	   	10.559	   	9.907	   	9.757	   	0.69	   	2.86	

119	^	   	J203857.5+580452	   	J20385772+5804567	   	N1E1000002	   		   	20 38 57.728	   	+58 04 56.74	   	15.04	   	G_B	   	14.22	   	U	   	11.424	   	10.914	   	10.79	   	0.82	   	2.80	

120	^	   	J203903.6+640707	   	J20390451+6407067	   	N1JQ000885	   	TYC 4254-18-1	   	20 39 04.512	   	+64 07 06.79	   	10.46	   	T	   	9.96	   	T	   	8.713	   	8.356	   	(8.508)	   	0.51	   	1.25	

121		   	J205405.4+601811	   	J20540505+6018041	   	N1FG000257	   		   	20 54 05.054	   	+60 18 04.14	   	15.86	   	G_B	   	13.71	   	G_V	   	10.098	   	9.450	   	9.256	   	(2.15)	   	5.22	

122	 ^∗	   	J210419.0+750359	   	J21042093+7504049	   	N0XV000343	   	TYC 4586-348-1	   	21 04 20.936	   	+75 04 04.97	   	11.81	   	T	   	11.15	   	T	   	9.804	   	9.404	   	9.325	   	0.66	   	1.35	

123	^	   	J210444.0+522326	   	J21044434+5223256	   	N30J000168	   	GSC 03600-00513	   	21 04 44.340	   	+52 23 25.63	   	12.12	   	G_B	   	11.47	   	U	   	10.297	   	9.972	   	9.885	   	0.65	   	1.17	

124	^	   	J210751.6+690923	   	J21075194+6909234	   	N1JE000111	   		   	21 07 51.942	   	+69 09 23.46	   	14.84	   	G_B	   	14.27	   	U	   	11.343	   	10.649	   	10.499	   	0.57	   	2.92	

125	^	   	J211000.9+603644	   	J21100200+6036455	   	N1FD000400	   	TYC 4248-1247-1	   	21 10 02.006	   	+60 36 45.55	   	12.56	   	T	   	11.81	   	T	   	10.409	   	10.08	   	9.976	   	0.75	   	1.40	

126	 ^∗	   	J211024.8+704600	   	J21102448+7045575	   	N1JH007278	   	TYC 4464-1372-1	   	21 10 24.483	   	+70 45 57.60	   	11.77	   	T	   	10.95	   	T	   	9.396	   	8.987	   	8.899	   	0.82	   	1.55	

127		   	J211114.9+614436	   	J21111668+6144388	   	N1F6000070	   	TYC 4248-411-1	   	21 11 16.685	   	+61 44 38.81	   	12.49	   	T	   	11.71	   	T	   	10.124	   	9.720	   	9.629	   	0.78	   	1.59	

128		   	J211232.5+741227	   	J21123576+7412339	   	N0WW000208	   	TYC 4473-229-1	   	21 12 35.768	   	+74 12 33.99	   	12.46	   	T	   	11.77	   	T	   	10.191	   	9.815	   	9.709	   	0.70	   	1.58	

129		   	J211627.5+575501	   	J21162559+5754571	   	N1DY000213	   	TYC 3961-84-1	   	21 16 25.596	   	+57 54 57.11	   	11.85	   	T	   	11.19	   	T	   	10.100	   	9.770	   	9.688	   	0.66	   	1.09	

130		   	J212606.8+555026	   	J21260610+5550242	   	N1AN000243	   	TYC 3970-530-1	   	21 26 06.103	   	+55 50 24.26	   	12.12	   	T	   	11.42	   	T	   	9.316	   	8.764	   	8.662	   	0.70	   	2.10	

131	^	   	J212929.0+621859	   	J21292533+6218582	   	N1EN000408	   	TYC 4253-1617-1	   	21 29 25.338	   	+62 18 58.23	   	12.16	   	T	   	11.47	   	T	   	9.684	   	9.141	   	8.965	   	0.68	   	1.79	

132	 ^∗	   	J213253.9+703751	   	J21325388+7037436	   	N1G6000228	   	GSC 04465-01410	   	21 32 53.889	   	+70 37 43.65	   	13.51	   	G_B	   	12.61	   	U	   	10.054	   	9.416	   	9.285	   	0.90	   	2.56	

133	 ^∗, ^	   	J213749.2+803228	   	J21374757+8032311	   	N0YD000068	   	TYC 4607-461-1	   	21 37 47.573	   	+80 32 31.15	   	12.48	   	T	   	11.54	   	T	   	9.147	   	8.554	   	8.396	   	0.94	   	2.39	

134	^	   	J214719.8+611618	   	J21471905+6116173	   	N1EL000789	   		   	21 47 19.051	   	+61 16 17.39	   	12.79	   	G_B	   	11.83	   	U	   	10.221	   	9.692	   	9.642	   	0.96	   	1.61	

135	^	   	J214909.0+591341	   	J21490916+5913348	   	N1B9000224	   		   	21 49 09.163	   	+59 13 34.81	   	13.68	   	G_B	   	11.99	   	U	   	9.937	   	9.289	   	9.099	   	1.67	   	2.05	

136		   	J220214.4+562800	   	J22021462+5628051	   	N1BX000508	   		   	22 02 14.625	   	+56 28 05.11	   	13.99	   	G_B	   	13.06	   	U	   	10.149	   	9.535	   	9.378	   	0.93	   	2.91	

137	 ^∗	   	J220524.6+655219	   	J22052579+6552198	   	N1GT000629	   	TYC 4275-1998-1	   	22 05 25.799	   	+65 52 19.87	   	11.66	   	T	   	11.08	   	T	   	9.690	   	9.321	   	9.252	   	0.58	   	1.39	

138		   	J220639.1+613425	   	J22063973+6134269	   	N1B7000261	   		   	22 06 39.736	   	+61 34 26.93	   	14.67	   	G_B	   	13.47	   	U	   	9.962	   	9.297	   	9.088	   	0.80	   	3.51	

139		   	J221055.6+632339	   	J22105525+6323533	   	N1GG000302	   	STF 2879C	   	22 10 55.258	   	+63 23 53.33	   	11.85	   	G_B	   	11.10	   	G_V	   	11.109	   	10.977	   	10.893	   	[0.75]	   	(-0.01)	

140	^	   	J221712.3+545100	   	J22171260+5451062	   	N1B3000489	   		   	22 17 12.610	   	+54 51 06.29	   	14.09	   	G_J	   	12.56	   	G_V	   	(11.637)	   	(11.077)	   	10.964	   	(1.53)	   	(0.92)	

141		   	J221828.6+695134	   	J22182783+6951402	   	N1H9000216	   	WW Cep	   	22 18 27.836	   	+69 51 40.23	   	11.77	   	T	   	10.77	   	T	   	8.957	   	8.515	   	8.385	   	0.99	   	1.81	

142		   	J222257.8+744322	   	J22225898+7443211	   	N0X8000186	   		   	22 22 58.986	   	+74 43 21.12	   	13.91	   	G_B	   	12.85	   	U	   	10.41	   	9.847	   	9.701	   	1.14	   	2.44	

143		   	J222405.9+881244	   	J22240615+8812498	   	N0SI000264	   		   	22 24 06.158	   	+88 12 49.81	   	14.28	   	G_J	   	13.62	   	U	   	10.167	   	9.495	   	9.311	   	[0.66]	   	3.45	

144	^	   	J222923.1+674923	   	J22292260+6749164	   	N1HA000396	   	TYC 4476-1415-1	   	22 29 22.601	   	+67 49 16.45	   	11.60	   	T	   	11.03	   	T	   	9.376	   	8.888	   	8.822	   	0.56	   	1.65	

145		   	J223613.9+703206	   	J22361592+7032042	   	N1H7000172	   	TYC 4480-965-1	   	22 36 15.929	   	+70 32 04.28	   	11.61	   	T	   	10.69	   	T	   	8.546	   	8.030	   	7.824	   	0.92	   	2.14	

146	^	   	J224000.2+642310	   	J22400038+6423130	   	N195000284	   		   	22 40 00.384	   	+64 23 13.04	   	14.10	   	G_J	   	13.34	   	U	   	9.633	   	9.037	   	8.784	   	(1.46)	   	3.71	

147	^	   	J224917.6+522634	   	J22491811+5226360	   	N17N000016	   	TYC 3633-2139-1	   	22 49 18.111	   	+52 26 36.05	   	12.05	   	T	   	10.62	   	T	   	8.692	   	8.091	   	7.961	   	1.43	   	1.93	

148	^⋆	   	J225059.7+781435	   	J22510533+7814216	   	N0YH000446	   		   	22 51 05.331	   	+78 14 21.63	   	13.00	   	G_B	   	12.21	   	U	   	10.46	   	10.143	   	10.098	   	0.79	   	1.75	

149	^	   	J225641.1+593031	   	J22564095+5930368	   	N1DH000105	   	TYC 3997-191-1	   	22 56 40.956	   	+59 30 36.87	   	12.07	   	T	   	11.40	   	T	   	10.002	   	9.695	   	9.563	   	0.68	   	1.40	

150		   	J225855.7+673117	   	J22585395+6731186	   	N1FU000550	   		   	22 58 53.957	   	+67 31 18.66	   	12.89	   	G_B	   	11.95	   	G_V	   	10.397	   	10.046	   	9.915	   	(0.73)	   	2.20	

151		   	J230604.0+635538	   	J23060482+6355339	   	N1A1000396	   	GJ 9809	   	23 06 04.827	   	+63 55 33.95	   	12.15	   	T	   	10.93	   	T	   	7.815	   	7.167	   	6.977	   	1.23	   	3.12	

152	^⋆, ^	   	J230822.7+790829	   	J23082206+7908236	   	N0YA000504	   		   	23 08 22.063	   	+79 08 23.69	   	13.99	   	G_B	   	12.49	   	U	   	10.084	   	9.511	   	9.271	   	1.50	   	2.40	

153	 ^∗, ^⋆, ^	   	J231616.5+784156	   	J23161828+7841558	   	N0YA000035	   	TYC 4605-170-1	   	23 16 18.287	   	+78 41 55.90	   	12.69	   	T	   	11.75	   	T	   	9.535	   	9.002	   	8.826	   	0.94	   	2.22	

154	^	   	J232209.7+575626	   	J23220944+5756296	   	N1D1000255	   		   	23 22 09.444	   	+57 56 29.63	   	14.65	   	G_B	   	13.36	   	U	   	9.939	   	9.293	   	9.088	   	1.29	   	3.43	

155	^	   	J232346.4+620620	   	J23234618+6206193	   	N1A6000239	   		   	23 23 46.183	   	+62 06 19.33	   	15.15	   	G_B	   	11.94	   	U	   	9.758	   	9.262	   	9.099	   	4.26	   	2.18	

156	^⋆, ^	   	J232647.5+770304	   	J23264947+7703062	   	N0WV000748	   		   	23 26 49.478	   	+77 03 06.22	   	14.33	   	G_J	   	12.95	   	G_V	   	10.269	   	9.573	   	9.416	   	(1.38)	   	(2.68)	

157	^⋆, ^	   	J233702.3+751625	   	J23370398+7516206	   	N0WQ000534	   	TYC 4602-862-1	   	23 37 03.981	   	+75 16 20.67	   	11.51	   	T	   	10.83	   	T	   	9.519	   	9.160	   	9.087	   	0.68	   	1.31	

158	^⋆	   	J234920.7+783000	   	J23492002+7829467	   	N0WG000199	   	TYC 4606-1905-1	   	23 49 20.027	   	+78 29 46.73	   	12.30	   	T	   	11.53	   	T	   	9.767	   	9.278	   	9.151	   	0.76	   	1.76	

159	^	   	J235502.1+541516	   	J23550237+5415171	   	N176000076	   		   	23 55 02.377	   	+54 15 17.13	   	13.25	   	G_B	   	12.39	   	G_V	   	10.406	   	9.812	   	9.638	   	(1.20)	   	2.63	



    15lStars only cross-identified with a source of the XMM-Newton catalog:



160	^⋆,	^   	184257	   	J22372780+7515256	   	N0XD010154	   	[KP93] 2-43 	   	22 37 27.806	   	+75 15 25.62	   	18.86	   	G_B	   	16.44	   	U	   	11.289	   	10.202	   	9.854	   	2.42	   	5.15	

161		   	186704	   	J23025635+5835565	   	N1DJ000620	   	LSPM J2302+5835	   	23 02 56.352	   	+58 35 56.55	   	14.63	   	G_J	   	13.70	   	U	   	9.999	   	9.373	   	9.150	   	(1.12)	   	3.70	

162	^	   	189583	   	J23364300+6204331	   	N19Y000541	   		   	23 36 43.006	   	+62 04 33.15	   	12.57	   	G_B	   	11.64	   	U	   	10.158	   	9.807	   	9.711	   	0.93	   	1.48	



    15lStars in <cit.> not selected using our multivariate analysis:



163	 ^∗, 	^⋆	   	J000002.5+733942	   	J00000208+7339463 	   	NACK000433	   	TYC 4306-1190-1	   	00 00 02.089	   	+73 39 46.37	   	13.00	   	T	   	11.93	   	T	   	9.779	   	9.261	   	9.094	   	1.06	   	2.15	

164	 ^∗, ^⋆, ^	   	J000142.0+773057	   	J00014256+7731061 	   	NACG000699	   	TYC 4496-2286-1	   	00 01 42.564	   	+77 31 06.19	   	13.15	   	T	   	12.03	   	T	   	10.037	   	9.451	   	9.281	   	1.12	   	1.99	

165	 ^∗, ^⋆	   	J004621.1+741251	   	J00462233+7412489 	   	NADB000010	   	GSC 04307-01640	   	00 46 22.335	   	+74 12 48.96	   	13.46	   	G_B	   	12.72	   	U	   	11.432	   	11.208	   	11.079	   	0.74	   	1.29	

166	 ^∗ 		   	J010117.1+713114	   	J01011729+7131126 	   	NABO000533	   	TYC 4304-1407-1	   	01 01 17.299	   	+71 31 12.65	   	11.73	   	T	   	10.73	   	T	   	8.947	   	8.453	   	8.353	   	1.00	   	1.78	

167	 ^∗, ^ 		   	J010929.0+683916	   	J01092883+6839146 	   	NB0A000048	   	V1065 Cas	   	01 09 28.832	   	+68 39 14.70	   	11.44	   	T	   	10.32	   	T	   	7.637	   	7.071	   	6.923	   	1.12	   	2.68	

168	 ^∗	   	J011934.6+713028	   	J01193440+7130318 	   	NB04000593	   	TYC 4305-1893-1	   	01 19 34.408	   	+71 30 31.81	   	12.12	   	T	   	11.39	   	T	   	(10.347)	   	(9.984)	   	(9.900)	   	0.73	   	(1.04)	

169	 ^∗, ^ 		   	J013925.5+701853	   	J01392593+7018500 	   	NB06000531	   	TYC 4314-1757-1	   	01 39 25.935	   	+70 18 50.05	   	10.80	   	T	   	10.16	   	T	   	8.451	   	8.002	   	7.882	   	0.63	   	1.71	

170	 ^∗, ^		   	J022613.0+681127	   	J02261282+6811329 	   	NB20000348	   	GSC 04312-00734	   	02 26 12.829	   	+68 11 32.96	   	13.17	   	G_B	   	12.42	   	U	   	10.721	   	10.373	   	10.242	   	0.75	   	1.70	

171	 ^∗ 		   	J200549.1+770550	   	J20054896+7705530 	   	N0Y0000647	   	TYC 4589-2335-1	   	20 05 48.967	   	+77 05 53.04	   	12.66	   	T	   	11.08	   	T	   	8.633	   	7.985	   	7.816	   	1.59	   	2.45	

172	 ^∗ 		   	J201151.4+783434	   	J20115370+7834374 	   	N0ZB000125	   	TYC 4589-369-1	   	20 11 53.700	   	+78 34 37.46	   	12.49	   	T	   	11.71	   	T	   	9.913	   	9.435	   	9.266	   	0.78	   	1.80	

173	 ^∗ 		   	J201948.8+653408	   	J20194855+6534095 	   	N1JZ000119	   	GSC 04241-01092	   	20 19 48.556	   	+65 34 09.56	   	11.79	   	G_B	   	11.19	   	U	   	10.571	   	10.186	   	10.088	   	0.60	   	0.61	

174	 ^∗ 		   	J202026.6+780717	   	J20202937+7807222 	   	N0ZB000672	   	TYC 4589-1101-1	   	20 20 29.379	   	+78 07 22.26	   	11.10	   	T	   	10.34	   	T	   	8.965	   	8.516	   	8.434	   	0.77	   	1.38	

175	 ^∗, ^		   	J203341.8+705321	   	J20334380+7053188 	   	N1JA000022	   	TYC 4451-1270-1	   	20 33 43.801	   	+70 53 18.86	   	13.43	   	T	   	11.65	   	T	   	10.215	   	9.675	   	9.621	   	1.78	   	1.44	

176	 ^∗ 		   	J204327.6+711546	   	J20432832+7115467 	   	N1J5000308	   	TYC 4455-856-1	   	20 43 28.322	   	+71 15 46.77	   	12.70	   	T	   	12.27	   	T	   	10.79	   	10.537	   	10.473	   	0.44	   	1.48	

177	 ^∗ 		   	J205312.2+792031	   	J20531202+7920218 	   	N0ZJ000194	   	GSC 04594-01127	   	20 53 12.024	   	+79 20 21.82	   	13.78	   	G_B	   	12.89	   	U	   	10.100	   	9.565	   	9.406	   	0.89	   	2.79	

178	 ^∗, ^		   	J205607.9+651033	   	J20560940+6510312 	   	N1KG000089	   	TYC 4255-314-1	   	20 56 09.407	   	+65 10 31.25	   	10.80	   	T	   	10.35	   	T	   	9.436	   	9.176	   	9.090	   	0.44	   	0.91	

179	 ^∗ 		   	J211127.5+761435	   	J21112933+7614290 	   	N0Y6000103	   	TYC 4586-1090-1	   	21 11 29.335	   	+76 14 29.02	   	12.45	   	T	   	11.47	   	T	   	10.192	   	9.735	   	9.692	   	0.98	   	1.28	

180	 ^∗ 		   	J211143.9+685428	   	J21114388+6854231 	   	N1JE000286	   	TYC 4460-1614-1	   	21 11 43.890	   	+68 54 23.13	   	11.19	   	T	   	10.58	   	T	   	9.455	   	9.144	   	9.059	   	0.60	   	1.13	

181	 ^∗ 		   	J214258.6+803021	   	J21425760+8030197 	   	N0YD000086	   	TYC 4607-611-1	   	21 42 57.600	   	+80 30 19.75	   	12.03	   	T	   	11.47	   	T	   	10.016	   	9.676	   	9.582	   	0.56	   	1.45	

182	 ^∗, ^⋆	   	J221107.9+791801	   	J22111127+7917599 	   	N0YI000354	   	GSC 04608-01986	   	22 11 11.277	   	+79 17 59.98	   	14.24	   	G_B	   	13.81	   	U	   	10.329	   	9.737	   	9.558	   	0.43	   	3.48	

183	 ^∗ 		   	J221158.7+681953	   	J22115779+6819524 	   	N1GX000280	   	TYC 4463-818-1	   	22 11 57.798	   	+68 19 52.46	   	12.50	   	T	   	11.47	   	T	   	9.763	   	9.208	   	9.093	   	1.03	   	1.71	

184	 ^∗, ^		   	J222706.6+652127	   	J22270525+6521313 	   	N1GU000092	   	GSC 04272-00174	   	22 27 05.254	   	+65 21 31.33	   	13.75	   	G_B	   	13.36	   	U	   	10.822	   	10.323	   	10.212	   	0.39	   	2.54	

185	 ^∗ 		   	J223345.1+703321	   	J22334483+7033181 	   	N1H7000161	   	TYC 4480-917-1	   	22 33 44.839	   	+70 33 18.19	   	12.97	   	T	   	11.16	   	T	   	8.508	   	7.817	   	7.616	   	1.81	   	2.65	

186	 ^∗, ^⋆	   	J223956.5+774934	   	J22395815+7749394 	   	N0WM000002	   	TYC 4604-743-1	   	22 39 58.155	   	+77 49 39.44	   	12.47	   	T	   	11.94	   	T	   	10.007	   	9.530	   	9.387	   	0.53	   	1.93	

187	 ^∗, ^⋆	   	J225133.9+763549	   	J22513566+7635537 	   	N0WL000167	   	TYC 4601-1894-1	   	22 51 35.668	   	+76 35 53.73	   	12.48	   	T	   	11.94	   	T	   	10.272	   	9.886	   	9.801	   	0.54	   	1.67	

188	 ^∗, ^⋆, ^	   	J230043.2+772833	   	J23004455+7728385 	   	N0WM000641	   	TYC 4605-2733-1	   	23 00 44.552	   	+77 28 38.54	   	11.76	   	T	   	11.42	   	T	   	9.409	   	8.977	   	8.840	   	0.34	   	2.01	

189	 ^∗, ^⋆	   	J230533.0+782238	   	J23053649+7822389 	   	N0YA000256	   	GSC 04605-00268	   	23 05 36.498	   	+78 22 38.98	   	14.36	   	G_B	   	13.46	   	U	   	10.307	   	9.656	   	9.508	   	0.90	   	3.15	

190	 ^∗, ^⋆	   	J230757.5+765146	   	J23075657+7651478 	   	N0WL000003	   	TYC 4601-938-1	   	23 07 56.571	   	+76 51 47.84	   	11.90	   	T	   	10.71	   	T	   	8.483	   	7.894	   	7.714	   	1.19	   	2.23	

191	 ^∗, ^⋆, ^	   	J230942.9+735725	   	J23094349+7357152 	   	N0XO000049	   	GSC 04489-00036	   	23 09 43.490	   	+73 57 15.29	   	14.10	   	G_B	   	12.94	   	U	   	9.757	   	9.081	   	8.906	   	1.16	   	3.18	

192	 ^∗, ^		   	J234342.3+684631	   	J23434195+6846271 	   	N1FN000105	   	GSC 04479-00348	   	23 43 41.954	   	+68 46 27.12	   	13.46	   	G_B	   	12.78	   	U	   	10.892	   	10.364	   	10.249	   	0.68	   	1.89	

193	 ^∗, ^⋆	   	J235107.5+785802	   	J23511013+7858050 	   	N0Y8000689	   	TYC 4610-1318-1	   	23 51 10.132	   	+78 58 05.00	   	12.39	   	T	   	11.34	   	T	   	9.572	   	9.184	   	9.041	   	1.04	   	1.77	



    15lOther young field stars projected towards the CO Cepheus void and its surrounding, which also appear either in <cit.> or in <cit.>:



G1	^⋆, ^	   	J000038.4+794037	   	 J00004121+7940398	   	NAA8000377	   	BD+78 853		   	00 00 41.214	   	+79 40 39.82	   	10.98	   	T	   	10.25	   	T	   	8.922	   	8.612	   	8.523	   	0.72	   	1.33	

G2	^⋆, ^	   	J001337.6+770210	   	J00134052+7702104 	   	NACH000519	   	TYC 4496-780-1	   	00 13 40.521	   	+77 02 10.49 	   	10.35	   	T	   	  9.78	   	T	   	8.208	   	7.758	   	7.570	   	0.57	   	1.57	

G3	^⋆, ^	   	J003804.2+790328	   	J00380610+7903206 	   	NAG3000270	   	TYC 4500-1478-1	   	00 38 06.100	   	+79 03 20.66	   	11.19	   	T	   	10.29	   	T	   	8.763	   	8.323	   	8.213	   	0.91	   	1.53	

G4	^⋆, ^	   	J003941.9+790526	   	J00394018+7905307 	   	NAG3000255	   	BD+78 19			   	00 39 40.184	   	+79 05 30.77	   	10.24	   	T	   	  9.57	   	T	   	8.303	   	7.933	   	7.854	   	0.67	   	1.27	

F1	^⋆, ^	   	J210621.9+690645	   	J21062175+6906410	   	N0133022143	   	BD+68 1182		   	21 06 21.750	   	+69 06 41.00	   	10.75	   	T	   	10.15	   	T	   	9.011	   	8.754	   	8.703	   	0.60	   	1.14 

F2	^⋆	   	J222316.2+774157	   	J22231885+7741577	   	N0103120435	   	BD+76 857a		   	22 23 18.857	   	+77 41 57.79	   	10.81	   	T	   	10.23	   	T	   	8.796	   	8.449	   	8.368	   	0.59	   	1.43  

F3	^⋆, ^	   	J232052.2+741359	   	J23205208+7414071	   	N0102321423	   	V395 Cep			   	23 20 52.090	   	+74 14 07.13	   	11.06	   	T	   	10.16	   	T	   	8.308	   	7.754	   	7.480	   	0.90	   	1.85  

F4	^⋆	   	J235115.0+773934	   	J23511729+7739351	   	N0102103473	   	TYC 4606-740-1	   	23 51 17.294	   	+77 39 35.16	   	11.74	   	T	   	10.69	   	T	   	8.788	   	8.316	   	8.191	   	1.05	   	1.90 




Notes associated to the recno. ^∗ Selected by both this study and the work of <cit.>; ^⋆ Towards the CO Cepheus void; ^ Multiple system (VB and SB). 

23.2cm
Notes. 
 ^a The B–V color indexes are mainly in the Johnson-Cousins system. The bracketed values are the GCS II photographic color indexes, while the square-bracketed ones are the result of a mixture of both systems. 
^b The V–J color index values are put in parentheses if the V magnitude is not in the Johnson-Cousins system or if the J magnitude is an upper limit or a poor quality value. 
 

References. T =  <cit.>; U =  <cit.>; Y =  <cit.>; G = <cit.> where the suffix corresponds to their B, j, or V-band magnitude. 




 



However, for the analysis of the spectral energy distribution (Sect. <ref>) we have updated the magnitudes with more accurate values of B and V retrieved from the AAVSO Photometric All Sky Survey (APASS, ) catalog. The V magnitudes are also available in the TASS Mark IV patches photometric catalog <cit.>. For most sources we retrieved the I_ C magnitudes from the TASS catalog or, if not available, from the catalog of <cit.>. In this way, the dataset of the magnitudes is homogeneous and avoids a mixture of photometric and photographic estimates. We found 177 (plus three whose V magnitude is not provided) and 166 sources in common with the APASS and TASS catalogs, respectively. The different datasets are consistent with the V magnitudes in Table <ref>, with a Pearson's correlation coefficient (PCC) of ∼0.967. We also note that the V magnitudes in APASS and TASS catalogs are fully consistent with each other (PCC ∼ 0.992). In the case of the bright sources (V ⩽13 mag), we obtained a good agreement between the various magnitudes and the spread increases towards the faintest objects, as expected in such a comparison. Regarding the faint objects (V > 13 mag), the V magnitudes in Table <ref> tend to be overestimated by 0.5 mag. This corresponds to the typical accuracy of the <cit.> relation at this brightness, which might be subject to systematic errors and other effects. 

The photometric standard errors of the Tycho sources with 9 <V_T<12 are typically 0.15 and 0.1 mag in B and V passbands, respectively, while they are ∼0.25 mag in both bands for the faintest sources. The tabulated errors of the GCS II sources are ∼0.3 mag for the V magnitudes and ∼0.4 mag for both the B and B_J magnitudes. The error on the optical magnitudes for the sources fainter than V=12 mag is considered to be at least of 0.5 mag. For our targets, the typical error for the APASS photometry is instead 0.05 mag.

Five of the six sources with a B–V color index below our threshold of 0.5 mag come from the inclusion of the <cit.> sample. The use of APASS magnitudes leads to the same statement for sources #176 and #178 only. Regarding the remaining source (#102), its color index of 0.546±0.276 mag in the APASS catalog fulfills our initial selection criterion.




 §.§ Observations and data reduction



To study the physical and kinematic properties of all these young star candidates, we conducted observing campaigns using three spectrographs (Table <ref>). We acquired both intermediate- and high-resolution optical spectra, sharing our candidates in an optimized way, depending on their brightness. 

We observed the brightest (V⩽12 mag) targets with two instrumental setups. 
From 26 to 27 September 2009, we used the cross-dispersed échelle SOPHIE[http://www.obs-hp.fr/guide/sophie/sophie-eng.shtml] spectrograph <cit.> mounted on the 1.93-m telescope of the Observatoire de Haute Provence (OHP, France). The EEV-4482 detector is a thinned, back-illuminated, anti-reflection coated 4k× 2k 15-μm-pixel CCD cooled at -100C, with fast-readout mode. We chose the high-efficiency mode equipped with a double-fiber scrambler to homogenize and stabilize the illumination of the spectrograph entrance. This allowed us to record the 39 spectral orders covering effectively the wavelength range 3872–6943 Å, with a resolution of about 39,000 at 5500 Å. The data were treated using the automatic data-reduction pipeline, adapted from the HARPS software.[http://www.eso.org/sci/facilities/lasilla/instruments/harps/]

From 2 to 5 October 2009 and on 12 December 2009, we completed our survey of the bright targets. The échelle spectra were taken with the fibre optics Cassegrain échelle spectrograph <cit.> at the 2.2-m telescope of the German-Spanish Calar Alto Observatory (CAHA, Sierra de Los Filabres, Spain). We adopted the unique-fiber mode and chose the Site#1d detector, a 2048×2048 24 μm-pixel CCD. We used the configuration with the 400 μm-slit width, leading to a resolution of about 28,000 and covering the wavelength range from 3800 to 10000 Å, in a total of 100 orders. Using tasks of the Echelle package within the IRAF environment, we reduced the data following the standard steps of background subtraction, division by a flat-field spectrum given by a halogen lamp, wavelength calibration using the emission lines of the Th-Ar arc lamp, and normalization to the continuum through a polynomial fit. 





r@l@lcr@c@lr@c@lcr@c@lr@c@lr@c@lr@c@ll
Radial and rotational velocities, atmospheric parameters, and lithium equivalent widths derived for our targets during the survey.



2c#^⋆	    Instrument	    H.J.D.					    3cRV			    3cvsin i		    SpT     3cT_ eff	    3clog g			    3c[Fe/H]	    3cW_ Li	    Note	

			   			   			    [2400000+]		    3c[km s^-1]	    3c[km s^-1]	                3c[K]			    3c[cm^2 s^-1]	    3c[dex]	    3c[mÅ]	    		



Continued. 


2c#^⋆	    Instrument	    H.J.D.					    3cRV			    3cvsin i		    SpT     3cT_ eff	    3clog g			    3c[Fe/H]	    3cW_ Li	    Note	

			   			   			    [2400000+]		    3c[km s^-1]	    3c[km s^-1]	                3c[K]			    3c[cm^2 s^-1]	    3c[dex]	    3c[mÅ]	    		






1			   		   	IDS		   	55079.6090728		   	2.2	   	±	   	0.3	   	17		   	±	    	9		   	G1.5V	   	5827	   	± 	   	61		   	4.07	   	± 	   	0.12	   	-0.12	   	± 	   	0.11	   	72	   	±	   	15	   		

2			   		   	IDS		   	55079.6255449		   	-75.7		    ±		   	5.6		   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…		   	RV1 of an SB2 system with two M-type stars (M3.5V)	

2			   		   	IDS		   	55079.6255449		   	10.6		    ±		   	8.4		   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…		   	RV2 of an SB2 system with two M-type stars (M3.5V)	

3			   		   	IDS		   	55079.5934565		   	-14.3	   	±	   	2.0	   	15		   	±	   	6		   	M4V		   	3397	   	±	   	50		   	4.56	   	±	   	0.15	   	-0.15	   	±	   	0.11	   	18	   	±	   	41	   		

4			   		   	SOPHIE	   	55101.4586116		   	3c…	   		3c…	   	…   	3c…	   	3c…	   	3c…	   	3c…	   	W UMa-type star	

5			   		   	IDS		   	55080.6417659		   	3.1	   	±	   	2.4	   	38		   	±	   	3		   	M4V		   	3397	   	±	   	50		   	4.58	   	±	   	0.16	   	-0.15	   	±	   	0.11	   	9	   	±	   	31	   		

5			   		   	IDS		   	55083.6659514		   	3.0	   	±	   	1.3	   	15		   	±	   	4		   	M5V		   	3339	   	±	   	70		   	4.57	   	±	   	0.18	   	-0.14	   	±	   	0.11	   	45	   	±	   	59	   		

6			   	c1	   	IDS		   	55084.6707247		   	-108.0	   	±	   	4.5	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system, strong Li line, Target = TYC 4500-1549-1	

6			   	c1	   	IDS		   	55084.6707247		   	83.1	   	±	   	4.6	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system, strong Li line, Target = TYC 4500-1549-1	

6			   	c1	   	IDS		   	55168.4497949		   	6.4	   	±	   	1.2	   	3c…	   	…   	3c…	   		3c…	   	3c…	   	3c…	   	Clear asymmetry in the CCF profile, strong Li line, Target = TYC 4500-1549-1 	

6			   	c1	   	IDS		   	55524.4605440		   	-94.0	   	±	   	3.8	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system, strong Li line, Target = TYC 4500-1549-1	

6			   	c1	   	IDS		   	55524.4605440		   	72.8	   	±	   	5.0	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system, strong Li line, Target = TYC 4500-1549-1	

6			   	c1	   	IDS		   	55524.4873016		   	-106.5	   	±	   	3.8	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system, strong Li line, Target = TYC 4500-1549-1	

6			   	c1	   	IDS		   	55524.4873016		   	79.1	   	±	   	4.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system, strong Li line, Target = TYC 4500-1549-1	

6			   	c2	   	IDS		   	55168.4497949		   	-9.1	   	±	   	1.2	   	29		   	±	   	7		   	M0V		   	3998	   	±	   	189	   	4.63	   	±	   	0.14	   	-0.16	   	±	   	0.13	   	335	   	±	   	55	   		

6			   	c2	   	IDS		   	55524.4873016		   	-8.4	   	±	   	0.8	   	15		   	±	   	8		   	M0V		   	3885	   	±	   	58		   	4.63	   	±	   	0.10		   	-0.08	   	±	   	0.12	   	313	   	±	   	48		   		 

6			   	c3	   	IDS		   	55524.4605440		   	-1.7	   	±	   	9.1	   	3c…	   	…   	3c…	   	3c…	   	3c…	   	3c…	   	Target = Gaia DR2 564707973733134080 
 
7			   		   	IDS		   	55081.7128973		   	-147.5	   	±	   	2.0	   	43		   	±	   	3		   	K1V		   	5011	   	±	   	91		   	3.94	   	±	   	0.23	   	-0.18	   	±	   	0.11	   	18	   	±	   	71	   	Double-peaked Hα profile (SB2?) 	

7			   		   	IDS		   	55081.7128973		   	3c∼80	   	3c…	   	…   	3c…	   	3c…	   	3c…	   	3c…	   	Radial velocity of faint source in case of an SB2 system	

8			   		   	IDS		   	55084.6961890		   	-83.0	   	±	   	0.7	   	15		   	±	   	9		   	K5III		   	3833	   	±	   	78		   	2.84	   	±	   	0.44	   	-0.11	   	±	   	0.11	   	3	   	±	   	41	   		

9			   		   	IDS		   	55082.7141749		   	-17.6	   	±	   	1.8	   	22		   	±	   	6		   	M2V		   	3625	   	±	   	62		   	4.63	   	±	   	0.15	   	-0.12	   	±	   	0.11	   	6	   	±	   	65	   		

10			   		   	SOPHIE	   	55102.5221099		   	50.6	   	±	   	0.6	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system, blended peaks	

10			   		   	SOPHIE	   	55102.5221099		   	21.5	   	±	   	0.8	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system, blended peaks	

11	   		   	IDS		   	55079.6372917		   	-30.7	   	±	   	0.6	   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…	   	RV1 of the SB2 system	

11	   		   	IDS		   	55079.6372917		   	27.2	   	±	   	6.3	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system (small and blended peak) 	

11	   		   	IDS		   	56225.5137565		   	3.2	   	±	   	0.7	   	18		   	±	   	2 		   	K0IV		   	4923	   	±	   	108	   	3.58	   	±	   	0.23	   	0.01	   	±	   	0.11	   	36	   	±	   	45	   	 	

12			   		   	IDS		   	55079.6563403		   	-20.6	   	±	   	2.9	   	15		   	±	   	2		   	M4V		   	3413	   	±	   	112	   	4.59	   	±	   	0.15	   	-0.14	   	±	   	0.11	   	29	   	±	   	39	   		

13			   		   	IDS		   	55080.7295766		   	-123.0	   	±	   	7.1	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

13			   		   	IDS		   	55080.7295766		   	85.7	   	±	   	7.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

13			   		   	IDS		   	55083.7103077		   	67.9	   	±	   	8.2	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

13			   		   	IDS		   	55083.7103077		   	-109.5	   	±	   	8.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

14			   		   	IDS		   	55079.7286600		   	-10.1	   	±	   	1.9	   	15		   	±	   	1		   	M3.5V	   	3563	   	±	   	80		   	4.41	   	±	   	0.24	   	-0.15	   	±	   	0.11	   	8	   	±	   	28	   		

15			   		   	IDS		   	55083.7314967		   	7.1	   	±	   	1.0	   	21		   	±	   	6		   	M0V		   	3912	   	±	   	67		   	4.62	   	±	   	0.15	   	-0.11	   	±	   	0.10	   	37	   	±	   	35	   		

16			   		   	IDS		   	55079.6711282		   	-7.3	   	±	   	0.4	   	17		   	±	   	3		   	K2V		   	5103	   	±	   	59		   	4.27	   	±	   	0.20	   	-0.10	   	±	   	0.10	   	200	   	±	   	32	   		

16			   		   	FOCES	   	55107.5866862		   	-6.23	   	±	   	0.18	   	15.0	   	±	   	1.9	      	K0V		   	5146	   	±	   	56		   	4.50	   	±	   	0.21	   	-0.03	   	±	   	0.05	   	208	   	±	   	30	   		

17			   		   	IDS		   	55079.6869501		   	-14.7	   	±	   	0.3	   	15		   	±	   	8		      K0III-IV	   	5204	   	±	   	91		   	3.58	   	±	   	0.25	   	-0.09	   	±	   	0.11  	   	11	   	±	   	23	   		

18			   		   	IDS		   	55079.7061001		   	58.0	   	±	   	2.2	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

18			   		   	IDS		   	55079.7061001		   	-57.2	   	±	   	4.1	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

19			   		   	SOPHIE	   	55102.5487604		   	60.335	   	±	   	0.018	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

19			   		   	SOPHIE	   	55102.5487604		   	-72.950	   	±	   	0.018	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

19			   		   	FOCES	   	55110.5642208		   	66.49	   	±	   	0.46	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

19			   		   	FOCES	   	55110.5642208		   	-77.81	   	±	   	0.44	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

20			   		   	IDS		   	55083.7504098		   	20.3	   	±	   	2.6	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system 	

20			   		   	IDS		   	55083.7504098		   	-41.3	   	±	   	2.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system 	

20			   		   	IDS		   	56225.5366156		   	22.6	   	±	   	2.8	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

20			   		   	IDS		   	56225.5366156		   	-47.0	   	±	   	3.5	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

21			   		   	IDS		   	55084.7172196		   	-10.9	   	±	   	1.0	   	15		   	±	   	15		   	M5V		   	3397	   	±	   	50		   	4.56	   	±	   	0.15	   	-0.15	   	±	   	0.11	   	17	   	±	   	36	   		

22			   		   	SOPHIE	   	55102.5667200		   	-10.284	   	±	   	0.005	   	10.0	   	±	   	1.0	   	K1V		   	5127	   	±	   	121	   	4.55	   	±	   	0.06	   	-0.06	   	±	   	0.10	   	258	   	±	   	12	   		

22			   		   	FOCES	   	55107.6229096		   	-10.38	   	±	   	0.09	   	9.5	   	±	   	1.0	   	K1V		   	5115	   	±	   	59		   	4.55	   	±	   	0.15	   	-0.02	   	±	   	0.05	   	287	   	±	   	24	   		

23			   		   	IDS		   	55084.7367683		   	30.4	   	±	   	1.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system with two M-type stars (M3.5V)	

23			   		   	IDS		   	55084.7367683		   	-64.4	   	±	   	1.6	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system with two M-type stars (M3.5V)	

24			   		   	IDS		   	55081.6962023		   	25.2	   	±	   	2.4	   	15		   	±	   	12		   	M2V		   	3607	   	±	   	50		   	4.60	   	±	   	0.16	   	-0.13	   	±	   	0.11	   	31	   	±	   	49	   		

25			   		   	IDS		   	55081.7295722		   	-22.2	   	±	   	0.7	   	15		   	±	   	1		   	K5V		   	4722	   	±	   	129	   	4.00	   	±	   	0.22	   	-0.04	   	±	   	0.11	   	0	   	±	   	28	   		

26			   		   	IDS		   	55084.7557299		   	3.2	   	±	   	1.2	   	25		   	±	   	7		   	M2V		   	3622	   	±	   	55		   	4.56	   	±	   	0.22	   	-0.05	   	±	   	0.13	   	28	   	±	   	81	   		

27			   		   	IDS		   	55082.7338377		   	-35.9	   	±	   	0.6 	   	17		   	±	   	2		   	K1III		   	4809	   	±	   	91		   	3.08	   	±	   	0.22	   	-0.03	   	±	   	0.11	   	56	   	±	   	24	   	Hα faint double-peaked emission	

28			   		   	SOPHIE	   	55101.6452849		   	-58.985	   	±	   	0.019	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

28			   		   	SOPHIE	   	55101.6452849		   	59.685	   	±	   	0.019	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

28			   		   	FOCES	   	55107.6445504		   	-74.43	   	±	   	0.29	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system	

28			   		   	FOCES	   	55107.6445504		   	76.57	   	±	   	0.41	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

29			   		   	IDS		   	55083.7657904		   	-7.2	   	±	   	0.8	   	26		   	±	   	10		   	M0V		   	3816	   	±	   	79		   	4.65	   	±	   	0.14	   	-0.11	   	±	   	0.10	   	35	   	±	   	58	   		

30			   		   	IDS		   	56226.6080778		   	-22.6	   	±	   	4.9		   	34		   	±	   	2		   	M4.5V	   	3436	   	±	   	56		   	4.50	   	±	   	0.33	   	-0.14	   	±	   	0.11	   	37		   	±	   	37		   	 	

31			   	c1	   	IDS		   	55524.5662608		   	-44.7	   	±	   	0.5	   	15		   	±	   	1		   	K1IV		   	4765	   	±	   	62		   	2.83	   	±	   	0.22	   	0.00	   	±	   	0.11	   	11	   	±	   	35	   	Target = Gaia DR2 475251432820143872	

31			   	c2	   	IDS		   	55524.5662608		   	18.0	   	±	   	0.7	   	25		   	±	   	1		   	K7V		   	4363	   	±	   	95		   	4.48	   	±	   	0.17	   	-0.18	   	±	   	0.12	   	59	   	±	   	39	   		

32			   		   	SOPHIE	   	55102.5925771		   	-11.906	   	±	   	0.013	   	15.0	   	±	   	1.03	   	K3V		   	4845	   	±	   	127	   	4.55	   	±	   	0.07	   	0.01	   	±	   	0.13	   	119	   	±	   	10	   	SB1	

32			   		   	FOCES	   	55107.6681762		   	7.53	   	±	   	0.12	   	14.8	   	±	   	0.5	   	K3V		   	4767	   	±	   	111	   	4.37	   	±	   	0.20	   	-0.03	   	±	   	0.04	   	142	   	±	   	16	   	SB1	

33			   		   	SOPHIE	   	55102.6191246		   	3c…	   	3c…	   	…   	3c…	   	3c…	   	3c…	   	3c…	   	Likely SB2 system composed of two fast rotators	

33			   		   	FOCES	   	55107.6911711		   	3c…	   	117.5	   	±	   	11.0	   	G5V		   	5483	   	±	   	313	   	4.32	   	±	   	0.31	   	-0.07	   	±	   	0.17	   	207	   	±	   	60	   	 	

33			   		   	FOCES	   	55110.5854832		   	3c…	   	120.1	   	±	   	13.6	   	G3IV		   	5359	   	±	   	361	   	4.24	   	±	   	0.35	   	-0.04	   	±	   	0.15	   	184	   	±	   	56	   		

34			   		   	IDS		   	56225.6732600		   	6.3	   	±	   	1.4	   	25		   	±	   	7		   	M0V		   	3887	   	±	   	61		   	4.64	   	±	   	0.11	   	-0.10	   	±	   	0.12	   	44		   	±	   	107		   	 	

35			   		   	IDS		   	55524.5899614		   	-94.7	   	±	   	0.6	   	19		   	±	   	3		   	K7V		   	4172	   	±	   	121	   	4.53	   	±	   	0.17	   	-0.16	   	±	   	0.12	   	104	   	±	   	52	   	Double-peaked Hα profile (SB2?)	

36			   		   	FOCES	   	55108.6540370		   	-7.19	   	±	   	0.34	   	41.4	   	±	   	2.5	   	K5V		   	4731	   	±	   	238	   	4.59	   	±	   	0.33	   	-0.05	   	±	   	0.10	   	69	   	±	   	27	   		

36			   		   	FOCES	   	55168.5676429		   	-8.5		   	±	   	3.5		   	39.2	   	±	   	3.7	   	K4V		   	4662	   	±	   	271	   	4.59	   	±	   	0.38	   	-0.06	   	±	   	0.11	   	23	   	±	   	38	   		

37			   	c1	   	SOPHIE	   	55101.6671374		   	-30.5		   	±	   	0.2		   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB2 system 		

37			   	c1	   	SOPHIE	   	55101.6671374		   	-63.7		   	±	   	0.8		   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB2 system	

37			   	c1	   	IDS		   	55524.6197432		   	-48.4	   	±	   	0.9	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of the SB3 system	

37			   	c1	   	IDS		   	55524.6197432		   	-105.7	   	±	   	1.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of the SB3 system	

37			   	c1	   	IDS		   	55524.6197432		   	11.6	   	±	   	9.1	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV3 of the SB3 system	

37			   	c2	   	IDS		   	55524.6197432		   	-53.9	   	±	   	0.6	   	18		   	±	   	13		   	F7IV		   	6107	   	±	   	86		   	3.91	   	±	   	0.11	   	-0.16	   	±	   	0.12	   	39	   	±	   	33	   	Small peak at RV = 242.4±8.5 km s^-1; Target = TYC 4354-793-1	

38			   		   	IDS		   	55082.7548248		   	18.2	   	±	   	1.2	   	17		   	±	   	3		   	K8V		   	4103	   	±	   	71		   	4.58	   	±	   	0.15	   	-0.10	   	±	   	0.10	   	12	   	±	   	34	   		

39			   		   	IDS		   	55524.6410282		   	-10.4	   	±	   	3.1	   	17		   	±	   	10		   	M1.5V	   	3466	   	±	   	122	   	4.77	   	±	   	0.24	   	-0.20	   	±	   	0.11	   	0		   	±	   	50		   		

40			   	c1	   	IDS		   	56381.4256583		   	-6.6		   	±	   	0.4	   	15		   	±	   	1		   	K5V		   	4597	   	±	   	54		   	4.61	   	±	   	0.10	   	0.00	   	±	   	0.11	   	1		   	±	   	44		   		

40			   	c2	   	IDS		   	56381.4256583		   	29.4		   	±	   	1.8	   	3c…		   	…   	3c…		   	3c…	   	3c…	   	3c…		   	RV1 of the SB2 system, Target = Gaia DR2 1116789735748819968		

40			   	c2	   	IDS		   	56381.4256583		   	-38.5		   	±	   	4.2	   	3c…		   	…   	3c…		   	3c…	   	3c…	   	3c…		   	RV2 of the SB2 system, Target = Gaia DR2 1116789735748819968		

40			   	c3	   	IDS		   	56381.4256583		   	-32.9		   	±	   	0.7		   	15		   	±	   	1		   	K1V		   	4976	   	±	   	82		   	4.49	   	±	   	0.14	   	-0.29	   	±	   	0.13	   	7		   	±	   	56		   	Target = Gaia DR2 1116789667029342080	

41			   		   	FOCES	   	55109.6976899		   	3c…	   	145.7	   	±	   	18.3	   	G5V		   	5443	   	±	   	227	   	4.31	   	±	   	0.22	   	-0.13	   	±	   	0.16	   	2	   	±	   	33	   		

41			   		   	IDS		   	56616.7658037		   	-81.5	   	±	   	9.2	   	167	   	±	   	9		   	G8V		   	5300	   	±	   	121	   	3.93	   	±	   	0.30	   	-0.53	   	±	   	0.15	   	6		   	±	   	38		   	SB1	

41			   		   	IDS		   	56708.5273948		   	62.6	   	±	   	3.5	   	131	   	±	   	18		   	K2V		   	5272	   	±	   	110	   	4.26	   	±	   	0.29	   	-0.47	   	±	   	0.14	   	16		   	±	   	31		   	SB1	

42			   	c1	   	FOCES	   	55110.6079134		   	-7.44	   	±	   	0.11	   	11.7	   	±	   	0.6	   	G1.5V	   	5802	   	±	   	119	   	4.38	   	±	   	0.10	   	-0.03	   	±	   	0.07	   	97		   	±	   	17	   		

42			   	c1	   	IDS		   	56707.6473027		   	-8.5	   	±	   	0.4	   	18		   	±	   	1		   	G4V	   	5787	   	±	   	86		   		4.31	   	±	   	0.12	   	-0.05	   	±	   	0.12	   	91		   	±	   	16		   		
	
42			   	c1	   	IDS		   	56708.5474164		   	-11.3	   	±	   	0.6	   	18		   	±	   	2		   	G4V	   	5788		   	±	   	79		   	4.29	   	±	   	0.12	   	-0.03	   	±	   	0.11	   	108	   	±	   	23		   		
	
42			   	c1	   	IDS		   	56708.5665972		   	-9.0	   	±	   	0.3	   	18		   	±	   	2		   	G1.5Vb	   	5822	   	±	   	72		   	4.37	   	±	   	0.12	   	-0.08	   	±	   	0.11	   	76		   	±	   	16		   			

42			   	c2	   	IDS		   	56708.5474164		   	-20.9	   	±	   	0.6	   	20		   	±	   	2		   	K7V	   	4318	   	±	   	82		   		4.60	   	±	   	0.10	   	-0.14	   	±	   	0.11	   	11		   	±	   	126	   		Target = Gaia DR2 1116535920362524928	

43			   		   	FOCES	   	55110.6333984		   	-86.14	   	±	   	1.62	   	56.7	   	±	   	6.0	   	G0IV		   	5717	   	±	   	310	   	4.19	   	±	   	0.18	   	-0.11	   	±	   	0.15	   	34	   	±	   	48	   	SB2?	

44			   	c1	   	IDS		   	55524.6959770		   	10		   	±	   	15		   	224	   	±	   	14		   	G2V		   	5732	   	±	   	73		   	3.96	   	±	   	0.20	   	-0.03	   	±	   	0.11	   	7	   	±	   	15	   		

44			   	c2	   	IDS		   	55524.6959770		   	-21.1	   	±	   	0.7	   	19		   	±	   	10		   	F6IV		   	6277	   	±	   	98		   	4.05	   	±	   	0.13	   	-0.16	   	±	   	0.11	   	9	   	±	   	15	   	Target = TYC 4618-329-1 / Gaia DR2 1149573805235028352	

45			   		   	FOCES	   	55110.6542632		   	-8.54	   	±	   	0.11	   	8.2	   	±	   	0.4	   	G2V		   	5798	   	±	   	78		   	4.33	   	±	   	0.08	   	0.04	   	±	   	0.09	   	73	   	±	   	16	   		

46			   		   	SOPHIE	   	55102.6724754		   	-15.664	   	±	   	0.014	   	16.9	   	±	   	1.0	   	K1V		   	5108	   	±	   	125	   	4.54	   	±	   	0.09	   	-0.11	   	±	   	0.12	   	159	   	±	   	9	   	Likely SB2 system with low M_2/M_1 mass ratio	

46			   		   	FOCES	   	55108.6932431		   	-15.61	   	±	   	0.11	   	19.0	   	±	   	1.4	   	K0V		   	5204	   	±	   	112	   	4.52	   	±	   	0.21	   	-0.10	   	±	   	0.06	   	170	   	±	   	22	   	Likely SB2 system with low M_2/M_1 mass ratio	

46			   		   	FOCES	   	55110.6764087		   	-15.90	   	±	   	0.28	   	18.4	   	±	   	1.4	   	K0V		   	5195	   	±	   	161	   	4.49	   	±	   	0.20	   	-0.08	   	±	   	0.08	   	204	   	±	   	43	   	Likely SB2 system with low M_2/M_1 mass ratio	

47			   		   	IDS		   	55524.7132031		   	-55	   	±	   	17		   	182	   	±	   	21		   	G2V		   	5684	   	±	   	79		   	4.05	   	±	   	0.13	   	-0.29	   	±	   	0.14	   	7	   	±	   	12	   	Double-peaked Hα profile (SB2?)	

49			   		   	IDS		   	56226.7552961		   	12.0	   	±	   	0.7	   	35		   	±	   	2		   	K1V		   	5065	   	±	   	97 	   	4.52	   	±	   	0.14	   	-0.20	   	±	   	0.14	   	30		   	±	   	36		   	SB1 	

49			   		   	IDS		   	56382.4941385		   	-128.0	   	±	   	0.8	   	35		   	±	   	2		   	K1V		   	5032	   	±	   	99 	   	4.51	   	±	   	0.14	   	-0.22	   	±	   	0.12	   	25		   	±	   	15		   	SB1 	

50			   		   	IDS		   	56383.4526273		   	-104.8	   	±	   	5.7	   	3c…		   	…   	3c… 	   	3c…	   	3c…	   	3c…		   	RV1 of the SB2 system	

50			   		   	IDS		   	56383.4526273		   	-230.9	   	±	   	9.1	   	3c…		   	…   	3c… 	   	3c…	   	3c…	   	3c…		   	RV2 of the SB2 system	

51			   		   	IDS		   	56379.5190672		   	-7.3	   	±	   	0.6	   	16		   	±	   	1		   	K4V		   	4411	   	±	   	86  	   	4.61	   	±	   	0.15	   	0.04	   	±	   	0.11 	   	21		   	±	   	23		   			

51			   		   	IDS		   	56383.4744413		   	-156.9	   	±	   	0.6	   	15		   	±	   	1		   	K6V		   	4411	   	±	   	84  	   	4.61	   	±	   	0.14	   	0.03	   	±	   	0.11 	   	9		   	±	   	21		   	Likely wrong RV	

51			   		   	IDS		   	56384.5122070		   	-147.5	   	±	   	0.9	   	15		   	±	   	1		   	K5V		   	4355	   	±	   	77 	   	4.61	   	±	   	0.11 	   	0.04	   	±	   	0.11 	   	3		   	±	   	23		   	Likely wrong RV	

51			   		   	IDS		   	56707.6040424		   	-8.3	   	±	   	0.5	   	16		   	±	   	1		   	K5V		   	4378	   	±	   	64		   	4.61	   	±	   	0.10	   	0.04	   	±	   	0.11	   	23		   	±	   	14		   			

52			   		   	IDS		   	56379.4905068		   	-47.0	   	±	   	1.2	   	56		   	±	   	7		   	G1.5Vb	   	5653	   	±	   	111 	   	3.90	   	±	   	0.19	   	-0.06	   	±	   	0.12	   	5		   	±	   	21		   	SB1		

52			   		   	IDS		   	56707.6221921		   	-26.6	   	±	   	0.8	   	48		   	±	   	1		   	G2V		   	5600	   	±	   	92		   	4.20	   	±	   	0.17	   	-0.00		   	±	   	0.12	   	76		   	±	   	16		   	SB1		

70			   		   	IDS		   	55080.3799252		   	-11.1	   	±	   	1.9	   	15		   	±	   	16		   	M2.5V	   	3624	   	±	   	55		   	4.52	   	±	   	0.23	   	-0.14	   	±	   	0.11	   	53	   	±	   	69	   	SB1?	

70			   		   	IDS		   	55081.3663773		   	-16.4	   	±	   	1.7	   	17		   	±	   	6		   	M2V		   	3607	   	±	   	50		   	4.60	   	±	   	0.15	   	-0.14	   	±	   	0.11	   	25	   	±	   	55	   	SB1?	

71			   		   	IDS		   	55084.3544051		   	2.1	   	±	   	0.5	   	15		   	±	   	1		   	K5V		   	4514	   	±	   	93		   	4.36	   	±	   	0.17	   	-0.07	   	±	   	0.11	   	7	   	±	   	29	   		

73			   		   	IDS		   	55081.3839854		   	-8.2	   	±	   	2.8	   	289	   	±	   	5		   	M1.5V	   	3666	   	±	   	76		   	3.30	   	±	   	0.32	   	-0.13	   	±	   	0.11	   	23	   	±	   	66	   	Double-peaked Hα profile (SB2?)	

76			   		   	IDS		   	55083.3602331		   	-2.9	   	±	   	1.3	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

76			   		   	IDS		   	55083.3602331		   	-69.5	   	±	   	4.9	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

77			   		   	IDS		   	55082.3663651		   	37.2	   	±	   	2.1	   	90		   	±	   	4		   	G8IV		   	5431	   	±	   	101	   	3.91	   	±	   	0.10	   	-0.01	   	±	   	0.11	   	7	   	±	   	28	   	Slight asymmetry of CCF profile (SB2?)	

78			   		   	IDS		   	56379.6028405		   	-245.7	   	±	   	2.6	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	Clear asymmetry in the CCF profile, SB2 with blended peaks, no Li, Wrong RV?		

78			   		   	IDS		   	56707.7128193		   	9.0	   	±	   	2.2	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	Slight asymmetry of CCF profile	

78			   		   	IDS		   	56708.6577932		   	-64.9	   	±	   	1.2	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	Clear asymmetry in the CCF profile, SB2 with blended peaks, no Li		

79			   		   	IDS		   	56379.6260616		   	-97.1	   	±	   	3.3	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1  of an SB2 system		

79			   		   	IDS		   	56379.6260616		   	-15.1	   	±	   	12.0	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2  of an SB2 system		

80			   		   	IDS		   	55081.4025855		   	-26.9	   	±	   	2.3	   	25		   	±	   	7		   	M2V		   	3623	   	±	   	55		   	4.55	   	±	   	0.22	   	-0.13	   	±	   	0.11	   	7	   	±	   	69	   		

81			   	c1	   	IDS		   	55084.3799811		   	-9.7	   	±	   	1.1	   	15		   	±	   	9		   	M2V		   	3650	   	±	   	116	   	4.59	   	±	   	0.16	   	-0.13	   	±	   	0.11	   	29	   	±	   		79	   		

81			   	c2	   	IDS		   	55084.3799811		   	-10.5	   	±	   	1.1	   	15		   	±	   	9		   	M5V		   	3397	   	±	   	50		   	4.57	   	±	   	0.15	   	-0.15	   	±	   	0.11	   	20	   	±	   	80	   	Target = Gaia DR2 1723454381704389248	

82			   		   	FOCES	   	55109.2943862		   	20.22	   	±	   	0.21	   	21.1	   	±	   	1.3	   	G2V		   	5714	   	±	   	136	   	4.36	   	±	   	0.09	   	-0.01	   	±	   	0.08	   	10	   	±	   	17	   	 	

82			   		   	IDS		   	56379.6476301		   	18.3	   	±	   	1.2	   	26		   	±	   	6		   	G8V		   	5513	   	±	   	70		   	4.32	   	±	   	0.12	   	-0.12	   	±	   	0.13	   	2		   	±	   	26		   		

83			   		   	IDS		   	55081.4207273		   	-155.2	   	±	   	1.5	   	97		   	±	   	3		   	K5V		   	4597	   	±	   	85		   	4.14	   	±	   	0.24	   	-0.08	   	±	   	0.11	   	15	   	±	   	44	   		

84			   		   	FOCES	   	55109.3127430		   	-108.40	   	±	   	0.35	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1  of an SB2 system	

84			   		   	FOCES	   	55109.3127430		   	72.46	   	±	   	0.43	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2  of an SB2 system	

85			   		   	IDS		   	55083.3820091		   	-13.0	   	±	   	1.6	   	15		   	±	   	8		   	M5V		   	3397	   	±	   	50		   	4.57	   	±	   	0.15	   	-0.14	   	±	   	0.11	   	11	   	±	   	45	   		

86			   		   	FOCES	   	55109.3305934		   	-20.85	   	±	   	0.08	   	15.8	   	±	   	0.5	   	K0V		   	5220	   	±	   	125	   	4.28	   	±	   	0.14	   	-0.06	   	±	   	0.05	   	215	   	±	   	17	   	SB1?	

86			   		   	IDS		   	56382.6981631		   	-28.5	   	±	   	0.5	   	17		   	±	   	1		   	K1V		   	5264	   	±	   	104	   	4.13	   	±	   	0.26	   	-0.01	   	±	   	0.11	   	207		   	±	   	18		   	SB1?	

87			   		   	FOCES	   	55110.2941155		   	-17.89	   	±	   	0.16	   	19.4	   	±	   	0.6	   	G9.5IV	   	5138	   	±	   	151	   	3.79	   	±	   	0.31	   	-0.04	   	±	   	0.07	   	29		   	±	   	12		   			

87			   		   	FOCES	   	55110.2941155		   	-52.65	   	±	   	1.85	   	3c…		   	…   	3c…		   	3c…			   	3c…		   	3c…		   	Radial velocity of faint source in case of an SB2 system		

88			   		   	IDS		   	55083.4036979		   	8.9	   	±	   	3.3	   	17		   	±	   	3		   	M5V		   	3343	   	±	   	70		   	4.59	   	±	   	0.19	   	-0.14	   	±	   	0.11	   	42	   	±	   	35	   		

89			   		   	FOCES	   	55110.3164964		   	-70.42	   	±	   	0.37	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

89			   		   	FOCES	   	55110.3164964		   	64.74	   	±	   	0.41	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

90			   		   	IDS		   	55083.4284131		   	171.0		   	±	   	5.9		   	215	   	±	   	35		   	K7V		   	4685	   	±	   	207	   	3.19	   	±	   	0.43	   	-0.17	   	±	   	0.15	   	19	   	±	   	45	   		

91			   		   	FOCES	   	55110.3377116		   	1.51	   	±	   	0.20	   	21.8	   	±	   	1.3	   	K0IV		   	5051	   	±	   	125	   	3.65	   	±	   	0.40	   	-0.13	   	±	   	0.07	   	29	   	±	   	18	   		

92			   		   	FOCES	   	55110.3577589		   	24.78	   	±	   	0.68	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB3 system	

92			   		   	FOCES	   	55110.3577589		   	-8.04	   	±	   	0.39	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB3 system	

92			   		   	FOCES	   	55110.3577589		   	-47.79	   	±	   	0.99	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV3 of an SB3 system	

92			   		   	IDS		   	56382.6735452		   	2.3	   	±	   	3.2	   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…		   	RV1  of an SB2 system 	

92			   		   	IDS		   	56382.6735452		   	-56.4	   	±	   	7.6	   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…		   	RV2  of an SB2 system 	

92			   		   	IDS		   	56383.6233936		   	-80.0	   	±	   	3.6	   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…		   	RV1  of an SB3 system	

92			   		   	IDS		   	56383.6233936		   	45.3	   	±	   	0.6	   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…		   	RV2  of an SB3 system	

92			   		   	IDS		   	56383.6233936		   	-15.1	   	±	   	0.7	   	3c…		   	…   	3c…	   	3c…	   	3c…	   	3c…		   	RV3  of an SB3 system	

93			   		   	IDS		   	56379.6709380		   	-10.5	   	±	   	1.1	   	32		   	±	   	1		   	G2V		   	5565	   	±	   	12		   	4.32	   	±	   	0.11	   	-0.05	   	±	   	0.13	   	200		   	±	   	22		   		

94			   		   	FOCES	   	55110.3774734		   	-10.56	   	±	   	0.30	   	26.0	   	±	   	1.3	   	G2.5V	   	5775	   	±	   	92		   	4.17	   	±	   	0.10	   	0.11	   	±	   	0.05	   	24	   	±	   	26	   		

95			   		   	IDS		   	55081.4400960		   	-18.4	   	±	   	0.6	   	15		   	±	   	1		   	K5V		   	4540	   	±	   	83		   	4.30	   	±	   	0.30	   	-0.03	   	±	   	0.11	   	11	   	±	   	48	   		

96			   		   	FOCES	   	55110.3949910		   	-12.78	   	±	   	0.47	   	25.0	   	±	   	1.3	   	G1.5Vb	   	5881	   	±	   	173	   	4.19	   	±	   	0.11	   	-0.01	   	±	   	0.10	   	28	   	±	   	24	   		

97			   		   	FOCES	   	55110.4120357		   	3c…		   	286.6	   	±	   	14.0	   	sdF8		   	6128	   	±	   	413	   	3.99	   	±	   	0.15	   	-1.00	   	±	   	0.31	   	3c…		   		

98			   		   	IDS		   	55079.4387020		   	-30.8	   	±	   	0.5	   	40		   	±	   	1		   	K3V		   	4836	   	±	   	67  	   	4.01	   	±	   	0.29	   	0.04	   	±	   	0.11	   	119	   	±	   	34	   	Slight asymmetry of CCF profile (SB2?)	

99			   		   	FOCES	   	55109.3509585		   	-22.48	   	±	   	0.05	   	3.3	   	±	   	1.7	   	G9III		   	4835	   	±	   	102	   	2.80	   	±	   	0.23	   	-0.12	   	±	   	0.06	   	16	   	±	   	11	   		

100			   		   	IDS		   	55082.4133394		   	-15.6	   	±	   	0.6 	   	16		   	±	   	3		   	G1.5V	   	5940	   	±	   	142	   	4.13	   	±	   	0.11	   	-0.08	   	±	   	0.11	   	23	   	±	   	19	   		

101			   		   	IDS		   	55082.3933040		   	-19.6	   	±	   	0.5	   	15		   	±	   	1		   	K4V		   	4583	   	±	   	99  	   	4.36	   	±	   	0.20	   	-0.01	   	±	   	0.11	   	3	   	±	   	13	   		

102			   		   	IDS		   	55082.4621634		   	-24.0	   	±	   	0.7	   	27		   	±	   	3		   	K3V		   	4858	   	±	   	103	   	3.31	   	±	   	0.18	   	0.02	   	±	   	0.11	   	166	   	±	   	58	   		

103			   		   	IDS		   	55082.4492793		   	-10.7	   	±	   	0.8	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system, blended CCF peaks	

103			   		   	IDS		   	55082.4492793		   	-65.8	   	±	   	9.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system, blended CCF peaks	

104			   		   	FOCES	   	55109.3745146		   	-27.96	   	±	   	0.06	   	7.3	   	±	   	1.0	   	K1III-IV	   	4709	   	±	   	98		   	2.69	   	±	   	0.26	   	-0.02	   	±	   	0.07	   	17	   	±	   	14	   		

105			   		   	SOPHIE	   	55102.3700894		   	16.135	   	±	   	0.011	   	13.4	   	±	   	1.4	   	K0V		   	5350	   	±	   	94		   	4.49	   	±	   	0.10	   	-0.14	   	±	   	0.10	   	5	   	±	   	7	   	SB1	

105			   		   	FOCES	   	55107.4723974		   	-83.71	   	±	   	0.11	   	15.4	   	±	   	0.4	   	K1V		   	5193	   	±	   	100	   	4.43	   	±	   	0.20	   	-0.06	   	±	   	0.05	   	12	   	±	   	24	   	SB1	

106			   	c1	   	IDS		   	55084.4198646		   	-11.6	   	±	   	0.9	   	60		   	±	   	1		   	G5V		   	5444	   	±	   	108	   	3.92	   	±	   	0.13	   	-0.05	   	±	   	0.10	   	248	   	±	   	40	   		

106			   	c1	   	FOCES	   	55108.3093674		   	-10.44	   	±	   	0.90	   	63.1	   	±	   	11.3	   	G5V		   	5439	   	±	   	218	   	4.25	   	±	   	0.37	   	-0.04	   	±	   	0.12	   	238		   	±	   	74		   		

106			   	c1	   	IDS		   	56383.6967227		   	-20.1	   	±	   	0.9	   	60		   	±	   	1		   	K1V		   	5259	   	±	   	82		   	4.29	   	±	   	0.21	   	-0.18	   	±	   	0.12	   	260	   	±	   	22		   		

106			   	c2	   	IDS		   	56383.6967227		   	-13.6	   	±	   	0.7	   	15		   	±	   	1		   	K0V		   	5187	   	±	   	69		   	3.99	   	±	   	0.16	   	0.02	   	±	   	0.11	   	28		   	±	   	93		   	Target = Gaia DR2 2248508292487691008	

107			   		   	IDS		   	55081.4609906		   	8.6	   	±	   	0.9	   	16		   	±	   	2		   	K7V		   	4080	   	±	   	139	   	4.54	   	±	   	0.15	   	-0.15	   	±	   	0.12	   	3	   	±	   	23	   		

108			   		   	IDS		   	55079.4549152		   	-30.6	   	±	   	0.3	   	15		   	±	   	1		   	K1III		   	4760	   	±	   	60		   	2.74	   	±	   	0.17	   	-0.03	   	±	   	0.11	   	25	   	±	   	13	   		

109			   		   	IDS		   	55084.4658235		   	-65.1	   	±	   	0.8	   	43		   	±	   	3		   	K1IV		   	4765	   	±	   	87		   	2.97	   	±	   	0.34	   	-0.09	   	±	   	0.11	   	96	   	±	   	27	   	Double-peaked Hα profile (SB2?)	

110			   		   	IDS		   	55084.4781905		   	-96.0	   	±	   	2.5	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

110			   		   	IDS		   	55084.4781905		   	59.4	   	±	   	2.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

110			   		   	IDS		   	55084.4781905		   	-35.0	   	±	   	21.0	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	Radial velocity of faint source in case of an SB3 system	

111			   		   	IDS		   	55083.4852060		   	-8.8	   	±	   	0.9	   	35		   	±	   	6		   	M2V		   	3676	   	±	   	74		   	4.64	   	±	   	0.16	   	-0.12	   	±	   	0.11	   	13	   	±	   	60	   		

112			   		   	FOCES	   	55110.4332919		   	-22.31	   	±	   	0.14	   	7.7	   	±	   	0.3	   	K1V		   	5118	   	±	   	80		   	4.40	   	±	   	0.15	   	-0.07	   	±	   	0.05	   	157	   	±	   	20	   		

112			   		   	IDS		   	56382.6854679		   	-25.2	   	±	   	0.7	   	15		   	±	   	1		   	K2.5V	   	4997	   	±	   	76		   	4.52	   	±	   	0.12	   	-0.05	   	±	   	0.11	   	158	   	±	   	13		   		

113			   		   	IDS		   	55084.5071613		   	-3.1	   	±	   	0.6	   	15		   	±	   	8		   	K7V		   	4151	   	±	   	120	   	4.53	   	±	   	0.15	   	-0.11	   	±	   	0.11	   	22	   	±	   	30	   		

114			   		   	FOCES	   	55109.3980335		   	-13.74	   	±	   	0.06	   	8.3	   	±	   	0.5	   	K3V		   	4813	   	±	   	91		   	4.35	   	±	   	0.21	   	0.02	   	±	   	0.06	   	29	   	±	   	10	   		

115			   		   	SOPHIE	   	55102.3938018		   	-11.178	   	±	   	0.007	   	9.6	   	±	   	0.9	   	G9.5IV	   	5125	   	±	   	187	   	4.01	   	±	   	0.42	   	-0.09	   	±	   	0.12	   	291	   	±	   	9	   		

115			   		   	FOCES	   	55108.3725324		   	-11.40	   	±	   	0.06	   	9.8	   	±	   	1.3	   	G9.5IV	   	5219	   	±	   	107	   	4.02	   	±	   	0.23	   	-0.02	   	±	   	0.07	   	290	   	±	   	16	   		

116			   		   	IDS		   	55082.4760161		   	-9.7	   	±	   	0.9	   	46		   	±	   	3		   	G8IV		   	5242	   	±	   	68		   	3.91	   	±	   	0.14	   	-0.10	   	±	   	0.11	   	112	   	±	   	25	   	Slight asymmetry of CCF profile (SB2?)	

117			   		   	IDS		   	55081.4803878		   	-65.7	   	±	   	0.7	   	15		   	±	   	1		   	K1III		   	4617	   	±	   	76		   	2.50	   	±	   	0.23	   	-0.07	   	±	   	0.11	   	8	   	±	   	35	   		

118			   		   	IDS		   	55079.4882147		   	-3.8	   	±	   	0.5	   	20		   	±	   	1		   	K5V		   	4628	   	±	   	146	   	3.96	   	±	   	0.25	   	-0.21	   	±	   	0.11	   	6	   	±	   	32	   		

119			   		   	IDS		   	55082.4935946		   	78.4	   	±	   	4.5	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

119			   		   	IDS		   	55082.4935946		   	-61.0	   	±	   	4.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

120			   		   	IDS		   	55084.5179598		   	-20.1	   	±	   	0.9	   	55		   	±	   	10		   	F8V		   	6061	   	±	   	81		   	4.01	   	±	   	0.13	   	-0.01	   	±	   	0.11	   	22	   	±	   	27	   		

121			   		   	IDS		   	55084.5687318		   	-24.4	   	±	   	0.5	   	16		   	±	   	3		   	M5V		   	3397	   	±	   	50		   	4.55	   	±	   	0.15	   	-0.14	   	±	   	0.11	   	0	   	±	   	54	   		

122			   		   	FOCES	   	55110.4532427		   	11.39	   	±	   	0.57	   	30.9	   	±	   	1.7	   	G2V		   	5708	   	±	   	146	   	4.30	   	±	   	0.16	   	0.02	   	±	   	0.10	   	41	   	±	   	20	   		

123			   		   	IDS		   	55079.4139454		   	-21.8	   	±	   	0.5	   	29		   	±	   	2		   	G2.5V	   	5685	   	±	   	116	   	3.96	   	±	   	0.14	   	-0.08	   	±	   	0.11	   	156	   	±	   	61	   		

123			   		   	IDS		   	55079.4221410		   	-23.0	   	±	   	0.3	   	24		   	±	   	2		   	G1.5bV	   	5647	   	±	   	94  	   	3.96	   	±	   	0.11	   	-0.09	   	±	   	0.11	   	195	   	±	   	31	   		

124			   		   	IDS		   	55083.5114570		   	-14.9	   	±	   	0.6	   	37		   	±	   	3		   	K7V		   	4261	   	±	   	166	   	4.48	   	±	   	0.17	   	-0.11	   	±	   	0.11	   	393	   	±	   	65	   		

124			   		   	IDS		   	55168.3269044		   	-12.1	   	±	   	0.7	   	37		   	±	   	3		   	K7V		   	4340	   	±	   	188	   	4.47	   	±	   	0.18	   	-0.12	   	±	   	0.11	   	430	   	±	   	81	   		

125			   		   	FOCES	   	55109.4220827		   	-21.44	   	±	   	0.09	   	13.4	   	±	   	1.5	   	K4V		   	5532	   	±	   	168	   	4.31	   	±	   	0.11	   	-0.01	   	±	   	0.07	   	181	   	±	   	37	   		

126			   		   	IDS		   	55084.5870534		   	37.8	   	±	   	0.6	   	30		   	±	   	1		   	K1V		   	5240	   	±	   	71		   	4.33	   	±	   	0.14	   	-0.07	   	±	   	0.11	   	47	   	±	   	16	   		

127			   		   	FOCES	   	55109.4465507		   	3c…		   	131.1	   	±	   	11.1	   	K1V		   	5212	   	±	   	296	   	4.42	   	±	   	0.35	   	-0.04	   	±	   	0.15	   	177	   	±	   	86	   		

128			   		   	SOPHIE	   	55102.4157992		   	-18.752	   	±	   	0.009	   	7.46	   	±	   	2.16	   	G1V		   	5682	   	±	   	131	   	4.28	   	±	   	0.19	   	-0.34	   	±	   	0.16	   	38	   	±	   	7	   	RV1 of a possible SB3 system	

128			   		   	SOPHIE	   	55102.4157992		   	41.8	   	±	   	0.9	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 in case of an SB3 system	

128			   		   	SOPHIE	   	55102.4157992		   	-72.3	   	±	   	0.9	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV3 in case of an SB3 system	

128			   		   	FOCES	   	55109.4719452		   	-19.14	   	±	   	0.09	   	10.5	   	±	   	1.3	   	G1V		   	5863	   	±	   	78		   	4.23	   	±	   	0.05	   	-0.05	   	±	   	0.08	   	62	   	±	   	13	   	RV1 of a possible SB3 system	

128			   		   	FOCES	   	55109.4719452		   	-46.36	   	±	   	0.75	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 in case of an SB3 system	

128			   		   	FOCES	   	55109.4719452		   	12.91	   	±	   	0.96	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV3 in case of an SB3 system	

129			   		   	FOCES	   	55109.4972983		   	-20.53	   	±	   	0.50	   	47.5	   	±	   	1.8	   	G1.5Vb	   	5799	   	±	   	163	   	4.23	   	±	   	0.11	   	0.00	   	±	   	0.11	   	147	   	±	   	35	   		

130			   		   	FOCES	   	55109.5207365		   	3c…		   	106.0	   	±	   	4.7	   	K2V		   	5069	   	±	   	244	   	4.40	   	±	   	0.34	   	-0.08	   	±	   	0.10	   	244	   	±	   	88	   		

131			   		   	FOCES	   	55109.5436838		   	-29.57	   	±	   	0.15	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

131			   		   	FOCES	   	55109.5436838		   	-3.04	   	±	   	0.23	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

132			   		   	IDS		   	55079.4708973		   	42.1	   	±	   	0.4	   	15		   	±	   	1		       K0III-IV	   	4824	   	±	   	68		   	3.21	   	±	   	0.21	   	-0.13	   	±	   	0.12	   	47	   	±	   	22	   		

133			   		   	SOPHIE	   	55102.4856691		   	25.297	   	±	   	0.007	   	11.9	   	±	   	0.8	   	K0III		   	4500	   	±	   	200	   	2.15	   	±	   	0.74	   	-0.29	   	±	   	0.22	   	77	   	±	   	10	   	SB1	

133			   		   	FOCES	   	55108.3992783		   	-18.49	   	±	   	0.08	   	11.7	   	±	   	0.7	   	K1IV		   	4761	   	±	   	131	   	2.96	   	±	   	0.43	   	-0.01	   	±	   	0.09	   	68	   	±	   	16	   	SB1	

134			   		   	IDS		   	55084.6008565		   	-4.8	   	±	   	0.8	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

134			   		   	IDS		   	55084.6008565		   	-62.8	   	±	   	6.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

135			   		   	IDS		   	55081.5434654		   	-37.3	   	±	   	0.7	   	30		   	±	   	1		   	K3V		   	4658	   	±	   	108	   	3.17	   	±	   	0.25	   	-0.06	   	±	   	0.11	   	29	   	±	   	27	   		

136			   		   	IDS		   	55079.5087978		   	-7.2	   	±	   	0.6 	   	15		   	±	   	1		   	K5V		   	4542	   	±	   	130	   	3.83	   	±	   	0.19	   	-0.07	   	±	   	0.10	   	44	   	±	   	26	   		

137			   		   	FOCES	   	55108.4214544		   	3c…	   	262.8	   	±	   	26.7	   	G1IV		   	5729	   	±	   	612	   	4.12	   	±	   	0.36	   	-0.16	   	±	   	0.25	   	3c…		   		

138			   	c1	   	IDS		   	55083.5351512		   	-69.3	   	±	   	0.7	   	15		   	±	   	1		   	K1III		   	4602	   	±	   	102	   	2.40	   	±	   	0.22	   	-0.09	   	±	   	0.12	   	18		   	±	   	19		   		

138			   	c1	   	IDS		   	55168.3536372		   	-70.2	   	±	   	0.4	   	15		   	±	   	1		   	K1III		   	4601	   	±	   	126	   	2.31	   	±	   	0.21	   	-0.09	   	±	   	0.11	   	25		   	±	   	38		   		

138			   	c2	   	IDS		   	55168.3536372		   	3c…	   	3c…	   	A9IV		   	7260	   	±	   	137	   	3.77	   	±	   	0.18	   	-0.13	   	±	   	0.16	   	62		   	±	   	82		   	Fast rotator, Target = Gaia DR2 2203366330791767552	

139			   		   	IDS		   	55168.3747409		   	3c…	   	3c…	   	A6V		   	7956	   	±	   	219	   	3.97	   	±	   	0.12	   	0.11	   	±	   	0.14	   	3c…		   	Fast rotator	

140			   	c1	   	IDS		   	55082.5169938		   	-16.3	   	±	   	0.6	   	15		   	±	   	1		   	K4V		   	4823	   	±	   	56		   	3.83	   	±	   	0.34	   	-0.05	   	±	   	0.11	   	37	   	±	   	62	   		

140			   	c2	   	IDS		   	55082.5169938		   	-17.5	   	±	   	1.6	   	28		   	±	   	9		   	G1V		   	5268	   	±	   	168	   	3.93	   	±	   	0.25	   	-0.06	   	±	   	0.11	   	21	   	±	   	43	   	Target = Gaia DR2 2005807146670408704	

141			   		   	FOCES	   	55108.4399839		   	60.85	   	±	   	0.07	   	11.3	   	±	   	1.5	   	K0V		   	5304	   	±	   	90		   	4.26	   	±	   	0.11	   	-0.06	   	±	   	0.05	   	16	   	±	   	12	   		

142			   		   	IDS		   	55081.5039811		   	-9.7	   	±	   	0.5	   	25		   	±	   	1		   	K3V		   	4828	   	±	   	56		   	4.30	   	±	   	0.18	   	-0.10	   	±	   	0.11	   	445	   	±	   	36	   		

142			   		   	IDS		   	55082.6200845		   	-8.4	   	±	   	0.6	   	23		   	±	   	2		   	K5V		   	4837	   	±	   	84		   	4.09	   	±	   	0.26	   	-0.10	   	±	   	0.12	   	419	   	±	   	57	   		

143			   		   	IDS		   	55081.5219193		   	-17.2	   	±	   	1.1	   	15		   	±	   	1		   	K8V		   	4166	   	±	   	127	   	4.53	   	±	   	0.15	   	-0.11	   	±	   	0.11	   	4	   	±	   	62	   		

144			   		   	FOCES	   	55108.4588134		   	20.90	   	±	   	0.08	   	15.7	   	±	   	0.6	   	K0V		   	5325	   	±	   	140	   	4.36	   	±	   	0.13	   	-0.13	   	±	   	0.07	   	35	   	±	   	11	   		

145			   		   	FOCES	   	55108.4772190		   	-31.43	   	±	   	0.06	   	11.5	   	±	   	0.3	   	K0IV		   	4975	   	±	   	114	   	3.28	   	±	   	0.45	   	-0.08	   	±	   	0.06	   	66	   	±	   	9	   		

146			   		   	IDS		   	55079.5256864		   	-47.9	   	±	   	1.2 	   	24		   	±	   	10		   	M3V		   	3659	   	±	   	70		   	4.64	   	±	   	0.15	   	-0.12	   	±	   	0.11	   	77	   	±	   	64	   		

147			   		   	IDS		   	55082.5508470		   	77.2	   	±	   	1.6	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1  of an SB2 system	

147			   		   	IDS		   	55082.5508470		   	-24.5	   	±	   	3.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2  of an SB2 system	

148			   		   	SOPHIE	   	55101.6074655		   	-17.543	   	±	   	0.011	   	6.9	   	±	   	1.0	   	F6IV		   	6075	   	±	   	198	   	3.84	   	±	   	0.18	   	-0.23	   	±	   	0.20	   	3	   	±	   	4	   		

149			   		   	FOCES	   	55109.5981177		   	3c…		   	102.8	   	±	   	15.6	   	K1V		   	5823	   	±	   	397	   	4.14	   	±	   	0.19	   	-0.08	   	±	   	0.22	   	146	   	±	   	71	   		

150			   		   	FOCES	   	55109.5706683		   	-13.43	   	±	   	0.48	   	42.8	   	±	   	3.3	   	G0V		   	5645	   	±	   	221	   	4.18	   	±	   	0.26	   	0.03	   	±	   	0.11	   	208	   	±	   	47	   		

151			   		   	FOCES	   	55110.4837770		   	-23.22	   	±	   	0.22	   	9.5	   	±	   	2.4	   	K7V		   	4354	   	±	   	79		   	4.47	   	±	   	0.18	   	-0.13	   	±	   	0.07	   	44	   	±	   	18	   		

152			   		   	IDS		   	55081.5570883		   	-8.8	   	±	   	0.9	   	30		   	±	   	1		   	K5V		   	4760	   	±	   	126	   	4.13	   	±	   	0.28	   	-0.09	   	±	   	0.11	   	428	   	±	   	98	   	Slight asymmetry of CCF profile (SB2?)	

153			   		   	SOPHIE	   	55101.4924232		   	-13.599	   	±	   	0.202	   	64.8	   	±	   	3.2	   	K2V		   	5050	   	±	   	76		   	4.57	   	±	   	0.06	   	-0.21	   	±	   	0.03	   	432	   	±	   	34	   	SB1	

153			   		   	FOCES	   	55107.5049149		   	-5.20	   	±	   	0.89	   	63.4	   	±	   	3.9	   	K3V		   	4837	   	±	   	217	   	4.57	   	±	   	0.51	   	-0.04	   	±	   	0.11	   	432	   	±	   	65	   	SB1	

153			   		   	FOCES	   	55108.5236282		   	-7.99	   	±	   	0.66	   	65.1	   	±	   	3.1	   	K3V		   	4831	   	±	   	192	   	4.54	   	±	   	0.63	   	-0.02	   	±	   	0.10	   	463	   	±	   	56	   	SB1	

154			   		   	IDS		   	55083.6251829		   	-75.8	   	±	   	1.3	   	39		   	±	   	8		   	M2V		   	3725	   	±	   	68		   	4.65	   	±	   	0.14	   	-0.12	   	±	   	0.11	   	12	   	±	   	43	   	SB1	

154			   		   	IDS		   	55168.4203365		   	-22.0	   	±	   	1.9	   	47		   	±	   	14		   	M0V		   	3789	   	±	   	78		   	4.65	   	±	   	0.15	   	-0.11	   	±	   	0.10	   	23	   	±	   	92	   	SB1	

155			   		   	IDS		   	55082.5984520		   	-10.8	   	±	   	0.8	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB3 system	

155			   		   	IDS		   	55082.5984520		   	-85.9	   	±	   	1.1	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB3 system	

155			   		   	IDS		   	55082.5984520		   	80.3	   	±	   	4.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV3 of an SB3 system	

156			   		   	IDS		   	55081.6114206		   	-10.7	   	±	   	1.1	   	15		   	±	   	1		   	K7V		   	4245	   	±	   	161	   	4.42	   	±	   	0.28	   	-0.17	   	±	   	0.12	   	473	   	±	   	53	   	Likely SB1 system	

156			   		   	IDS		   	55083.6014848		   	-4.6	   	±	   	0.6	   	15		   	±	   	8		   	K7V		   	4356	   	±	   	98		   	4.38	   	±	   	0.27	   	-0.11	   	±	   	0.11	   	457	   	±	   	40	   	Likely SB1 system	

157			   		   	SOPHIE	   	55101.5735636		   	-10.958	   	±	   	0.007	   	7.8	   	±	   	0.7	   	G5V		   	5649	   	±	   	149	   	4.24	   	±	   	0.18	   	0.02	   	±	   	0.12	   	52	   	±	   	7	   		

158			   		   	SOPHIE	   	55101.5440024		   	-8.209	   	±	   	0.015	   	25.0	   	±	   	1.0	   	K1V		   	5089	   	±	   	74		   	4.38	   	±	   	0.37	   	-0.09	   	±	   	0.09	   	331	   	±	   	16	   		

158			   		   	FOCES	   	55109.6300243		   	-8.91	   	±	   	0.22	   	25.6	   	±	   	1.0	   	K2V		   	5084	   	±	   	71		   	4.41	   	±	   	0.23	   	-0.07	   	±	   	0.05	   	357	   	±	   	35	   		

159			   		   	IDS		   	55080.6631020		   	-24.5	   	±	   	1.5	   	32		   	±	   	6		   	G8III		   	4998	   	±	   	100	   	3.30	   	±	   	0.22	   	-0.12	   	±	   	0.12	   	56		   	±	   	26		   		

159			   		   	IDS		   	55081.6316086		   	-58.7	   	±	   	1.2	   	30		   	±	   	1		   	K0IV		   	4800	   	±	   	85		   	3.32	   	±	   	0.22	   	-0.13	   	±	   	0.11	   	117		   	±	   	55		   	 	

159			   		   	IDS		   	55081.6316086		   	59.4	   	±	   	8.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	Radial velocity of faint source in case of an SB2 system 	

159			   		   	IDS		   	55081.6476659		   	-59.1	   	±	   	0.9	   	28		   	±	   	2		   	K2V		   	5055	   	±	   	102	   	3.62	   	±	   	0.24	   	-0.19	   	±	   	0.12	   	98		   	±	   	64		   		

159			   		   	IDS		   	55081.6476659		   	67.0	   	±	   	9.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	Radial velocity of faint source in case of an SB2 system 	

161			   		   	IDS		   	55083.5823330		   	-6.9	   	±	   	1.2	   	15		   	±	   	9		   	M2V		   	3607	   	±	   	50		   	4.60	   	±	   	0.15	   	-0.13	   	±	   	0.11	   	66	   	±	   	67	    		

161			   		   	IDS		   	55168.3958781		   	-8.8	   	±	   	1.8	   	16		   	±	   	13		   	M2V		   	3606	   	±	   	50		   	4.61	   	±	   	0.15	   	-0.13	   	±	   	0.11	   	66	   	±	   	67	   		

162			   		   	IDS		   	55084.6344091		   	43.7	   	±	   	2.2	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1  of an SB2 system	

162			   		   	IDS		   	55084.6344091		   	-62.3	   	±	   	2.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2  of an SB2 system	

163			   	c1	   	IDS		   	55524.4297626		   	-45.3	   	±	   	0.6	   	32		   	±	   	2		   	G8IV		   	5529	   	±	   	68		   	3.80	   	±	   	0.16	   	-0.02	   	±	   	0.11	   	35	   	±	   	19	   	Slight asymmetry of CCF profile (SB2?)       

163			   	c2	   	IDS		   	55524.4297626		   	-4.3	   	±	   	2.3	   	275	   	±	   	11 	   	F2IV		   	6740	   	±	   	103	   	4.26	   	±	   	0.11	   	-0.03	   	±	   	0.11	   	2	   	±	   	41	         Target = Gaia DR2 537608345003955840	     

164			   		   	IDS		   	56227.5352424		   	-9.9	   	±	   	1.1	   	3c…		   	…   	3c…		   	3c…	   	3c…	   	3c…		   	RV1 of an SB2 system	

164			   		   	IDS		   	56227.5352424		   	84.2	   	±	   	4.0	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system		

165			   		   	IDS		   	55525.4337780		   	-32.1	   	±	   	2.5	   	93		   	±	   	12		   	F3IV		   	6753	   	±	   	100	   	4.13	   	±	   	0.11	   	0.00	   	±	   	0.10	   	61	   	±	   	43	   		

166			   		   	IDS		   	55525.4543251		   	-2.6	   	±	   	1.3	   	80		   	±	   	4		   	G5III		   	5576	   	±	   	87		   	3.81	   	±	   	0.15	   	0.02	   	±	   	0.10	   	51	   	±	   	26	   	Slight asymmetry of CCF profile (SB2?)	

167			   		   	IDS		   	55525.4693819		   	45.1	   	±	   	1.4	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

167			   		   	IDS		   	55525.4693819		   	-29.1	   	±	   	5.6	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

168			   	c1	   	IDS		   	55525.4910577		   	-11.6	   	±	   	0.8	   	15		   	±	   	1		   	F8V		   	6059	   	±	   	97		   	4.05	   	±	   	0.13	   	0.03	   	±	   	0.11	   	78		   	±	   	94		   		

168			   	c1	   	IDS		   	55528.4448003		   	-6.0	   	±	   	1.0	   	15		   	±	   	8		   	F8V		   	5679	   	±	   	121	   	3.94	   	±	   	0.13	   	-0.10	   	±	   	0.14	   	16		   	±	   	189		   		

168			   	c1	   	IDS		   	55528.4898928		   	-7.9	   	±	   	0.4	   	15		   	±	   	7		   	G1.5bV	   	5844	   	±	   	79		   	4.03	   	±	   	0.14	   	-0.10	   	±	   	0.11	   	17		   	±	   	24		   		

168			   	c2	   	IDS		   	55525.4910577		   	-38.5	   	±	   	1.4	   	39		   	±	   	28		   	G3V		   	5812	   	±	   	184	   	3.95	   	±	   	0.12	   	-0.17	   	±	   	0.13	   	90		   	±	   	250		   	Target = Gaia DR2 534835788997551488		

168			   	c2	   	IDS		   	55528.4898928		   	-37.5	   	±	   	0.6	   	26		   	±	   	20		   	F8IV		   	5906	   	±	   	150	   	3.98	   	±	   	0.13	   	-0.24	   	±	   	0.12	   	65		   	±	   	44		   	Target = Gaia DR2 534835788997551488		

169			   	c1	   	IDS		   	55524.5177831		   	26.2	   	±	   	1.9	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

169			   	c1	   	IDS		   	55524.5177831		   	-33.7	   	±	   	2.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

169			   	c1	   	IDS		   	55528.5188044		   	1.1	   	±	   	0.7	   	50		   	±	   	4		   	G0V		   	5960	   	±	   	76		   	4.05	   	±	   	0.15	   	0.00	   	±	   	0.11	   	44		   	±	   	32		   	SB2 with blended peaks	

169			   	c1	   	SOPHIE	   	55589.3272880		   	9.750		   	±	   	0.005		   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

169			   	c1	   	SOPHIE	   	55589.3272880		   	-16.5		   	±	   	1.8		   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

169			   	c1	   	IDS		   	56613.5135269		   	-24.1	   	±	   	1.7	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV1 of an SB2 system	

169			   	c1	   	IDS		   	56613.5135269		   	30.5	   	±	   	4.1	   	3c…	   	…   	3c…	   		3c…	   		3c…	   	3c…	   	RV2 of an SB2 system	

169			   	c2	   	IDS		   	55524.5177831		   	-20.6	   	±	   	0.6	   	18		   	±	   	5		   	F7IV		   	5961	   	±	   	94		   	4.01	   	±	   	0.13	   	-0.10	   	±	   	0.11	   	32		   	±	   	35		   	Target = Gaia DR2 533784174844087168		

174			   	c1	   	IDS		   	56380.7696598		   	3.5	   	±	   	3.9	   	120	   	±	   	5		   	K0IV		   	5300	   	±	   	77		   	4.26	   	±	   	0.17	   	-0.11	   	±	   	0.13	   	273		   	±	   	53		   		

174			   	c2	   	IDS		   	56380.7696598		   	-30.7	   	±	   	0.7	   	43		   	±	   	16		   	F4V		   	6575	   	±	   	82		   	4.01	   	±	   	0.12	   	-0.15	   	±	   	0.11	   	0		   	±	   	30		   	Target = Gaia DR2 2291000598671699200	

179			   		   	IDS		   	56381.7515829		   	-147.8	   	±	   	0.8	   	32		   	±	   	2		   	K1V		   	5181	   	±	   	67	   	3.98	   	±	   	0.19		   	-0.14	   	±	   	0.11	   	236		   	±	   	31		   	Likely wrong RV	

182			   		   	IDS		   	55525.3646672		   	-11.4	   	±	   	0.5	   	15		   	±	   	1		   	K5V		   	4464	   	±	   	119	   	4.28	   	±	   	0.30	   	-0.10	   	±	   	0.12	   	441	   	±	   	39	   		

184			   	c1	   	IDS		   	56227.4707076		   	-5.0	   	±	   	0.7	   	19		   	±	   	2		   	K0V		   	5110	   	±	   	67		   	4.33	   	±	   	0.10	   	0.02	   	±	   	0.11	   	316		   	±	   	36		   	SB1?	

184			   	c1	   	IDS		   	56384.7604811		   	-10.0	   	±	   	0.7	   	18		   	±	   	1		   	K2.5V	   	5096	   	±	   	71		   	3.96	   	±	   	0.32	   	-0.01	   	±	   	0.11	   	335		   	±	   	42		   	SB1?		

184			   	c2	   	IDS		   	56227.4707076		   	-98.8	   	±	   	0.9	   	15		   	±	   	1		   	K5III		   	3977	   	±	   	79		   	1.30	   	±	   	0.26	   	-0.10	   	±	   	0.11	   	56		   	±	   	76		   	Target = Gaia DR2 2206637339215351936	

184			   	c2	   	IDS		   	56384.7604811		   	-104.4	   	±	   	1.0	   	15		   	±	   	8		   	K3.5IIIb	   	3949	   	±	   	68		   	1.14	   	±	   	0.20	   	-0.10	   	±	   	0.11	   	51		   	±	   	79		   	Target = Gaia DR2 2206637339215351936		

185			   	c1	   	IDS		   	56226.4549371		   	-16.4	   	±	   	0.7	   	15		   	±	   	8		   	K0III		   	4664	   	±	   	83		   	2.61	   	±	   	0.22	   	-0.08	   	±	   	0.13	   	326		   	±	   	29		   			

185			   	c2	   	IDS		   	56226.4549371		   	-55.4	   	±	   	0.8	   	15		   	±	   	8		   	G8IV-V	   	5232	   	±	   	90		   	3.78	   	±	   	0.17	   	-0.07	   	±	   	0.12	   	0		   	±	   	98		   	Target = Gaia DR2 2226453257466755328		

186			   		   	IDS		   	56226.4757748		   	-3.8	   	±	   	0.7	   	19		   	±	   	2		   	K2V		   	5085	   	±	   	79		   	4.50	   	±	   	0.12	   	-0.07	   	±	   	0.12	   	349		   	±	   	24		   		

188			   		   	IDS		   	56226.4922890		   	-11.1	   	±	   	0.7	   	15		   	±	   	7		   	K1V	   	5242	   	±	   	83			   	4.25	   	±	   	0.20	   	-0.07	   	±	   	0.12	   	255		   	±	   	18		   		

189			   		   	IDS		   	56226.5114830		   	-5.6	   	±	   	0.7	   	17		   	±	   	1		   	K4V	   	4503	   	±	   	86			   	4.62	   	±	   	0.10	   	0.01	   	±	   	0.10	   	360		   	±	   	31		   		

191			   	c1	   	IDS		   	56227.4891806		   	-7.6	   	±	   	0.8	   	16		   	±	   	1		   	K7V		   	4066	   	±	   	72		   	4.63	   	±	   	0.10	   	-0.06	   	±	   	0.12	   	551		   	±	   	41		   		

191			   	c2	   	IDS		   	56227.4891806		   	-7.1	   	±	   	1.3	   	24		   	±	   	7		   	M1.0V	   	3701	   	±	   	81		   	4.69	   	±	   	0.13	   	-0.15	   	±	   	0.11	   	540		   	±	   	95		   	Target = Gaia DR2 2231866565525667712	

192			   		   	IDS		   	56225.4960186		   	-10.3	   	±	   	0.8	   	38		   	±	   	2		   	K2V		   	5039	   	±	   	85		   	4.48	   	±	   	0.14	   	-0.06	   	±	   	0.10	   	313		   	±	   	40		   		

193			   		   	FOCES	   	55168.4199992		   	-7.58	   	±	   	0.39	   	11.0	   	±	   	1.0	   	K1V		   	5172	   	±	   	100	   	4.27	   	±	   	0.22	   	-0.06	   	±	   	0.06	   	305	   	±	   	48	   		

193			   		   	IDS		   	55524.4053541		   	-7.6	   	±	   	0.5	   	15		   	±	   	1		   	K2V		   	5142	   	±	   	68		   	4.20	   	±	   	0.21	   	-0.10	   	±	   	0.10	   	296	   	±	   	21	   		

G1			   		   	IDS		   	55079.5501320		   	-11.2	   	±	   	0.4	   	32		   	±	   	4		   	G1V 		   	5561	   	±	   	77		   	4.27	   	±	   	0.12	   	-0.07	   	±	   	0.11	   	210	   	±	   	38	   		

G1			   		   	SOPHIE	   	55102.4611823		   	-7.932	   	±	   	0.008	   	29.2		   	±	   	1.0	   	G2V		   	5711	   	±	   	139	   	4.40		   	±	   	0.11	   	-0.04		   	±	   	0.05	   	208		   	±	   	20		   	 	

G1			   		   	FOCES	   	55108.5564041		   	-8.90	   	±	   	0.19	   	30.6		   	±	   	0.7	   	G2V		   	5696	   	±	   	158	   	4.33		   	±	   	0.13	   	0.00		   	±	   	0.07	   	211		   	±	   	24		   	 	

G1			   		   	FOCES	   	55110.5085252		   	-8.38	   	±	   	0.49	   	30.6		   	±	   	0.8	   	G2V		   	5757	   	±	   	128	   	4.32		   	±	   	0.11	   	0.03		   	±	   	0.09	   	207		   	±	   	27		   	 	

G3			   	c1	   	IDS		   	55079.5690304		   	-9.3	   	±	   	0.3	   	15		   	±	   	1	   	K1V	   	5105		   	±	   	56	   	4.28		   	±	   	0.18	   	-0.09		   	±	   	0.10
    310   ±   22   
    
    G3			   	c1	   	SOPHIE	   	55102.4410682		   -8.977   ±   0.009   12.0   ±   1.0   	K1V		   5108   ±   81   4.12   ±   0.49   -0.07   ±   0.10   316   ±   12   
    
    G3			   	c1	   	FOCES	   	55108.5807998		   -9.14   ±   0.09   12.3   ±   0.5   	K1V		   5145   ±   96   4.39   ±   0.22   -0.05   ±   0.04   303   ±   19   
    
    G3			   	c1	   	FOCES	   	55110.5331687		   -9.33   ±   0.15   13.3   ±   1.4   	K0V		   5148   ±   159   4.30   ±   0.32   -0.05   ±   0.07   289   ±   37   
    
    G3			   	c1	   	IDS		   	55525.4020459		   -8.5   ±   0.4   15   ±   1   	K2V		   5143   ±   69   4.23   ±   0.18   -0.08   ±   0.10   316   ±   26   
    
    G3			   	c2	   	IDS		   	55525.4020459		   -8.7   ±   0.7   32   ±   3   	K7V		   4262   ±   166   4.49   ±   0.17   -0.11   ±   0.11   453   ±   90   	Target = Gaia DR2 564698451789359104	
    
    G4			      	IDS		   	55079.5781353		   -9.8   ±   0.3   3c…   …   3c…   3c…   3c…   3c…   	SB2 with blended peaks	
    
    G4			      	IDS		   	55080.6849896		   -10.3   ±   0.9   3c…   …   3c…   3c…   3c…   3c…   	SB2 with blended peaks	
    
    G4			      	IDS		   	55081.5941743		   -29.1   ±   1.8   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system 	
    
    G4			      	IDS		   	55081.5941743		   15.9   ±   1.9   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	IDS		   	55082.6486286		   -35.8   ±   2.0   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system	
    
    G4			      	IDS		   	55082.6486286		   17.1   ±   2.0   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	IDS		   	55083.6483453		   19.5   ±   2.1   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system 	
    
    G4			      	IDS		   	55083.6483453		   -41.5   ±   2.3   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	IDS		   	55084.6542722		   -43.6   ±   2.2   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system 	
    
    G4			      	IDS		   	55084.6542722		   24.5   ±   2.3   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	SOPHIE	   	55101.5200320		   -46.449   ±   0.013   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system	
    
    G4			      	SOPHIE	   	55101.5200320		   28.267   ±   0.013   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	FOCES	   	55107.5591610		   -30.69   ±   0.29   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system	
    
    G4			      	FOCES	   	55107.5591610		   11.91   ±   0.30   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	FOCES	   	55108.5935676		   -27.41   ±   0.17   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system	
    
    G4			      	FOCES	   	55108.5935676		   8.31   ±   0.18   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	FOCES	   	55109.6618153		   -24.63   ±   0.21   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system	
    
    G4			      	FOCES	   	55109.6618153		   5.99   ±   0.22   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	FOCES	   	55110.5460213		   3.83   ±   0.34   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system	
    
    G4			      	FOCES	   	55110.5460213		   -23.22   ±   0.33   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    
    G4			      	FOCES	   	55168.3934106		   33.80   ±   0.55   3c…   …   3c…   3c…   3c…   3c…   RV1 of an SB2 system	
    
    G4			      	FOCES	   	55168.3934106		   -51.59   ±   0.60   3c…   …   3c…   3c…   3c…   3c…   RV2 of an SB2 system	
    ^⋆ During one IDS observation, several apertures might be visible on the cuts perpendicular to the spectral direction. In such a case, 
     we ranked the sources in reverse order to their maximum intensity (i.e., “c1” = the brightest one).
    lr@c@l@r@c@l@r@c@l@r@c@lr@c@l@r@c@l@r@c@lr@c@l@r@c@l@r@c@lr@c@lclGalactic positions and space velocities of the targets, along with the astrometry in Gaia DR2, and the average RV values and lithium equivalent widths obtained during our survey.
    1c#^⋆   3cπ   3cμ_αcosδ   3cμ_δ   3c⟨ RV ⟩   3cX   3cY   3cZ   3cU_   3cV_   3cW_   3c⟨ W_ Li⟩   	A_v    Note	
       3c[mas]   3c[mas yr^-1]   3c[mas yr^-1]   3c[km s^-1]   3c[pc]   3c[pc]   3c[pc]   3c[km s^-1]   3c[km s^-1]   3c[km s^-1]   3c[mÅ]    [mag]	   
    Continued.
    1c#^⋆   3cπ   3cμ_αcosδ   3cμ_δ   3c⟨ RV ⟩   3cX   3cY   3cZ   3cU_   3cV_   3cW_   3c⟨ W_ Li⟩   	A_v    Note	
       3c[mas]   3c[mas yr^-1]   3c[mas yr^-1]   3c[km s^-1]   3c[pc]   3c[pc]   3c[pc]   3c[km s^-1]   3c[km s^-1]   3c[km s^-1]   3c[mÅ]    [mag]	   
    
    1		   0.3580   ±   0.0294   -4.088   ±   0.043   -3.706   ±   0.041   2.2   ±   0.3   1210   ±   100   2495   ±   205   -330   ±   27   -41.6   ±   4.0   35.6   ±   2.0   -48.5   ±   4.1   72   ±   15   1.76   
    
    2		   53.6844   ±   0.0763   -123.729   ±   0.114   4.509   ±   0.071   3c   …   7.762   ±   0.017   16.297   ±   0.024   -4.598   ±   0.016   3c…   3c…   3c…   3c…   …   	SB2	
    
    3		   33.8287   ±   0.0602   208.768   ±   0.097   -35.025   ±   0.068   -14.3   ±   2.0   13.498   ±   0.028   25.394   ±   0.046   -6.840   ±   0.025   19.7   ±   0.9   -26.1   ±   1.7   -3.4   ±   0.5   18   ±   41   0   	VB	
    
    4		   5.7787   ±   0.0258   -12.682   ±   0.045   0.420   ±   0.033   3c   …   87.57   ±   0.39   141.29   ±   0.63   48.11   ±   0.22   3c…   3c…   3c…   3c…   …   	W UMa-type star	
    
    5		   74.2071   ±   0.9587   447.857   ±   1.179   132.925   ±   0.941   3.05   ±   0.93   6.434   ±   0.083   11.485   ±   0.148   -2.879   ±   0.037   24.0   ±   0.6   -12.5   ±   0.8   12.9   ±   0.2   27   ±   26   0.49   
    
    6 c1  	   6.4739   ±   0.1404   24.376   ±   0.307   -3.003   ±   0.209   3c   …   79.2   ±   1.7   125.2   ±   2.7   43.77   ±   0.95   3c…   3c…   3c…   3c…   …   	SB2, VB, Cep I member	
    
    6 c2		   6.7211   ±   0.0321   23.318   ±   0.061   -2.834   ±   0.046   -8.75   ±   0.56   76.32   ±   0.36   120.56   ±   0.58   42.17   ±   0.21   8.3   ±   0.3   -15.9   ±   0.5   -5.3   ±   0.2   324   ±   27   0   	Cep I member	
    
    6 c3  	   0.6803   ±   0.0424   5.705   ±   0.074   7.679   ±   0.057   -1.7   ±   9.1   754   ±   47   1191   ±   74   416   ±   26   46.5   ±   5.2   -24.8   ±   7.5   40.9   ±   4.1   3c…   …   
    
    7		   7.9526   ±   0.0297   -1.495   ±   0.043   -9.372   ±   0.047   3c   …   68.31   ±   0.26   104.88   ±   0.39   12.019   ±   0.068   3c…   3c…   3c…   3c…   0   	Likely an SB2 system	
    
    8		   0.1731   ±   0.0331   -0.951   ±   0.039   -0.495   ±   0.042   -83.0   ±   0.7   3240   ±   620   4750   ±   910   -575   ±   110   -66.6   ±   4.2   -54.7   ±   2.9   -18.2   ±   2.8   3   ±   41   0.94   
    
    9		   36.0837   ±   0.0377   163.840   ±   0.039   -132.775   ±   0.047   -17.6   ±   1.8   16.160   ±   0.017   22.438   ±   0.024   -1.851   ±   0.013   8.3   ±   1.0   -28.2   ±   1.5   -14.6   ±   0.1   6   ±   65   0   
    
    10		   5.2527   ±   0.0256   3.741   ±   0.045   -17.551   ±   0.045   3c   …   107.04   ±   0.52   154.47   ±   0.75   30.43   ±   0.17   3c…   3c…   3c…   3c…   …   	SB2	
    
    11		   2.4320   ±   0.0250   -6.039   ±   0.049   0.370   ±   0.037   3c   …   202.5   ±   2.1   310.5   ±   3.2   177.8   ±   1.8   3c…   3c…   3c…   3c…   …   	SB2	
    
    12		   23.0372   ±   0.0313   102.226   ±   0.034   -44.68   ±   0.039   -16.8   ±   2.9   25.667   ±   0.035   34.862   ±   0.048   -3.179   ±   0.016   7.6   ±   1.7   -26.7   ±   2.3   -6.0   ±   0.2   29   ±   39   0   
    
    13		   5.6032   ±   0.0235   158.233   ±   0.039   12.937   ±   0.040   3c   …   101.30   ±   0.43   142.12   ±   0.60   37.30   ±   0.17   3c…   3c…   3c…   3c…   …   	SB2	
    
    14		   48.4853   ±   0.0351   -139.231   ±   0.044   8.374   ±   0.052   -10.1   ±   1.9   12.562   ±   0.010   16.342   ±   0.012   0.706   ±   0.010   -16.9   ±   1.2   0.5   ±   1.5   1.33   ±   0.07   8   ±   28   0.27   
    
    15 ^†   18.4   ±   2.7   78.8   ±   2.3   -17.6   ±   2.2   7.1   ±   1.0   36.78   ±   5.4   39.3   ±   5.8   -7.7   ±   1.1   20.1   ±   2.3   -8.8   ±   2.1   0.7   ±   1.1   37   ±   35   0.13   
    
    16		   5.6542   ±   0.0258   27.276   ±   0.035   -10.930   ±   0.039   -6.8   ±   0.4   112.43   ±   0.51   135.25   ±   0.62   18.61   ±   0.10   12.2   ±   0.3   -22.0   ±   0.3   -4.51   ±   0.07   204   ±   16   0.01   
    
    17		   1.1687   ±   0.0240   8.010   ±   0.045   -0.711   ±   0.045   -14.7   ±   0.3   504   ±   10   651   ±   13   232   ±   5   15.3   ±   0.5   -32.1   ±   0.5   4.2   ±   0.3   11   ±   23   1.66   
    
    18		   6.9947   ±   0.0256   47.790   ±   0.048   -54.249   ±   0.042   3c   …   72.90   ±   0.27   107.29   ±   0.39   60.13   ±   0.22   3c…   3c…   3c…   3c…   …   	SB2, VB	
    
    19		   5.4731   ±   0.0333   40.407   ±   0.045   -30.676   ±   0.061   3c   …   121.53   ±   0.74   133.34   ±   0.81   28.89   ±   0.20   3c…   3c…   3c…   3c…   …   	SB2	
    
    20		   1.2991   ±   0.0357   7.673   ±   0.075   -4.235   ±   0.065   3c   …   591   ±   16   491   ±   13   -51.7   ±   1.5   3c…   3c…   3c…   3c…   …   	SB2	
    
    21		   28.8414   ±   0.0377   -106.525   ±   0.045   -14.385   ±   0.059   -10.9   ±   1.0   25.409   ±   0.034   23.550   ±   0.032   1.404   ±   0.015   -20.0   ±   0.7   4.1   ±   0.7   -3.90   ±   0.04   17   ±   36   0   
    
    22		   14.7594   ±   0.0241   58.050   ±   0.035   -48.909   ±   0.041   -10.332   ±   0.041   44.692   ±   0.074   48.947   ±   0.080   14.048   ±   0.030   3.40   ±   0.04   -25.80   ±   0.04   -4.88   ±   0.03   273   ±   14   0.07   
    
    23		   19.7872   ±   0.2785   -67.072   ±   0.353   54.409   ±   0.435   3c   …   35.72   ±   0.51   35.03   ±   0.50   7.14   ±   0.20   3c…   3c…   3c…   3c…   …   	SB2	
    
    24		   44.3712   ±   0.0418   106.167   ±   0.112   -195.529   ±   0.076   25.2   ±   2.4   17.338   ±   0.017   14.398   ±   0.015   0.129   ±   0.010   26.5   ±   1.8   -4.3   ±   1.5   -21.87   ±   0.02   31   ±   49   0   
    
    25		   9.2418   ±   0.0296   -55.973   ±   0.044   -47.168   ±   0.044   -22.2   ±   0.7   80.98   ±   0.26   70.72   ±   0.23   12.22   ±   0.05   -38.1   ±   0.5   -5.5   ±   0.5   -20.5   ±   0.1   0   ±   28   0.19   	VB	
    
    26		   20.9650   ±   0.0303   -57.998   ±   0.045   0.564   ±   0.048   3.2   ±   1.2   36.664   ±   0.054   29.943   ±   0.045   5.856   ±   0.018   -5.8   ±   0.9   10.1   ±   0.8   -6.8   ±   0.1   28   ±   81   0   
    
    27		   1.2592   ±   0.0232   -1.625   ±   0.040   -4.432   ±   0.039   -35.9   ±   0.6   493   ±   9   566   ±   10   259   ±   5   -32.1   ±   0.4   -21.7   ±   0.5   10.2   ±   0.3   56   ±   24   0.41   
    
    28		   6.5852   ±   0.0215   34.434   ±   0.038   -44.658   ±   0.044   3c   …   77.98   ±   0.26   112.44   ±   0.37   65.86   ±   0.22   3c…   3c…   3c…   3c…   …   	SB2	
    
    29		   3c…   3c…   3c…   -7.2   ±   0.8   3c…   3c…   3c…   3c…   3c…   3c…   35   ±   58   …   
    
    30		   28.7320   ±   0.0629   60.480   ±   0.089   52.074   ±   0.089   -7.2   ±   0.8   28.197   ±   0.063   19.911   ±   0.046   4.449   ±   0.022   1.0   ±   0.6   -3.0   ±   0.5   14.7   ±   0.1   37   ±   37   0   
    
    31 c1	   1.8134   ±   0.0309   16.712   ±   0.048   -14.941   ±   0.050   -44.7   ±   0.5   446.9   ±   7.6   314.1   ±   5.4   75.7   ±   1.3   -16.7   ±   0.6   -69.8   ±   0.7   16.6   ±   0.7   11   ±   35   0.83   
    
    31 c2	   7.4244   ±   0.0323   -4.818   ±   0.050   -65.643   ±   0.045   18.0   ±   0.7   109.17   ±   0.48   76.70   ±   0.34   18.46   ±   0.09   7.1   ±   0.6   -21.2   ±   0.4   -39.9   ±   0.2   59   ±   39   0.21   
    
    32		   16.0546   ±   0.0294   46.852   ±   0.038   -65.595   ±   0.048   3c…   37.640   ±   0.071   43.835   ±   0.081   23.269   ±   0.045   3c…   3c…   3c…   131   ±   10   0.06   	SB1	
    
    33		   5.9174   ±   0.0310   4.733   ±   0.042   -22.797   ±   0.059   3c…   110.62   ±   0.58   113.38   ±   0.60   58.88   ±   0.31   3c…   3c…   3c…   196   ±   30   0   	Likely an SB2 system	
    
    34		   18.8651   ±   0.0766   0.455   ±   0.088   -103.492   ±   0.133   6.3   ±   1.4   40.439   ±   0.167   31.143   ±   0.132   14.305   ±   0.067   -2.1   ±   1.1   19.3   ±   0.8   -18.4   ±   0.4   44   ±   107   0.13   
    
    35		   11.9227   ±   0.1175   28.985   ±   0.157   -151.159   ±   0.192   -94.7   ±   0.6   53.39   ±   0.53   56.83   ±   0.57   30.88   ±   0.31   -74.6   ±   0.6   -71.0   ±   0.5   45.9   ±   0.4   104   ±   52   0.24   	SB2? 	
    
    36		   17.4243   ±   1.3576   47.673   ±   1.903   -56.696   ±   1.902   -7.19   ±   0.34   40.4   ±   3.2   36.3   ±   2.9   18.7   ±   1.6   -1.88   ±   0.95   -21.02   ±   0.96   3.5   ±   1.1   46   ±   23   0.57   
    
    37 c1	   2.9523   ±   0.9175   10.377   ±   1.508   2.675   ±   1.446   3c   …   234   ±   73   216   ±   67   115   ±   36   3c…   3c…   3c…   3c…   …   	SB3	
    
    37 c2	   3.2707   ±   0.0247   11.665   ±   0.037   8.623   ±   0.043   -53.9   ±   0.6   203.0   ±   1.5   187.3   ±   1.4   131.2   ±   1.0   -20.1   ±   0.4   13.8   ±   0.4   52.5   ±   0.3   39   ±   33   0.08   	SB2?	
    
    38		   19.1742   ±   0.0778   47.633   ±   0.085   -118.803   ±   0.113   18.2   ±   1.2   41.94   ±   0.17   26.97   ±   0.12   15.28   ±   0.07   12.1   ±   1.0   -30.3   ±   0.6   -16.3   ±   0.4   12   ±   34   0   	VB	
    
    39		   22.9945   ±   0.0554   -31.231   ±   0.083   48.491   ±   0.118   -10.4   ±   3.1   26.080   ±   0.071   29.316   ±   0.077   18.754   ±   0.046   -6.3   ±   1.9   12.9   ±   2.1   6.6   ±   1.3   0   ±   50   0.51   
    
    40 c1	   7.4974   ±   0.0222   -2.118   ±   0.032   19.196   ±   0.040   -6.6   ±   0.4   88.29   ±   0.26   82.99   ±   0.25   55.75   ±   0.17   -0.2   ±   0.3   12.2   ±   0.3   6.7   ±   0.2   1   ±   44   0.26   
    
    40 c2	   7.4445   ±   0.0401   -2.593   ±   0.053   16.775   ±   0.078   3c…   88.92   ±   0.48   83.58   ±   0.45   56.15   ±   0.30   3c…   3c…   3c…   3c…   …   	SB2	
    
    40 c3	   3.0993   ±   0.0479   -14.653   ±   0.067   -28.313   ±   0.099   -32.9   ±   0.7   213.6   ±   3.3   200.7   ±   3.1   134.9   ±   2.1   -53.8   ±   0.7   -23.7   ±   0.6   0.5   ±   0.5   7   ±   56   0.21   
    
    41 		   8.5741   ±   0.0262   0.767   ±   0.049   -50.389   ±   0.053   3c…   69.29   ±   0.21   78.62   ±   0.24   51.18   ±   0.16   3c…   3c…   3c…   8   ±   17   0   	SB1	
    
    42 c1	   6.9216   ±   0.0477   -10.073   ±   0.065   3.677   ±   0.075   -9.06   ±   0.44   95.90   ±   0.66   88.5   ±   0.61   62.01   ±   0.43   -9.2   ±   0.3   6.8   ±   0.3   2.4   ±   0.2   99   ±   10   0   
    
    42 c2	   3.2707   ±   0.0247   11.665   ±   0.037   8.623   ±   0.043   -20.9   ±   0.6   203.0   ±   1.5   187.3   ±   1.4   131.20   ±   0.99   1.8   ±   0.4   7.8   ±   0.4   28.5   ±   0.3   11   ±   126   0   
    
    43		   5.7831   ±   0.0218   4.642   ±   0.032   -22.886   ±   0.041   -86.14   ±   1.62   88.53   ±   0.34   126.03   ±   0.48   78.60   ±   0.30   -49.9   ±   0.8   0.3   ±   1.2   72.8   ±   0.7   34   ±   48   0   	SB2?, VB	
    
    44 c1	   4.1646   ±   0.0237   -4.263   ±   0.039   -41.491   ±   0.042   10   ±   15   138.72   ±   0.79   162.15   ±   0.92   110.10   ±   0.63   -19   ±   9   -43   ±   10   -11   ±   7   7   ±   15   0   
    
    44 c2	   2.4455   ±   0.0231   -1.912   ±   0.039   -31.611   ±   0.042   -21.1   ±   0.7   236.1   ±   2.2   276.2   ±   2.6   187.5   ±   1.8   -42.8   ±   0.6   -46.9   ±   0.6   13.4   ±   0.3   9   ±   15   0   
    
    45		   6.4866   ±   0.0274   -12.031   ±   0.039   5.834   ±   0.045   -8.54   ±   0.11   101.11   ±   0.43   91.64   ±   0.39   71.73   ±   0.30   -8.84   ±   0.08   9.48   ±   0.07   -0.64   ±   0.07   73   ±   16   0   
    
    46		   7.1974   ±   0.0844   2.489   ±   0.145   -51.861   ±   0.133   -15.725   ±   0.081   91.10   ±   1.07   82.41   ±   0.97   64.91   ±   0.76   -25.3   ±   0.3   -25.3   ±   0.3   11.6   ±   0.1   178   ±   14   0.01   	Likely an SB2 system	
    
    47		   7.9920   ±   0.0264   -7.424   ±   0.037   -89.250   ±   0.049   -55   ±   17   78.32   ±   0.26   75.30   ±   0.25   62.06   ±   0.21   -63   ±   11   -19   ±   10   39   ±   8   7   ±   12   0.38   	SB2?, VB	
    
    48		   76.3524   ±   0.0354   -291.565   ±   0.063   -599.348   ±   0.077   3c…   7.4080   ±   0.0034   8.7695   ±   0.0041   6.3049   ±   0.0029   3c…   3c…   3c…   3c…   …   	No obs	
    
    49		   10.8249   ±   0.0274   -101.079   ±   0.057   -137.703   ±   0.067   3c…   55.10   ±   0.14   56.49   ±   0.15   48.03   ±   0.12   3c…   3c…   3c…   28   ±   13   0   	SB1	
    
    50		   5.5026   ±   0.0186   -18.795   ±   0.036   -23.996   ±   0.038   3c…   93.26   ±   0.32   129.53   ±   0.44   86.90   ±   0.29   3c…   3c…   3c…   3c…   …   	SB2	
    
    51		   14.8348   ±   0.0256   -41.177   ±   0.047   -61.103   ±   0.044   -7.8   ±   0.4   37.237   ±   0.067   43.156   ±   0.076   35.985   ±   0.064   -23.2   ±   0.2   -8.5   ±   0.3   2.7   ±   0.2   14   ±   10   0.10   
    
    52		   2.5699   ±   0.0295   20.772   ±   0.069   -7.142   ±   0.072   3c   …   201.9   ±   2.3   269.3   ±   3.1   195.2   ±   2.2   3c…   3c…   3c…   76   ±   16   0   	SB1	
    
    53		   5.8065   ±   0.0851   24.885   ±   0.131   0.041   ±   0.196   3c   …   94.1   ±   1.4   97.2   ±   1.4   106.6   ±   1.6   3c…   3c…   3c…   3c…   …   	No Obs	
    
    54		   24.9252   ±   0.0482   110.257   ±   0.084   10.349   ±   0.076   3c   …   19.726   ±   0.040   26.901   ±   0.054   22.289   ±   0.048   3c…   3c…   3c…   3c…   …   	No Obs	
    
    55		   13.7809   ±   0.0560   -60.794   ±   0.078   -25.573   ±   0.060   3c   …   35.19   ±   0.15   49.03   ±   0.20   40.30   ±   0.17   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    56		   3.2342   ±   0.0213   -18.996   ±   0.039   19.453   ±   0.032   3c   …   142.5   ±   0.9   214.1   ±   1.4   171.6   ±   1.1   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    57		   9.2549   ±   0.0876   -51.835   ±   0.184   -5.563   ±   0.142   3c   …   50.13   ±   0.48   75.72   ±   0.72   58.56   ±   0.57   3c…   3c…   3c…   3c…   …   	No Obs, VB	 
    
    58		   4.2768   ±   0.0502   -33.077   ±   0.107   20.811   ±   0.075   3c   …   91.9   ±   1.1   145.8   ±   1.7   158.1   ±   1.9   3c…   3c…   3c…   3c…   …   	No Obs	
    
    59		   2.8816   ±   0.0262   -10.664   ±   0.048   -5.061   ±   0.044   3c   …   165.0   ±   1.5   255.7   ±   2.3   166.8   ±   1.5   3c…   3c…   3c…   3c…   …   	No Obs	
    
    60		   3.1480   ±   0.0238   8.920   ±   0.054   -43.060   ±   0.040   3c   …   126.52   ±   0.95   218.3   ±   1.7   193.0   ±   1.5   3c…   3c…   3c…   3c…   …   	No Obs	
    
    61		   11.0816   ±   0.0209   -53.993   ±   0.043   2.051   ±   0.034   3c   …   33.33   ±   0.06   61.05   ±   0.12   57.49   ±   0.11   3c…   3c…   3c…   3c…   …   	No Obs	
    
    62		   75.4702   ±   0.0477   224.138   ±   0.083   -15.142   ±   0.074   3c   …   4.9439   ±   0.0051   9.0343   ±   0.0075   8.3372   ±   0.0083   3c…   3c…   3c…   3c…   …   	No Obs	
    
    63		   3.8375   ±   0.0262   -59.593   ±   0.051   -15.637   ±   0.040   3c   …   65.38   ±   0.45   164.6   ±   1.1   191.2   ±   1.3   3c…   3c…   3c…   3c…   …   	No Obs	
    
    64		   3.0534   ±   0.0193   -44.860   ±   0.039   31.579   ±   0.039   3c   …   47.12   ±   0.31   199.4   ±   1.3   255.5   ±   1.6   3c…   3c…   3c…   3c…   …   	No Obs	
    
    65		   6.2061   ±   0.0534   4.768   ±   0.115   14.430   ±   0.087   3c   …   18.02   ±   0.19   100.46   ±   0.87   124.68   ±   1.07   3c…   3c…   3c…   3c…   …   	No Obs	
    
    66		   6.6284   ±   0.0305   -38.712   ±   0.052   22.158   ±   0.048   3c   …   39.06   ±   0.18   104.30   ±   0.48   101.77   ±   0.47   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    67		   2.4303   ±   0.0206   9.664   ±   0.044   12.593   ±   0.039   3c   …   85.27   ±   0.73   280.8   ±   2.4   288.5   ±   2.4   3c…   3c…   3c…   3c…   …   	No Obs	
    
    68		   5.0937   ±   0.0235   -21.055   ±   0.039   50.833   ±   0.040   3c   …   66.38   ±   0.31   147.60   ±   0.68   111.13   ±   0.51   3c…   3c…   3c…   3c…   …   	No Obs	
    
    69		   20.201   ±   0.9409   -28.939   ±   1.691   -63.378   ±   1.797   3c   …   13.61   ±   0.86   37.0   ±   1.8   30.0   ±   1.5   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    70		   38.9953   ±   0.0241   -44.449   ±   0.055   132.876   ±   0.050   -13.75   ±   2.08   4.3145   ±   0.0093   19.021   ±   0.013   16.650   ±   0.011   4.2   ±   0.4   -8.3   ±   1.5   -19.8   ±   1.4   39   ±   33   0   	SB1?	
    
    71		   20.6676   ±   1.1712   46.597   ±   2.011   15.837   ±   2.412   2.1   ±   0.5   9.2   ±   1.0   36.5   ±   2.1   30.4   ±   1.8   10.7   ±   0.6   3.7   ±   0.6   1.6   ±   0.6   7   ±   29   0.10   
    
    72		   2.7087   ±   0.0198   -2.164   ±   0.046   25.359   ±   0.045   3c   …   67.53   ±   0.51   279.6   ±   2.0   231.4   ±   1.7   3c…   3c…   3c…   3c…   …   	No Obs	
    
    73		   13.236   ±   0.0635   -65.135   ±   0.121   -109.923   ±   0.125   -8.2   ±   2.8   21.68   ±   0.12   58.28   ±   0.28   42.91   ±   0.21   -42.7   ±   0.8   15.4   ±   2.2   10.0   ±   1.6   23   ±   66   0.04   	SB2?	
    
    74		   5.3235   ±   0.0613   12.598   ±   0.122   17.661   ±   0.120   3c   …   21.41   ±   0.30   144.7   ±   1.7   117.9   ±   1.4   3c…   3c…   3c…   3c…   …   	No Obs	
    
    75		   13.6064   ±   0.0584   35.568   ±   0.111   -2.158   ±   0.121   3c   …   2.951   ±   0.062   56.11   ±   0.24   47.37   ±   0.21   3c…   3c…   3c…   3c…   …   	No Obs	
    
    76		   3.5706   ±   0.0319   -9.927   ±   0.050   12.871   ±   0.062   3c   …   59.48   ±   0.55   220.0   ±   2.0   162.8   ±   1.5   3c…   3c…   3c…   3c…   …   	SB2	
    
    77		   4.9581   ±   0.0220   -6.434   ±   0.037   9.490   ±   0.049   37.2   ±   2.1   33.81   ±   0.17   161.16   ±   0.72   116.46   ±   0.52   6.6   ±   0.4   -18.1   ±   1.7   33.7   ±   1.2   7   ±   28   0   	SB2?	
    
    78		   3.4832   ±   0.0344   -19.142   ±   0.060   -15.277   ±   0.073   3c   …   68.23   ±   0.69   230.8   ±   2.3   156.5   ±   1.5   3c…   3c…   3c…   3c…   …   	SB2	
    
    79		   3.1255   ±   0.0227   -15.645   ±   0.047   1.572   ±   0.053   3c   …   24.81   ±   0.24   264.1   ±   1.9   179.0   ±   1.3   3c…   3c…   3c…   3c…   …   	SB2	
    
    80		   25.5038   ±   0.0242   -15.571   ±   0.050   88.112   ±   0.047   -26.9   ±   2.3   11.912   ±   0.019   31.700   ±   0.031   19.770   ±   0.019   -2.3   ±   0.7   -14.2   ±   1.9   -28.2   ±   1.2   7   ±   69   0   
    
    81 c1	   18.4582   ±   0.0300   22.243   ±   0.057   -8.491   ±   0.054   -9.7   ±   1.1   21.475   ±   0.041   42.400   ±   0.070   26.003   ±   0.043   -0.4   ±   0.4   5.0   ±   0.9   -10.3   ±   0.5   29   ±   79   …   
    
    81 c2	   18.4850   ±   0.0246   23.474   ±   0.048   -13.040   ±   0.045   -10.5   ±   1.1   21.443   ±   0.029   42.339   ±   0.056   25.965   ±   0.035   -1.1   ±   0.4   6.2   ±   0.9   -10.9   ±   0.5   20   ±   80   …   
    
    82		   5.3350   ±   0.1333   9.708   ±   0.267   30.734   ±   0.302   19.26   ±   0.76   39.1   ±   1.1   157.2   ±   3.9   94.3   ±   2.4   25.0   ±   0.7   -18.6   ±   0.7   14.8   ±   0.5   6   ±   11   0   
    
    83		   8.7512   ±   0.0221   -22.065   ±   0.039   32.895   ±   0.047   -155.2   ±   1.5   14.077   ±   0.067   97.80   ±   0.25   57.39   ±   0.15   -20.4   ±   0.2   -27.7   ±   1.3   152.9   ±   0.8   15   ±   44   0   
    
    84		   6.2996   ±   0.0226   5.755   ±   0.041   30.190   ±   0.042   3c   …   -6.375   ±   0.071   137.86   ±   0.49   78.44   ±   0.28   3c…   3c…   3c…   3c…   …   	SB2	
    
    85		   18.9468   ±   0.1350   25.464   ±   0.239   123.209   ±   0.229   -13.0   ±   1.6   6.78   ±   0.13   45.58   ±   0.33   25.73   ±   0.19   18.9   ±   0.3   -24.9   ±   1.4   -13.6   ±   0.8   11   ±   45   0   
    
    86		   9.1725   ±   0.0563   -6.353   ±   0.089   24.018   ±   0.113   -24.7   ±   2.7   17.64   ±   0.16   93.87   ±   0.58   52.57   ±   0.32   -0.8   ±   0.4   -14.8   ±   2.3   -23.6   ±   1.3   211   ±   9   0   	SB1?	
    
    87		   2.8321   ±   0.0211   -1.789   ±   0.037   -12.790   ±   0.041   3c   …   -11.7   ±   0.16   313.1   ±   2.3   162.7   ±   1.2   3c…   3c…   3c…   29   ±   12   0   	Likely an SB2 system	
    
    88		   60.9596   ±   0.0417   123.984   ±   0.067   210.513   ±   0.079   8.9   ±   3.3   5.408   ±   0.013   13.528   ±   0.010   7.5390   ±   0.0054   18.4   ±   1.1   -8.8   ±   2.7   4.9   ±   1.5   42   ±   35   0.23   
    
    89		   6.1821   ±   0.0214   -4.278   ±   0.035   20.837   ±   0.049   3c   …   31.45   ±   0.13   140.86   ±   0.49   73.03   ±   0.25   3c…   3c…   3c…   3c…   …   	SB2	
    
    90		   3.1178   ±   0.0136   2.981   ±   0.029   -32.215   ±   0.033   171.0   ±   5.9   43.69   ±   0.21   284.2   ±   1.2   142.06   ±   0.62   5.6   ±   0.8   79.4   ±   5.2   159.1   ±   2.6   19   ±   45   0.72   
    
    91		   2.9807   ±   0.0777   -17.761   ±   0.147   -6.453   ±   0.196   1.51   ±   0.20   24.22   ±   0.83   304.1   ±   7.9   139.6   ±   3.6   -29.8   ±   0.4   -1.5   ±   0.4   4.1   ±   0.7   29   ±   18   0.43   	VB	
    
    92		   4.8178   ±   0.0318   2.645   ±   0.063   2.795   ±   0.069   3c   …   -4.63   ±   0.12   191.1   ±   1.3   80.85   ±   0.54   3c…   3c…   3c…   3c…   …   	SB3	
    
    93		   5.1302   ±   0.0273   4.877   ±   0.056   11.036   ±   0.045   -10.5   ±   1.1   34.07   ±   0.20   174.39   ±   0.93   80.15   ±   0.43   6.4   ±   0.2   -10.6   ±   1.0   -9.0   ±   0.5   200   ±   22   0   
    
    94		   4.6757   ±   0.0217   -30.967   ±   0.042   8.135   ±   0.041   -10.56   ±   0.30   -10.380   ±   0.090   200.74   ±   0.93   73.06   ±   0.34   -26.14   ±   0.07   -21.3   ±   0.3   -5.5   ±   0.2   24   ±   26   0   
    
    95		   8.8428   ±   0.0227   3.651   ±   0.049   23.806   ±   0.056   -18.4   ±   0.6   5.008   ±   0.057   105.37   ±   0.27   40.76   ±   0.11   5.60   ±   0.05   -16.7   ±   0.6   -13.9   ±   0.2   11   ±   48   0.45   
    
    96		   4.4582   ±   0.0349   1.089   ±   0.079   23.109   ±   0.059   -12.78   ±   0.47   25.87   ±   0.24   205.9   ±   1.6   85.16   ±   0.67   8.9   ±   0.2   -25.6   ±   0.4   -5.6   ±   0.2   28   ±   24   0   
    
    97		   4.5618   ±   0.0233   8.716   ±   0.051   37.931   ±   0.052   3c…   -9.00   ±   0.11   207.8   ±   1.1   69.24   ±   0.36   3c…   3c…   3c…   3c…   0.01   
    
    98		   3c…   3c…   3c…   -30.8   ±   0.5   3c…   3c…   3c…   3c…   3c…   3c…   119   ±   34   …   	SB2?	
    
    99		   0.6552   ±   0.0203   3.535   ±   0.043   -5.721   ±   0.048   -22.48   ±   0.05   219.5   ±   6.8   1397   ±   43   575   ±   18   4.6   ±   1.3   36.3   ±   0.4   -39.2   ±   0.8   16   ±   11   0.08   
    
    100		   7.2575   ±   0.7471   20.703   ±   1.708   55.176   ±   1.547   -15.6   ±   0.6   18.0   ±   2.5   127.4   ±   13.1   49.4   ±   5.2   23.4   ±   3.6   -33.8   ±   1.2   -6.2   ±   2.0   23   ±   19   0   	VB	
    
    101 ^†   36.0   ±   6.9   78.1   ±   5.3   135.9   ±   5.2   -19.6   ±   0.5   -0.126   ±   0.024   26.4   ±   5.1   8.5   ±   1.6   15.4   ±   3.3   -20.3   ±   0.9   -12.7   ±   2.2   3   ±   13   0.09   
    
    102		   3.9580   ±   0.0213   6.072   ±   0.042   12.173   ±   0.040   -24.0   ±   0.7   36.77   ±   0.22   232.7   ±   1.3   91.37   ±   0.49   8.5   ±   0.1   -20.1   ±   0.6   -19.1   ±   0.3   166   ±   58   0.02   	VB	
    
    103		   2.7289   ±   0.0329   1.937   ±   0.066   18.633   ±   0.048   3c   …   35.50   ±   0.46   342.3   ±   4.1   125.9   ±   1.5   3c…   3c…   3c…   3c…   …   	SB2	
    
    104		   1.9334   ±   0.0183   -9.797   ±   0.037   -11.373   ±   0.041   -27.96   ±   0.06   -10.45   ±   0.20   493.9   ±   4.7   153.1   ±   1.5   -30.6   ±   0.3   6.70   ±   0.09   -34.0   ±   0.2   17   ±   14   0.40   
    
    105		   6.7536   ±   0.0191   1.544   ±   0.033   -24.437   ±   0.041   3c   …   61.81   ±   0.18   117.84   ±   0.33   64.94   ±   0.18   3c…   3c…   3c…   8.5   ±   8.1   0   	SB1	
    
    106 c1	   5.3075   ±   0.0202   4.973   ±   0.041   8.978   ±   0.044   -14.0   ±   1.6   24.04   ±   0.11   175.84   ±   0.67   63.27   ±   0.24   5.1   ±   0.2   -11.8   ±   1.5   -10.7   ±   0.5   249   ±   23   0   
    
    106 c2	   1.5153   ±   0.0161   4.395   ±   0.032   -2.662   ±   0.037   -13.6   ±   0.7   84.02   ±   0.89   615.9   ±   6.5   221.5   ±   2.4   8.3   ±   0.2   4.9   ±   0.7   -18.7   ±   0.3   28   ±   93   0.02   
    
    107		   12.2966   ±   0.0554   33.271   ±   0.106   -32.095   ±   0.117   8.6   ±   0.9   16.22   ±   0.11   74.19   ±   0.33   29.10   ±   0.14   9.0   ±   0.2   17.6   ±   0.8   -1.1   ±   0.3   3   ±   23   0.10   
    
    108		   3c…   -7.436   ±   1.367   1.816   ±   1.254   -30.6   ±   0.3   3c…   3c…   3c…   3c…   3c…   3c…   25   ±   13   …   
    
    109		   2.4886   ±   0.0235   6.109   ±   0.047   10.938   ±   0.053   -65.1   ±   0.8   60.27   ±   0.59   375.9   ±   3.5   128.7   ±   1.2   7.8   ±   0.2   -45.9   ±   0.8   -51.4   ±   0.3   96   ±   27   0.50   	SB2?, VB	
    
    110		   8.0362   ±   0.0372   7.506   ±   0.079   39.679   ±   0.096   3c   …   19.23   ±   0.13   116.39   ±   0.54   39.59   ±   0.19   3c…   3c…   3c…   3c…   …   	SB2	
    
    111		   11.511   ±   0.0169   0.985   ±   0.032   -41.117   ±   0.035   -8.8   ±   0.9   23.649   ±   0.042   77.23   ±   0.11   31.984   ±   0.048   -8.3   ±   0.3   10.2   ±   0.8   -13.9   ±   0.3   13   ±   60   0   
    
    112		   14.4045   ±   0.0436   13.28   ±   0.084   28.408   ±   0.071   -23.76   ±   1.04   -3.292   ±   0.046   67.08   ±   0.20   17.584   ±   0.062   5.46   ±   0.06   -18.8   ±   1.0   -17.0   ±   0.3   158   ±   8   0.27   
    
    113		   27.1943   ±   0.1297   -9.618   ±   0.300   -99.601   ±   0.243   -3.1   ±   0.6   4.608   ±   0.071   34.87   ±   0.17   10.739   ±   0.069   -7.0   ±   0.1   12.8   ±   0.6   -10.0   ±   0.2   22   ±   30   0.09   
    
    114		   7.5609   ±   0.0199   23.899   ±   0.043   45.681   ±   0.037   -13.74   ±   0.06   21.133   ±   0.067   124.84   ±   0.33   38.23   ±   0.10   20.2   ±   0.07   -28.63   ±   0.06   -2.19   ±   0.06   29   ±   10   0   
    
    115		   6.2609   ±   0.0195   9.216   ±   0.035   13.006   ±   0.037   -11.29   ±   0.08   43.88   ±   0.14   143.80   ±   0.45   53.90   ±   0.17   6.50   ±   0.04   -13.44   ±   0.07   -7.09   ±   0.04   291   ±   6   0   
    
    116		   1.5591   ±   0.0237   -11.737   ±   0.047   -17.026   ±   0.044   -9.7   ±   0.9   60.45   ±   0.94   625.9   ±   9.5   126.6   ±   1.9   -46.0   ±   0.7   31.9   ±   0.9   -30.3   ±   0.7   112   ±   25   0.58   	SB2?	
    
    117 		   0.6502   ±   0.0323   2.313   ±   0.051   1.043   ±   0.056   -65.7   ±   0.7   56.4   ±   2.9   1517   ±   75   237   ±   12   15.4   ±   0.7   -43.4   ±   0.7   -50.4   ±   0.8   8   ±   35   0.88   
    
    118		   6.8174   ±   0.0533   -9.090   ±   0.104   -30.432   ±   0.110   -3.8   ±   0.5   33.49   ±   0.29   136.5   ±   1.1   41.98   ±   0.34   -12.8   ±   0.2   13.9   ±   0.5   -12.0   ±   0.2   6   ±   32   0.41   
    
    119		   3.6599   ±   0.0173   7.367   ±   0.033   -7.720   ±   0.035   3c   …   20.26   ±   0.12   268.3   ±   1.3   47.62   ±   0.23   3c…   3c…   3c…   3c…   …   	SB2, VB	
    
    120		   5.7303   ±   0.0288   17.652   ±   0.067   -4.347   ±   0.060   -20.1   ±   0.9   27.50   ±   0.16   167.40   ±   0.84   40.91   ±   0.22   10.0   ±   0.2   -7.8   ±   0.9   -21.7   ±   0.2   22   ±   27   0   	VB	
    
    121		   15.9895   ±   0.0465   -43.788   ±   0.112   -66.512   ±   0.085   -24.4   ±   0.5   7.831   ±   0.047   61.12   ±   0.18   10.708   ±   0.048   -19.12   ±   0.08   -1.2   ±   0.5   -28.0   ±   0.1   0   ±   54   0   
    
    122		   5.3036   ±   0.0247   26.598   ±   0.050   31.165   ±   0.048   11.39   ±   0.57   60.64   ±   0.29   168.37   ±   0.78   59.38   ±   0.28   33.7   ±   0.2   -12.6   ±   0.5   13.4   ±   0.2   41   ±   20   0.26   
    
    123		   3.4269   ±   0.0251   8.190   ±   0.050   5.784   ±   0.050   -22.4   ±   0.5   11.21   ±   0.14   291.0   ±   2.1   18.33   ±   0.17   10.9   ±   0.1   -20.7   ±   0.5   -12.1   ±   0.1   176   ±   27   0   	Multiple system	
    
    124		   4.1805   ±   0.0346   9.568   ±   0.057   6.836   ±   0.057   -13.50   ±   1.04   60.84   ±   0.51   223.6   ±   1.9   59.46   ±   0.50   8.6   ±   0.3   -14.7   ±   1.0   -8.3   ±   0.3   412   ±   39   0   	VB	
    
    125		   3.4229   ±   0.0223   6.410   ±   0.041   6.161   ±   0.042   -21.44   ±   0.09   44.38   ±   0.30   285.5   ±   1.9   43.53   ±   0.29   6.69   ±   0.08   -20.80   ±   0.09   -11.57   ±   0.08   181   ±   37   0.15   	Multiple system	
    
    126		   8.8830   ±   0.0254   13.314   ±   0.047   -25.113   ±   0.044   37.8   ±   0.6   31.089   ±   0.097   104.05   ±   0.30   29.657   ±   0.092   13.5   ±   0.2   35.6   ±   0.6   14.5   ±   0.2   47   ±   16   0   
    
    127		   5.2719   ±   0.0222   5.876   ±   0.044   39.134   ±   0.043   3c…   31.83   ±   0.14   184.51   ±   0.78   30.39   ±   0.14   3c…   3c…   3c…   177   ±   86   0.07   
    
    128		   3.6596   ±   0.0202   12.548   ±   0.044   7.840   ±   0.038   -18.9   ±   0.1   86.93   ±   0.49   245.8   ±   1.4   81.67   ±   0.46   11.7   ±   0.1   -20.4   ±   0.1   -13.2   ±   0.1   50   ±   10   0.33   	SB3?	
    
    129		   4.4840   ±   0.0419   14.574   ±   0.075   9.986   ±   0.070   -20.53   ±   0.50   28.60   ±   0.29   219.9   ±   2.1   23.82   ±   0.25   13.7   ±   0.2   -22.1   ±   0.5   -9.8   ±   0.2   147   ±   35   0   
    
    130		   8.5911   ±   0.0294   22.051   ±   0.055   9.817   ±   0.048   3c…   13.892   ±   0.064   115.31   ±   0.39   7.577   ±   0.050   3c…   3c…   3c…   244   ±   88   0.07   
    
    131 	   6.7559   ±   0.0739   30.093   ±   0.165   11.946   ±   0.136   3c…   29.72   ±   0.35   143.5   ±   1.6   20.84   ±   0.27   3c…   3c…   3c…   3c…   …   	SB2, VB	
    
    132		   2.3376   ±   0.0228   -4.435   ±   0.038   14.822   ±   0.037   42.1   ±   0.4   127.3   ±   1.2   395.4   ±   3.9   102.2   ±   1.0   11.4   ±   0.2   11.0   ±   0.4   50.1   ±   0.2   47   ±   22   0.64   
    
    133		   2.8409   ±   0.0221   20.435   ±   0.040   15.224   ±   0.051   3c…   141.2   ±   1.1   297.6   ±   2.3   124.2   ±   1.0   3c…   3c…   3c…   73   ±   7   0.83   	SB1	
    
    134		   4.8381   ±   0.0433   -29.203   ±   0.074   12.606   ±   0.082   3c…   44.78   ±   0.42   200.7   ±   1.8   21.26   ±   0.23   3c…   3c…   3c…   3c…   …   	SB2	
    
    135		   2.4955   ±   0.0229   11.907   ±   0.046   26.296   ±   0.049   -37.3   ±   0.7   79.27   ±   0.74   391.7   ±   3.6   29.26   ±   0.30   18.4   ±   0.4   -62.7   ±   0.7   11.4   ±   0.4   29   ±   27   0   	VB	
    
    136		   12.1772   ±   0.0319   43.307   ±   0.067   6.028   ±   0.058   -7.2   ±   0.6   15.814   ±   0.051   80.57   ±   0.21   1.352   ±   0.035   15.2   ±   0.1   -9.5   ±   0.6   -4.50   ±   0.04   44   ±   26   0.59   
    
    137		   3.7221   ±   0.0237   15.461   ±   0.040   -2.988   ±   0.041   3c…   77.94   ±   0.50   254.2   ±   1.6   38.60   ±   0.26   3c…   3c…   3c…   3c…   0.09   
    
    138 c1	   0.7272   ±   0.0222   5.052   ±   0.044   -3.012   ±   0.041   -69.75   ±   0.42   345   ±   11   1326   ±   40   113.1   ±   3.5   12.6   ±   0.9   -49.1   ±   0.5   -61.4   ±   0.8   22   ±   14   1.05   
    
    138 c2	   0.5547   ±   0.0176   -3.437   ±   0.034   -2.566   ±   0.032   3c…   453   ±   14   1739   ±   55   148.3   ±   4.7   3c…   3c…   3c…   62   ±   82   0.96   
    
    139		   1.1202   ±   0.0288   -0.286   ±   0.057   -3.048   ±   0.052   3c…   245.7   ±   6.3   853   ±   22   92.0   ±   2.4   3c…   3c…   3c…   3c…   0.44   
    
    140 c1	   4.6715   ±   0.0166   15.432   ±   0.028   2.258   ±   0.029   -16.3   ±   0.6   44.11   ±   0.16   209.39   ±   0.74   -5.955   ±   0.051   11.9   ±   0.1   -17.4   ±   0.6   -8.46   ±   0.05   37   ±   62   0   	VB	
    
    140 c2	   0.8896   ±   0.0234   -0.651   ±   0.040   -3.487   ±   0.041   -17.5   ±   1.6   231.7   ±   6.1   1100   ±   29   -31.22   ±   0.82   -6.5   ±   0.5   -3.2   ±   1.6   -24.7   ±   0.5   21   ±   43   0.93   
    
    141		   9.3979   ±   0.0199   146.72   ±   0.037   17.614   ±   0.035   60.85   ±   0.07   36.436   ±   0.080   97.96   ±   0.21   19.945   ±   0.051   90.6   ±   0.1   30.5   ±   0.1   10.7   ±   0.1   16   ±   12   0.04   
    
    142		   6.1631   ±   0.0258   17.354   ±   0.047   7.584   ±   0.046   -9.05   ±   0.54   62.53   ±   0.27   143.99   ±   0.60   41.03   ±   0.18   9.8   ±   0.2   -13.2   ±   0.5   -4.7   ±   0.1   432   ±   25   0   	Cep III member	
    
    143		   13.6259   ±   0.0236   59.780   ±   0.044   49.546   ±   0.034   -17.2   ±   1.1   34.795   ±   0.062   56.240   ±   0.098   31.819   ±   0.058   15.3   ±   0.5   -27.6   ±   0.8   -5.6   ±   0.5   4   ±   62   0.30   
    
    144		   8.7382   ±   0.0309   -4.442   ±   0.048   -6.498   ±   0.042   20.90   ±   0.08   38.93   ±   0.14   106.26   ±   0.38   17.026   ±   0.073   4.35   ±   0.04   19.64   ±   0.07   7.10   ±   0.03   35   ±   11   0.24   	VB	
    
    145		   4.0426   ±   0.0235   22.659   ±   0.044   23.516   ±   0.040   -31.43   ±   0.06   91.34   ±   0.53   225.4   ±   1.3   45.38   ±   0.28   17.7   ±   0.2   -46.3   ±   0.1   1.7   ±   0.2   66   ±   9   0.52   
    
    146		   20.4651   ±   0.0262   144.623   ±   0.042   -38.632   ±   0.042   -47.9   ±   1.2   16.099   ±   0.024   45.935   ±   0.059   4.299   ±   0.019   14.9   ±   0.4   -44.2   ±   1.1   -36.3   ±   0.1   77   ±   64   0   	VB	
    
    147		   1.5399   ±   0.0263   -10.450   ±   0.040   -4.875   ±   0.038   3c…   164.8   ±   2.8   624   ±   11   -68.7   ±   1.2   3c…   3c…   3c…   3c…   …   	SB2	
    
    148		   2.0655   ±   0.0185   -12.114   ±   0.034   2.945   ±   0.033   -17.543   ±   0.011   209.0   ±   1.9   413.6   ±   3.7   140.1   ±   1.3   -29.4   ±   0.2   -10.2   ±   0.1   12.7   ±   0.1   3   ±   4   0.50   
    
    149		   2.2842   ±   0.0251   5.193   ±   0.048   -0.221   ±   0.041   3c…   141.3   ±   1.6   414.3   ±   4.5   -1.40   ±   0.15   3c…   3c…   3c…   146   ±   71   0.23   	Multiple system	
    
    150		   2.6622   ±   0.0217   7.054   ±   0.037   -1.329   ±   0.033   -13.43   ±   0.48   142.5   ±   1.2   344.6   ±   2.8   45.55   ±   0.39   6.1   ±   0.2   -14.3   ±   0.4   -10.1   ±   0.1   208   ±   47   0.36   
     
    151		   41.5395   ±   0.0282   173.626   ±   0.046   -58.869   ±   0.039   -23.22   ±   0.22   8.8728   ±   0.0078   22.334   ±   0.015   1.4204   ±   0.0089   9.43   ±   0.08   -23.7   ±   0.2   -18.1   ±   0.02   44   ±   18   0.93   
    
    152		   7.0082   ±   0.0198   22.582   ±   0.037   4.888   ±   0.037   -8.8   ±   0.9   64.00   ±   0.18   120.30   ±   0.34   42.35   ±   0.13   9.9   ±   0.4   -13.8   ±   0.8   -5.7   ±   0.3   428   ±   98   0.95   	SB2?, VB, Cep III member	
    
    153		   6.1071   ±   0.0229   21.034   ±   0.046   4.317   ±   0.034   3c…   74.11   ±   0.28   138.21   ±   0.52   47.08   ±   0.18   3c…   3c…   3c…   442   ±   26   0.37   	SB1, Cep II member	
    
    154		   6.0218   ±   1.1249   -6.251   ±   1.790   -27.815   ±   1.871   3c…   60   ±   11   155   ±   29   -8.4   ±   3.2   3c…   3c…   3c…   18   ±   34   0   	SB1	
    
    155		   3c…   3c…   3c…   3c…   3c…   3c…   3c…   3c…   3c…   3c…   3c…   …   	SB3	
    
    156		   6.0080   ±   0.6900   17.991   ±   1.375   9.678   ±   1.053   -7.7   ±   2.2   75.8   ±   8.7   142   ±   16   43.0   ±   5.2   10.6   ±   2.0   -14.4   ±   2.0   0.3   ±   1.4   465   ±   24   0.39   	Likely SB1 system, Cep III member	
    
    157		   7.8348   ±   0.0488   8.660   ±   0.064   -1.105   ±   0.073   -10.958   ±   0.007   58.67   ±   0.37   109.60   ±   0.68   28.92   ±   0.20   -0.69   ±   0.04   -11.45   ±   0.03   -4.04   ±   0.04   52   ±   7   0   	VB	
    
    158		   6.6269   ±   0.0296   23.351   ±   0.056   1.640   ±   0.043   -8.56   ±   0.25   71.97   ±   0.32   125.93   ±   0.56   41.62   ±   0.19   10.2   ±   0.1   -14.8   ±   0.2   -5.5   ±   0.1   344   ±   16   0.16   	Cep II member	
    
    159		   1.8441   ±   0.0369   13.252   ±   0.047   17.193   ±   0.036   3c…   224.3   ±   4.5   488.3   ±   9.8   -72.8   ±   1.5   3c…   3c…   3c…   90   ±   26   0.63   	SB1 or SB2?	
    
    160		   2.8245   ±   0.0701   6.988   ±   0.123   0.194   ±   0.112   3c…   142.6   ±   3.5   311.5   ±   7.7   89.3   ±   2.2   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    161		   19.7195   ±   0.0352   168.459   ±   0.053   21.141   ±   0.048   -7.85   ±   1.01   16.662   ±   0.033   47.881   ±   0.086   -1.192   ±   0.022   35.5   ±   0.3   -21.3   ±   1.0   -3.00   ±   0.04   66   ±   34   0   
    
    162		   3.5435   ±   0.0276   -5.603   ±   0.041   -19.832   ±   0.040   3c…   116.15   ±   0.91   257.2   ±   2.0   2.28   ±   0.11   3c…   3c…   3c…   3c…   …   	SB2	
    
    163 c1	   2.3150   ±   0.3444   1.808   ±   0.643   -4.241   ±   0.541   -45.3   ±   0.6   207   ±   31   370   ±   55   84   ±   13   -20.2   ±   1.3   -39.5   ±   0.9   13.1   ±   1.7   35   ±   19   0.93   	SB2?	
    
    163 c2	   1.3287   ±   0.0176   1.946   ±   0.026   1.397   ±   0.028   -4.3   ±   2.3   361.1   ±   4.8   644.1   ±   8.5   145.6   ±   1.9   4.8   ±   1.1   -7.8   ±   2.0   2.6   ±   0.5   2   ±   41   1.02   
    
    164		   1.7550   ±   0.0227   17.782   ±   0.048   -5.156   ±   0.037   3c…   276.7   ±   3.6   476.0   ±   6.2   146.6   ±   1.9   3c…   3c…   3c…   3c…   …   	SB2	
    
    165		   0.8193   ±   0.0263   -2.022   ±   0.040   -2.205   ±   0.040   -32.1   ±   2.5   644   ±   21   1008   ±   32   240.1   ±   7.7   -29.1   ±   1.4   -20.6   ±   2.1   -7.6   ±   0.7   61   ±   43   0.76   
    
    166		   1.4660   ±   0.0258   -1.493   ±   0.046   -2.800   ±   0.042   -2.6   ±   1.3   374.4   ±   6.6   560.9   ±   9.9   102.7   ±   1.8   -6.8   ±   0.7   0.2   ±   1.1   -8.1   ±   0.3   51   ±   26   0.53   	SB2?	
    
    167		   2.2415   ±   0.0285   6.647   ±   0.044   -12.438   ±   0.042   3c…   251.9   ±   3.2   365.4   ±   4.6   45.39   ±   0.60   3c…   3c…   3c…   3c…   …   	SB2	
    
    168 c1	   3.3354   ±   0.0607   35.354   ±   0.119   -6.973   ±   0.104   -8.50   ±   0.90   170.7   ±   3.1   242.2   ±   4.4   45.66   ±   0.87   34.2   ±   0.9   -37.4   ±   0.9   -11.3   ±   0.3   17   ±   24   0   
    
    168 c2	   1.9104   ±   0.0273   15.207   ±   0.043   14.083   ±   0.047   -38.00   ±   0.61   298.1   ±   4.3   422.8   ±   6.0   79.7   ±   1.1   14.2   ±   0.6   -48.8   ±   0.6   38.8   ±   0.5   65   ±   44   …   
    
    169 c1	   3.7323   ±   0.0304   16.785   ±   0.044   -14.285   ±   0.047   3c…   159.7   ±   1.3   212.0   ±   1.7   36.46   ±   0.31   3c…   3c…   3c…   3c…   …   	SB2	
    
    169 c2	   1.0620   ±   0.0188   1.891   ±   0.026   -4.733   ±   0.029   -20.6   ±   0.6   561   ±   10   745   ±   13   128.2   ±   2.7   -8.47   ±   0.4   -24.9   ±   0.5   -15.8   ±   0.4   32   ±   35   1.10   
    
    170		   3.8271   ±   0.0294   35.034   ±   0.033   -24.659   ±   0.041   3c…   172.2   ±   1.3   194.0   ±   1.5   31.51   ±   0.26   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    171		   2.0881   ±   0.0237   -1.111   ±   0.044   1.466   ±   0.045   3c…   149.2   ±   1.7   416.8   ±   4.7   182.5   ±   2.1   3c…   3c…   3c…   3c…   …   	No Obs	
    
    172		   1.4190   ±   0.0202   -2.503   ±   0.040   4.729   ±   0.048   3c…   236.1   ±   3.4   605.6   ±   8.6   272.3   ±   3.9   3c…   3c…   3c…   3c…   …   	No Obs	
    
    173		   3.3140   ±   0.0234   6.048   ±   0.066   6.157   ±   0.044   3c…   47.50   ±   0.35   286.0   ±   2.0   83.50   ±   0.60   3c…   3c…   3c…   3c…   …   	No Obs	
    
    174 c1	   5.1913   ±   0.0263   17.103   ±   0.049   15.759   ±   0.049   3.5   ±   3.9   64.13   ±   0.33   166.51   ±   0.84   72.59   ±   0.37   20.1   ±   1.3   -7.6   ±   3.4   1.3   ±   1.5   273   ±   53   0   
    
    174 c2	   2.3286   ±   0.0287   -5.234   ±   0.044   1.331   ±   0.050   -30.7   ±   0.7   143.0   ±   1.8   371.2   ±   4.6   161.8   ±   2.0   -18.4   ±   0.3   -20.6   ±   0.6   -17.3   ±   0.3   0   ±   30   0   
    
    175		   7.0641   ±   0.0212   13.429   ±   0.040   18.865   ±   0.038   3c…   34.59   ±   0.11   130.30   ±   0.39   43.19   ±   0.13   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    176		   3.0180   ±   0.0258   0.069   ±   0.041   -1.761   ±   0.043   3c…   85.34   ±   0.74   304.6   ±   2.6   98.60   ±   0.85   3c…   3c…   3c…   3c…   …   	No Obs	
    
    177		   1.7855   ±   0.0225   -4.142   ±   0.041   3.931   ±   0.039   3c…   204.3   ±   2.6   479.8   ±   6.0   204.3   ±   2.6   3c…   3c…   3c…   3c…   …   	No Obs	
    
    178		   4.4875   ±   0.2181   22.593   ±   0.471   24.558   ±   0.447   3c…   42.7   ±   2.2   213.1   ±   10.3   49.1   ±   2.5   3c…   3c…   3c…   3c…   …   	No Obs, VB	
    
    179 ^△   4.5968   ±   0.0190   10.676   ±   0.036   8.783   ±   0.038   -9.74   ±   2.88   74.03   ±   0.31   192.24   ±   0.79   69.93   ±   0.29   9.3   ±   1.0   -13.3   ±   2.5   -6.0   ±   0.9   236   ±   31   0   
    
    180		   4.0183   ±   0.2705   24.296   ±   0.433   13.133   ±   0.443   3c…   63.6   ±   4.4   233   ±   16   60.1   ±   4.1   3c…   3c…   3c…   3c…   …   	No Obs	
    
    181		   1.4237   ±   0.0198   -4.132   ±   0.040   -3.404   ±   0.040   3c…   283.5   ±   3.9   593.8   ±   8.3   245.7   ±   3.4   3c…   3c…   3c…   3c…   …   	No Obs	
    
    182		   6.9380   ±   0.0210   19.547   ±   0.041   10.796   ±   0.038   -11.4   ±   0.5   59.15   ±   0.18   123.00   ±   0.37   46.35   ±   0.15   9.1   ±   0.2   -15.6   ±   0.4   -6.0   ±   0.2   441   ±   39   0.20   	Cep III member	
    
    183		   8.7931   ±   0.0268   22.613   ±   0.050   40.33   ±   0.044   3c…   36.53   ±   0.12   105.92   ±   0.32   19.509   ±   0.071   3c…   3c…   3c…   3c…   …   	No Obs	
    
    184 c1	   3.1496   ±   0.0250   10.564   ±   0.042   -3.011   ±   0.042   -7.5   ±   1.8   100.70   ±   0.80   298.9   ±   2.4   36.38   ±   0.31   12.1   ±   0.6   -7.2   ±   1.7   -11.5   ±   0.2   326   ±   21   	0.47
        SB1?, VB	
        
        184 c2	   0.0992   ±   0.0397   -1.808   ±   0.063   -1.025   ±   0.063   -101.6   ±   2.0   3197   ±   1279   9490   ±   3798   1155   ±   462   -119   ±   30   -40   ±   9   -66   ±   25   54   ±   39   2.54   
        
        185 c1	   0.9852   ±   0.0233   -1.890   ±   0.042   2.795   ±   0.048   -16.4   ±   0.7   371.9   ±   8.8   925   ±   22   188.4   ±   4.5   -11.8   ±   0.4   -18.3   ±   0.7   7.6   ±   0.4   326   ±   29   1.22   
        
        185 c2	   1.9591   ±   0.0452   -13.348   ±   0.076   4.914   ±   0.077   -55.4   ±   0.8   187.1   ±   4.3   465   ±   11   94.7   ±   2.2   -47.5   ±   0.7   -44.6   ±   0.8   -2.0   ±   0.5   0   ±   98   0.55   
        
        186		   4.9378   ±   0.0247   15.025   ±   0.055   5.091   ±   0.043   -3.8   ±   0.7   85.22   ±   0.43   174.20   ±   0.87   58.35   ±   0.30   12.2   ±   0.3   -9.1   ±   0.6   -3.7   ±   0.2   349   ±   24   0.16   	Cep III member	
        
        187		   3.6518   ±   0.0259   -2.478   ±   0.046   3.446   ±   0.039   3c…   115.91   ±   0.82   237.3   ±   1.7   72.53   ±   0.52   3c…   3c…   3c…   3c…   …   	No Obs	
        
        188		   5.9488   ±   0.0245   20.620   ±   0.045   4.577   ±   0.043   -11.1   ±   0.7   73.19   ±   0.30   144.14   ±   0.59   46.10   ±   0.20   10.3   ±   0.3   -16.0   ±   0.6   -6.7   ±   0.2   255   ±   18   0.10   	VB, Cep II member		
        
        189		   3.1191   ±   0.9470   22.926   ±   1.637   4.261   ±   1.703   -5.6   ±   0.7   142   ±   43   272   ±   83   92   ±   28   29.0   ±   9.4   -18.4   ±   3.7   -10.4   ±   5.2   360   ±   31   0.41   
        
        190		   1.8118   ±   0.0299   13.866   ±   0.065   0.523   ±   0.068   3c…   242.1   ±   4.0   474.5   ±   7.8   144.64   ±   2.4   3c…   3c…   3c…   3c…   …   	No Obs	
        
        191 c1	   5.3870   ±   0.3028   16.134   ±   0.533   1.344   ±   0.628   -7.6   ±   0.8   79.3   ±   4.5   163.0   ±   9.2   40.1   ±   2.5   9.5   ±   0.9   -11.7   ±   0.8   -5.9   ±   0.6   551   ±   41   0.10   	Cep III member	
        
        191 c2	   4.9829   ±   0.0316   16.721   ±   0.054   -0.773   ±   0.055   -7.1   ±   1.3   85.74   ±   0.54   176.2   ±   1.1   43.36   ±   0.28   10.8   ±   0.6   -11.1   ±   1.1   -8.1   ±   0.3   540   ±   95   0.41   	Cep III member	
        
        192		   3.5560   ±   0.0303   17.308   ±   0.050   1.352   ±   0.040   -10.3   ±   0.8   126.1   ±   1.1   249.2   ±   2.1   32.85   ±   0.30   16.0   ±   0.4   -18.9   ±   0.7   -5.2   ±   0.1   313   ±   40   0.17   	Multiple system	
        
        193		   5.9923   ±   0.0252   21.618   ±   0.045   1.055   ±   0.045   -7.59   ±   0.22   79.93   ±   0.34   138.67   ±   0.58   47.25   ±   0.21   10.8   ±   0.1   -14.1   ±   0.2   -5.9   ±   0.1   301   ±   18   0   	Cep II member	
        
        G1		   6.3842   ±   0.0331   23.205   ±   0.046   0.753   ±   0.044   -8.40   ±   0.28   76.17   ±   0.40   128.94   ±   0.67   45.90   ±   0.25   10.3   ±   0.2   -15.1   ±   0.2   -5.8   ±   0.1   209   ±   14   0.08   	VB, Cep II member	
        
        G2 ^   5.7214   ±   0.0317   22.091   ±   0.053   -1.511   ±   0.055   3c…   86.60   ±   0.48   145.53   ±   0.81   43.24   ±   0.25   3c…   3c…   3c…   175   ±   10   …   	VB, Cep III member	
        
        G3 c1	   6.7087   ±   0.0416   20.413   ±   0.100   -1.844   ±   0.062   -9.2   ±   0.1   76.43   ±   0.47   121.03   ±   0.75   41.59   ±   0.27   6.6   ±   0.1   -15.3   ±   0.3   -4.11   ±   0.05   307   ±   12   0.08   	Cep I member	
        
        G3 c2	   6.7211   ±   0.0320   24.902   ±   0.059   -3.909   ±   0.051   -8.7   ±   0.7   76.29   ±   0.36   120.81   ±   0.58   41.51   ±   0.20   9.0   ±   0.4   -16.4   ±   0.6   -6.4   ±   0.2   453   ±   90   0.29   	Cep I member	
        
        G4 ^∗   6.7016   ±   0.0218   23.419   ±   0.059   -3.861   ±   0.035   -9.54   ±   0.41   76.67   ±   0.25   121.03   ±   0.39   41.71   ±   0.14   7.7   ±   0.2   -16.7   ±   0.3   -5.9   ±   0.1   216   ±   17   …   	SB2, VB, Cep I member	
        
        F1 ^   4.7892   ±   0.3432   11.015   ±   0.588   10.377   ±   0.665   -10.01   ±   1.96   52.7   ±   3.9   195   ±   14   52.2   ±   3.8   10.2   ±   1.1   -14.2   ±   1.9   -4.4   ±   1.1   205   ±   62   0   	VB	
        
        F2 ^   5.4139   ±   0.1187   17.066   ±   0.211   7.164   ±   0.191   -7.45   ±   1.80   75.2   ±   1.7   159.7   ±   3.5   54.3   ±   1.2   11.7   ±   0.8   -12.5   ±   1.6   -4.9   ±   0.6   245   ±   50   0.12   	Cep III member	
        
        F3 ^   5.2788   ±   0.0307   18.273   ±   0.050   -0.341   ±   0.050   -5.69   ±   1.00   83.35   ±   0.49   165.13   ±   0.96   40.86   ±   0.25   11.7   ±   0.4   -10.7   ±   0.9   -7.1   ±   0.2   365   ±   44   0.30   	Multi. syst., Cep III member	
        
        F4 ^   4.7005   ±   0.6512   18.328   ±   1.128   0.835   ±   0.968   -9.05   ±   0.72   102   ±   14   178   ±   25   55.7   ±   8.0   11.4   ±   2.5   -16.0   ±   1.4   -6.2   ±   1.1   330   ±   76   0.30   	Cep III member	
        22cmNote.
        ^⋆ If we put two sources on the slit during one IDS observation, the brightest and faintest sources are “c1” and “c2”, respectively.  
        ^† Astrometry from the URAT Parallax Catalog <cit.>.
        ^ Radial velocity and lithium equivalent width from Paper III.
        ^∗ Lithium equivalent width from Paper III. Radial velocity near the conjunction reported in Paper III (i.e., at HJD = 2455077.6191).
        ^△ We used the RV measurement quoted in Gaia DR2 to compute the space-velocity components. 
        rlcrrrrrrrComoving companions of our targets whose names are in bold. We reported the astrometry, G magnitude and radial velocity RV_Gaia released in the Gaia DR2 catalog. We derived their angular separation (ρ), position angle (θ), and projected physical separation (s) with regard to the brightest star, along with the associated errors.
        #   1cGaia DR2 name   1cπ   1cμ_αcosδ   1cμ_δ   1cGmag   1cRV_Gaia   1cρ   1cθ   1cs
              1c[mas]   1c[mas yr^-1]   1c[mas yr^-1]   1c[mag]   1c[km s^-1]   1c[ ± mas]   1c[ ± ]   1c[AU]
        Continued.
        #   1cGaia DR2 name   1cπ   1cμ_αcosδ   1cμ_δ   1cGmag   1cRV_Gaia   1cρ   1cθ   1cs
              1c[mas]   1c[mas yr^-1]   1c[mas yr^-1]   1c[mag]   1c[km s^-1]   1c[ ± mas]   1c[ ± ]   1c[AU]
        
        3    Gaia DR2 394177942214683520    33.8287 ± 0.0602     208.768 ± 0.097   -35.025 ± 0.068   11.8573 ± 0.0010   -12.39 ± 0.56   …   …   …
           Gaia DR2 394177946510277248   33.7578 ± 0.1084     209.999 ± 0.175   -29.251 ± 0.105   14.3724 ± 0.0009   …   2.27± 0.125   300.89± 47.17   67.2±0.1
        
        6    Gaia DR2 564707973733132800    6.4739 ± 0.1404   24.376 ± 0.307   -3.003 ± 0.209   11.6041 ± 0.0081   …   …   …   …
           Gaia DR2 564707973733132032   6.7211 ± 0.0321   23.318 ± 0.061   -2.834 ± 0.046   12.9056 ± 0.0009   -8.34 ± 2.37   12.01 ± 0.127   322.07 ± 3.02   1856 ± 9
           Gaia DR2 564802050695978752    6.9090 ± 0.0928   23.770 ± 0.156   -3.458 ± 0.135   17.1583 ± 0.0013   …   205.48 ±  0.185   358.53 ± 0.05   31740 ± 160
        
         18     Gaia DR2 575921721024508928   6.9947 ± 0.0256   47.790 ± 0.048   -54.249 ± 0.042   12.6970 ± 0.0012   …   …   …   …
           Gaia DR2 575921721024509312    7.0859 ± 0.0239   47.536 ± 0.048   -54.317 ± 0.039   14.2886 ± 0.0005   …   5.84 ± 0.031   224.01 ± 2.03   835.1 ± 3.1
        
        25    Gaia DR2 488038959210617088   9.2418 ± 0.0296   -55.973 ± 0.044   -47.168 ± 0.044   11.9592 ± 0.0005   -24.49 ± 0.67   …   …   …
           Gaia DR2 488038959205988224    9.2593 ± 0.0346   -55.936 ± 0.052   -52.590 ± 0.051   12.4361 ± 0.0018   -42.59 ± 7.78   1.58 ± 0.045   303.83 ± 21.77   170.8 ± 0.5
        
        38    Gaia DR2 479904016269140608    19.1742 ± 0.0778     47.633 ± 0.085   -118.803 ± 0.113   11.4949 ± 0.0017   16.71 ± 0.6   …   …   …
           Gaia DR2 479904016271304704   18.6521 ± 0.1506     51.896 ± 0.184   -120.795 ± 0.266   11.6018 ± 0.0050   …   1.16 ± 0.077   275.43 ± 372.2   60.6 ± 0.2
        
        40    Gaia DR2 1116789731452567936   7.4974 ± 0.0222   -2.118 ± 0.032   19.196 ± 0.040   12.3937 ± 0.0003   -12.18 ± 0.62   …   …   …
           Gaia DR2 1116789735748819968    7.4445 ± 0.0401   -2.593 ± 0.053   16.775 ± 0.078   13.8940 ± 0.0007   …   2.52 ± 0.032   115.13 ± 24.35   336 ± 1
        
        43    Gaia DR2 1152331242957967104   5.7831 ± 0.0218   4.642 ± 0.032   -22.886 ± 0.041   10.7027 ± 0.0012   -60.88 ± 14.28   …   …   …
           Gaia DR2 1152331238662558464    5.9419 ± 0.0331   6.956 ± 0.054   -22.798 ± 0.062   12.2297 ± 0.0002   -24.09 ± 1.36   4.70 ± 0.013   102.13 ± 52.21   812 ± 3
        
        47    Gaia DR2 1138420290562688640   7.9920 ± 0.0264   -7.424 ± 0.037   -89.250 ± 0.049   10.7933 ± 0.0085   …   …   …   …
           Gaia DR2 1138420256203049344    5.6153 ± 0.5873   -6.225 ± 0.929   -91.593 ± 1.173   15.5622 ± 0.0020   …   44.98 ± 0.573   211.14 ± 2.46   5630 ± 19
        
        50    Gaia DR2 1151984484476815360   5.5026 ± 0.0186   -18.795 ± 0.036   -23.996 ± 0.038   10.5904 ± 0.0042   …   …   …   …
           Gaia DR2 1151984484477988096    5.5095 ± 0.0257   -20.891 ± 0.061   -22.002 ± 0.056   14.2201 ± 0.0024   …   2.52 ± 0.028   234.75 ± 9.59   458 ± 2
        
        55    Gaia DR2 1134776955703665280   13.7809 ± 0.0560     -60.794 ± 0.078   -25.573 ± 0.06   10.5182 ± 0.0029   …   …   …   …
           Gaia DR2 1134776955704678656    13.6886 ± 0.1067     -56.688 ± 0.108   -28.878 ± 0.08   13.1162 ± 0.0016   -14.72 ± 4.62   3.77 ± 0.093   26.20 ± 3.86   273 ± 1
        
        56    Gaia DR2 1720278167490425472   3.2342 ± 0.0213   -18.996 ± 0.039   19.453 ± 0.032   11.5351 ± 0.0103   -23.0 ± 18.23   …   …   …
           Gaia DR2 1720278167488409472    2.7156 ± 0.1770   -18.663 ± 0.341   19.584 ± 0.244   17.3547 ± 0.0061   …   2.78 ± 0.112   230.75 ± 23.71   859 ± 6
        
        57    Gaia DR2 1726350151734755200   9.2549 ± 0.0876   -51.835 ± 0.184   -5.563 ± 0.142   12.6675 ± 0.0013   -27.80 ± 6.27   …   …   …
           Gaia DR2 1726350147444401280    9.5762 ± 0.0199   -45.295 ± 0.044   -4.474 ± 0.032   12.8263 ± 0.0040   -19.96 ± 3.41   1.77 ± 0.078   220.33 ± 13.86   191 ± 2
        
         66     Gaia DR2 1698467189688877568   6.6284 ± 0.0305   -38.712 ± 0.052   22.158 ± 0.048   10.9682 ± 0.0013   -8.01 ± 0.74   …   …   …
           Gaia DR2 1698467185393807872    6.6712 ± 0.0818   -36.373 ± 0.156   28.191 ± 0.137   14.4617 ± 0.0010   …   5.37 ± 0.098   34.04 ± 4.566   810 ± 4
        
        69    Gaia DR2 1703801775293097472   20.2010 ± 0.9409     -28.939 ± 1.691   -63.378 ± 1.797   12.7115 ± 0.0014   -3.55 ± 11.63   …   …   …
           Gaia DR2 1703801779587789568    16.7651 ± 0.0512     -24.593 ± 0.120   -56.745 ± 0.094   13.2566 ± 0.0015   …   0.93 ± 0.904   142.97 ± 267.5   46 ± 2
        
        81    Gaia DR2 1723454381704388992   18.4582 ± 0.0300     22.243 ± 0.057   -8.491 ± 0.054   13.0280 ± 0.0008   -5.87 ± 1.68   …   …   …
           Gaia DR2 1723454381704389248    18.4850 ± 0.0246     23.474 ± 0.048   -13.04 ± 0.045   13.4170 ± 0.0006   …   2.78 ± 0.030   121.52 ± 12.19   150.9 ± 0.2
        
        91    Gaia DR2 2253412973338518784   2.9807 ± 0.0777   -17.761 ± 0.147   -6.453 ± 0.196   10.8272 ± 0.0020   -35.88 ± 8.43   …   …   …
           Gaia DR2 2253412969042676736    2.9785 ± 0.1922   -18.378 ± 0.325   -6.364 ± 0.421   18.5588 ± 0.0031   …   18.40 ± 0.269   304.35 ± 11.71   6174 ± 161
        
         100     Gaia DR2 2260807635712585600   7.2575 ± 0.7471   20.703 ± 1.708   55.176 ± 1.547   9.0816 ± 0.0002   -15.97 ± 0.80   …   …   …
           Gaia DR2 2260807635712585472    7.2367 ± 0.0559   21.517 ± 0.124   49.504 ± 0.092   11.2562 ± 0.0006   -17.18 ± 0.37   8.45 ± 0.820   9.85 ± 11.67   1164 ± 120
        
        102    Gaia DR2 2260953836398942336   3.9580 ± 0.0213   6.072 ± 0.042   12.173 ± 0.04   12.0336 ± 0.0007   …   …   …   …
           Gaia DR2 2260953836398942464    3.9283 ± 0.0160   5.779 ± 0.031   11.954 ± 0.03   14.0640 ± 0.0028   …   4.10 ± 0.039   39.65 ±  2.97   1036 ± 6
        
        109    Gaia DR2 2248238121865016576   2.4886 ± 0.0235   6.109 ± 0.047   10.938 ± 0.053   11.0831 ± 0.0041   …   …   …   …
           Gaia DR2 2248237980127605248    1.3161 ± 0.7362   5.041 ± 1.383   10.004 ± 1.785   20.1520 ± 0.0060   …   73.40 ± 0.777   228.14 ± 5.19   29496 ± 279
        
        119    Gaia DR2 2187341189325433472   3.6599 ± 0.0173   7.367 ± 0.033   -7.720 ± 0.035   12.8377 ± 0.0018   …   …   …   …
           Gaia DR2 2187341185028860160    3.7446 ± 0.3248   7.536 ± 0.635   -8.336 ± 0.618   18.9285 ± 0.0033   …   16.67 ± 0.261   108.59 ± 44.52   4555 ± 22
        
        120    Gaia DR2 2245078881361655424   5.7303 ± 0.0288   17.652 ± 0.067   -4.347 ± 0.060   9.8023 ± 0.0007   …   …   …   …
           Gaia DR2 2245078881361655296    5.7351 ± 0.0283   16.396 ± 0.065   -2.411 ± 0.069   11.3453 ± 0.0012   -22.06 ± 1.26   3.29 ± 0.050   288.51 ± 49.46   574 ± 3
        
        123    Gaia DR2 2170325177440567168    3.4592 ± 0.0458   6.629 ± 0.093   6.635 ± 0.089   7.8058 ± 0.0004   …   …   …   …
           Gaia DR2 2170325181728860416    3.4235 ± 0.0432   8.333 ± 0.089   4.261 ± 0.108   9.2669 ± 0.0002   …   1.89 ± 0.063   264.15 ± 1157.8   545 ± 7
           Gaia DR2 2170324941214308992   3.4269 ± 0.0251   8.190 ± 0.050   5.784 ± 0.050   11.3293 ± 0.0012   -21.86 ± 1.54   94.03 ± 0.063   110.92 ± 1.38   27180 ± 360
        
        124    Gaia DR2 2270675683853260672    4.1241 ± 0.0298   9.217 ± 0.049   6.193 ± 0.047   9.4318 ± 0.0003   …   …   …   …
           Gaia DR2 2270675683853258880   4.1805 ± 0.0346   9.568 ± 0.057   6.836 ± 0.057   13.5652 ± 0.0010   -13.47 ± 16.34   23.96 ± 0.030   259.64 ± 16.87   5810 ± 42
        
        125    Gaia DR2 2192552221605362048   3.4229 ± 0.0223   6.410 ± 0.041   6.161 ± 0.042   11.7654 ± 0.0011   -24.71 ± 2.53   …   …   …
           Gaia DR2 2192552221600855168    4.2636 ± 0.2240   5.895 ± 0.407   6.299 ± 0.615   16.0953 ± 0.0080   …   1.39 ± 0.189   75.71 ± 875.0   406 ± 3
           Gaia DR2 2192364548713717632	    1.8968 ± 1.2094   6.057 ± 2.366   7.104 ± 3.024   20.7648 ± 0.0136   …   44.55 ± 1.425   129.23 ± 17.82   13016 ± 85
        
         131     Gaia DR2 2216911008366802304   6.7559 ± 0.0739   30.093 ± 0.165   11.946 ± 0.136   11.2458 ± 0.0014   …   …   …   …
           Gaia DR2 2216910630409680000    6.9383 ± 0.0608   33.032 ± 0.146   11.696 ± 0.127   15.1823 ± 0.0009   …   6.74 ± 0.137   224.17 ± 8.08   998 ± 11
        
        135    Gaia DR2 2202658309713224064   2.4955 ± 0.0229   11.907 ± 0.046   26.296 ± 0.049   11.8941 ± 0.0020   -76.97 ± 17.84   …   …   …
           Gaia DR2 2202656763526368896    2.6578 ± 0.1110   11.862 ± 0.215   26.498 ± 0.212   17.7468 ± 0.0012   …   58.26 ± 0.144   191.86 ± 0.32   23350 ± 214
        
        140    Gaia DR2 2005807146670436608   4.6715 ± 0.0166   15.432 ± 0.028   2.258 ± 0.029   13.1907 ± 0.0010   -19.68 ± 1.90   …   …   …
           Gaia DR2 2005807868208768000    4.1101 ± 1.7711   15.398 ± 3.165   11.763 ± 3.721   20.7617 ± 0.0147   …   27.63 ± 1.664   303.56 ± 46.66   5914 ± 21
        
        144    Gaia DR2 2225093917495923968   8.7382 ± 0.0309   -4.442 ± 0.048   -6.498 ± 0.042   10.6755 ± 0.0009   16.78 ± 12.30   …   …   …
           Gaia DR2 2225093780056968448    8.7790 ± 0.1087   -4.265 ± 0.170   -6.110 ± 0.140   16.6411 ± 0.0022   …   87.47 ± 0.095   233.31 ± 0.71   10010 ± 35
        
        146    Gaia DR2 2211369980859065344   20.4651 ± 0.0262     144.623 ± 0.042   -38.632 ± 0.042   12.0832 ± 0.0008   8.56 ± 10.75   …   …   …
           Gaia DR2 2211369882080370304	    20.5554 ± 0.0594     144.773 ± 0.091   -38.223 ± 0.090   15.4719 ± 0.0005   …   50.66 ± 0.056   112.39 ± 2.29   2475 ± 3
        
        149    Gaia DR2 2014273111312397312   2.2842 ± 0.0251   5.193 ± 0.048   -0.221 ± 0.041   11.2336 ± 0.0010   -8.75 ± 3.61   …   …   …
           Gaia DR2 2014273111308595072    2.4920 ± 0.0913   4.900 ± 0.172   -1.325 ± 0.113   15.0804 ± 0.0054   …   1.68 ± 0.082   181.91 ± 2.42   734 ± 8
           Gaia DR2 2014278952464130688    2.3238 ± 0.1147   6.028 ± 0.247   -1.345 ± 0.310   16.6528 ± 0.0030   …   95.17 ± 0.067   92.99 ± 137.6   41667 ± 458
           Gaia DR2 2014278982529501696	    2.1865 ± 0.4348   5.814 ± 0.778   -1.442 ± 0.654   19.7632 ± 0.0047   …   56.18 ± 0.358   51.68 ± 3.67   24600 ± 270
        
        152    Gaia DR2 2282683892719472640   7.0082 ± 0.0198   22.582 ± 0.037   4.888 ± 0.037   12.2306 ± 0.0030   …   …   …   …
           Gaia DR2 2282683897015937920    7.0380 ± 0.0670   23.568 ± 0.138   6.382 ± 0.129   14.7476 ± 0.0024   …   1.56 ± 0.056   297.25 ± 55.59   222.6 ± 0.6
        
        157    Gaia DR2 2232420856825041920    7.7011 ± 0.0639   10.553 ± 0.082   -1.275 ± 0.070   10.2980 ± 0.0007   -11.77 ± 0.71   …   …   …
           Gaia DR2 2232420856822289408   7.8348 ± 0.0488   8.660 ± 0.064   -1.105 ± 0.073   10.6758 ± 0.0007   -11.72 ± 0.49   17.64 ± 0.050   247.11 ± 6.50   2291 ± 19
        
         160     Gaia DR2 2279559531646356608   2.8245 ± 0.0701   6.988 ± 0.123   0.194 ± 0.112   15.0669 ± 0.0059   …   …   …   …
           Gaia DR2 2279559531646356352    2.8066 ± 0.0903   6.948 ± 0.158   0.858 ± 0.140   16.4999 ± 0.0012   …   5.36 ± 0.089   245.82 ± 32.96   1899 ± 47
        
        170    Gaia DR2 517737008795018624   3.8271 ± 0.0294   35.034 ± 0.033   -24.659 ± 0.041   12.0255 ± 0.0018   13.20 ± 8.43   …   …   …
           Gaia DR2 517736940075550336    3.8645 ± 0.0553   34.923 ± 0.061   -24.626 ± 0.073   16.0898 ± 0.0006   …   65.27 ± 0.058   181.03 ± 0.070   17055 ± 131
        
         175     Gaia DR2 2274551496699656064   7.0641 ± 0.0212   13.429 ± 0.040   18.865 ± 0.038   11.7748 ± 0.0022   -18.98 ± 0.63   …   …   …
           Gaia DR2 2274551496699655808    7.1643 ± 0.0866   14.315 ± 0.152   18.704 ± 0.170   16.8503 ± 0.0016   …   6.41 ± 0.075   295.38 ± 19.76   907 ± 3
        
        178    Gaia DR2 2197589634127618304   4.4875 ± 0.2181   22.593 ± 0.471   24.558 ± 0.447   10.2647 ± 0.0005   …   …   …   …
           Gaia DR2 2197589531048403712    3.9381 ± 0.1092   22.499 ± 0.218   24.416 ± 0.220   18.1145 ± 0.0014   …   59.43 ± 0.353   184.23 ± 0.55   13244 ± 644
        
         184     Gaia DR2 2206637343514771328   3.1496 ± 0.0250   10.564 ± 0.042   -3.011 ± 0.042   12.5093 ± 0.0017   -1.55 ± 3.31   …   …   …
           Gaia DR2 2206637343514769152    3.0842 ± 0.0842   10.685 ± 0.144   -3.222 ± 0.138   17.1744 ± 0.0031   …   8.82 ± 0.050   262.85 ± 157.9   2800 ± 22
        
        188    Gaia DR2 2281573729572210432   5.9488 ± 0.0245   20.620 ± 0.045   4.577 ± 0.043   10.8089 ± 0.0028   -8.84 ± 1.36   …   …   …
           Gaia DR2 2281573733870090240    5.5481 ± 0.2645   21.096 ± 0.446   5.664 ± 0.269   14.6213 ± 0.0085   …   1.39 ± 0.205   9.84 ± 15.41   234 ± 1
        
        191    Gaia DR2 2231866561228307840   5.3870 ± 0.3028   16.134 ± 0.533   1.344 ± 0.628   12.1211 ± 0.0014   -11.41 ± 2.83   …   …   …
           Gaia DR2 2231866565525667712    4.9829 ± 0.0316   16.721 ± 0.054   -0.773 ± 0.055   13.9459 ± 0.0038   …   3.80 ± 0.350   210.74 ± 18.68   706 ± 40
        
         192     Gaia DR2 2214142433789105920   3.5560 ± 0.0303   17.308 ± 0.050   1.352 ± 0.040   12.3241 ± 0.0013   -16.46 ± 4.41   …   …   …
           Gaia DR2 2214142884764242432    3.6330 ± 0.0946   16.939 ± 0.157   1.472 ± 0.118   16.9661 ± 0.0009   …   70.52 ± 0.050   277.48 ± 15.93   19830 ± 170
           Gaia DR2 2214143194002143488    3.9328 ± 0.2903   18.200 ± 0.477   2.197 ± 0.403   18.6291 ± 0.0030   …   9.09 ± 0.258   320.64 ± 8.99   2557 ± 22
        
        G1    Gaia DR2 564638150446547200   6.3842 ± 0.0331   23.205 ± 0.046   0.753 ± 0.044   10.0725 ± 0.0015   -6.89 ± 1.59   …   …   …
           Gaia DR2 564638120384153472    6.3519 ± 0.0500   22.692 ± 0.081   0.081 ± 0.071   15.0214 ± 0.0008   …   20.27 ± 0.023   259.71 ± 20.90   3175 ± 16
        
        G2    Gaia DR2 540216042984524800   5.7214 ± 0.0317   22.091 ± 0.053   -1.511 ± 0.055   9.5837 ± 0.0013   -6.68 ± 2.03   …   …   …
           Gaia DR2 540216042986714368    5.5658 ± 0.0688   21.230 ± 0.211   -3.130 ± 0.239   11.3110 ± 0.0077   …   1.39 ± 0.110   227.82 ± 38.68   243 ± 1
        
         G3     Gaia DR2 564698451788613376   6.7087 ± 0.0416   20.413 ± 0.100   -1.844 ± 0.062   10.2465 ± 0.0019   …   …   …   …
           Gaia DR2 564698451789359104	    6.7211 ± 0.0320   24.902 ± 0.059   -3.909 ± 0.051   13.0051 ± 0.0033   -17.46	 ± 18.82   8.53 ± 0.023   261.12 ± 62.21   1272 ± 8
        
        G4    Gaia DR2 564695879105287936   6.7016 ± 0.0218   23.419 ± 0.059   -3.861 ± 0.035   9.4249 ± 0.0009   …   …   …   …
           Gaia DR2 564695879105289344    6.6812 ± 0.0656   24.390 ± 0.142   -2.793 ± 0.104   16.0252 ± 0.0008   …   15.32 ± 0.074   195.30 ± 0.513   2286 ± 7
        
        F1    Gaia DR2 2270685442018922112   4.7892 ± 0.3432   11.015 ± 0.588   10.377 ± 0.665   10.0239 ± 0.0010   -10.35 ± 1.63   …   …   …
           Gaia DR2 2270685442018921984    5.3159 ± 0.0465   11.187 ± 0.099   8.137 ± 0.086   15.9652 ± 0.0018   …   12.67 ± 0.407   26.44 ± 5.79   2645 ± 190
        
         F3     Gaia DR2 2231801002846066304   5.2788 ± 0.0307   18.273 ± 0.050   -0.341 ± 0.050   9.8850 ± 0.0019   …   …   …   …
           Gaia DR2 2231801007144857856    5.2670 ± 0.0665   17.705 ± 0.118   -0.675 ± 0.113   14.2899 ± 0.0007   …   9.25 ± 0.094   155.79 ± 1.537   1751 ± 10
           Gaia DR2 2231794547514058624    5.1245 ± 0.1204   18.268 ± 0.204   -0.226 ± 0.207   17.6214 ± 0.0022   …   384.01 ± 0.036   89.15 ± 342.3   72746 ± 423
        
        The optically faint candidates (12<V<14.5 mag) were observed with the Intermediate Dispersion Spectrograph (IDS)[http://www.ing.iac.es/Astronomy/instruments/ids/] at the 2.5-m Isaac Newton Telescope (INT) of the Observatorio del Roque de los Muchachos (La Palma, Canary Islands, Spain). We acquired long-slit spectra during several observing runs that took place in 4–10 September 2009, 23–28 November 2010, 24–27 October 2012, 27 March to 2 April 2013, 16–20 November 2013, and 18–20 February 2014. During the observing night of 12 to 13 December 2009, some of our targets were also observed in queue mode. We used a slit width of 095 and the H1800V dispersion grating with the 235 mm Camera (2148×4200 EEV10a CCD detector until 2010 and 2k×4k RED+2 CCD detector since 2012) and with slow-readout mode. We chose the central wavelength of 6500 Å. As the outer regions of the dispersed light beam are severely vignetted by the camera optics, only 2070 of the pixels (roughly from pixel number 1000 to 3070 in the direction of the dispersion) are clear and unvignetted regarding the H1800V grating. This allows for efficient coverage of the wavelength range 6200–6800 Å, with a resolving power of about 9200. For most of our targets and standard stars, we set the slit position angle to the current parallactic angle. Using the typical  IRAF tasks, all spectra were de-biased, flat-fielded, distortion-corrected, wavelength calibrated (using the emission lines of the Cu-Ar and Cu-Ne lamps), and finally normalized to the continuum. When a source was already reported as a visual binary in the literature or was identified as such during our observing runs (i.e., with a small angular separation), we aligned the slit on its position angle to simultaneously acquire the spectra of both sources. In this way we made sure to observe the optical counterpart(s) of the unresolved X-ray source. We subsequently examined whether or not the two stars form a physical binary system. When their seeing profiles are partially overlapped on the CCD, we extracted the two spectra by means of a  IDL code similar to that of <cit.>, rather than the  IRAF task  APALL (see Appendix <ref> for details). The use of a double Gaussian profile optimizes the spectrum extraction of the fainter source, which may be heavily contaminated by the brighter one.
        
        
        We removed the telluric water vapor lines only in the spectral region around the Hα line of every spectrum, in all instrumental setups. We applied a method similar to that described by <cit.> using telluric templates taken with the same instrumentation as the targets. We show a few results for the case of SOPHIE spectra (Fig. <ref>) to illustrate its effectiveness. 
        
        
        Owing to bad weather conditions during our IDS observing runs, we were unable to obtain a spectrum for 35 of our targets. All the unobserved targets have a lower priority because their Galactic latitude is higher than 25 or they were not classified as WTTSs by <cit.>. Figure <ref> shows the spectra acquired in the region around the Liiλ6707.8 lines. 
        
        
        
        
        § ANALYSIS AND RESULTS
        
        
         §.§ Radial velocity and multiplicity
        
        
        We measured the heliocentric radial velocities (RVs) using the cross-correlation technique. We distinguished spectroscopic systems from single stars (or single-lined binaries) based on the number of peaks visible in the cross-correlation function (CCF).  
        
        
        Regarding the IDS data, we cross-correlated each long-slit spectrum of our targets with that of RV-standard stars observed during the same night. For this purpose, we have upgraded the  IDL procedure described in <cit.> and Paper I. We masked the spectral range around the Hα line because of its strong wings and the possible chromospheric emission in the core that can considerably broaden and distort the CCF peak. For the same reason we discarded the spectral regions strongly affected by telluric absorption lines. When only one CCF peak was detected, the code performs an additional analysis to report any asymmetry of the CCF profile, possibly interpreted as an SB2 system observed near the conjunction. Such a procedure is only relevant when the masses of the two stars differ significantly. We computed the errors of the pixel shift from the center of the Gaussian function fitting the CCF. We computed the RV errors as a function of the fitted peak height and the antisymmetric noise through the R factor, as described in <cit.>.
        
        For the FOCES data we derived the RV values with the  IRAF task  FXCOR, by cross-correlating each échelle order of the target spectra with the corresponding one of the most similar RV-standard star, which was acquired during the same run. We discarded the orders heavily contaminated by telluric lines or those including very broad lines and activity indicators, such as the Caii H & K lines, the Balmer series (Hα and Hβ), and the Caii IR triplet lines. We fitted the entire CCF peak with a Gaussian to measure more precisely the RV values, which were obtained as the weighted average of all the individual RV measurements computed by  FXCOR per each échelle order. The resulting RV uncertainty is the standard error of the weighted mean, σ_RV.  
        
        The RV measurements derived from the target spectra acquired with the SOPHIE spectrograph were performed with the cross-correlation analysis that is included in the automatic data-reduction pipeline developed by the OHP staff. We used the most appropriate mask depending on the B–V color index (or spectral type) of the target, among the five available ones. This procedure failed for some of the multiple systems and fast rotators. From a first guess of their spectral type (Sect. <ref>), we selected the most appropriate synthetic spectrum from the POLLUX database <cit.> to be used as template for computing the CCF, which was automatically fitted by a procedure similar to that used for IDS data. Taking advantage of the high resolution of these spectra, we improved the code to detect and fit the CCF peak of a companion even having a much lower brightness in a stellar binary system, that is, with a low mass-ratio. This requires careful analysis of the CCF residues after subtracting the best fit, especially when the two peaks are severely blended (i.e., one CCF peak with an asymmetric shape). 
        
        Table <ref> contains all our RV measurements and associated errors, with one entry for each acquired spectrum and, in case of multiple systems, for each component. 
        
        
        Since our  IDL procedure and the task  FXCOR use the RV-standard stars as templates, we need an accurate RV value for them. So we used the RV measurements available from the Élodie archive,[http://atlas.obs-hp.fr/elodie/] which were derived from high-resolution spectra. Table <ref> lists all these values that agree with those in <cit.> or other compilations of RV measurements <cit.>.
        
        
        For multiple systems, we adopted an independent Gaussian fit for each CCF peak whenever they are not blended (i.e., far from the conjunctions). We used instead a multiple-Gaussian fit algorithm when the spectral lines are partially blended. Moreover, we automatically looked for any significant peaks in the CCF and fitted them with single, double, or multiple functions (i.e., up to four Gaussian profiles), using our  IDL code that computes the CCF and treats the errors as  FXCOR does. We refer the reader to Paper I for details on  this code and its performances.
        
        
        Among the 47 sources observed at multiple epochs, eleven sources display a large variation in radial velocity (Table <ref>). We classified those with RV change significantly larger than the RV errors as single-lined binaries ( SB1) and those with smaller RV variation as possible SB1 systems ( SB1?). We discovered that 44 of the surveyed sources are multiple spectroscopic systems, which are distributed as follow: nine SB1 (4.8 %), 28 double-lined (SB2) plus four likely SB2 (17.2 %), and three triple (SB3;  1.6 %) systems (see Table <ref>). This corresponds to 20 % of the overall sample (i.e., our targets, plus the 20 sources listed in Table <ref> and the eight sources from Papers II and III) and to 24 % of the sources with new observations presented here, as listed in Table <ref>. For the 17 sources classified as possible spectroscopic systems (Table <ref>), additional observations are needed to draw firm conclusions on their multiplicity.   
        
        
        
        
         §.§ Spectral classification and projected rotational velocity
        
        
        We applied the  IDL code  ROTFIT<cit.> to perform the physical characterization of SB1 systems and single stars, that is, those with only one peak in the CCF profile. This code searches for the best combination of parameters by comparing the target spectrum with reference star spectra that are rotationally broadened until a minimum χ^2 was reached. As in our previous works (Papers I and III), we determined the spectral type (SpT), effective temperature (T_ eff), gravity (log g), and metallicity ([Fe/H]) using as templates a library of 270 high-resolution spectra of low-activity and slowly rotating stars retrieved from the Élodie archive <cit.>. For these stars we took the atmospheric parameters (APs) from the PASTEL catalog <cit.>. We report these results in Table <ref> in which any source observed at several epochs[whether with different instruments (usually for the bright sources) or with the same instrumental setting (in case of the faint ones).] has multiple entries. The typical accuracy on the spectral type is about one subclass. We refer the reader to Appendix <ref> for a description of our procedures dedicated to the analysis of the M-type stars.
        
        
        To minimize possible effects on projected rotational velocities (v sin i) due to different resolutions and instrumental setups between the target spectra (acquired with both IDS and FOCES) and the Élodie ones we also used a smaller library of template spectra taken with these spectrographs during our observing runs. Table <ref> lists them as well as all their relevant information. Analogous to the treatment of the full library of Élodie templates, the rotation velocity of each template is progressively increased by convolving its spectrum with a rotational profile of a given v sin i. The best match of the template spectrum with the target spectrum, found by χ^2 minimization, gives us the value of v sin i. We note that most v sin i values derived with the Élodie templates are slightly underestimated compared to those obtained when the spectra are taken with the same instrumental setup. This is probably caused by the resampling of the Élodie spectra on the points of the IDS or FOCES ones. We thus adopted the v sin i values obtained with the template acquired with the same spectrograph as the target (Table <ref>).  At the IDS, FOCES, and SOPHIE resolutions, any vsin i determination is reliable only if the vsin i value is larger than 15 km s^-1, 5 km s^-1, and 2 km s^-1, respectively. We determined these lower limits with simulations similar to those made by <cit.>.
        
        
        
        
         §.§ Stellar luminosity and extinction
        
        
        We analyzed the spectral energy distribution (SED) of our targets with the aim of checking the spectroscopic atmospheric parameters, of estimating the extinction, A_V, and of deriving the stellar luminosities. The BVI_ CJHK_ s SEDs were constructed using the optical and NIR photometric data described in Sect. <ref>. We completed them with mid-infrared photometry provided by the WISE All-Sky survey <cit.>. 
        
        
        Figure <ref> shows the Hertzsprung-Russell (HR) diagram for the targets with accurate parallaxes (Table <ref>) and APs derived in the present study (Table <ref>). For 187 of our targets we made use of the Gaia DR2 parallax, while we adopted the values of 18.4 ± 2.7 mas and 36.0 ± 6.9 mas for the sources #15 and #101, respectively, as quoted in the URAT Parallax Catalog <cit.>. No parallax is available for the remaining four targets. Evidently, the values of log g found by our spectroscopic analysis are fully consistent with the evolutionary status in the HR diagram, demonstrating the reliability of APs derived by  ROTFIT (Sect. <ref>).  Most targets are located close to (or slightly above) the zero-age main sequence (ZAMS) and show log g>3.5. These are good young star candidates. As for the 16 sub-giant or giant stars, the X-ray emission can be related to their evolutionary status or to the presence of an unseen companion, which forces the evolved star into fast rotation.
        
        
        We adopted the grid of NextGen low-resolution synthetic spectra, with log g in the range 3.5–5.0 and solar metallicity by <cit.>, to fit the optical-NIR portion (from B to H band) of the SEDs, in the same way as in Paper III. We fixed T_ eff and log g of each target to the values found with  ROTFIT (Table <ref>) and let the angular stellar diameter and the extinction A_V vary until a minimum χ^2 was reached. For the stars with a known distance, this also provides us with a measure of the stellar radius and luminosity that was obtained by integrating the best-fit model spectrum. As listed in Table <ref>, we found low extinction values (A_V<0.5 mag), with the exception of the more distant targets, which are mostly sub-giant or giant stars.
        
        
        In line with our selection criteria, most of our targets are consistent with late-type stars near the main sequence (Fig. <ref>), with no or low reddening (Table <ref>). These results fully agree with the distribution of our targets in the infrared color-color diagram (Fig. <ref>). We found nine sources that lie outside the locus of main-sequence (MS) stars. For a better readability the source #120 with H–K_ s = -0.152±0.045 mag is not shown. Sources #8 and #160 likely suffer from extinction, as they lie at the upper right corner in the color-color diagram (J–H > 0.9 mag and H–K_ s > 0.3 mag). These color excesses E(J–H) and E(H–K_ s) allow us to estimate their extinction A_V by means of the mid-infrared extinction law of <cit.> and the standard optical one R_V=3.1. We classified the source #8 as a K5 giant star with a temperature T_ eff=3833± 78 K and a surface gravity log g = 2.84 ± 0.44, while its infrared colors place it near the position of an M6 giant star, implying an extinction of ∼2 mag. Moreover, this source is at least 2 mag fainter than giants having a similar J–K_ s color index in the LSPM-North catalog <cit.>. This is consistent with a high reddening, as also indicated by the SED analysis. Source #160 is a known member of the L1251 cloud <cit.> and classified as a WTTS with spectral type K5 <cit.>, implying an extinction of ∼3 mag.
        The other sources outside the locus of MS stars include two visual binary candidates (#102 and #120, see Table <ref>), one spectroscopic system (#20), and four possible single stars (#1, #3, #139, and #165). We note that the entire photometry of the source #139 could be affected by the extended halo of light of the nearby B5 binary V447 Cep (see Appendix <ref>).
        
        
        
        
         §.§ Lithium content and age
        
        
        Lithium is a fragile element that is progressively depleted in the deep convective envelopes of late-type stars where it is brought at temperatures of about 3×10^6 K. Therefore, the strength of the Liiλ6707.8 Å line can be used as an age proxy for dwarfs with spectral type later than mid-G; for these stars, a high lithium abundance is a clear sign of youth <cit.>. 
        
        
        In all instrumental setups used in this study, the lithium line and the nearby Feiλ6707.4 Å line are blended, at least partly. However, when applying the spectral subtraction technique <cit.>, this contamination is automatically corrected because the best-fitted lithium-poor template, which is rotationally broadened by  ROTFIT to the vsin i of the target, faithfully reproduces the spectral behavior around the lithium line (Fig. <ref>). We measured the Lii equivalent width, W_ Li, for the whole sample of single stars and SB1 systems (Table <ref>). We then derived the lithium abundance, log N(Li), based on the <cit.> calculations. 
        
        
        Following the classification of Papers I and III, we defined as Pleiades-like the stars lying between the lower and upper envelopes of the Pleiades cluster in the  T_ eff–W_ Li diagram (filled squares in Fig. <ref>). Since the lower envelope of the Pleiades nearly coincides with the upper envelope of the 300-Myr-old UMa cluster <cit.>, the age of Pleiades-like objects should range between 100 and 300 Myr. Analogously, we have considered as PMS-like the stars lying above the Pleiades upper envelope (filled circles in Fig. <ref>). 
        
        
        In the literature, a significant scattering of log N(Li) was found for stars belonging to the same cluster. This can be due to a real age spread within the cluster or to further parameters affecting the lithium depletion, such as stellar rotation <cit.>. For a field star, this prevents any direct conversion of log N(Li) into age. 
        
        However, a relative age estimate can be obtained by comparing the position in the T_ eff–log N(Li) diagram with that of stars with a well-defined age and similar APs. We therefore overplot the envelopes of clusters IC 2602, Pleiades, and Hyades <cit.>, along with the locus of known members of the β Pictoris and Tucana-Horologium associations whose quoted ages are about 12 and 30 Myr, respectively <cit.>. As a result, most PMS-like stars are distributed similarly to the β Pictoris members and slightly above those of the Tucana-Horologium association (Fig. <ref>).
        
        We got an alternative estimate of the ages of our targets by comparing their position in the HR diagram with pre-main-sequence isochrones from <cit.>, as shown in Fig. <ref>. Most PMS-like stars are located between the isochrones at 10 and 30 Myr, while six sources (#6 c2, #189, #191 c1 & c2, F3, F4) are found between the isochrones at 1 and 10 Myr (Fig. <ref>). This agrees with the young age assumed in Paper II. In contrast, the Pleiades-like stars are mostly below the isochrone at 30 Myr. We are finally able to confirm that all the PMS-like and Pleiades-like sources are likely young stars, with the exception of four sources (#109, #133, #159, #185 c1), which are likely lithium-rich sub-giant or giant stars (Figs. <ref> and <ref>).
        
        
        
        
         §.§ Calculation of spatial-kinematic coordinates
        
        
        To study the kinematics of our targets in the XYZUVW space, we combined the average radial velocities derived in Sect. <ref> with the sky positions, proper motions, and parallaxes reported in Gaia DR2. For sources #15 and #101, we actually derived their kinematics by making use of the sky positions from the 2MASS catalog and the astrometry from the URAT Parallax Catalog. We then computed the Galactic positions (X,Y,Z) and heliocentric space-velocity components (U,V,W) in the left-handed coordinate system.[X and U are pointing towards the Galactic anti-center; Y and V in the Galactic rotation direction; Z and W towards the North Galactic pole.] All these values are listed in Table <ref>.
        
        
        As shown in Fig. <ref>, the (U,V) plane of targets with astrometry and RV measurement (Table <ref>) shows that most PMS-like and Pleiades-like stars are located in the young-disk (YD) population in the solar neighborhood, according to <cit.>. However we found three PMS-like (#35, #146, #185c1) and two Pleiades-like (#46, #109) in the region populated by old-disk stars. While the sources #109 and #185c1 are Li-rich giant stars, additional observations are needed to confirm any possible variation in radial velocities for the others. Our observations reveal that the sources #35, #46, #109 are possible SB2 systems due to a double-peaked Hα profile or their CCF shape (i.e., slightly asymmetric or with a possible small peak below our detection limit; Table <ref>). Regarding source #179, we do not exclude a problem in the wavelength calibration. From our RV value of -147.8±0.8 km s^-1, this source might be located in the old-disk (OD) area. Thus this RV value must be used with care, especially because this source is not a high-proper-motion star and its RV value in Gaia DR2 is of -9.74±2.88 km s^-1, which we use afterwards (Table <ref>). Finally, we note that the signal-to-noise of the spectrum acquired for source #146 is not high enough to obtain an accurate W_ Li value.
        
        
        Figure <ref> shows the distribution of our targets in various 2D planes of the XYZUVW space restricting the parameter ranges to the locus of the young sources. We used the probabilistic approach described in <cit.> to assess their membership to the five young stellar kinematic groups denoted in Fig. <ref>. Their ages are adopted from Table 1 of <cit.>. In the kinematic velocity space, the populations of PMS-like and Pleiades-like stars are located in well-distinguishable regions. On the one hand, the heliocentric space-velocity components of a compact group of PMS-like stars are marginally consistent with those of the Castor moving group. Nevertheless, such a link is hardly compatible because of the age difference between these two groups of young stars, but above all because the PMS-like stars are only weakly dispersed in the XYZUVW space. 
        On the other hand, 75 % of the 12 Pleiades-like single stars with an RV value in Table <ref> have membership probability to the Pleiades moving group larger than 40 %. These nine sources are #16, #22, #102, #112, #123, #125, #129, #151, and #179. Our procedure disregarded two sources  (#31c2, #86) in the YD area due to a space-velocity component W lower than -23 km s^-1, along with source #46 located in the OD area (Fig. <ref>). These three sources probably exhibit some variation in radial velocity.
        
        
        
        
        § DISCUSSION
        
        
        
         §.§ Properties of the sample
        
        
        Our study confirms that the multivariate analysis allows for the optimization of the disentangling of the stellar population from X-ray emitting extragalactic components. In fact, only one (#99) of the 162 sources is wrongly classified as a star due to a rather singular spatial configuration of the different sources (Fig. <ref>) and the photometric properties of this galaxy that are similar to late M-type stars (Appendix <ref>). The main stellar populations in our sample are young objects, multiple systems (Appendix <ref>), and low-mass stars (Appendix <ref>). This latter group includes 36 M-type dwarfs (i.e., from M0 to M4.5; see Table <ref>).
        
        
        We selected young stars more efficiently than in our previous works. This may be linked to a sampling of more distant sources in comparison to previous studies, as explained by the Gould Disk scenario <cit.>. It could also be related to the sky region considered here in which stars younger than 30 Myr are found at three different distance scales: the visual binary V368 Cep and its comoving companion NLTT 56725 <cit.>, the Cepheus association (Table <ref>), and the Cepheus Flare region <cit.>.
        
        
        We identified 59 lithium-rich sources. Most of them prove to be young but four sub-giant or giant stars also display a strong lithium line in absorption (Sect. <ref>). This is consistent with the discovery of several lithium-rich giants from our previous studies of the stellar X-ray population (Papers I and III). We classified 18 targets as Pleiades-like sources (age =100–300 Myr) and 37 as PMS stars (age =10–30 Myr). These two distinct stellar populations are found in different sky areas (Fig. <ref>). While the former are mainly located towards the Galactic plane, the latter are mostly projected in front of the CO Cepheus void, in the Cepheus Flare region. 
        
        
        During our survey of 186 sources, we identified 44 (24 %) spectroscopic multiple systems. This fraction is 30 % lower with respect to Papers I and III. Nine and six of them also display a strong and very strong lithium line (Table <ref>), respectively. Using Gaia DR2 data, we found that 40 of our targets and six of eight young stars in Papers II and III have comoving companions with an angular separation ranging from a few arcsecond to a few arcmin (Table <ref>). Five of these visual binaries (#6, #18, #119, #131, G4) also have one component classified as an SB2 system. They are, therefore, likely hierarchical triple systems. 
        
        
        
        
         §.§ Young stars towards the CO Cepheus void
        
        
        The possible detection of a new young association in Cepheus (age =10–20 Myr; Paper II) is supported by our identification of 20 PMS stars (plus three small-separation companions observed during our spectroscopic campaigns) in the same region (Fig. <ref>) and our discovery of their eight comoving companions (Table <ref>). These are overplotted on the visible extinction A_V,RQ map of <cit.>,[The map results from the renormalization of the visible extinction one based on the analysis of quasi-stellar objects observed in the Sloan Digital Sky Survey. This A_V,RQ map is available from the Planck Legacy Archive (http://pla.esac.esa.int/pla/#home) and corresponds to the file: 
        COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits[AV_RQ].] derived from the thermal dust emission modeling presented by <cit.>. The PMS stars are highly clumped near the Galactic coordinates (X,Y,Z) = (76, 130, 43) pc (Fig. <ref>). To better see their distribution, we zoomed in this smaller region (Fig. <ref>). 
        
        
        Almost all PMS stars towards the CO Cepheus void are related to the Cepheus association (Fig. <ref>), except for sources #160 and #189 that are located at larger distances (354±9 and 320±97 pc, respectively). The former is a known member of the molecular cloud L1251 (see Sect. <ref>), while the astrometry of the latter suffers from large uncertainties. According to the 6D phase-space data of the remaining PMS stars in this restricted area, we can divide them into three subgroups, as explained below. We summarize their properties in Table <ref>.
        
        We first identified the highest density of PMS stars in the projection of the sky positions (Fig. <ref>) and in the various planes in Galactic coordinates (Fig. <ref>). Up to now, this group (henceforth Cep I) is composed of one visual binary (G3) and two triple hierarchical systems (#6 and G4). It is highlighted by a hexagon in Figs. <ref> and <ref>.  Moreover, source #6 has an additional wide-separation companion (Appendix <ref>).
        
        Five additional young sources with similar properties are located in a more extended area (henceforth Cep II; cyan circles in Figs. <ref> and <ref>). In addition to the three Cep I members, this group includes two single stars (#158 and #193), one SB1 system (#153), and two visual binaries (#188 and G1). 
        
        Finally, the largest group (henceforth Cep III; blue circles in Figs. <ref> and <ref>) is composed of five single stars (#142, #182, #186, F2, F4), one SB1 system (#156), four visual binaries (#152, #191, G2 and F3), and the Cep II members. The source F3 has also a wide-separation companion (Table <ref>). 
        
        
        
        
         §.§ Additional CO Cepheus void stars from Gaia
        
        
        To see the extent of the association in Cepheus, we built a new sample that is hereinafter referred to as Gaia–2MASS. We selected all sources brighter than K_ s = 12 mag from the PPMXL catalog <cit.>, using a cone search centered at (RA, DEC) = (0h, +77) with a radius of 6, which covers all the sky area devoid of interstellar matter. Subsequently we matched this dataset with Gaia DR2 (radius =1). 
        
        
        An asymmetry is clearly visible in the distribution of the proper motions in right ascension (middle panels of Fig. <ref>), in particular in the range of proper motions of the members of the Cepheus association (delimited by vertical lines). This results in an excess of sources with positive μ_αcosδ values with respect to a normal symmetric distribution. The total number of the excess Gaia–2MASS sources is significantly larger than the number of young stars identified up to now in the CO Cepheus void. To search for a possible link between this excess of Gaia–2MASS stars and the Cepheus association, we performed a comparison with a simulation based on the Besançon model <cit.>. 
         
        Due to the right ascension of the members of the Cepheus association ranging from 22h to 1h, we have to use a rectangular area covering Galactic longitude l ranging from 114 to 126 and Galactic latitude b from 85 to 205, together with the same cut in K_s magnitude that we had applied to build the Gaia–2MASS sample. This region slightly differs from the area covered by the selected Gaia–2MASS sources but both are consistent in terms of number of sources. The distributions of distance and proper motions are well reproduced by the simulation for both cases of the maximum distance threshold considered here (400 and 1000 pc; Fig. <ref>). Therefore, the asymmetry seen in the distribution of the μ_αcosδ values is likely due to large-scale dynamical processes in the Galaxy rather than the result of the unknown supernova shock expected to be at the origin of the CO Cepheus void <cit.>. Thus, this excess alone cannot be used as a criterion to identify possible new members in this young association and a deeper analysis is required. 
        
        To this end, we compared the density map obtained from the Gaia-2MASS sources and the Besançon model (Fig. <ref>). While the (μ_δ, distance) diagram looks the same for the Gaia–2MASS distribution and the Besançon model, the (μ_αcosδ, distance) diagram reveals a clear over-density in the Gaia–2MASS sample (delimited by the polygonal shape). Coupled to the location of members of the Cepheus association on this density map  (Fig. <ref>), it is indisputable that the excess Gaia–2MASS sources are attributable to the  young stars in this region. These are the best member candidates to the Cepheus association to investigate with future observations.
        
        
        
        
         §.§ Cepheus association and runaway stars
        <cit.> discovered an excess of stellar X-ray sources in Cepheus where <cit.>, and Papers II and III had identified together 15 young stars belonging to the association. The current study has added 14 new members (i.e., six PMS stars and eight comoving companions of these 21 young stars).  
        
        
        All but two PMS stars towards the CO Cepheus void have the same kinematic properties (Table <ref>) and therefore a common origin. We also found that eight of the young stars in <cit.> belong to this association, confirming their assumption. The discovery of such a large number of young stars in this region is more easily explained by the in-situ model than by the runaway hypothesis. As mentioned by <cit.> and Paper II, these sources are close to a faint, low density cloud that could be the remnant of the parent cloud already dissipated. 
        
        
        We see a decline in multiple systems and a shift from the mean Galactic position Y to positive values in the more scattered group (Cep III) with respect to the densest group (Cep I). This agrees with the dispersion of the cluster members driven by the rotation of the Galaxy. This also explains the gradient found in the (μ_αcosδ, distance) diagram (Fig. <ref>) because the members of the most extended stellar group tend to move further away from the others. Based on Table <ref>, the properties of the three stellar groups could be interpreted as follows: i) the strongest concentration of young stars (Cep I) could be the remnant of the past Cepheus cluster core, ii) the sources belonging to the group Cep II could correspond to the members that are still gravitationally bound, and iii) the most extended group (Cep III) denotes the original cluster. The latter corresponds to the Cepheus association reported in Paper II. 
        
        
        The group 38 of <cit.> and <cit.> actually coincides with the Cepheus association analyzed here and lists three additional members (HIP 115764, HIP 117376, and TYC 4500-616-1). Their astrometries and the RV value of TYC 4500-616-1 in Gaia DR2 perfectly agree with those of the Cep II members (Fig. <ref>), while the RV value of HIP 117376  suggests a possible variation in radial velocity. The source HIP 115764 would be the warmest member of the association with an effective temperature of 8020_-140^+420 K in Gaia DR2. We also note that the angular separation between HIP 117376 and our target #158 is about 830±0.044 mas. This brings the number of current bona fide members to 32.
        
        
        We discovered six PMS stars outside the CO Cepheus void (#93, #106 c1, #115, #124, #150, and F1) with space-velocity components similar to the members of the Cepheus association. These correspond to the red circles in the (U, W) plane of Fig. <ref>. Their distances range from 160 to 240 pc, except for #150 (distance = 375±3 pc). The five remaining sources (and their two comoving companions; Table <ref>) could be runaway stars. This list of sources includes one of the PMS stars from Paper III and one WTTS from <cit.>. 
        
        
        
        
        § CONCLUSIONS
        
        
        We present the results of a spectroscopic survey of optical counterparts of X-ray sources in the Cepheus region (near the North Celestial pole) aimed at discovering further young objects around the four comoving stars reported by us in Paper II. Based on multivariate analysis methods, we selected optical and infrared counterparts of ROSAT All-Sky Survey and XMM-Newton X-ray sources, which are young star candidates. The analysis of the spectra of these candidates allowed us to determine their atmospheric parameters, radial and rotational velocities, and atmospheric lithium content. These data, along with the parallaxes and proper motions from the Gaia DR2 catalog, were used to characterize our sample and identify new young stars in this region. The main stellar populations composing this sample are young or active stars and multiple systems. We identified two distinct populations of young stars that are spatially and kinematically separated. The 18 Pleiades-like objects with an age between 100 and 300 Myr are mostly projected towards the Galactic plane, while 23 of the 37 sources younger than 30 Myr are located in the sky area of 8 degree-diameter filling the CO Cepheus void. Among these, 21 PMS stars (including five spectroscopic binaries) and their eight comoving companions belong to the Cepheus association, which is the first nearby (distance =157± 10 pc) young (age = 10–20 Myr) stellar association found northward of δ = +30. 
        
        
        We provide the first comprehensive view of the Cepheus association. All studies carried out so far in this sky region have found a total of 32 bona fide members and nine member candidates of this young association, to which 14 (44 %) members and six (67 %) candidates are new discoveries. The kinematics of its members reveals a substantial mixture of the original cluster within the local population of the Galactic plane. The runaway hypothesis is highly improbable for explaining the formation of this homogeneous stellar group because of their kinematic properties and the identification of several new members. This raises the question of the in-situ star-formation scenario in low-mass cloud environments (as in many other SFRs). 
        
        
        Coupled to the Cepheus association properties derived from the current analysis, our Gaia-2MASS sample should contribute to the identification of new candidates to be followed up in the future.
        
        
        
        We thank the anonymous referee for useful suggestions. 
        This work is supported by the Universidad Complutense de Madrid and Spanish Ministerio de Ciencia e Innovación y Universidades (MICINN) under grant AYA2016-79425-C3-1-P. 
        A.K. and D.M. were also supported by AstroMadrid (CAM S2009/ESP-1496), and MICINN under grants AYA2008-00695 and AYA2008-06423-C03-03. 
        Part of this study is also supported by the Italian Ministero dell'Istruzione, Università e Ricerca (MIUR), the French Centre National d'Études spatiales (CNES), and the Région Alsace. 
        This research made use of the SIMBAD database, the VIZIER catalog access and the X-Match service, which are operated at the Centre de Données astronomiques de Strasbourg (CDS). 
        This publication makes use of the data products from ROSAT and XMM-Newton X-ray observatories, the Two Micron All Sky Survey, and the European Space Agency (ESA) missions Gaia and Planck. 
        The ROSAT All-Sky Survey catalogs were produced by the ROSAT Scientific Data Center at the Max-Planck-Institut für Extraterrestrische Physik (MPE), Garching (Germany).
        The 2XMMi-DR3 catalog is the fifth publicly released XMM-Newton X-ray source catalog produced by the XMM-Newton Survey Science Centre (SSC) consortium on behalf of ESA. The 2XMMi-DR3 is one of two incremental versions of the 2XMM catalog.
        The Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, was funded by the National Aeronautics and Space Administration and the National Science Foundation. 
        The data from the ESA mission Gaia (<https://www.cosmos.esa.int/gaia>) was processed by the Gaia Data Processing and Analysis Consortium (DPAC, <https://www.cosmos.esa.int/web/gaia/dpac/consortium>). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
        Planck (http://www.esa.int/Planck) is an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. 
        This publication used the POLLUX database (http://pollux.graal.univ-montp2.fr) operated at LUPM (Laboratoire Univers et Particules de Montpellier, Université Montpellier II – CNRS, France) with the support of the French Programme National de Physique Stellaire and Institut national des sciences de l'Univers.
        aa
        
        § EXTRACTION OF SPECTRA OF BINARY-PAIR CANDIDATES WITH A DOUBLE GAUSSIAN PROFILE
        
        
        To benefit from the IDS instrumental setup, we sought to identify possible binary-pair candidates within our target list before starting our observing runs. However, during the observations themselves, we found additional likely visual binaries having a lower angular separation. We did not identify them previously because the resolution of public images is not enough to resolve such binaries with sufficient confidence, before the launch of Gaia observatory. In such cases, we oriented the slit with the position angle of the two components to simultaneously image them. Hereafter, we illustrate this work on the source #40 (= 1RXS J061946.4+771933) because the alignment of three sources allows us to validate our work process. 
        
        
        The source 2MASS J06194548+7719330 seems to have a weakly-elongated shape with respect to that of nearby stars (Fig. <ref>), which is typical of unresolved binaries and sources with a low angular separation. During our observing runs because we actually saw two sources close to the coordinates of our candidate. These turn out to be comoving stars (Table <ref>). To position the slit on these two objects, we then set the slit position angle to about 114. Based on the Gaia DR2 coordinates, this angle is rather similar to the position angle θ of 11513±2435 between these two sources, and of 11444±295 between the source #40 and 2MASS J06195324+7719222. On the cuts perpendicular to the spectral direction, the aperture of the three components are clearly visible, regardless of the line used, even if the apertures C1 and C2 are partially blended (Fig. <ref>). 
        
        
        We firstly used the procedure of extraction within the  IRAF environment,  APALL. As the spectrum obtained from the second aperture (C2) was contaminated by the light of the bright source (C1), we needed to perform an extraction by means of a double Gaussian profile in order to accurately fit each trace and thus substantially reduce such a contamination. In this context, we adapted the code of <cit.> to the IDS data. As the 235 mm camera optics severely vignettes the outer regions of the dispersed light beam, only 2070 of the CCD pixels are useful for the H1800V dispersion grating (Fig. <ref>). We determined the shape of each aperture by fitting all the perpendicular cuts along the spectral direction of clear and unvignetted lines. We extracted the two spectra from the partially blended apertures C1 and C2 using a double Gaussian profile, while we fitted the third aperture (C3) with an additional simple Gaussian profile. The traces for the three sources are displayed on Fig. <ref>. 
        
        
        Using the 2MASS, NOMAD, and WISE coordinates, we found a spatial scale of 0.42–0.43 arcsec/pixel. This agrees with the value of 0.44 arcsec/pixel tabulated for this detector. From the clear and unvignetted lines, we found an average gap of 5.8±0.1 and 65.0±0.1 pixels between the main aperture (C1) and the two others (C2 and C3, respectively). These correspond to an angular separation ρ of 249 ± 007 and 280 ± 04. These are consistent with the angular separation derived from the 2MASS coordinates (ρ_C_1-C_3 = 27707±0079) and the Gaia DR2 ones (ρ_C_1-C_2 = 252±0.032 mas and ρ_C_1-C_3 = 2839±0.040 mas). 
        
        
        
        § MULTIPLE SYSTEMS
        
        
        The main goal of this analysis is to identify all the members of the Cepheus association among our targets and to derive the maximum information about their physical and kinematic properties. This includes their multiplicity on both small (i.e., spectroscopic systems or visual binaries with small angular separation) and large (i.e., common proper-motion binaries) scales. 
        
        
        
         §.§ Binary-pair candidates
        
        
        During our observing runs with the IDS spectrograph, it has happened that two sources are located at the coordinates of our targets. To be sure to observe the optical counterpart(s) of the unresolved X-ray source, we oriented the spectrograph slit with the position angle of such a binary-pair candidate to image them simultaneously. For the 18 targets listed in Table <ref> we acquired their long-slit spectra to characterize both of them. We subsequently determined if they are physically associated or if that is just a spurious association. We note that the sources #6 and #40 have two entries in this Table. Since the separation between the two apertures was large enough to avoid any contamination of the spectrum extracted from the second aperture by the light of the bright source (and for the sake of homogenization of data reduction), we used the procedure of extraction within the  IRAF environment,  APALL, with the exception of the source #40. Nevertheless, we applied the procedure detailed in Appendix <ref> to estimate the average separation in pixels between the two apertures. We then converted it into an angular separation ρ according to the spatial scale indicated above.
        
        
        Based on our estimate of the angular separation and the position angle value recorded in the header of the raw data, we were able to identify each of sources located near one of our targets by relying mainly on the Gaia DR2 catalog (Table <ref>). 
        
        
        
         §.§ Comoving stars in Gaia DR2
        
        
        To search for any common proper-motion companions to our targets, we made use of a search cone of a radius of 2 around each of them in Gaia DR2. Taking advantage of the very accurate astrometry in this catalog, we found comoving stars for 46 of our targets (Table <ref>). In 90 % of cases, we identified one companion only. Nevertheless, the sources #123, #125, #192, and F3 have two comoving companions, while we are able to list three for source #149. These five targets have one close companion (ρ < 10) and at least another more distant one (ρ > 40). 
        
        For the closest systems (π⩾4 mas), we also extended the radius of search cone up to 10. We then found that i) the source #6 has another common proper-motion companion with a large angular separation (ρ=344 ± 0.185 mas) and ii) the sources G3 and G4 are separated by 496 ± 0.033 mas. 
        
        
        
         §.§ Spectroscopic systems
        
        Table <ref> lists 44 spectroscopic systems found from our analysis of the CCF profiles (Sect. <ref>). We also include 17 possible spectroscopic systems for which the CCF profile is slightly asymmetric or the profile of the Hα line is double-peaked. In the latter case, the absence of a second peak in the CCF profile can be explained by a mass ratio of the two sources much different from 1, but that the activity of the fainter star is sufficiently strong so that its Hα line is visible in the spectrum obtained during the combined observation of the two sources. 
        
         
        Table <ref> also highlights the lithium-rich systems. Except for the SB1 systems, the determination of W_ Li value for each component of the SB2 and SB3 systems goes beyond the scope of the work presented here (see  and  for a detailed analysis of SB2 and SB3 systems, respectively). We therefore decided to characterize the profile of the multiple Lii λ6707.8 lines qualitatively. To this end, we compared their intensity with respect to that of the nearby Cai λ6717.7 line. We selected any system with Lii lines  deeper than about the half of the Cai ones. We divided them into two groups by assuming that the Lii lines deeper than about the Cai ones are very strong. The remaining sources are therefore listed as displaying a strong lithium line. Among the 44 spectroscopic systems, the lithium line is visible in the spectrum of 22 (50 %) sources. This includes nine (20 %) and six sources (14 %) with a strong and very strong lithium line, respectively.
        
        
        Figure <ref> displays the complexity of some systems and the need to carefully analyze the CCF residues after subtracting the fitting, especially when the two peaks are severely blended (i.e., one peak with a clearly asymmetric shape) on several orders. We consider the source #10 as an SB2 system observed near the conjunction but we have also to point out the possible detection of an additional smaller peak in its CCF profile. However its amplitude remains below our threshold. 
        
        
        
        § LOW-MASS STARS
        
        
        We used Eq. (12) from <cit.> to convert the V–J color index listed in the Table <ref> into spectral type. We found that 45 of our targets are likely M-type stars (Table <ref>). For six of them (#20, #48, #54, #61, #62, #69), we were not able to acquire a spectrum to confirm this classification. 
        
        
        Due to their low luminosity and our observational strategy, the survey of low-mass stars could only be conducted with the IDS spectrograph. For these sources, we normalized the spectra in two different ways to perform their spectral typing. 
        
        First, we defined the pseudo-continuum as a smooth line passing through the heads of molecular bands <cit.>. In this way, all the molecular bands are fully in absorption and only the band-heads reach the 1.0 level. Such a task is impossible to be performed automatically. Normalized spectra are obtained by dividing each target spectrum by its continuum. This optimizes the comparison of our spectra with the Élodie library of standard stars, within the code  ROTFIT. We refer the reader to <cit.> for an application of this code to M-type stars. The results are listed in Table <ref>. 
        
        Secondly, we divided each target spectrum by the continuum level in the spectral region near the Hα line. This procedure allows us to perform the spectral typing of the M-type stars through a comparative analysis of the spectral shape of our targets with those of standard stars observed with the same instrumental setup (Table <ref>). To this end, we discarded the wavelength ranges contaminated by strong telluric lines or by chromospheric activity (e.g., the Balmer series). We looked for the best matches by means of a least-square minimization technique similar to that used by <cit.> for the M-type stars from the CARMENES Input Catalog <cit.>. Based on an internal comparison of the CARMENES results as well as with three independent works, <cit.> highlighted the reliability of this approach. The spectral typing resulting from both our procedures are fully compatible with each other. Table <ref> compares the spectral-type classifications resulting from our analysis with those available in the literature, and shows that they agree with each other with an accuracy of about one subclass. We finally found that three of these low-mass stars are late-K stars rather than early-M ones. Figure <ref> shows the spectra of the 36 surveyed M-type stars, sorted by spectral type (from M0 to M4.5).
        
        
        
        § INFORMATION ABOUT SOME STARS
        
          * 1RXS J003904.2+791912 (Source #6): 
        The infrared counterpart identified for this source corresponds to the faint companion of the source [TNK2005] 5 that is known as a WTTS in Cepheus <cit.>. Our target was only detected in photometry and classified as an M2-type companion candidate by the aforementioned authors. During one of our observing nights, both components were positioned simultaneously on the slit. These display a deep lithium absorption and the brightest component is an SB2 system (Fig. <ref>). Based on our analysis, this source therefore is a hierarchical triple system composed of a close inner binary plus a tertiary component in a long-period orbit. Moreover, we found an additional wide-separation companion (ρ=344 ± 0.185 mas; see Table <ref>).  All these stars are associated to Cep I.
        
        
          * 1RXS J010112.8+570839 (Source #8): 
        
        While its intrinsic color agrees with a late-M giant (see Fig. <ref>, along with Fig. 2 of ), we classified it as a K5 giant with a large uncertainty on its surface gravity (log g = 4.20 ± 0.95 dex). This is consistent with the extinction of A_V∼0.94 mag derived from our SED analysis (Sect. <ref>). Moreover, this source is more than 2 mag fainter compared to giants included in the LSPM-North catalog <cit.>, with a similar J–K_ s color index. 
        
        
          * 1RXS J174104.6+842458 (Source #81): 
        This visual binary is composed of an M1 and an M2.5-type star, with a small angular separation (Table <ref>). These are the only M-type stars displaying the Heiλ6678 Å line in emission (Fig. <ref>).
        
        
          * 1RXS J185131.1+584258 (Source #92): 
        
        We observed this source thrice. At the first epoch, it appears as an SB3 system. We then re-observed this star during our IDS runs in order to learn more about the temporal variation of this system. Since the source turned out to be an SB2 system, we repeated the observation. Within this time span of about one day its spectrum has drastically changed and a third peaks is clearly visible in the CCF profile (Fig. <ref>). At this stage, it is complicated to put forward any hypothesis about the dynamics of this system, but the radial velocity of the three components seem to change quickly. This is in contrast with the three SB3 systems analyzed by <cit.>.
        
        
          * 1RXS J192215.6+673918 (Source #99): 
        
        We selected the source 2MASS J19221478+6739142 as its infrared counterpart. With an angular separation of ∼642, this source fulfilled all our criteria. Its infrared colors suggest a late M-type star according to <cit.>. At this position, however, we observed a giant star (T_ eff = 4835±102 K, log g = 2.80±0.23 dex, and spectral type = G9 III) with a small lithium absorption line: EW(Li)  =16 ± 11 mÅ, and log N(Li) ∼ 0.9 dex. Seeking to understand the inconsistency between the photometric and spectroscopic data, we found that  2MASX 19221485+6739143 from the catalog of the 2MASS extended sources <cit.> has similar coordinates. Therefore the infrared counterpart of this target is indeed the galaxy GALEX J192214.8+673914. 
        
        
        It appears that we observed the source TYC 4444-1831-1 (or 2MASS J19221289+6739053) that is somewhat more distant with a separation of  ∼2042 to the X-ray source. We illustrated the space configuration of these three sources on Fig. <ref>. Moreover, its photometry is consistent with a late-G or early-K star and its small proper motions are in agreement with the expectation for a giant star. The probabilities of <cit.> are rather close that the radio/X-ray association is erroneous (51 %) and this X-ray source is a star (42 %), while the probability to be a galaxy is only of 7 %. 
        
        
          * 1RXS J221055.6+632339 (Source #139): 
        
        As in <cit.>, we consider the early-type star STF 2879 C (Fig. <ref>) as being its optical counterpart due to its B–V color index of about 0.75±0.44 mag from the GSC II photometric data. In contrast, the APASS catalog reported a more reliable color index (B–V=0.320±0.031 mag). This source has probably passed through the cracks because of its proximity to the B5 binary V447 Cep whose extended halo of light could affect the entire photometry of our target (Fig. <ref>). Nevertheless, the particularity of this source is not limited to this aspect. Its magnitudes quoted in the final release of the WISE all-sky survey catalog are also atypical. With a W1 magnitude of 10.819±0.023 mag and a W1–W4 of 4.691±0.050 mag, this source falls in the area mainly populated by T Tauri stars displaying an infrared excess (Guillout, priv. com.). 
        
        
          * 1RXS 184257 (Source #160):
        This source <cit.> is too faint in optical to acquire a spectrum with the instruments at our disposal in a reasonable exposure time. It is known as a visual binary whose primary component is a young star (1-Myr-old WTTS in  or a CTTS in ) and one of the strongest X-ray emitters during the XMM-Newton and Chandra observations of the L1251 cloud <cit.>. 
        
        
          * 1RXS J003941.9+790526 (Source G4):
        We followed a procedure similar to <cit.> to derive its orbital parameters. For this purpose we combined the radial velocities that we previously reported in Paper III with those obtained during the observing runs analyzed in the current paper. However it turns out that most measurements (HJD =2455077–2455111) only cover half of the orbit of this system. From our preliminary analysis the period would be estimated at ∼70 days.
        
        
        
        § ADDITIONAL MATERIALS ONLINE
        
        
        All long online tables are available at the CDS. Table <ref> summarizes the optical and infrared names of each X-ray source, along with those appearing in Simbad and some main parameters coming from the literature. The three additional online tables present our results. Table <ref> reports the radial velocity of all the stars, including the measurements for each component of a spectroscopic system, along with the rotational velocity, atmospheric parameters, and lithium equivalent widths derived for the targets identified as single stars or SB1 systems. Table <ref> provides the astrometry in Gaia DR2, the Galactic positions, and the extinction estimate of our targets, as well as the space velocities of those identified as single stars. Table <ref>  lists all the sources that are comoving with one of our targets. 
        
        
        To derive the radial and rotational velocities of our targets and to perform their spectral typing, we made use of a smaller library of template spectra taken with FOCES and IDS during our observing runs. Their spectral type, atmospheric parameters, and radial and rotational velocities are given in Table <ref>. 
        
        
        We show the efficiency of our procedure for removing telluric lines in the case of a few SOPHIE spectra (Fig. <ref>). For each target observed during our survey, we display only one spectrum in the region around the Liiλ6707.8 line (Fig. <ref>).
