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Beatdown: Benson Henderson
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Benson Henderson joined the Beatdown crew on Wednesday.
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Beatdown: John Dodson, Weidman Trainer Ray Longo May 27, 2015 Cheap Seats: UFC 187 Recap, Listener Calls May 26, 2015 Beatdown After The Bell: UFC 187 Johnson Vs Cormier May 23, 2015 Roundtable: UFC 187 Johnson Vs Cormier May 22, 2015 Beatdown: 'The Carny' Nik Lentz May 20, 2015


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$175.00 1 bid <1m
Vintage High School Class Ring from Benedictine Military High School in Savannah GA. Class of 1950. 10 Karat Yellow Gold. Weight - 10 grams. Size men's 10.5. Interior stamp MJ10K.
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Amyris, Inc. (NASDAQ:AMRS)
- Quote
- Commentary
- Scorecard
- Historical Prices
- Chart
- Stats
- Ratios
- Earnings/Growth Rates
- Statements
- SEC Filings
- Show Me:
- Sort by:
No tangible book. No profits in the last year and no earnings in the last year. Currently anything speculative is being punished severely in the market. Expect AMRS to be punished, too.
Just read Maxx's article. http://www.fool.com/investing/general/2014/03/12/can-amyris-inc-save-deep-sea-sharks-and-expand-thi.aspx At this price, I think it's worth taking a shot.
Short. Former Biopharma company, now specialty chem. Revs down 73% Issuing tons of stock and debt.
Biofuel>> until the company produces for the market it will be speculative, but when it does it might be too late to get in ~early.
Its a strong company with many potential technologies. Green tech is growing rapidly
It is a biochemical company which can turn plant sugars into more valuable commodities using designer microbes, an entirely new human capability. The company is ran by idealistic, practical leaders, with special strength in several nations, e.g. Brazil.
AMRS is undervalued at these levels. There is resistance at the $20.50 level. If it breaks $21 is could squirt all the way to $30 in no time. They are well backed and respected in the VC community.
On the cusp of profitability and have gained capital through the IPO.
Weakening Earnings Opinion
Here's the buy rec:
The long term arc is that oil is going to cost more and more to extract. This company's products OTOH need no refining and have an abundantly available feedstock. They can be shunted into pathways for use as gasoline, diesel, or jet fuel substitutes and exceed the original's performance. And eventually aviation will be charged for its carbon emissions as well, justifying an additional premium for this alternative.
Meanwhile the company will eke by at first by producing other specialty products as they get their production costs down and the costs of oil and associated with its use go up. I suspect that "capital light" may even eventually mean selling just the bugs as IP.
A long term play but worth it for an investor with tolerance for risk and a long term horizon.


text:
General Resources
Glossary that gives brief definitions of archaeological terms. Good for a quick "look up" of words.
Basic Information
Handbook of South American Archaeology
Publication Date: 2008
Be sure to use the "within this book" box to search for your information.
South America, ca. 1892
Other Resources on South America
South American Atlas: Maps and Online Resources
Map of South America and articles on flags, geography, history, statistics, disasters current events, and international relations. Allows you to call up information on each country.
HowStuffWorks: "Physiological Features of South America"
Describes the physical features of South America.
ArchNet -- South America: Resources
Mix of print, electronic, and online resources dealing with archaeology in South America. The site is maintained by the Archaeological Research Institute at Arizona State University.
Anthropology and Human Environmental Sciences Librarian
Contact Info
2-1 Young Library
Send Email
Profile & Guides
International Programs
Contact Info
Director of UK Libraries International Programs
1-85 William T. Young Library
Send Email
Profile & Guides


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I'm dipping into this bio now, and man, Gia sounds like a total mess. The mother sounds selfish and delusional, and her dad was apparently a total violent pig. Whatever happened to Elyssa Golden, her longtime GF? Did Sandy Linter ever admit to being her belle? Whatever happened to her brothers? Let's dish about this doomed beauty.
DataLounge get your fix of gay gossip, news and pointless bitchery.
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I'm wondering if anything has come of this. I have a five year old boy and I think Boy Scouts sign ups start in first grade (next year). I'm choosing to avoid BSA (for reasons that can live in another thread!) and so we're looking for alternatives. I found out about Earth Scouts in another mothering forum thread but when I visit their site, I can't seem to find where to search for local chapters. I'm doubtful there is anything in our area but I'd be interested to see what's involved in getting started and if there was enough interest with the families in my area to start a group. Any feedback you can share is greatly appreciated! Thanks!
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I brought it back to papi, ain't trying to take no losses
He focuses on my emotionless young dealer face then pauses
He gives me powder, he has faith in Nas' ambitions to distribute coke
from Rick Ross (Ft. Nas) – Triple Beam Dreams Lyrics on Genius
Because, as he explained in the prior line, the coke he was trying to sell wasn't good, he took it back to the guy he got it from. .
Nas tells him that he refuses to sell it because he can't make a profit, and the man respects Nas for having the balls to do that, and knows that Nas really wants to sell it. So he gives him more coke, presumably better, which Nas continues to sell.
To help improve the quality of the lyrics, visit Rick Ross (Ft. Nas) – Triple Beam Dreams Lyrics and leave a suggestion at the bottom of the page


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Page 1
arXiv:astro-ph/0605460v2 23 May 2006
Mon. Not. R. Astron. Soc. 000, 1–13 (2005)Printed 5 February 2008(MN LATEX style file v2.2)
Deep spectroscopy of 9C J1503+4528: a very young CSS radio
source at z=0.521
K.J. Inskip1⋆, D. Lee2, Garret Cotter2, T.J. Pearson3, A.C.S. Readhead3,
R.C. Bolton4, C. Chandler5, G. Pooley4, J. M. Riley4and E. M. Waldram4
1Department of Physics & Astronomy, University of Sheffield, Sheffield S3 7RH
2Astrophysics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH
3California Institute of Technology, Pasadena, CA 91125, USA
4Astrophysics, Cavendish Laboratory, J J Thomson Avenue, Cambridge CB3 0HE
5NRAO VLA, Array Operations Center, PO Box O, 1003 Lopezville Road, Socorro NM 87801-0387, USA
5 February 2008
9C J1503+4528 is a very young CSS radio galaxy, with an age of order 104years. This
source is therefore an ideal laboratory for the study of the intrinsic host galaxy/IGM proper-
ties, interactions between the radio source and surroundingISM, links between star formation
and AGN activity and the radio source triggering mechanism. Here we present the results
of a spectroscopic analysis of this source, considering each of these aspects of radio source
We find that shock ionization by the young radio source is important in the central re-
gions of the galaxy on scales similar to that of the radio source itself, whilst evidence for an
AGN ionizationcone is observedat greaterdistances.Line andcontinuumfeaturesrequirethe
presence of a young stellar population, the best-fit model for which implies an age of 5×106
years, significantly older than the radio source.
Most interestingly, the relative sizes of radio source and extended emission line region
suggest that both AGN and radio source are triggered at approximately the same time.
If both the triggering of the radio source activity and the formation of the young stellar
population had the same underlying cause, this source provides a sequence for the events
surrounding the triggering process. We propose that the AGN activity in 9C J1503+4528 was
caused by a relatively minor interaction, and that a super-massive black hole powering the
radio jets must have been in place before the AGN was triggered.
Key words: galaxies: active – galaxies: evolution – galaxies: ISM – galaxies: stellar content
– radio continuum: galaxies – galaxies: individual: 9C J1503+4528
The triggering of powerful radio sources is still poorly understood.
It is generally thought that some mechanism must channel signifi-
cant quantities of gas into the central regions of the host to fuel the
AGN, wherein a rapidly spinning black hole may power the radio
jets (e.g Blandford and Znajek, 1977).
Two scenarios have been proposed. The first is the infall of
gas which has cooled in the halo of a galaxy, or a cooling flow in
a cluster (Bremer, Fabian & Crawford 1997); this proposition has
received much interest recently because it may have a thermostat
feedback effect to prevent runaway cooling in clusters (Br¨ uggen
and Kaiser 2002, Fabian et al. 2003). However it is most likely that
this mechanism in fact causes a renewal of activity in an existing
0E-mail: firstname.lastname@example.com
radio source (Nipoti and Binney 2005), rather than being related to
the original triggering.
The second is associated with the long-standing idea that a
merger between two galaxies, at least one of which is gas rich, is a
precursor to AGN activity (e.g. Heckman et al 1986). Wilson and
Colbert (1995) suggested that the coalescence of black holes fol-
lowing a major merger creates the necessary rapidly-spinning black
hole, which suggests links between radio sources and other merger
systems such as ULIRGs, and implies that evidence for young stel-
lar populations and disturbed morphologies should be present at
some level in observations of young radio sources.
The merger scenario is supported by an increasing amount of
anecdotal evidence. For instance, there are several cases known
where the host galaxy of a powerful radio source appears to be
undergoing a major merger (e.g., Johnston et al. 2005). Similarly,
thereisincreasing evidence that powerful high-redshift radiogalax-
Page 2
K.J. Inskip et al
ies lie in forming clusters (see e.g. Venemans et al. 2005); such en-
vironments would be rich in major mergers. This evidence in turn
takes us back to the first scenario above; massive cluster galax-
ies may host a spinning black hole as a relic of their early history,
which is generally quiescent but which becomes active when fu-
elled by cooling gas. It is clearly evident that radio sources play a
significant part in hierarchical galaxy and structure formation (e.g.
Croton et al 2006), so the precise ingredients for radio source for-
mation are a cause of renewed interest.
In any case, our understanding of this early phase of radio
galaxy evolution is hampered by the difficulty of compiling uni-
form samples of radio sources in the first few millennia of their
growth, and indeed the impossibility of pinpointing galaxies im-
mediately prior to this stage. However, it is is now widely accepted
that Compact Steep Spectrum (CSS) and some Gigahertz Peaked
Spectrum (GPS) radio sources represent the earliest stages of radio
source evolution, being the progenitors of the larger FRII source
population (e.g. Fanti 1995, Readhead 1996, Snellen et al 2000,
Murgia 2003). The study of such sources in the stages immediately
after triggering may be avaluable way of elucidating theevents that
have occurred beforehand.
In an effort to secure a uniform sample of young sources, we
have turned to the 9C survey (Waldram et al 2003). This was car-
ried out at 15 GHz with the Ryle Telescope to identify foreground
sources for the Very Small Array (VSA) microwave background
experiment. Over the past several years, extensive followup of the
radio properties of this population has been carried out (Bolton et
al 2003, 2004, 2006; Bolton et al submitted), both to understand
the effects on microwave background experiments better and to in-
vestigate the sources themselves; the high survey frequency has
proved a good way of selecting significant numbers of CSS and
GPS sources, as well as sources peaking in the ∼ 10 GHz range.
We are now undertaking optical followup of the CSS and GPS
sources, and in this paper we present a detailed spectroscopic study
of one of these compact sources, 9C J1503+4528, a classical dou-
ble FRII radio galaxy at a redshift of z ∼ 0.5 with an angular size
of 0.5′′.
Details of the observations are presented in section 2, analysis
of the emission line strengths and ionization state in section 3, gas
kinematics in section 4, emission morphology in section 5 and a
discussion of the implications of our results in section 6. We give a
summary of our conclusions in section 7.
Values for the cosmological parameters of Ω0 = 0.27, ΩΛ =
0.73 and H0 = 65km s−1Mpc−1are assumed throughout.
The observed source, 9C1503+4528 (see Fig. 1), was selected as
our first target for detailed study for several reasons.
First, the source has a rest-frame 1.4 GHz luminosity of 1.33
×1025W Hz sr−1, well above the FRI/FRII break. Second, the
source is resolved, and clearly shows a classical double structure in
the radio map presented in Bolton et al. (2004). The angular size
of the source is 0.5′′, corresponding to a projected linear size of
≈ 3 kpc. It is currently accepted that GPS and CSS sources are at
a young stage in the evolution of the radio source (see e.g. Snellen
et al 2000). The picture in which sources are young is strongly sup-
ported by observations of the hotspot advance speed in many of
the most compact sources. These observations find hotspot advance
speeds in the range 0.1–0.4c (e.g. Polatidis and Conway 2003; Tay-
lor et al 2000; Owsianik, Conway & Polatidis 1998), which in the
case of 9C J1503+4528 implies that the source has an age of or-
der ∼ 104years. This places the source very close to its time of
triggering, since the typical lifetime of an FRII source is ∼ 107to
108years (e.g. Kaiser, Dennett-Thorpe and Alexander 1997). Fi-
nally, the source redshift (z ∼ 0.5) makes many useful diagnostic
lines and the 4000-˚ A break accessible to moderate-resolution spec-
troscopy in a wavelength range region relatively clear of night sky
emission. With these facts in mind, the young CSS radio source
9C J1503+4528 is therefore a particularly appropriate object for
the study of the intrinsic host galaxy/IGM properties, interactions
between the radio source and surrounding ISM, links between star
formation and AGN activity and the underlying radio source trig-
gering mechanism.
2.1VLA imaging
The 22-GHz data obtained by Bolton at el. (2004) were re-analysed
to obtain the map shown in Fig. 1. Both the central component
and the SE compact component are unresolved. The most obvi-
ous interpretation of the radio morphology is that the bright cen-
tral component is the core, with the SE compact component be-
ing a hotspot, and the SE and NW extensions being lobes. Given
the overall steep spectrum, it is implausible that the source is be-
ing viewed at an angle close to the line of sight; in such a case, a
strongly boosted flat-spectrum jet component would be expected
to dominate in this high-frequency map. We thus conclude that
the source has a double-lobed structure with an overall extent of
∼ 3kpc.
2.2Optical and infrared imaging
An image using the Isaac Newton telescope Wide Field Camera r-
band filter was taken on the night of 2005 April 11. This filter has
the advantage of not including the strong [OII] and [OIII] emission
lines at the source redshift. Five 600-s images were taken, offset at
the centre and corners of a 20′′pattern, and stacked. The resulting
image is shown in Fig. 1.
A K-band image was also obtained, on the night of 2006
March 5 using the UFTI instrument at UKIRT. Nine 60-s jittered
observations were taken and reduced using the standard ORAC-DR
pipeline; the resulting image is also displayed in Fig. 1. The see-
ing, measured from an observation of UKIRT standard star P177-D
taken immediately after the target observation, was 0.6 arcseconds.
2.3 Optical Spectroscopy
The spectroscopic observations were carried out on 2004 July 18,
using the Keck LRIS spectrograph (Oke et al 1995). Seeing was
∼ 0.8′′, and a 1′′slit was used. The 600/7500 grating was used,
providing a wavelength range of ∼ 5200 − 7800˚ A, a spatial scale
of 0.215 arcsec/pixel, a spectral scale of 1.26˚ A/pixel, and a spec-
tral resolution of ∼ 4.4˚ A. For an object lying at a redshift of
z ∼ 0.5, the corresponding rest-frame spectral range is approx-
imately 3500 − 5200˚ A, thereby including emission lines from
[OII]3727˚ A up to [OIII]5007˚ A. Slit PAs of +45◦and −45◦were
chosen, aligning the slit either parallel or perpendicular to the radio
source axis. Long-slit spectra were obtained with total integration
timesof 1800s at each slitPA.Theintegrationsweresplitinto900-s
exposures to aid the removal of cosmic rays.
Standard packages within the NOAO IRAF reduction software
Page 3
9C J1503+4528: a young radio source
15h 03m 25.5s25.0s24.5s24.0s23.5s
Right Ascension
45o 28' 35''
15h 03m 25.5s25.0s24.5s24.0s23.5s
Right Ascension
45o 28' 35''
1 10 100
Flux density (mJy)
Frequency (GHz)
PLot file version 1 created 03-MAR-2006 18:12:08
Peak flux = 1.8390E-02 JY/BEAM
Levs = 1.100E-03 * (5, 6, 7, 8, 9, 10, 11, 12, 13,
14, 15, 16, 17, 18, 19)
15 03 24.5624.55 24.5424.53 24.52 24.5124.50 24.49 24.48
45 28 44.6
Figure 1. The compact radio source 9C J1503+4528. Left: UFTI K−band (top) and WFC r−band (bottom) images of the host galaxy, an R ≈ 19 elliptical.
The two spectroscopic slit PAs, parallel and perpendicular to the radio source axis are indicated on each diagram by the solid and dashed lines respectively.
Centre: VLA 22GHz radio contours. Right: VLA and OVRO radio spectrum for this source, from Bolton et al (2004).
were used to reduce the raw data. Corrections were made for over-
scan bias subtraction, and the data were then flat-fielded using in-
ternal lamps. The flat fields were taken immediately after each ob-
servation of the target, to minimize the effects of fringe drift in the
CCD. The two-dimensional frames were wavelength calibrated and
corrected for distortions in the spatial direction using wavelength-
calibration arc exposures. Taking care not to subtract any of the
extended line emission, the sky background was removed. Obser-
vations of the smooth-spectrum standard star BD +28 4211 were
used to provide accurate flux calibration of the final spectra and to
remove the telluric A- and B-band absorption features. The central
regions of the parallel and perpendicular spectra effectively probe
the same region of the host galaxy. These two spectra were com-
bined in order to produce a higher signal-to-noise spectrum, for
use in analysing the emission from the central regions of the radio
The resulting parallel and perpendicular 2-d spectra are dis-
played in Fig. 2. In the parallel spectrum, the presence of narrow
emission, extended over a distance of ∼ 5′′(approximately 10
timeslarger thantheradiosourceitself)canclearlybeseen, inaddi-
tion to a broader component lying close to the continuum centroid.
The [OII] emission is particularly strong compared to ø3, and the
continuum emission short of the 4000˚ A break is also substantially
more luminous than would be expected for an old stellar popula-
tion alone. The perpendicular spectrum displays similar properties,
with the exception that extended narrow emission is not observed.
A 1-d spectrum extracted from the central 2′′of the combined per-
pendicular and parallel spectra is displayed in Fig. 3.
Determining the precise systemic redshift of 9C J1503+4528
was complicated by the inherent structure in the emission lines: the
redshift implied by the peak of the line emission on the contin-
uum centroid differs substantially from that of the narrow extended
component. However, the various absorption features in the spectra
(Ca H & K, high-order Balmer lines) all suggest a redshift identical
to that determined from the extended narrow component, giving a
value of z = 0.521.
One-dimensional spectra were extracted from the parallel, perpen-
dicular and combined 2-d frames. The extractions were carried out
over 2′′(∼ 12kpc) for the parallel, perpendicular and combined
frames, and additionally over 5′′(∼ 31kpc) for the parallel and
perpendicular frames. The lines were then fitted by gaussians; the
resulting fluxes and equivalent widths are presented in Appendix
Spectra were also extracted in 0.5′′steps across the slit, in or-
der to investigate the changing ionization state of the emission line
gas with position via ionization state diagnostic diagrams (Bald-
win, Phillips & Terlevich 1981). For an effective analysis, model
predictions should be well separated and results should be consis-
tent over several different diagrams/line combinations. Line pairs
should ideally be close in wavelength and of the same species, to
limit the effects of reddening and variations in gas composition.
The most appropriate lines available from our optical spectra are
[OII]3727˚ A, ø34363˚ A, Hβ and ø35007˚ A.
Figure 4 displays the diagnostic diagram for the line pairs
[OII]3727˚ A/Hβ and ø35007˚ A/Hβ, extracted from the parallel
spectra in 0.5′′steps, together with various theoretical model
tracks. These include: (i) the shock models of Dopita & Suther-
land (1996), which also incorporate the effects of a precursor ion-
ization field, (ii) the mixed medium (matter bounded vs. ionization
bounded) photoionization tracks of Binette et al (1996), plus (iii)
simple AGN photoionization tracks (Groves et al 2004a, 2004b),
Page 4
K.J. Inskip et al
Figure 2. Sections of particular interest (rest frame 3730-4070˚ A and 5190-
5490˚ A) from the 2-d optical spectra of 9C1503+4528, with the slit aligned
parallel (left) and perpendicular (right) to the radio source axis. Wavelength
increases from the bottom to the top of the diagram, as indicated by the
direction of the arrow, and the position of the 4000˚ A break is denoted by
the dashed line. The extracted regions are approximately 10′′wide. Thefive
prominent emission lines are (bottom to top): [OII]3727˚ A, [NeIII]3869˚ A,
Hβ, ø34959˚ A and ø35007˚ A.
also incorporating the effects of dust. The photoionization models
displayed are for solar metallicityand a density of n = 1000cm−3.
For reference, the photoionization tracks display little variation for
lower values of n, while the n = 10000cm−3track is shifted to
smaller values of log([OII]/Hβ) by ∼ 0.2dex. The 2Z⊙metallicity
tracks are generally similar to those of solar metallicity, whereas
lower Z tracks are shifted to smaller values of both log([OII]/Hβ)
and log(ø3/Hβ).
Figure 3. Spectrum of 9C J1503+4528 obtained from the central 2′′of the
combined parallel and perpendicular data. This spectrum provides the high-
est signal-to-noise ratio for our data, and provides a good illustration of the
relative emission line strengths and the fairly blue colour of the continuum.
This diagram clearly shows the changing ionization state rel-
ative to distance from the nucleus. The spectra extracted from the
central regions of the host galaxy lie close to the predictions of the
shock ionization models (and also the far end of the mixed medium
ionization track). At intermediate distances (∼ 1′′, i.e. sampling
emission from just outside the radio source), the shock plus precur-
sor photoionization models are most suited. Beyond 1-1.5′′(i.e. the
extended narrow emission region), the data are well described by
simple AGN photoionization. High values of the ionization param-
eter, U, are the most plausible, and a dusty medium isfavoured. For
the photoionized gas, the ionization state at larger radii suggests ei-
ther a lower spectral index (α ∼ −2.0 rather than α ∼ −1.2),
higher gas density or lower metallicity. The mixed medium mod-
els of Binette et al only provide a good explanation for a few of
the data points, and it seems unlikely that this system can be well
described using that particular model. The observed line ratios are
not likely to be affected by internal reddening, as the Balmer line
ratios in our spectra are in good agreement with the predictions
of case B recombination. Balmer line absorption could potentially
have some influence on the exact positioning of the data points in
this figure; while we believe we have correctly accounted for the
errors on our measurement of H-β, additional shifts of up to 0.2dex
towards smaller line ratios cannot be completely ruled out. How-
ever, this would not have any effect on our overall interpretation of
the data.
The picture provided by these results is as follows. The UV
continuum emission from the AGN ionizes the gas at all locations
within the ionization cone, decreasing in intensity at larger dis-
tances. The innermost regions of the galaxy, of order the same size
as the fledgling radio source, have an additional ionization con-
tribution from shocks. The UV radiation field produced by these
shocks adds another ionization component to the emission from
gas at intermediate distances.
The relative ionization states of the parallel and perpendicular
spectra can be compared in Fig. 5. This figure displays the same
tracks as in Fig. 4, for spectra extracted from various regions of our
2-d spectra. These include the central 2′′regions of the combined,
parallel and perpendicular spectra. The results for the central 1-2′′
should not be greatly different, as both spectra sample essentially
the same region. However, the impact of AGN and shock ioniza-
tion will be greatly lessened at larger distances, for material which
Page 5
9C J1503+4528: a young radio source
-0.2 0.00.20.4 0.60.8 1.0 1.2
log10([OII] 3727 / H-β)
log10([OIII] 5007 / H-β)
+2.25. ″
+1.75. ″
+1.25. ″
+0.75. ″
+0.25. ″
-0.25. ″
-0.75. ″
-1.25. ″
-1.75. ″
Figure 4. Ionization mechanism diagnostic plot for 9C1503+4528, using
the line ratios [OII]3727/Hβ and [OIII]5007/Hβ. Data points represent
spectra extracted in 0.5′′steps, and are labelled in terms of their distance
(in arcseconds) from the continuum centroid. The model tracks include: (1)
shock ionization (Dopita & Sutherland 1996), with and without a precursor
photoionization region (light & dark shading respectively), (2) the matter-
bounded photoionization track (dashed dark blue track, Binette, Wilson &
Storchi-Bergmann 1996), and (3) simple AGN photoionization tracks (light
blue tracks), including the effects of dust (solid black tracks; Groves, Do-
pita & Sutherland 2004a,b). The photoionization models are for n=1000
cm−3, solar metallicity and various values of the ionization index α (from
1.2 < α < 2.0). A brief description of the effects of changes in metallicity
and/or gas density is given in the main text; we refer the reader to Groves et
al (2004a,b) for full details.
lies off the radio source axis and well outside the ionization cone
of the AGN. Also displayed are the observed emission line ratios
for spectra extracted at distances from the continuum centroid of
+1.5′′to +2.5′′and −1.5′′to −2.5′′, for both the parallel and
perpendicular spectra. The large errors on the data points for the
extended regions of the perpendicular spectra reflect the very weak
line emission present at these distances. In the case of the −1.5′′
to −2.5′′data point, shocks are not a plausible option, and the data
should lie outside the ionization cone of the AGN. Instead, the po-
sition of this data point suggests that ionization by young, hot stars
may provide a better explanation (see e.g. Kewley, Geller & Jansen
(2004) and Rola, Terlevich & Terlevich (1997) for appropriate lo-
cations on the [OII]/Hβ vs. ø3/Hβ diagnostic plot for HII regions;
suchemission lineratioswould generallybeexpected tolietowards
the lower left quadrant of Fig. 5). A combination of ionization by
young stars and the AGN could also be relevant for the −1.75′′and
+2.25′′data points on Fig. 4.
Figure6shows the
ø35007˚ A/ø34363˚ A and [OII]3727˚ A/ø35007˚ A line ratios, to-
gether with the observed data from our parallel spectra in spatial
steps of 0.5′′. Note that the mixed medium model track, which
bent towards the data points at low values of AM/I1in Fig. 4,
tends towards higher values of ø35007˚ A/ø34363˚ A on Fig. 6 as
opposed to the lower values of this line ratio observed in the data.
Although the error bars are large for the ø35007˚ A/ø34363˚ A line
ratio, we nevertheless have a certain amount of consistency with
the previous diagnostic diagrams: once again the central regions
of the galaxy favour the predictions of shocks, while more distant
1The solid-angle ratio of matter-bounded to ionization-bounded material
in the mixed-medium model of Binette et al 1996.
log10([OII] 3727 / H-β)
log10([OIII] 5007 / H-β)
4 v=500
Figure 5. Ionization mechanism diagnostic plots for 9C1503+4528, us-
ing the line ratios [OII]3727/Hβ and [OIII]5007/Hβ. Data points represent
spectra extracted from various regions of the spectra taken perpendicular
and parallel to the radio axis, and include: (i) the central 2′′of the paral-
lel, perpendicular & combined (best signal-to-noise) spectra, (ii) 1′′wide
sections of the parallel and perpendicular spectra lying ±2′′from the con-
tinuum centroid. The model tracks are the same as those in Fig. 4a.
1.0 1.2 1.4
log10([OIII] 5007/ [OIII] 4363)
1.6 1.82.02.2 2.4
log10([OII] 3727 / [OIII] 5007)
+2.25. ″
+1.75. ″
+1.25. ″
+0.75. ″
+0.25. ″
-0.25. ″
-0.75. ″
-1.25. ″
-1.75. ″
Figure 6. Ionization mechanism diagnostic plots for 9C1503+4528, using
the line ratios [OII]3727/[OIII]5007and [OIII]5007/[OIII]4363.Data points
represent spectra extracted in 0.5′′steps, and are labelled in terms of their
distance from the continuum centroid. The model tracks are the same as
those in Fig. 4a, and include: (1) shock ionization (Dopita & Sutherland
1996), with and without a precursor photoionization region (light & dark
shading respectively), (2) the matter-bounded photoionization track (dashed
dark blue track, Binette, Wilson & Storchi-Bergmann 1996), and (3) Sim-
ple AGN photoionization tracks (light blue, various styles), including the
effects of dust (solid black tracks, Groves, Dopita & Sutherland 2004a,b).
locations lie closer to the dusty AGN photoionization tracks.
The relatively low ø35007˚ A/ø34363˚ A ratio is indicative of high
temperatures and/or densities in the emitting gas, of the order of
several 104K in the low density limit (e.g. Osterbrock 1989), fully
consistent with the presence of shocks in these regions.
We have also investigated the changing gas kinematics, via an anal-
ysis of the profiles of the [OII]3727˚ A and ø3 (4959+5007˚ A) lines.
Page 6
K.J. Inskip et al
Figure 7. Example line profile fits for the ø3(4959+5007)˚ A emission lines.
The top figure is for the spectrum extracted at a distance of 2.25′′to the SE
of the continuum centroid, and the bottom figure for a region lying at a dis-
tance of 0.75′′in the same direction. The data were modelled with several
components (dotted lines): a continuum level, and 1-3 separate Gaussian
components for each line. For ø3, the relative strengths and positions of the
4959˚ A and 5007˚ A lines were fixed. The combination of gaussians with the
lowest reduced χ2determined the maximum number of velocity compo-
nents which could be fitted to the data.
Two-dimensional regions around each of these emission lines were
extracted, and from these a sequence of one-dimensional spectra
were extracted along the slit direction, stepped every 0.5′′.
After allowing for continuum subtraction, the data were fitted
by up to three successive gaussian components, which were only
accepted if their FWHM was larger than the instrumental resolu-
tion and the signal-to-noise ratio was greater than approximately
five (excepting the outermost spectra, for which a fainter, single
gaussian component could be detected at a lower signal-to-noise.)
The combination of gaussians with the lowest reduced χ2were
then taken to be the maximum number of velocity components
which could be fitted to the data (we also fixed the relative posi-
tions and strengths of the 4959˚ A and 5007˚ A lines). Example fits
are displayed in Fig. 7.
The integrated line flux, the velocity relative to that at the cen-
tre of the galaxy, and the emission line FWHM were determined
for each gaussian fit. We calculated the FWHM by subtracting in
quadrature theinstrumental FWHM,asdeterminedfromunblended
sky lines. We then calculated errors for these three parameters, al-
lowing for the fact that a range of possible fits are equally accept-
able at low S/N. This approach allows us to search for high velocity
components in the emission line gas, or other structures incompat-
ible with a fit to a single velocity component. Given the observed
emission line profile of this source, such a step was a necessity, and
broader emission line components are clearly present in the central
parts of the extended emission line region.
Figure 8. Gas kinematics for 9C J1503+4528. The changing line fluxes
(top), widths (centre) and offsets (bottom) with position are displayed
for the [OII] (left) and ø3 (right) emission lines, extracted and fitted in
0.5′′steps from the parallel spectrum. Up to three emission line compo-
nents are modelled at each position. Negative offsets are towards the NW,
and positive offsets towards the SE.
The results of our analysis of the kinematics of the parallel
spectrum are presented in Fig. 8.
An unresolved emission component is present in the outer re-
gions of the extended emission line region (hereafter EELR), in
both [OII] and ø3, at wavelengths consistent with the emitting ma-
terial lying at rest relative to the host galaxy. This narrow com-
ponent can be traced across the galaxy in ø3. The [OII] emission
line is of substantially higher luminosity, particularly in the central
regions of the galaxy. Because of this, the narrow component of
[OII] can only be observed in the outer regions, and is lost in the
centre in favour of one or more broader components. The relative
strengths of the narrow components of [OII] and ø3 are consistent
with simple AGN photoionization, as demonstrated by our diag-
nostic diagrams in the previous section.
The broader emission line components extend to approxi-
mately 1-1.5′′from the continuum centroid. Note that the [OII]
emission is substantially stronger than the ø3 emission; such a low
ionization state in the emitting material is suggestive of shocks as-
sociated with the radio source, in which case the emitting material
would displaylarger linewidthsthanmore settledmaterial. Usually
a single broad component is sufficient, except in the central regions
where two broad components are preferred. The broad components
on the SE side of the galaxy (see the 2-d spectrum presented in
Fig. 2) usually lie at shorter wavelengths, with a velocity shift of
a few hundred km s−1, whilst the emission from the opposite side
of the galaxy is shifted to longer wavelengths by a similar amount.
Of these two distinct components, the blue-shifted emission line
Page 7
9C J1503+4528: a young radio source
Figure 9. Gas kinematics for 9C J1503+4528. The changing line fluxes
(top), widths (centre) and offsets (bottom) with position are displayed for
the [OII] (left) and ø3 (right) emission lines, extracted and fitted in 0.5′′
steps from the perpendicular spectrum. Up to three emission line compo-
nents are modelled at each position. Negative offsets are towards the SW,
and positive offsets towards the NE.
component is generally more luminous, and has a larger line width
(400-600 km s−1, cf 200-400km s−1for the red-shifted emission).
We also present the results of a similar analysis of the spec-
trum aligned perpendicular to the radio source axis (Fig. 9). As
the line emission in the perpendicular spectrum is much less exten-
sive, larger extracted spectra of 1′′in width have been modelled to
boost the signal-to-noise. The first main feature of note is the lack
of an extended narrow component. This is strong evidence that the
source of the ionizing photons for the extended narrow component
is the ionization cone of the AGN, which does not intersect with
the perpendicular spectrum except in its centre.
In the central regions of the perpendicular spectrum, broad
emission components are observed. These are very similar to those
in the parallel spectrum, with the exception that there is no clear
tendency for the blue- or red-shifted emission to preferentially lie
on one side of the galaxy or the other. This suggests that outflows
along the radio axis are a plausible option for explaining the gas
kinematics, as an alternative to simple rotation. The greater lumi-
nosity and extent of the material to the SE side of the galaxy, to-
gether with the blueshifted broader component, suggests that the
SE radio lobe would be orientated towards the observer; given the
observed radio asymmetries (section 2.1) and quiescent extended
emission line component at larger radii the outflow scenario is in-
deed highly plausible.
The continuum emission of 9C1503+4528 is remarkably blue. To-
gether with the clear presence of Balmer absorption lines and the
young age of the radio source this suggests a significant young stel-
lar population. If thetriggering of radio source activity isconnected
with the star formation, the properties of any young stellar popu-
lation formed as part of that process can shed light on the exact
mechanisms and timescales involved. Wehave thereforecarried out
continuum modelling of our spectra, with the aim of placing limits
on both the mass and age of any young stellar population present in
this galaxy.
For the continuum modelling, we combined both the parallel
and perpendicular 2-d frames and extracted a 1-d spectrum from
the central 2′′(Fig. 3).
The first stage was to remove the contribution of nebular con-
tinuum emission (Dickson et al 1995). Although subject to stel-
lar absorption features, the Balmer line strengths are in general
consistent with the predictions of case B recombination, and in-
ternal reddening is unlikely to be a major issue. The Hβ flux can be
well modelled, and was used todetermine the contribution from the
various nebular continuum emission processes (free-free emission,
bound-free emission, two-photon emission and the Balmer forest
pseudo-continuum), assuming an electron temperature of 15000K.
(Checks with alternative temperatures, allowing for the error on our
evaluation of the Hβ flux, do not produce significantly different re-
sults.) The corrected spectrum was binned in blocks of ∼ 30˚ A,
excluding any regions where emission lines were present.
To fit the remaining stellar continuum we used a combina-
tion of young and old stellar population SEDs from the models of
Bruzual & Charlot (2003). A Chabrier initial mass function and
solar metallicity were selected, and the stellar populations were as-
sumed to form in an instantaneous burst. We consider stellar pop-
ulation ages ranging from < 105years up to 9 × 109years (the
expected age of the old stellar population in a z ∼ 0.5 galaxy, as-
suming a formation redshift of z ∼ 10 − 20). Reduced χ2fitting
was used to determine the relative proportions of old/young stars
for all combinations of SED models.
Figure 10 displays the results of our best-fit model. This con-
sists of an old (6 Gyr) stellar population, plus a 5×106year young
stellar population accounting for 0.065% of the total stellar mass,
and roughly 70% of the total continuum flux at a wavelength of
∼ 3600˚ A. Our modelling implies that the total stellar mass in the
central region of the galaxy probed by our spectra is approximately
1010M⊙, whereas the overall stellar mass of the galaxy (based on
our K−band modelling in section 6) is closer to 1011M⊙. The
largest residuals lie near the Ca absorption feature at ∼ 3970˚ A,
which is subject to infilling by line emission at 3967˚ A due to Hǫ +
A plot of best-fit reduced χ2as a function of young stellar
population (hereafter YSP) age is displayed in Fig. 11. A contribu-
tion from a young stellar population is very much favoured over an
old stellar population alone. Fits obtained using different ages for
the majority old stellar population (ranging from 5 to 9 Gyr in age)
do not lead to any significant variation in the resulting best-fit YSP.
We must also consider the potential presence of a power-law
ionizing continuum associated with the AGN. If the presence of
a power-law component is simply added to our modelling, allow-
ing its flux and shape to vary freely, the resulting best-fit model
generally prefers an unrealistically strong power-law flux, and it is
therefore necessary to place constraints on the power law contri-
bution in order to make a meaningful assessment of its effects. To
Page 8
K.J. Inskip et al
Figure 10. Continuum fits to the central 2′′of the combined spectrum (Fig. 3). The top frame (a) displays the observed spectrum (dotted line), the best-fit
model (dark solid) and the two component (old and young) SEDs which make up the best-fit model. Also displayed in frame (a) are the model residuals for
each of the bins used in the fitting procedure. For clarity, we also display the observed data (frame (b), centre left), the best-fit model (frame (c), lower left),
the old stellar population component (a 6 Gyr old stellar population, frame (d), centre right) and the young stellar population component (a 5 million year old
stellar population, frame (e), lower right) as separate spectra.
determine the balance between YSP age/mass and power-law con-
tribution, we repeated our fitting procedure using fixed power-law
contributions ranging from 0% to 50% of the total flux at a wave-
length of λ ∼ 3600˚ A. The spectral index of the power law (defined
as Fλ ∝ λα) is constrained to be one of three values, α = −1,
−2 or −3. The fitting procedure was then repeated for all combi-
nations of stellar populations and power-law parameters. The re-
sulting best-fit YSP parameters (age, mass, reduced χ2) for each of
the different power law contributions considered are displayed in
Appendix B.
With the exception of the fits with the very highest power-law
contribution (> 25%), the best-fit YSP mass and age remain rela-
tively unchanged. The similar strengths of the narrow line emission
components either side of the galaxy centroid in the parallel spec-
tra (suggesting that this source is observed with the ionization cone
aligned in a direction nearly perpendicular to the line of sight) also
implythatatwo-component stellarpopulation provides amorethan
Page 9
9C J1503+4528: a young radio source
Figure 11. Reduced χ2of best-fit model vs. young stellar population com-
ponent age for the continuum fitting of 9C J1503+4528. The best-fit model
includes a YSP component with an age of 5 × 106years, accounting for
0.065% of the total stellar mass of the host galaxy, and roughly 70% of
the observed continuum flux at a wavelength of ∼ 3600˚ A. The age of the
majority old stellar population in the best-fit model is approximately 6Gyr.
adequate explanation of the observed continuum emission, and that
no power-law is required.
6.1Morphological properties of the host galaxy
Given the spectroscopic evidence for a young stellar population,
we examined the galaxy morphology for evidence for a merger or
other interaction which may have caused the starburst. Our calcu-
lated 0.06% 5Myr YSP would be expected to contribute only 0.02
magnitudes to the K-band flux, and so the K-band image will be
dominated by the old stellar populations of the host galaxy and any
merging companion or tidal tails.
We fitted the galaxy morphology using the methods detailed
in Inskip et al. (2005), which can be briefly summarised as follows.
The point spread function for the UFTI fieldisdetermined from un-
saturated stars within the mosaic field; we extract their 2-d profile,
normalise to unit flux and take the average profile. S´ ersic profile
(S´ ersic 1968) galaxy models were then convolved with the point
spread function and fitted to the surface profile of the galaxy, using
available least squares minimisation IDL routines2. Free parame-
ters are the galaxy flux, centroid, effective radius, S´ ersic index and
fractional nuclear point source contribution. Galaxy ellipticity was
also allowed to vary, but in the case of this object a circular model
with ǫ = 0 was preferred.
From the K-band data, our resulting best-fit model, residu-
als and 1-d radial profile are displayed in Fig. 12. We find that the
host galaxy appears to have a simple de Vaucouleurs elliptical mor-
phology, with a preferred S´ ersic index of 4.0 ± 0.2, and a best-fit
(χ2= 1.03) effective radius of reff = 1.70′′± 0.15′′(equivalent
to 11.5 ± 1.0kpc at z = 0.521). We find no evidence for any nu-
clear point source contribution at K band (preferred point source
percentage < 1%).
2MP2DFUNFIT.PRO, part of Craig Markwardt's MPFIT non-linear least
squares curve fitting package available via http://astrog.physics.wisc.edu/
Radius (arcsec)
Figure 12. Host galaxy morphology fits for 9C J1503+4528. The K−band
galaxy image is presented in frame (a), with the model galaxy given in
frame (b) and the residuals after subtracting the best fitting model from the
data displayed in frame (c). Frame (d) illustrates a 1-d cut through the data
(dotted line and binned points) with the best-fit model (solid line) overlaid.
The r-band data are too noisy to make an accurate fit to the
data; the effective radius is constrained only to lie between 1.3′′±
0.5′′and 1.6′′± 0.5′′. This is, however, consistent with the K-
band fit. Most importantly, we find no significant residual emission
which would indicate the presence of a close companion galaxy or
tidal tails.
Any galaxy interaction/merger activity must therefore either
have been very minor in nature, or have occurred sufficiently long
ago that the old stellar population of the host galaxy has returned to
an undisturbed morphology. In the latter case, the interaction must
have taken place several dynamical timescales before the present
observations. We estimate the dynamical timescale Tdynas reff/σ,
where σ is the velocity dispersion of the galaxy, which in turn we
estimate by taking the FWHM of the narrow component of the
emission lines (∼ 200 km s−1). This gives Tdyn ∼ 60 Myr, so
any previous interaction must have occurred at a time very much
earlier that the formation of the YSP. We thus conclude that the
YSP and present AGN activity were caused by, at most, a minor
6.2Evidence from the extended emission-line region
As with many other radio galaxies the properties of the extended
emission lineregion of 9C J1503+4528 vary substantially with spa-
tial position. The changes in ionization state confirm our expecta-
tions that shocks are important in the vicinity of the young radio
source, and that AGN photoionization dominates elsewhere. The
kinematic properties of the emission line gas confirm this picture,
with the broader emission lines highlighting the disturbed kinemat-
ics of the central regions, in contrast to the kinematically quiescent
material at larger radii.
The projected physical size of the EELR is ≈ 34 kpc. Emis-
Page 10
K.J. Inskip et al
sion line regions of this scale are by no means unusual, and are
often substantially larger in the case of FRII radio sources (for
example, ∼50–100 kpc for extended 3C and 6C sources, Best,
R¨ ottgering & Longair 2000; Inskip et al 2002). However, there
are significant contrasts between this EELR and those of more ex-
tended radio galaxies.
First, the EELR of 9C J1503+4528 has a very sharp cutoff,
rather than the more gradual decline in emission line luminosity
observed in thecases of other sources (e.g. Best, R¨ ottgering &Lon-
gair 2000; Inskip et al 2002). Second, and of great significance, is
the fact that the EELR is a factor of ten larger than the size of the
radio source. Unlike the case of the 3C and 6C sources, where the
EELR is significantly affected by the passage of the radio source,
here we have a case where the EELR could very well correspond
to the limiting distance reached by the ionization front of an AGN,
illuminating the region ahead of the radio source before it leaves
the centre of the host galaxy.
This factor of ≈ 10 difference between radio source size and
EELR size has a significant implication. In combination with the
typical 0.1 c source expansion speed, we find it highly plausible
that the radio jets and AGN were triggered simultaneously, some
∼ 104years prior to our observations.
6.3Spatial distribution of star formation
The material lying at larger angles to the radio source axis (i.e.
the regions probed by the perpendicular spectrum) is also of in-
terest. The line emission along this axis is far less extensive (as ex-
pectedfor theregionslyingontheedgeof, oroutside, theionization
cone). Its ionization state suggests a lower ionization parameter U
(i.e. fewer and/or less energetic ionizing photons), and the weak
line emission in these regions could be better explained as being
due to ionization by young OB stars (HII regions). Our continuum
modelling in the preceding section finds clear evidence for a young
stellar population with an age of roughly 5 million years, but does
not allow us to pinpoint its location. However, the varying strength
of the Balmer absorption features in the parallel and perpendicular
spectra (Fig. 13) can give us some idea of how widely distributed
this young stellar population might be.
This plot displays the Hβ line profile for the parallel and per-
pendicular spectra, using increasing extraction widths of 1′′to 5′′,
beyond which point increased aperture widths only lead to a deteri-
oration of the signal-to-noise. In the perpendicular extracted spec-
tra, Balmer absorption can be clearly observed, and becomes in-
creasingly apparent as emission from regions at a greater distance
from the AGN is included (i.e. for increased aperture widths). The
line emission in the parallel spectra isroughly 50-100% more lumi-
nous (see Appendix A), and the evidence for the same trend in the
strength of the absorption component is less clear-cut. Whilst the
line emission is strongest in the central regions of the host galaxy,
the distribution of the line absorption must therefore be less well
peaked, otherwise we would not observe a strengthening of the
absorption component in wider apertures. This suggests that any
young stellar population responsible for the Balmer absorption fea-
tures is unlikely to lie predominantly within the central few pc. The
pronounced appearance of the Balmer absorption in the perpendic-
ular spectra suggests that the underlying young stellar population
is not linked to the location of the growing radio source but rather,
more widely distributed throughout the galaxy. Indeed, given the
relative ages of YSP and radio source (5 × 106years and ∼ 104
years respectively), a radio-source induced star formation scenario
would seem unlikely.
Figure 13. Hβ line profiles for the parallel (left) and perpendicular (right)
spectra, extracted using increasing aperture widths of (from top): 1′′, 2′′,
3′′, 4′′and 5′′. Balmer absorption is most clear in the perpendicular spectra,
and generally becomes more pronounced with the inclusion of emission at
greater distances from the AGN (i.e. the larger extraction apertures).
It is interesting to contrast the derived properties of the YSP
detectedinthespectraof 9CJ1503+4528 withthosefoundfor other
sources. Recent work on the GPS radio source PKS1345+12 (Ro-
driguez et al, in prep) finds evidence for a very similar young stellar
population to that of 9C J1503+4528: an age of roughly 5 million
years (c.f. ∼ 103years for the radio source itself) and a mass of
∼ 106M⊙. Imaging observations locate the YSPs in several super
star clusters lying in the outer regions of the host galaxy, rather than
in a nuclear starburst ring such as that observed for Cygnus A (e.g.
Jackson, Tadhunter & Sparks 1998). A further point of interest is
the finding that the hosts of high luminosity AGN observed as part
of the Sloan Digital Sky Survey (Kauffmann et al 2003) typically
have younger mean stellar ages than normal elliptical galaxies ex-
Page 11
9C J1503+4528: a young radio source
isting at the same epoch. Additionally, the young stars are not pref-
erentially located near the galaxy nuclei, but rather are spread out
over a much wider scale. These properties are strikingly similar to
those observed in 9C J1503+4528.
6.4Gas kinematics
The observed changes in gas kinematics and dominant ionization
mechanism in different regions of the EELR are not unexpected,
given the expected location of radio source shocks, but do provide
two key results: the clumpy ISM/IGM responsible for the EELRs
observed around powerful radio sources does appear to be in place
prior to the expansion of the radio source, and the kinematic prop-
erties of the extended regions are relatively undisturbed. Any dis-
turbance of the ISM/IGM due to an earlier interaction/merger has
since settled down.
6.5Spectroscopic evidence of a prior merger
If the triggering of radio source activity in this galaxy was due to a
merger or interaction, theproperties of any young stellar population
formed as part of that process can shed light on the exact mecha-
nisms and time scales involved. Our continuum modelling of these
spectra confirms the presence of a young stellar population, whose
formation occurred several million years in advance of the onset
of AGN activity. The mass of this YSP component is a low pro-
portion of the total stellar mass of the host galaxy. Together with
the the quiescent kinematics in the outer regions of the EELR, and
the morphological evidence described above, this suggests that if a
merger/interaction was responsible for both the eventual triggering
of the radio source activity and the formation of the young stellar
population, it is most likely to have been fairly minor in nature.
9C J1503+4528 provides a detailed insight into many of the events
associated with the triggering of a powerful radio source. Our ob-
servations have shown that:
• The relative sizes of EELR and radio source (the former being
≈ 10 times larger), together with typical compact radio source ex-
pansion velocities of 0.1 c, suggest that both the luminous quasar
nucleus responsible for photoionizing the outer regions of the
EELR, and the radio source itself, were triggered simultaneously.
• The EELR ionization state is consistent with shocks being im-
portant on scales comparable to the radio source, with AGN pho-
toionization within the ionization cones being the dominant mech-
anism further from the AGN, beyond the extent of the radio lobes.
• The gas kinematics confirm that weak shocks could be im-
portant close to the radio source, and that the outer regions of the
EELR are relatively undisturbed. The kinematics suggest that mo-
tion along the radio axis may be taking place, which may indicate
the presence of outflows.
• The blue continuum emission and Balmer absorption features
suggest that recent star formation has occurred, but their spatial
distribution suggests that it isnot caused by the passage of the radio
• Modelling of the observed continuum emission gives a best-fit
age for the young stellar population of 5 × 106years, and a mass
of roughly 0.06% of the total stellar mass of the host galaxy.
• Imagingobservations ofthehostgalaxyreveal asimpleellipti-
cal morphology; fitting of the K−band image suggests an effective
radius of ∼ 11.5kpc.
• A timescale of events can be built up from these results: star
formation is triggered by some event; in this case, any tidal interac-
tion or merger must have been relatively minor. AGN/radio source
activity follows the onset of star formation by several million years.
As a final consideration, we speculate on scenarios where the
lack of evidence for a recent merger may be significant. As noted
in the introduction, it is thought that the crucial ingredient for a
radio-loud AGN is that the central black hole is rapidly spinning,
a process which is most naturally explained by the coalescence of
two smaller black holes (Wilson & Colbert 1995). Indeed, the cos-
mic evolution of AGN activity can be well-described in terms of
the expected halo merger rate (Mahmood, Devriendt & Silk 2005).
However, the timescales involved in the black hole coalescence af-
ter the halo merger are extremely uncertain; while it is thought
that SMBHs can be brought within ∼ one parsec of each other
on a timescale similar to the dynamical friction timescale (e.g.
Milosavljvic & Merrit 2001), the mechanism for the final merger
is unknown.
One possibility is that the formation of an accretion disc
around one or both black holes provides the final necessary dynam-
ical friction (e.g. Armitage & Natarajan 2005). If we assume that
the central black hole of 9C J1503+4528 was spun up as part of the
AGN triggering process, the apparent simultaneity of the trigger-
ing of both the optical AGN activity (requiring an accretion disc)
and the radio jets (requiring the SMBH to be spinning rapidly) for
9C J1503+4528 would demand that the final SMBH coalescence
must take place on a very short timescale indeed. If this were not
the case, and SMBH coalescence occurred more slowly, one would
expect a period of radio-quiet AGN activity to precede the forma-
tion of the jets, which is ruled out in the case of this source by the
relative sizes of the EELR and radio source.
Giventhelackof evidence forarecent majormerger, wethere-
fore propose that the host galaxy of 9C J1503+4528 contained a
rapidly spinning SMBH prior to the present period of AGN activ-
ity. In this case, the SMBH would have been spun up a significant
time in the past, most likely during one or more mergers of smaller
gas-rich discs which, in hierarchical clustering models, are the pro-
genitors of ellipticals (e.g. Springel et al 2005). This scenario has
the advantage that radio-loud AGN may be "re-lit" by relatively
small gas injections from time to time, which provides a natural
route for the necessary mechanical energy feedback in the intra-
cluster medium (Nipoti & Binney 2005; Best et al 2005). However,
both 9C J1503+4528 and the well-studied cluster radio sources are
observed at relatively recent cosmic time. The time delay between
the initial creation of a binary SMBH pair and the onset of jet activ-
ity may have been significantly shorter in the early universe, where
gas-richmergerswere significantlymore prevalent. Suchascenario
could be tested by investigating any time lag between the evolu-
tion of the radio luminosity function at high redshift (which is still
poorly constrained, e.g. Willottet al. 2001) and thehalo merger rate
as predicted by hierarchical clustering models.
We thank Clive Tadhunter & Joanna Holt for useful discussions
and allowing us to develop the CONFIT software for our own use;
Daniel Smith and Matt Jarvis for obtaining the r-band image; and
Andy Adamson for obtaining the K-band image.
Page 12
K.J. Inskip et al
Some of the data presented herein were obtained at the W.
M. Keck Observatory, which is operated as a scientific partner-
ship among the California Institute of Technology, the University
of California, and the National Aeronautics and Space Administra-
tion. The Observatory was made possible by the generous financial
support of the W. M. Keck Foundation.
UKIRT is operated by the Joint Astronomy Centre on behalf
of PPARC.
KJI acknowledges a PPARC research fellowship, DL a
PPARC PhD studentship and GC support from PPARC observa-
tional rolling grant PPA/G/O/2003/00123.
It is a pleasure to express our gratitude and respect to the in-
digenous people of Hawai'i, from whose sacred mountain Mauna
Kea our observations were made.
We thank the anonymous referee for their very useful com-
ments on this paper.
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Ivezi´ cˇZ., White S.D.M., 2005, MNRAS, 362, 25
Best P.N., R¨ ottgering H.J.A., Longair M.S., 2000, MNRAS, 311, 1
Binette L., Wilson A.S., Storchi-Bergmann T., 1996, A&A, 312, 365
Blandford R. D., Znajek R. L., 1977, MNRAS, 179, 433
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C.J., Mason B.S., Pearson T.J., Readhead A.C.S., 2004, MNRAS,
354, 485
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Table A2. Changes to the best-fit YSP model with the inclusion of a power
law component. Columns 1 and 2 give the percentage of the power-law
component at a wavelength of ∼ 3600˚ A, and its spectral index, α (defined
as Fλ∝ λα). Column 3 gives the best-fit old stellar population age in Gyr.
The best-fit young stellar population age (in Myr) and mass (as a percentage
of the total stellar mass of the host galaxy) are given in columns 4 & 5
respectively. The reduced χ2for the best-fit model is listed in column 6.
Power law %
at ∼ 3600˚ A
Old SP
age (Gyr)
YSP properties
age (Myr)
mass %
(5) (2)
Osterbrock D.E., 1989, Astrophysics of Gaseous Nebulae and Active
Galactic Nuclei, University Science Books, Mill Valley, CA
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460, 634
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Schlegel D.J., Finkbeiner D.P., Davis M., 1998, ApJ, 500, 525
S´ ersic J.L., 1968, Atlas de Galaxias Australes (C´ ordoba: Observatorio As-
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R¨ ottgering H.J.A., 2000, MNRAS, 319, 445
Springel V., et al, 2005, Nature, 435, 629
Taylor G.B., Marr J.M., Pearson T.J., Readhead A.C.S., 2000, ApJ, 541,
Venemans B. P., et al., 2005, A&A, 431, 793
Waldram E.M., Pooley G.G., Grainge K.J.B., Jones M.E., Saunders
R.D.E., Scott P.F., Taylor A.C., 2003, MNRAS, 342, 915
Willott C.J., Rawlings S., Blundell K.M., Lacy M., Eales S.A., 2001, MN-
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Herewepresent theresultsof our emission-line fittingfor theparal-
lel, perpendicular and combined 2-d frames. Fluxes relative to both
[OII]3727˚ A and Hβ are tabulated in Table A1, as well as their
equivalent widths. Although flux ratios quoted relative to Hβ are
more common, the presence of Balmer absorption lines reduces the
Page 13
9C J1503+4528: a young radio source
Table A1. Spectroscopic properties of 9C1503+4528, determined from various spectra obtained perpendicular and parallel to the radio source. The spectra
were extracted with various width apertures, so as to probe the properties of the central and exterior regions of the extended emission structures. The total
integrated fluxes for the [OII] and Hβ emission lines are provided, given in units of 10−17Wm−2. All other emission lines are quoted in terms of their flux
ratios relative to both [OII] and Hβ within the extracted one-dimensional spectra. This has been done due to the fact that the levels of Balmer absorption
vary with position throughout the galaxy, and therefore a comparison with the Hβ line flux, though popular in the literature, may not be the most appropriate
option for this source. The errors on the Hβ and [OII] line fluxes are dominated by calibration errors, estimated to be<
this calibration error are added in quadrature with the errors arising from photon statistics. All quoted values in this table are corrected for galactic extinction
using the E(B − V ) for the Milky Way (Schlegel, Finkbeiner & Davis 1998) and the parametrized galactic extinction law of Howarth (1983).
∼10%. Errors on the other lines and
Details of extracted spectrum
[OII] flux
Hβ flux
Combined, 2′′
Parallel, 2′′
Perpendicular, 2′′
Parallel, 5′′
Perpendicular, 5′′
[OII]3727[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
[OII] Flux Ratio
Hβ Flux Ratio
Equiv. width
100100 100100 100
1635 ± 177
8.5 ± 0.9
139 ± 16.2
0.7 ± 0.2
12.1 ± 3.4
0.6 ± 0.2
9.1 ± 3.1
2.7 ± 0.4
43.7 ± 6.5
0.7 ± 0.3
11.6 ± 4.8
3.3 ± 0.5
54.2 ± 7.7
1.2 ± 0.3
19.8 ± 5.1
6.1 ± 0.7
10.7 ± 1.1
175 ± 19.7
22.6 ± 2.4
370 ± 41.2
1701 ± 191
8.7 ± 1.0
148 ± 18.2
1.6 ± 0.3
26.4 ± 5.8
1.0 ± 0.2
16.4 ± 3.0
3.0 ± 0.4
50.0 ± 7.3
0.9 ± 0.4
14.4 ± 6.3
3.7 ± 0.5
63.0 ± 8.7
1.1 ± 0.3
19.1 ± 5.6
5.9 ± 0.7
9.9 ± 1.1
169 ± 20.2
23.7 ± 2.5
403 ± 46.3
1588 ± 195
8.1 ± 1.0
128 ± 17.9
1.1 ± 0.3
16.7 ± 5.6
< 0.3
< 5.3
2.7 ± 0.5
43.3 ± 9.1
0.6 ± 0.4
9.4 ± 6.0
2.8 ± 0.5
44.1 ± 8.5
0.8 ± 0.3
12.8 ± 4.8
6.3 ± 0.8
10.5 ± 1.2
167 ± 21.8
24.1 ± 2.7
383 ± 50.7
1715 ± 231
9.5 ± 1.1
162 ± 24.3
1.3 ± 0.5
21.6 ± 7.9
0.6 ± 0.3
10.8 ± 4.8
1.9 ± 0.4
31.7 ± 7.0
0.8 ± 0.7
13.6 ± 12.4
3.7 ± 0.6
62.2 ± 11.3
1.4 ± 0.4
23.2 ± 7.4
5.8 ± 0.8
13.5 ± 1.6
232 ± 33.5
30.5 ± 3.2
523 ± 72.9
1766 ± 290
11.1 ± 1.5
196 ± 36.7
< 0.3
< 5.2
< 0.6
< 10.3
2.0 ± 0.7
35.0 ± 13.5
< 0.5
< 8.3
1.5 ± 0.5
25.4 ± 10.1
0.7 ± 0.4
12.0 ± 6.7
5.7 ± 0.9
12.4 ± 1.6
219 ± 39.6
25.2 ± 3.3
446 ± 83.1
[NeIII] 3869
Hζ 3889
Hǫ+[NeIII] 3967
Hδ 4102
Hγ 4340
ø3 4363
Hβ 4861
ø3 4959
ø3 5007
usefulness of this ratio. The values in Table A1 have been corrected
forgalacticextinction,usingvalues fortheHI column densityofthe
Milky Way taken from the NASA Extragalactic Database (NED),
and the parametrized galactic extinction law of Howarth (1983).
As part of our modelling, we consider the effects of the inclusion of
a power-law component on the best-fit YSP parameters. The pre-
ferred age of the young stellar population remains unchanged at
5Myr except for the strongest power-law contributions (> 25%).
However, the reduced χ2values indicate that models with a strong
power law contribution are not favoured.


text:
Date: 05/15/2013
Time: 8:30 AM - 6:00 PM
Location: 1210 Heller Hall
Cost: Free
Researching and Archiving the Estonians in America. A joint symposium of the Immigration History Research Center and Baltic Heritage Network
The symposium will bring interested parties together to share their experience, expertise and ideas as well as map and discuss future scenarios for growth, development and cooperation in researching and archiving the Estonians in America. Proposals are invited on (but not limited to) the following topics: archiving, history, cultural studies, literary studies, musicology, sociology.
The Immigration History Research Center at the University of Minnesota is home to the largest collection of archival materials about Estonians in the United States. It has become a popular destination for diaspora scholars and archivist alike.
Baltic Heritage Network (est. 2008) is a non-profit with a mission to foster cooperation between national and private archives, museums, libraries, institutions of research, public associations and organizations collecting and studying the cultural heritage of the global Baltic diaspora.
Abstracts of up to 500 words are welcome to be submitted by April 1, 2013 to Maarja Merivoo-Parro: email@example.com
Please register online at http://www.eventbrite.com/event/6342214735
8.30: Registration
9.00: Opening remarks by Erika Lee, Director of the Immigration History Research Center, Kris Kiesling, Director of Archives and Special Collections, Enda-Mai Holland-Michelson, Director of the Estonian Archive in the US, Maarja Merivoo-Parro, Board Member of Baltic Heritage Network
9.30: Keynote speaker Piret Noorhani - Communities, Culture and Heritage of the Estonian Diaspora in the Year of Cultural Heritage 2013
10.30: Peeter Väljas, Aet Tõnissoo - Common Interest and Joint Efforts: Co-operation of Immigration History Research Center, Estonian National Archives and Baltic Heritage Network in Researching and Archiving the Estonians in America - Past, Present and Perspectives
11.00: Break
11.30: Daniel Necas - Estonian American collection at the IHRC Archives: From humble beginnings to a great resource
12.00: Liisi Eglit - Estonia and Estonians as a Research Subject at Stanford University: an Overview of Sources and Projects of Stanford University Libraries and Hoover Institution
12.30: Lunch and tour of IHRC
14.30: Maarja Merivoo-Parro - Narrating ethnicity and the diasporic condition: a researchers perspective on American Estonian history
15.00: Ben Maegi - What Can Estonian Immigration Teach Us About U.S. Immigration History?
15.30: Kalju Kubits - Growing Up as an Estonian in Minnesota
16.00: Discussion
17.00: ROOM 90 FERGUSON HALL 17.00 Kelley Sundin (and performers) Estonian Choral Music: A source of National and Cultural Identity
Disability Options:
To request disability accommodations, please contact the Immigration History Research Center at 612-625-4800.


text:
Food Wrap
There are few food wraps as flexible as butcher paper. In addition to wrapping your sandwiches or meats in it, you can use it as a table cover. However, if you need specialized food wraps, like high yield, premium meat films or polyethylene-coated freezer paper for your church or school cafeteria, you'll find those at Nassco as well. They're right there next to the aluminum foil, plastic wrap and waxed paper. Shop online today and most of our in stock food wraps will be shipped nationwide or delivered locally to most of Wisconsin and northern Illinois tomorrow.


text:
Watch: Koalas get it on behind Andy Roddick
Andy Roddick was recently made the unwitting co-star of a steamy koala celebrity sex video during an interview he gave about his preparation for the Australian Open.
Wed, Jan 06, 2010 at 11:35 AM
Koala's just don't give a bleep. They'll do it anywhere, anytime, anyplace, even if if it's right behind tennis star Andy Roddick while he's giving an interview with a TV reporter ahead of the Australian Open. Watch it on MSNBC's Daily Joe.
Visit msnbc.com for breaking news, world news, and news about the economy
Are you on Twitter? Follow me (@sheagunther) there, I give good tweets.
And if you really like my writing, you can join my Facebook page.
The opinions expressed by MNN Bloggers and those providing comments are theirs alone, and do not reflect the opinions of MNN.com. While we have reviewed their content to make sure it complies with our Terms and Conditions, MNN is not responsible for the accuracy of any of their information.


text:
yes. so simple & perfect. notice the hasbeens. photos by the ever glorious vanessa jackman.
yes. so simple & perfect. notice the hasbeens. photos by the ever glorious vanessa jackman.
some of my favourite recent street style shots
credits: [1 + 2] styleclicker [3 +4] vanessa jackman [5] garance dore [6] hanneli mustaparta [7 + 8] mr. newton [9+10] all the pretty birds [11+12] stockholm street style
leather and skirt…. the words don't even sound right together. but it works! nice in winter, but you don't want to be caught in a heat wave in a leather skirt – that's for sure.
both images: vanessa jackman
i did a wee guest post about winter fashion over at kim gray yesterday, go have a look see.
(all images: vanessa jackman – my faaaaavourite street style blog)
woot toot toot jump on the mid week bumper fashion special train – #21 for those who are keeping count!
we are handsome (thanks to kate desmarais)
style sightings (perfect! just perfect)
katrin schacke (not really fashion but…. food from clothes! my two favourite things?)
bumper fashion special #17 – all the spring shows are starting to blur into one, will pick up with more 'normal' fashion specials next week!
moschino cheap & chic
luisa beccaria
gianfranco ferre
alberta ferretti
eley kishimoto
a détacher
after looking over my selections these past few weeks, i realised i will never tire of the cinched waist. i am also really intrigued by eley kishimoto's african / asian / retro fabrics.
and some street style, there have been some fantastic looks the past few weeks…
the sartorialist
vanessa jackman
been skimping on my bumper fashion special (#9) – apologies.
italian stylist / fashion editor – often seen on various street style blogs
via sartorialist, garance & vanessa jackman
i will cut my hair like that one day, i will! pic via vanessa jackman
i know the bumper fashion special usually comes on a sunday but, i couldn't wait!


text:
yeah i found some gears of war 2 dlc link is :
yeah i found some gears of war 2 dlc link is :
Game » consists of 13 releases. Released Nov 07, 2008
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Trey Songz ft. Fabolous - What I Be On
Artist: Trey Songz
Featuring: Fabolous
Producer: Phenom & Troy Taylor
Album: Inevitable EP
Avg Rating: 2.7 ( 21 votes )
Update: Click "Listen Now" above to watch Trey Songz' "What I Be On" video.
If you've had your browser locked to the Booth, you know that, in addition to his usual R&B sh*t, the Trey Songz has also been on some "other sh*t"—more specifically, rap sh*t. Fresh off showcasing those respective sh*ts on two separate mixtapes (Anticipation 2 and #LemmeHolDatBeat 2, both released today), Trigga delivers some combination-type sh*t (OK, I'm done saying "sh*t," I promise) on the lead single off his next studio album, mixing the heavy swag and paper-stacking subject matter of his hip-hop material with his characteristically smooth vocal style. What I Be On, Phenom and Troy Taylor's mechanical, synth-accented strut sets the stage for braggadocious verses from the heavyweight crooner. After Songz is done soulfully flaunting his bulging bankroll and his female appeal, East Coast mainstay Fabolous grabs the mic to do a little caked-up stunting of his own. So, Booth readers, are you feeling what Trey Songz is on? If so, keep it locked to The DJBooth for the latest news and tunes leading up to the release of Inevitable EP out November 28, and Chapter 5 in 2012.
Trey SongzFabolous Music VideosR&B/PopHitmakerClub
Written by richard on Nov 01, 2011
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text:
Even though we knew it was coming there were many questions surrounding how it would be executed. The speculation ended today with the unveiling of the Shaqtue.
Shaquille O'Neal implemented a plan he announced a few weeks ago while a guest on 98.5 The Sports Hub's "Toucher and Rich Show" promoting his All-Star Comedy Jam and played statue in Harvard Square.
During the interview, Shaq said he would be venturing to Harvard Square at a date to be tweeted later and would sit on a bench and act like a statue for an hour. While there fans would be allowed to take pictures and sit next to him, but you would not be able to talk to him because, in Shaq's words, "I'm a statue."
With a tweet in the early afternoon, Shaq announced he was on his way to Harvard Square for his street performance, and hundreds followed.
When Shaq arrived he made his way to a bench and as promised, just sat there. Local media tried to interview the Shaqtue but he remained stoic and did not speak. Many fans fought for position to get a picture with the big man who sat, hands crossed, on a bench. Even with fans putting their arms around him, Shaq never moved.
In this day and age it is hard to imagine an athlete, especially one as recognizable as Shaq, doing anything like this. There is a reason Shaq is such a fan favorite and stunts like this show why.
ESPN's Chris Forsberg spoke with a few of Shaq's teammates, none of whom showed up on the rainy afternoon to watch, for their thoughts on what Shaq was doing.
"What's he going to do?" asked Celtics captain Paul Pierce. "He's just going to sit there? Somebody get a picture of that and tweet it."
Celtics forward Kevin Garnett was asked if he would be attending the spectacle.
"Absolutely not," said Garnett. "I will not be taking pictures of Shaq with bird [expletive] and all types of other people taking pictures. I'm cool. I see him in here; I'll take my pictures around here."
I hope this is only the beginning for Shaq and his public demonstrations in Boston. It would also be fantastic if these ideas rubbed of on his teammates and they all join in. Maybe a they join the ducks crossing the road? Only time will tell.


text:
Brey: Irish should aim for Big East title
Updated: October 11, 2012, 9:21 PM ETAssociated Press
SOUTH BEND, Ind. -- Heading into what could be Notre Dame's last season before joining the Atlantic Coast Conference, coach Mike Brey would like the Fighting Irish to take something with them as they prepare to leave the Big East: their first ever outright regular-season title.
Brey said he began talking about that goal with his players in March, after they squandered a 10-point lead midway through the second half and lost 67-63 to Xavier in the first round of the NCAA tournament. He's ...
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Environmental awareness is a growing part of B.C. culture. The care and stewardship of our natural resources is a responsibility that we're taking seriously. While we strive to be leaders in this regard, we also know there's room for improvement, too. Explore what our environment has to offer.
Years of pollution produced by humans is causing unprecedented changes to the environment including global warming. This has caused the whole world's climate to change which leads to things like melting glaciers and stronger storms.
Get inspired by the province's natural beauty and make plans for your next outdoor adventure. Take advantage of the many recreation opportunities available across the diverse landscape of mountains, rivers, lakes and coastlines.
Monitor your home and property or any other area where pests are a concern. Be prepared to take appropriate action when pests cause damage or health issues. Learn about using less harmful pesticides and integrated pest management techniques to help protect natural environments.
British Columbia is home to tens of thousands of plant and animal species living in a rich diversity of habitats and ecosystems. Responsible decision making and positive action on our part will help protect B.C. wildlife and their home.
B.C. is proud to be a leader in sustainable environmental management – with air and water quality that ranks among the highest in the world. Effective waste management procedures and solutions contribute a great deal to preserving our environment.
All living things depend on air and water to survive. Caring for our environment includes keeping our air and water supply fresh, clean and healthy.
Sharing key scientific and technical information is an important part of monitoring and managing our natural resources.


text:
Utah Jazz v Detroit Pistons
Similar imagesView all
Will Bynum of the Detroit Pistons goes in for the easy layup against... News PhotoAuburn Hills,Basketball - NBA Pro,Basketball - Sport,Detroit Pistons,Horizontal,Independence,Lay Up,Match - Sport,Michigan,Palace,Sport,Taking a Shot - Sport,USA,Utah Jazz,Will BynumPhotographer Dan LippittCollection: National Basketball Association 2013 NBAEAUBURN HILLS, MI - JANUARY 12: Will Bynum #12 of the Detroit Pistons goes in for the easy layup against the Utah Jazz during the game on January 12, 2013 at The Palace of Auburn Hills in Auburn Hills, Michigan. NOTE TO USER: User expressly acknowledges and agrees that, by downloading and/or using this photograph, User is consenting to the terms and conditions of the Getty Images License Agreement. Mandatory Copyright Notice: Copyright 2013 NBAE (Photo by Dan Lippitt/NBAE via Getty Images)


text:
Together On The Sand
Charlie Brown Jr.
Together on the sand,
We walked hand in hand
On the beach front,
She smiled at me
As she tightly held my hand
I had my finger up her...
Country music played on the radio, so I turned it off
And we walked down to the water,
As she grabbed on to my honker
A wave swept us away
What a ho 3x
Composição: Sabe quem é o compositor? Envie pra gente.
Enviada por Vitor
Enviada por Vitor


text:
Single Mom: In Pursuit of Self-Care
The constant pursuit of self-care is important for all parents to consider, but especially if you're a single mom.
Finally Figuring Out A Healthier Me
by Mir Kamin
As someone who has always loved food and hated exercise, learning how to take care of myself has been surprisingly fraught (but ultimately rewarding).
Let's Talk About Sex, Baby
by Mir Kamin
Teenagers and burgeoning sexuality. The conversations are becoming more difficult, but we'll keep having them, because communication and knowledge are key.
On Finding a Breast Lump
by Amalah
A young woman found a breast lump and her doctor has asked her to schedule a mammogram and ultrasound. Even though the doctor is not worried, she is freaking out and needs some perspective.
Everything You Always Wanted to Know About Lice* (*But Were Too Grossed Out to Ask)
by Wendi Aarons
LICE, is a four-letter word for a reason. We wade through all the myths surrounding lice leaving you with the truth and how to get rid of the buggers.
Bug Repellents for Kids: What Should I Be Thinking About?
by Wendi Aarons
There's more to think about when it come to protection from insects, like mosquitoes and ticks, than just "let's spray THIS." We look at DEET and other considerations.


text:
Pune: The University of Pune senate has approved a massive annual budget of Rs555 crore for 2014-15 fiscal year, which is its highest ever. The budget, showing a deficit of Rs159 crore, has substantial allocations for skill development, industrial development, innovation centre, science park, folk art and research centre. However, questions regarding the implementation of the proposed schemes in the coming days haven't yet been addressed. In addition, the varsity has earmarked Rs44.75 crore for students' inclusive development, under which students from earn-and-learn scheme have been included. For students from the affiliated colleges, Rs50 lakh has been allocated under the Students Insurance Scheme.
Senate member Dr Sunanda Navale presented the budget before the senate, which was formally approved after cut-motions and other suggestions made by other senate members. "Though the university sets aside funds under different heads, they are not utilised. It unnecessarily inflates the overall budget, showing deficit," said senate members Ashok Kamble and Mahes Abale.
Abale said that in the last budget there were budgetary provision for colleges in tribal areas. However, it was not spent and a suggestion has been made that the varsity should make sure that it should be spent on the particular heads after allocation of funds.
New plans
Skill Development Centre : In the current budget, in order to hone skills of the students who are industry-ready, the varsity has proposed to start a skill development centre in the university premises.
Industry Development Centre : In order to increase entrepreneurship skills among students and to help them set up their own startups, the varsity has plans to start a Centre for Industry Development.
Innovation Centre : To encourage students to carry out innovative research in various fields which can later be commercialised, an innovation centre will be set in the premises of the university. The centre will be a crucial vital cog between the university and the industry.
Science Park : To inculcate the interest among the students with respect to science, a well-equipped science park is on the anvil.
Other budgetary provisions: Plans for a folk art study and research centre, multilingual research centre, and a well-equipped Information Technology cell is also on the cards.


text:
Jeff Gage
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Five years after the death of Marcus Homer, Viu completes his training and begins his quest. While passing through St. Louis he meets a man who shares the same mission and dedication as himself. This man is Will Johnstone, and he is a master of ropes! Does Viu have a new partner?!
Story and art by Nobuhiro Watsuki.
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"I don't know, I haven't thought about it," she said. "If I did, it's, skipping my mind."
McCoy said that about 20 years ago, former town supervisor Lou Tessier created a line in the budget called "Title Pay" which over the years included specific extra amounts above base pay and longevity stipends for certain employees, based on merit, educational certification, or extra work details.
In past years, some of these stipends were not formally approved by the town board, and at times, certain board members may not have been aware of them, McCoy said.
The public might not have been fully aware of the stipends, either.
The title pay amounts were not listed in pay ledgers published for the public and approved in annual organizational meetings, McCoy said. They were only listed in an aggregate sum under a special budget code, town officials said.
McCoy said these extra stipends, over the most recent five years that the auditors were focusing on, accounted for $234,000 - and perhaps far more if the auditors had taken all 20 or more years and examined all the town's employees payroll records, rather than just 20 employees records.
"These were not indiscriminate raises," McCoy said. "Title Pay" was awarded to those who deserved it based on performance, extra training, or working above and beyond expectations."
Former Lake George Town Supervisor Lou Tessier defended his practice of awarding the extra stipends.
He said that Title Pay was awarded based on extra work performed or additional responsibilities. he said it was a way to assure that new employees would not start out at the higher pay levels earned by those employees who retired.
"Our employees were paid well, and they provided good services to the town's residents," Tessier said. "They got paid what they deserved."
He said that the state should have voiced their objections to Title Pay years ago in three audits performed over 26 years. He said an auditor hired by the town over many years had no objection to the practice either.
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