         answer_2: ''
         answer_3: ''
         answer_4: ''
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-  
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+
   astronomers:
     heading: 'Galaxy Zoo for Astronomers'
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     explanation:
       goals: 'This page aims to give background to the scientific motivation behind the project for a more technical audience.'
       data: 'You may be looking for data - public Galaxy Zoo data is available in a range of formats <a href="http://data.galaxyzoo.org">here</a>.'
       papers: 'Alternatively, you can browse a list of papers published by the team <a href="https://www.zooniverse.org/#/about/publications">here</a>.'
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     morphology:
       heading: 'Why is galaxy morphology important?'
       body: '''To first order, the morphology of a galaxy is a tracer of the orbital dynamics of the stars in it, but it also carries an imprint of the processes driving star formation and nuclear activity in galaxies. Visual morphology produces classifications which are strongly correlated with other, physical parameters. To give a single example, the presence of multiple nuclei and extended tidal features indicates that the dominant mechanism driving star formation is an ongoing merger. Equally, the absence of such features implies that the evolution of the galaxy may be being driven by slower ('secular') processes.'''
       reference: '''Traditionally morphology has been derived either by visual inspection of galaxy images (e.g. <a href="http://adsabs.harvard.edu/abs/1926ApJ....64..321H" target="_blank">Hubble 1926</a>, <a href="http://heasarc.nasa.gov/W3Browse/all/rc3.html" target="_blank">de Vaucouleurs 1991</a>, and more recently e.g. <a href="http://arxiv.org/abs/1001.2401" target="_blank">Nair and Abraham 2010</a>) or via morphological parameters, such as Concentration, Asymmetry, Clumpiness, M20, the Gini coefficient, etc (e.g. <a href="http://arxiv.org/abs/astro-ph/0303065" target="_blank">Conselice 2003</a>, <a href="http://adsabs.harvard.edu/abs/2008ApJ...672..177L" target="_blank">Lotz et al. 2008</a>). Strictly speaking, these parameters are morphological 'proxies', each with its own attendant biases, which are typically checked and calibrated against visual inspection. A visual approach is generally more resistant to changing signal-to-noise and resolution in images (e.g. <a href="http://labs.adsabs.harvard.edu/adsabs/abs/2008ApJS..179..319L">Lisker 2008</a>), making it an ideal method for determining galaxy morphology. Nevertheless, morphological parameters have been valuable for classifying large survey-scale datasets, for which visual inspection by individuals (or small groups of researchers) can be prohibitively time-consuming.'''
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     classification:
       heading: 'Classifications of large survey datasets using Galaxy Zoo'
       body: 'Galaxy Zoo (<a href="http://arxiv.org/abs/0804.4483" target="_blank">Lintott et al. 2008</a>, <a href="http://arxiv.org/abs/1007.3265" target="_blank">2011</a>) pioneered a novel method for performing large-scale visual classifications of survey datasets. Using more than half a million members of the general public, the project has classified – via direct visual inspection - the entire Sloan Digital Sky Survey spectroscopic sample and all existing Hubble Space Telescope surveys (around 1.5 million galaxies in total). With more than 40 classifications per object, Galaxy Zoo provides both a visual classification and an associated uncertainty (which is challenging to estimate if there are only a few human classifiers). The classifications themselves have been demonstrated to be of comparable accuracy to those derived by expert astronomers (see Lintott et al. 2008).'
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     highlights:
       heading: 'Galaxy Zoo science highlights'
       body: '''The Galaxy Zoo science programme has contributed to a diverse set of topics, largely focused on the nearby and intermediate-redshift Universe. Some recent highlights include the largest studies of galaxy mergers (<a href="http://arxiv.org/abs/0903.4937">Darg et al. 2010</a>), tidal dwarf galaxies (<a href="http://arxiv.org/abs/1108.4410">Kaviraj et al. 2012</a>), dust lanes in early-type galaxies (<a href="http://arxiv.org/abs/1107.5306">Kaviraj et al. 2012</a>) and bars in disc galaxies (<a href="http://arxiv.org/abs/1003.0449">Masters et al. 2011</a>, <a href="http://arxiv.org/abs/1205.5271">2012</a>) in the nearby Universe to date. One of the unique aspects of Galaxy Zoo over automated morphological measurements is the possibility of serendipitous discoveries (often aided by volunteer led discussion on the <a href="http://www.galaxyzooforum.org">Galaxy Zoo Forum</a>). These have included the discovery of 'green peas' (a class of compact extremely star-forming galaxies in the local Universe; <a href="http://arxiv.org/abs/0907.4155">Cardamone et al. 2009</a>) and perhaps most famously "Hanny's Voorwerp" (<a href="http://arxiv.org/abs/0906.5304">Lintott et al. 2009</a>) along with a survey of similar AGN-ionised gas clouds (<a href="http://arxiv.org/abs/1110.6921">Keel et al. 2012</a>). The availability of a large sample of galaxies with both color and morphological information has led to the important realisation that color, not morphology, is most strongly correlated with environment (<a href="http://arxiv.org/abs/0805.2612">Bamford et al. 2009</a>; <a href="http://arxiv.org/abs/0811.3970">Skibba et al. 2009</a>), leading to intriguing subclasses of galaxies like red spiral galaxies (<a href="http://arxiv.org/abs/0910.4113">Masters et al. 2010</a>) and blue ellipticals (<a href="http://arxiv.org/abs/0903.3415">Schawinski et al. 2009</a>).'''
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     relaunched:
       heading: 'Galaxy Zoo Relaunched'
       sdss: '''The current site has incorporated images from a variety of different telescopes, including SDSS, HST, UKIRT, VST and the CTIO 4-m Blanco telescope. The SDSS images are from DR8 and the Southern Galactic cap, which increases the sample size of galaxies in the local universe by 40%. The HST images are from <a href="http://candels.ucolick.org">CANDELS</a>, the largest HST Treasury Program. This survey is designed to take advantage of the advent of Wide Field Camera 3 (WFC3), which is rapidly opening up a new window into galaxies at z > 1 – the first 50% of the lifetime of the Universe. Previous HST imaging at these epochs largely sampled the rest-frame ultraviolet, since the available survey instruments (e.g. ACS) operated in the optical wavelengths. However, the near-infrared capabilities of the WFC3 (a factor of 20 better than NICMOS) are providing us with unprecedented rest-frame optical data of galaxies at z > 1.'''

        answer_2: 'larger'
        answer_3: 'more luminous'
        answer_4: 'less massive'
      
      question_2:
        text: 'The three spectral curves shown in the graphs illustrate the energy output versus wavelength for three Stars A, B, and C. Which of the stars has the highest temperature?'
        answer_0: 'Star A'

        'a-0': 'Tight'
        'a-1': 'Medium'
        'a-2': 'Loose'

    'candels-14':
      text: "How many spiral arms are there?"
      title: "Spiral"
