     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="http://www.zooniverse.org/publications?project=hubble">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>.'
     
     morphology:
       heading: 'Why is galaxy morphology important?'

    
    relaunched:
      heading: 'Galaxy Zoo Relaunched'
      sdss: '''The current site incorporates images from three different telescopes: SDSS, HST, and UKIRT. 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 CANDELS, 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.'''
      candels: 'CANDELS is using the WFC3 near-infrared filters to image 800 arcmin<sup>2</sup> in established HST legacy fields (e.g. GOODS, COSMOS). The near-infrared WFC3 images are particularly important because morphological analysis is best performed in rest-frame optical wavelengths, which trace the underlying stellar population of the galaxy rather than just the UV-bright star-forming regions.'
      combination: 'The combination of the SDSS and CANDELS Galaxy Zoo samples will offer a formidable tool for answering significant open questions that demand a morphological analysis. For example, at what epochs was the Hubble sequence established? How and when were the primordial spheroids formed? What was the relative role of major mergers and secular processes in driving star formation and black hole growth in the early Universe?'
      ukidss: 'The UKIRT images are from the Large Area Survey (LAS) as part of UKIDSS, which imaged 4000 sq. deg. of the sky overlapping with the SDSS fields. We selected all galaxies classified in Galaxy Zoo 2 that had high-quality UKIDSS imaging, totaling about 70,000 galaxies. The images shown on the site are a colour-composite of the Y, J, and K-band images (where the J-band uses dithered observations to improve the angular resolution in that channel). These images will allow us to trace morphology as a function of wavelength; for example, whether the observed bar fraction increases for galaxies in the rest-frame infrared.'
      ferengi: 'Galaxy Zoo also includes a small set of SDSS images that have been artificially processed to simulate the observed effects of redshift. This set used a morphologically diverse sample of galaxies from Galaxy Zoo 2 and were processed using the FERENGI code (<a href="http://www.mpia-hd.mpg.de/FERENGI/">Barden, Jahnke, & Hausler 2008</a>) out to redshifts of z=1. Results from these images will be used as calibration for galaxies in the GZ: Hubble and CANDELS data, since it allows us to assess resolution and brightness-dependent biases independent of true galaxy evolution.'
      newdata: 'In early 2015, three new sets of data were put into Galaxy Zoo. Two of them are from Hubble surveys for which we already have GZ morphological classifications --- GOODS and CANDELS. The new images explore how changing the depth of data (a surface brightness limit) affects the morphological measurements. The new CANDELS images are from 2-epoch data (which is shallower than the 5-epoch data already cataloged), and the GOODS images come from the full-depth images, supplementing the shallow observations already completed in GZH. Finally, we added roughly 1000 images each of galaxies from SDSS in their monochrome <i>ugriz</i> filters, which will allow a more careful measurement of morphology as a function of wavelength.'
      conclusion: 'The purpose of the Galaxy Zoo project is to answer such questions, prepare the ground for morphological work using future instruments like the JWST and produce samples of morphologically selected high-redshift galaxies for follow-up using instruments like the extremely large telescopes and ALMA.'
  
  
  classify:

    p11: 'A new generation of surveys using the WFC3 is giving us an unprecedented view into the first third of the lifetime of the Universe: the first 3-4 billion years after the Big Bang. Foremost among these is the Cosmic Assembly Deep Extragalactic Near-infrared Survey (CANDELS). The largest treasury survey using the Hubble Space Telescope to date, CANDELS is surveying several patches of sky to put together the largest collection of deep infrared images of galaxies in the early Universe. The combination of Galaxy Zoo and CANDELS offers a formidable tool in our quest to understand the earliest stages of the evolution of the visible Universe, one of the fundamental questions in observational cosmology today.'
    p12: '''While astronomers have learned an amazing amount from the SDSS and Hubble images, there are also areas we can only probe if we look at galaxies in wavelengths beyond those seen by the human eye. For objects that radiate thermally (such as stars), the wavelength used probes the temperature of the object being observed. Stars like our own Sun have temperatures around 5500 K, which show up strongly in the optical wavelengths used in SDSS imaging. If we look at galaxies in ultraviolet wavelengths, however, hotter regions become more prominent; in galaxies, this means we're picking out young, massive stars and individual star-forming regions (often leading to a patchier appearance). For galaxies observed at infrared wavelengths, cooler regions become more prominent; these include older and lower-mass stars, as well as clouds of dust that are heated by the stars and then re-emit that light at lower energies.'''
    p13: '''Comparing the morphologies of galaxies at multiple wavelengths gives astronomers a much more complete picture of the processes that govern their astrophysics. Tracing stars by temperature gives us proxies for their age and chemical evolution, while identifying star formation regions tells us where the densest parts of the disk are and where the mass in these galaxies is being built up.'''
    p14: '''Infrared images on Galaxy Zoo come from the United Kingdom Infared Survey Telescope (UKIRT), a 3.8m telescope located on the summit of Mauna Kea in Hawaii at nearly 14,000 ft. elevation. Starting in 2005, UKIRT began an infrared survey of the northern sky called UKIDSS, covering 7500 square degrees at wavelengths of 1--2.5 microns. A portion of this survey was dedicated to covering the same regions as the SDSS. This means that the new UKIDSS images in Galaxy Zoo have already been classified by users in Galaxy Zoo 2; this will let us do direct comparisons for the two samples and examine how morphology (like the fraction of galaxies with bars, for example) changes with the wavelength being used.'''
  
  
  story:
