     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?'

    candels_2epoch: 'CANDELS 2-epoch'
    ukidss: 'UKIDSS'
    sdss_singleband: 'Single-band images'
    ferengi: 'Artificially redshifted images'
    dr8: 'Data Release 8'
    sdss_id: 'SDSS ObjectID'

    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:
