Page Comparison

• generate draft of research proposal by end of today. 
  • intro about SFR vs. redshift
  • observable proxies for SFR (emission line EW)
  • why study this in high mass clusters, previous work.
  • Why is SPT sample special?
    • highest-mass clusters across wide range of redshifts
    • existing spectroscopic data that includes some emission line galaxies
    • independent x-ray mass estimates for many of these clusters. 
  • we can therefore explore the redshift dependence of SFR in the most extreme cluster environments, across 0.2<z<1.

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The galaxy cluster sample we plan to use is selected from South Pole Telescope (SPT; Carlstrom et al. 2011) observation exploiting the Sunyaev-Zeldovich effect. The sample consists of high-mass clusters across a wide range of redshift (0.2 < z < 1.3), of which most also have spectroscopic data (from Magellan, Dressler et al., 2006 or Gemini, Hook et al., 2004) with emission line measurements. Furthermore, independent mass estimates from hot gas X-ray emission are also available for many of these clusters. Using these data (and perhaps more if follow-up observations are possible), we will be able to explore the redshift dependence of SFR in the highest-mass clusters.

• Go through and learn the spectroscopy reduction process using raw data files provided by Jonathan
• discuss with Chris about the project. How about Matt's suggestion of "SPIRE image of SPT clusters"?
• write quick summary of key papers, including a clip out of key plots.

• arrange meetings with 1) jonathan ruel, 2) matt bayliss to talk about Gemini and Magellan existing spectroscopy.

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