Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N....
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Transcript of Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N....
![Page 1: Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N. Scoville Kyoto, May 23, 2005.](https://reader030.fdocuments.us/reader030/viewer/2022032800/56649d3b5503460f94a16239/html5/thumbnails/1.jpg)
Redshift Evolution of the Correlation Function
Peter Capak
J. Blazek, D. Sanders, I. Szapudi, N. Scoville
Kyoto, May 23, 2005
![Page 2: Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N. Scoville Kyoto, May 23, 2005.](https://reader030.fdocuments.us/reader030/viewer/2022032800/56649d3b5503460f94a16239/html5/thumbnails/2.jpg)
Correlation function
• Probability above random that you will find two objects at a given (projected) distance
• Should trace the growth of structure• eSpICE allows for computation of 2pt function
in ~30sec for cosmos data– Allows for many measurements as a function of
many different parameters
• Results shown are preliminary
![Page 3: Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N. Scoville Kyoto, May 23, 2005.](https://reader030.fdocuments.us/reader030/viewer/2022032800/56649d3b5503460f94a16239/html5/thumbnails/3.jpg)
![Page 4: Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N. Scoville Kyoto, May 23, 2005.](https://reader030.fdocuments.us/reader030/viewer/2022032800/56649d3b5503460f94a16239/html5/thumbnails/4.jpg)
Correlation with Redshift and Magnitude
![Page 5: Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N. Scoville Kyoto, May 23, 2005.](https://reader030.fdocuments.us/reader030/viewer/2022032800/56649d3b5503460f94a16239/html5/thumbnails/5.jpg)
Correlation with Redshift and Type
![Page 6: Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N. Scoville Kyoto, May 23, 2005.](https://reader030.fdocuments.us/reader030/viewer/2022032800/56649d3b5503460f94a16239/html5/thumbnails/6.jpg)
Preliminary Results
• Brighter and older galaxies are more strongly clustered
• Increase in the correlation strength with redshift for bright galaxies
• Increase in the correlation slope with redshift