1. Kevin Cooke

2.  Galaxy Characteristics and Importance  Sloan Digital Sky Survey: What is it?  IRAF: Uses and advantages/disadvantages ◦ Fits files?  Question: Can we observe the red sequence from the cluster total redness? What are the observed features of SDSSJ1336?

3. M89 Hubble Space Telescope

4.  Lack of cold dust in low redshift ellipticals ◦ This manifests in low star formation.  Redness, defined here as the difference between blue and red, should increase with z.  Little to no ionization emission lines due to lack of ionizing radiation.

5.  8 year project from 4000-10000 A ◦ 8400 square degrees covered  Includes over 930,000 Galaxies! ◦ > 120,000 quasars  More than a quarter of the sky and capable of measuring redshift. ◦ 3D Universe generation possible!

7.  Apache Point Observatory, Sunspot, NM ◦ Maintained by New Mexico State University  Dedicated 2.5 m telescope. 120 megapixels  5 filters ◦ u - 3543 A ◦ g - 4770 A ◦ r - 6231 A ◦ i - 7625 A ◦ z - 9134 A

8.  Total of 3 surveys performed since 2000. ◦ SDSS I 2000-2005 ◦ SDSS II 2005-2008 ◦ SDSS III 2008-2014  The SDSS was funded by the Alfred P. Sloan Foundation, NSF, and the Department of Energy.

9.  Organized by the National Optical Astronomy Observatory (NOAO)  A collection of tasks using Unix architecture rather than one program.  No error or exception feedback, the impetus for PyRAF.

10.  A fits file is an image storage file extension first developed in the 1980s. Support office available at NASA GSFC.  Stores data as a table of values in multiple ‘dimensions’ that can be called individually.  This allows for multiple wavelength files to be in one file together (Hopefully properly labeled)

11.  A measurement of the redness of the population of ellipticals in clusters. Done by Mike Gladders and H.K.C. Yee at the University of Toronto.  Can we observe the trend purely based on a photometrically derived redness for the entire cluster? ◦ Could be a rough estimation device.

12. Gladders, M., & Yee, H. (2000). A new method for galaxy cluster detection.  Clusters have differentiation of each galaxy type at each redshift.  Each color-color relation can be plotted alongside.  Important - Ellipticals do not overlap!

13.  A redward trend is visible at low confidence.  Caveat: Total color, not individual color.  More data is needed.

14.  The modeled color-color plot of galaxy clusters was for a apparent magnitude of - 22.  Projection effects from incorrect masking during photometry in the pipeline.  Filter wavelengths may not have the same coverage.

15.  Attain data on constituents of cluster.  Test for layering of ellipticals, spirals, etc.  Develop alternative analytical methods. ◦ IDL ◦ QfitsView  Focus on a few important galaxies, or at least that have easily read data…

16.  Brightest Cluster Galaxy ◦ Dominant elliptical at the center of a cluster. ◦ Lensing?  Z = 0.1764 ◦ This translates to 2.1 Gyr ago. ◦ Redshift applies to all colors.

21.  SDSSJ1336 has detectable OIII, Hβ ◦ OIII/Hβ=0.46

22.  SDSSJ1336 is a LINER Galaxy.  The Red Sequence may be visible with average color, however high margin for error.  Many display tools are available for data, and future work should focus on this possibilities.

23.  SDSS Visual Spectra Interactive Display  IRAF  Gladders, M., & Yee, H. (2000). A New Method for Galaxy Cluster Detection.