1. Rapture of the Deep Sky Mel Ulmer Dept of Physics & Astronomy Northwestern University http://www.astro.northwestern.edu/~ulmer This talk posted on http://www.astro.northwestern.edu/~ulmer/private/coma/Rapture_of_the_Deep_sky.ppt Also need http://www.astro.northwestern.edu/~ulmer/private/comahttp://www.astro.northwestern.edu/~ulmer/private/coma/mirror_comparison_lg.mov [quicktime] Also need http://www.astro.northwestern.edu/~ulmer/private/coma/lens0.mpeghttp://www.astro.northwestern.edu/~ulmer/private/coma/lens0.mpeg [quicktime]

2. Clusters come into existence? Age of Universe about 13.7 Gyr

4.  M h 2  h 2

8. k[h Mpc –1 ] P(k) [h –3 Mpc 3 ] [h Mpc –1 ] [h Mpc –1 ] P(k) Complementary measure crucial; Improves w and dw/dz by ~ factor 4

10. dN/dz + P(k): Time-dependence of w(z) w(z)=w 0 + w 1 z / (1+z) cf WMAP fiducial model Mass limit to mimic X-ray survey (~10 14 -10 15 M  ) 10,000 square degrees Errors from 6x6 Fisher matrix dN/dz P(k) dN/dz + alone alone P(k)  w 1 0.52 0.67 0.15  w 0 0.15 0.14 0.048  0.014 0.017 0.006  8 0.007 0.019 0.0033  H 0 0.30 0.26 0.015  n s 0.07 0.05 0.05 From Z. Haiman: Work in progress with S.Wang & J. Khoury (Columbia) M. May (Brookhaven) Majumdar & Mohr (2003)

13. 2.5 arcmin/1.1 Mpc RCS1325+2858 z=0.95 Smoothed X-ray emission contours

14. The Coma Cluster Rich cluster Relatively close by: distance = 95 Mpc redshift = 0.02 High galactic latitude: Ra = 12h 59m 48s Dec = 27d 58.8m NGC 4889 NGC 4874 NGC 4911 10’ 280 kpc

15. Coma Cluster Zoomed

16. 300 kpc

17. Coma Cluster X-ray residuals

18. Color-Magnitude Relation Many of our LSBs fall on the CMR! => Same origin and aging as larger galaxies From R= 18!

19. The CMR and LSBs Evolution CMR is a metallicity effect: elliptical galaxies undergo extended star formation at high redshifts creating the CMR and then evolve passively LSBs along the CMR sequence were formed at the same time as bright ellipticals and evovled in the same fashion Consistent with cluster formation simulations: first galaxies created are in the center (CMR LSBs) Contours of CMR LSBs 4889 4874 4911

21. Blue LSBs Residual from X-rays after isothermal sphere fit subtracted All LSBs

22. 0.5-2.0 keV X-rays ROSAT, raw data

23. 0.5-2.0 keV X-rays ROSAT, wavelet filter processed

24. Cl 1205+44 z = 0.6

25. Cl 11205+44 X-rays and Radio

27. Cl 1257+47 z = 0.9 color visible + near IR

28. Cl 1257+47 left color, visble=> near IR; right X-ray plus near IR

29. Compilation of L x of Clusters versus z

30. Chandra Mirror Blank

31. XMM-newton Area vs energy

33. XMM-Newton coated mandrel

34. Resulting XMM-Newton Ni Mirror Au coated on inside

35. Wolter I X-ray optic design

36. Chandra X-ray Observatory CXC Schematic of Grazing Incidence, X-ray Mirrors

37. 7 keV image made at APS UNIT-CAT

38. XMM- Newton CCD camera

39. What a low temp detector (LTD) does for you vs a CCD CCD Energy resolutionLTD Energy Resolution

41. Dream Machine: 3,000 sq cm 10 eV energy Resolution 1 degree FOV 10 arc sec angular resolution Sky coverage between 1,000 and 10,000 sq degrees yielding approximately 10,000 clusters === Focal Length approximately 3 meters, diameter less than 2 meters. => NO Shuttle Launch Required!

42. Competition: XMM (1,00 sq mc) 10 degrees “deep” (approximately 50ksec/pointing) contiguous, 200 degrees shallower (approximately 10 ksec/exposure) and discontinuous, CCD energy resolution average angular resolution approximately 20 arc seconds. Chandra collection area ~400 sq cm, 0.5 arc second angular resolution. Steradian coverage approximately the same as XMM.

43. Hero Dr. Mel: Untouched comic strip. Reminds us we live on 4-D surface in 5-D manifold