Rapture of the Deep Sky

Mel Ulmer

Dept of Physics & Astronomy

Northwestern University

http://www.astro.northwestern.edu/~ulmer

This talk posted onhttp://www.astro.northwestern.edu/~ulmer/private/coma/Rapture_of_the_Deep_sky.ppt

Also need

http://www.astro.northwestern.edu/~ulmer/private/coma/mirror_comparison_lg.mov [quicktime]

Also need

http://www.astro.northwestern.edu/~ulmer/private/coma/lens0.mpeg [quicktime]

Clusters come into existence?

Age of Universe about 13.7 Gyr

M

M

hh22

hh22

k[h Mpc k[h Mpc –1–1]]

P(k

) [h

P

(k)

[h –3–

3 Mpc

M

pc 33 ]]

[h Mpc [h Mpc –1–1]]

P(k) Complementary measure crucial; Improves w and dw/dz by ~ factor 4

2.5 arcmin/1.1 Mpc

RCS1325+2858 z=0.95 Smoothed X-ray emission contours

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 4874NGC 4911

10’

280 kpc

Coma Cluster Zoomed

300 kpc

300 kpc

Coma Cluster X-ray residuals

Color-Magnitude Relation

Many of our LSBs fall on the CMR!

=> Same origin and aging as larger galaxies

From R= 18!

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

Blue LSBs

Blue LSBs

Residual from X-rays after isothermal sphere fit subtracted

All LSBs

0.5-2.0 keV X-rays ROSAT, raw data

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

Cl 1205+44 z = 0.6

Cl 11205+44 X-rays and Radio

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

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

Compilation of Lx of Clusters versus z

Chandra Mirror Blank

XMM-newton Area vs energy

XMM-Newton coated mandrel

Resulting XMM-Newton Ni Mirror Au coated on inside

Wolter I X-ray optic design

Chandra X-ray Observatory

CXC

Schematic of Grazing Incidence, X-ray Mirrors

7 keV image made at APS UNIT-CAT

XMM-Newton CCD camera

What a low temp detector (LTD) does for you vs a CCD

CCD Energy resolution LTD Energy Resolution

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!

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.

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