Rapture of the Deep Sky
description
Transcript of Rapture of the Deep Sky
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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]
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Clusters come into existence?
Age of Universe about 13.7 Gyr
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M
M
hh22
hh22
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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
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2.5 arcmin/1.1 Mpc
RCS1325+2858 z=0.95 Smoothed X-ray emission contours
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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
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Coma Cluster Zoomed
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300 kpc
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300 kpc
Coma Cluster X-ray residuals
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Color-Magnitude Relation
Many of our LSBs fall on the CMR!
=> Same origin and aging as larger galaxies
From R= 18!
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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
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Blue LSBs
Blue LSBs
Residual from X-rays after isothermal sphere fit subtracted
All LSBs
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0.5-2.0 keV X-rays ROSAT, raw data
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0.5-2.0 keV X-rays ROSAT, wavelet filter processed
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Cl 1205+44 z = 0.6
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Cl 11205+44 X-rays and Radio
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Cl 1257+47 z = 0.9 color visible + near IR
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Cl 1257+47 left color, visble=> near IR; right X-ray plus near IR
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Compilation of Lx of Clusters versus z
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Chandra Mirror Blank
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XMM-newton Area vs energy
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XMM-Newton coated mandrel
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Resulting XMM-Newton Ni Mirror Au coated on inside
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Wolter I X-ray optic design
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Chandra X-ray Observatory
CXC
Schematic of Grazing Incidence, X-ray Mirrors
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7 keV image made at APS UNIT-CAT
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XMM-Newton CCD camera
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What a low temp detector (LTD) does for you vs a CCD
CCD Energy resolution LTD Energy Resolution
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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!
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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.
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Hero Dr. Mel: Untouched comic strip. Reminds us we live on 4-D surface in 5-D manifold