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Cluster: MS 0906.5+1110
ObsID: 924

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Cluster Core Image Cooling Time Profile Density Profile
Entropy Profile Gravitating Mass Profile Light Curve
Metal abundance profile Pressure Profile SDSS/DSS Image
Spectral Analysis Surface Brightness Profile Temperature Profile
Wide-Field Image

Col. (1) Exposure time; col. (2) right ascension of cluster center; col. (3) declination of cluster center; col. (4) Galactic absorbing column density, NH; col. (5) redshift; col. (6) maximum radius from cluster center, Rmax; col. (7) minimum counts used per TX annulus; col. (8) average cluster temperature; col. (9) average cluster metal abundance; and col. (10) bolometric luminosity;
Exp
Time		 R.A. Decl. NH z Rmax Min. cts. TX Abund. Lbol
ksec hr:min:sec deg:min:sec 1020 cm-2 --- pixels counts keV Solar 1044 ergs/s
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
29.7 09:09:12.753 +10:58:32.00 3.60 0.1630 585 5000 8.10 0.30 4.690

Click here to download a master table of profiles for this cluster.
All images generated using SAOImage DS9, developed by the Smithsonian Astrophysical Observatory.

Smoothed and binnd wide-field Chandra X-ray image of cluster
924 MS 0906.5+1110
A gaussian smoothing kernel with size 2 was applied to the flare-cleaned, level-2 events file binned with a factor of 8 to produce this image. Point sources have not been excluded and no exposure correction has been applied to this image.

Smoothed and binned Chandra X-ray image of the cluster "core"
924 MS 0906.5+1110
Same as the wide-field image above but the binning factor used here was 2.

SDSS/DSS footprint overlaid on cluster core
924 MS 0906.5+1110
The SDSS/DSS footprint (white box) is centered on the cluster core.

Sloan Digital Sky Survey (SDSS) image of cluster core
924 MS 0906.5+1110
Image taken from Sloan Digital Sky Survey (SDSS)

Background light curve
924 light curve
To check for contamination from background flares or periods of excessively high background, light curve analysis was performed using Maxim Markevitch's contributed CIAO script lc_clean.sl. Periods with count rates >= 3sigma and/or a factor >= 1.2 of the mean background level of the observation were removed from the GTI file.

Surface brightness profile
924 surface brightness profile
We began by extracting surface brightness profiles from the 0.7-2.0 keV energy range using concentric annular bins of size 5" (~10 ACIS pixels) originating from the X-ray center. To remove the effects of vignetting and exposure time fluctuations we corrected each surface brightness profile by an observation specific normalized radial exposure profile.

Annuli used for generating temperature profile
924 temperature bins
Each annulus is centered at RA: 09:09:12.753, Decl: +10:58:32.00 and contains 5000 counts. Links to an image of each spectrum and the corresponding best-fit MeKaL model (solid-line) are provided below the image.

Links to images of spectra
Annulus 1 Annulus 2 Annulus 3 Annulus 4 Annulus 5

Temperature profile
924 temperature profile
The temperature profile corresponding to the image and annuli shown above. Uncertainties are 90% confidence.

Metal abundance profile
924 abundance profile
The abundance profile corresponding to the image and annuli shown above. Uncertainties are 90% confidence.

Density profile
924 density profile
Electron gas density profile derived from deprojecting the surface brightness with spectral information.

Pressure profile
924 pressure profile
Electron gas pressure profile derived from the density and temperature profiles.

Entropy profile
924 entropy profile
Entropy profile derived from density and temperature as K=Tne-2/3. The dashed line is the best-fit for the model K(r) = K0+K100(r/100 kpc)α with fit values:
K0 = 104.23 ± 14.89 keV cm2
K100 = 97.32 ± 19.55 keV cm2
α = 1.15 ± 0.17.
The dashed-dotted line is the best-fit for the model K=K100(r/100 kpc)α.

Conduction suppresion profile
924 fc profile
Conduction suppression factor, fc profile derived from the entropy profile assuming Spitzer conduction.

Cooling time profile
924 cooling profile
Gas cooling time profile using the formulation tcool=(3/2 nkT)/(nenpΛ(T,Z)) for isochoric cooling. The dashed horizontal line represents the age of the Universe at the redshift of the cluster.

Gravitating mass profile
924 grav mass profile
Gravitating mass profile derived from assuming hydrostatic equilibrium and differentiating the log-space electron density profile with a piecewise method. The d(ln T)/dr term has been assumed to be negligible (a terrible assumption). **CAUTION** THIS WAS NOT THE FOCUS OF OUR WORK, USE AT YOUR OWN RISK!

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