<i>Chandra</i>X‐Ray Analysis of the Massive High‐Redshift Galaxy Clusters Cl J1113.1−2615 and Cl J0152.7−1357

Maughan, Ben; Jones, Laura; Ebeling, H.; Perlman, E.; Rosati, P.; Frye, Christopher; Mullis, C. R.

doi:10.1086/368151

Cited by 73 publications

(150 citation statements)

References 38 publications

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“…Also, the metallicity is well constrained at a relatively high value, Z ¼ 0:40 AE 0:18 Z . Our results are consistent, within the errors, with the analysis of Maughan et al (2003). A8.…”

Section: A7 Rx J11131à2615supporting

confidence: 91%

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Iron Abundance in the Intracluster Medium at High Redshift

Tozzi

Rosati

Ettori

et al. 2003

ApJ

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We present the analysis of the X-ray spectra of 18 distant clusters of galaxies with redshift 0:3 < z < 1:3. Most of them were observed with the Chandra satellite in long exposures ranging from 36 to 180 ks. For two of the z > 1 clusters, we also use deep XMM-Newton observations. Overall, these clusters probe the temperature range 3 keVdkTd8 keV. Our analysis is aimed at deriving the iron abundance in the intracluster medium (ICM) out to the highest redshifts probed to date. Using a combined spectral fit of cluster subsamples in different redshift bins, we investigate the evolution of the mean ICM metallicity with cosmic epoch. We find that the mean Fe abundance at z h i ¼ 0:8 is Z ¼ 0:25 þ0:04 À0:06 Z , consistent with the local canonical metallicity value, Z ' 0:3 Z , within the 1 confidence level (c.l.). Medium-and low-temperature clusters (kT < 5 keV) tend to have larger iron abundances than hot clusters. At redshift z h i $ 1:2 (four clusters at z > 1), we obtain a statistically significant detection of the Fe K line in only one cluster (Z > 0:10 Z at the 90% c.l.). Combining all the current data sets from Chandra and XMM at z > 1, the average metallicity is measured to be Z h i ¼ 0:21 þ0:10 À0:05 Z (1 error), thus suggesting no evolution of the mean iron abundance out to z ' 1:2.

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“…Also, the metallicity is well constrained at a relatively high value, Z ¼ 0:40 AE 0:18 Z . Our results are consistent, within the errors, with the analysis of Maughan et al (2003). A8.…”

Section: A7 Rx J11131à2615supporting

confidence: 91%

“…This cluster was discovered in the Wide Angle ROSAT Pointed X-Ray Survey (WARPS; Perlman et al 2002;Maughan et al 2003). We detected $1200 net counts in the 0.3-10 keV band from a 39>4 radius circular region.…”

Section: A7 Rx J11131à2615mentioning

confidence: 83%

Iron Abundance in the Intracluster Medium at High Redshift

Tozzi

Rosati

Ettori

et al. 2003

ApJ

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121

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“…Otherwise, there is no obvious additional evolution of the normalization of the M−T relation after the redshift evolution correction. This was also found for the other distant clusters in Maughan et al (2003) and Ettori et al (2003). As shown in Fig.…”

Section: Scaling Relationssupporting

confidence: 79%

X-ray properties in massive galaxy clusters: XMM-Newton observations of the REFLEX-DXL sample

Zhang

Böhringer

Finoguenov

et al. 2006

A&A

100

171

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We selected an unbiased, flux-limited and almost volume-complete sample of 13 distant, X-ray luminous (DXL, z ∼ 0.3) clusters and one supplementary cluster at z = 0.2578 from the REFLEX Survey (the REFLEX-DXL sample). We performed a detailed study to explore their X-ray properties using XMM-Newton observations. Based on the precise radial distributions of the gas density and temperature, we obtained robust cluster masses and gas mass fractions. The average gas mass fraction of the REFLEX-DXL sample at r 500 , 0.116 ± 0.007, agrees with the previous cluster studies and the WMAP baryon fraction measurement. The scaled profiles of the surface brightness, temperature, entropy, gas mass and total mass are characterized by a self-similar behaviour at radii above 0.2−0.3 r 500 . The REFLEX-DXL sample confirms the previous studies of the normalization of the scaling relations (L−T , L−M, M−T and M gas −T ) when the redshift evolution of the scaling relations is accounted for. We investigated the scatter of the scaling relations of the REFLEX-DXL sample. This gives the correlative scatter of (0.20, 0.10) for variable of (M, T ) of the M 500 −T relation, for example.

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“…RX J0152.7À1357 was found independently by a number of X-ray surveys, and its properties have been studied with the Röntgensatellit (ROSAT ), BeppoSAX, XMM-Newton, and Chandra (Ebeling et al 2000;Della Ceca et al 2000;Maughan et al 2003). It exhibits a complex X-ray morphology, including two main components with temperatures of 6:7 þ1:2 À1:0 and 8:7 þ2:4 À1:8 keV (I.…”

Section: Introductionmentioning

confidence: 99%

Clusters at Half Hubble Time: Galaxy Structure and Colors in RX J0152.7−1357 and MS 1054−03

Blakeslee

Holden

Franx

et al. 2006

ApJ

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We study the photometric and structural properties of spectroscopically confirmed members in the two massive X-ray-selected z % 0:83 galaxy clusters MS 1054-03 and RX J0152.7À1357 using three-band mosaic imaging with the Hubble Space Telescope Advanced Camera for Surveys. The samples include 105 and 140 members of RX J0152.7À1357 and MS 1054-03, respectively, to i 775 < 24:0. A quantitative classification scheme using Sérsic indices and ''bumpiness'' (the ratio of the rms residuals to the model mean) was found to correlate well with visual morphological type. The color-magnitude residuals correlate well with the local density, as measured from both galaxy numbers and weak lensing. Weaker correlations are found with cluster radius (the fundamental dependence is on local density). We identify a threshold surface mass density of AE % 0:1, in units of the critical density, above which there are relatively few blue (star-forming) galaxies. In RX J0152.7À1357, there is an offset of 0:006 AE 0:002 in the mean redshifts of the early-and late-type galaxies, possibly from an infalling foreground association of late-type galaxies. A range of star-formation time-scales are needed to reproduce the galaxy loci in the color-color diagrams. We find rest-frame scatters for the ellipticals of 0:03 AE 0:01 mag in U À B and 0:07 AE 0:01 mag in U À V . The mean colors and their scatters imply ages $3.5 Gyr, or formation at z % 2:2. Thus, when the universe was half its present age, cluster ellipticals were about half the age of the universe; the same is coincidentally true of the median ages of ellipticals today. However, the most massive local ellipticals have ages k10 Gyr, consistent with our results for their likely progenitors at z k 0:8.

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ChandraX‐Ray Analysis of the Massive High‐Redshift Galaxy Clusters Cl J1113.1−2615 and Cl J0152.7−1357

Cited by 73 publications

References 38 publications

Iron Abundance in the Intracluster Medium at High Redshift

Iron Abundance in the Intracluster Medium at High Redshift

X-ray properties in massive galaxy clusters: XMM-Newton observations of the REFLEX-DXL sample

Clusters at Half Hubble Time: Galaxy Structure and Colors in RX J0152.7−1357 and MS 1054−03

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