2011A&A...529A..65Y


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.16CET03:51:53

2011A&A...529A..65Y - Astronomy and Astrophysics, volume 529A, 65-65 (2011/5-1)

Measuring redshifts using X-ray spectroscopy of galaxy clusters: results from Chandra data and future prospects.

YU H., TOZZI P., BORGANI S., ROSATI P. and ZHU Z.-H.

Abstract (from CDS):

The ubiquitous presence of the Fe line complex in the X-ray spectra of galaxy clusters offers the possibility of measuring their redshift without resorting to spectroscopic follow-up observations. In practice, the blind search of the Fe line in X-ray spectra is a difficult task and is affected not only by limited S/N (particularly at high redshift), but also by several systematic errors, associated with varying Fe abundance values, ICM temperature gradients, and instrumental characteristics. We assess the accuracy with which the redshift of galaxy clusters can be recovered from an X-ray spectral analysis of Chandra archival data. We present a strategy to compile large surveys of clusters whose identification and redshift measurement are both based on X-ray data alone. We apply a blind search for K-shell and L-shell Fe line complexes in X-ray cluster spectra using Chandra archival observations of galaxy clusters. The Fe line can be detected in the ICM spectra by simply analyzing the C-statistics variation Δ Cstat as a function of the redshift parameter, when all the other model parameters are frozen to the best-fit values. We repeat the measurement under different conditions, and compare the X-ray derived redshift zX with the one obtained by means of optical spectroscopy zo. We explore how a number of priors on metallicity and luminosity can be effectively used to reduce catastrophic errors. The ΔCstat provides the most effective means of discarding wrong redshift measurements and estimating the actual error in zX. We identify a simple and efficient procedure for optimally measuring the redshifts from the X-ray spectral analysis of clusters of galaxies. When this procedure is applied to mock catalogs extracted from high sensitivity, wide-area cluster surveys, such as those proposed with Wide Field X-ray Telescope (WFXT) mission, it is possible to obtain complete samples of X-ray clusters with reliable redshift measurements, thus avoiding time-consuming optical spectroscopic observations. Our analysis shows that, in the case of WFXT, a blind Fe line search is 95% successful for spectra with more than 1000 net counts, whenever ΔCstat>9, corresponding formally to a 3σ confidence level. The average error in the redshift zX decreases rapidly for higher values of Δ Cstat. Finally, we discuss how to estimate the completeness of a large cluster samples with measured zX. This methodology will make it possible to trace cosmic growth by studying the evolution of the cluster mass function directly using X-ray data.

Abstract Copyright:

Journal keyword(s): X-rays: galaxies: clusters - galaxies: clusters: general - techniques: spectroscopic - galaxies: high-redshift - cosmology: observations - galaxies: clusters: intracluster medium

Simbad objects: 46

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Number of rows : 46

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 ClG 0016+16 ClG 00 18 33.3 +16 26 36           ~ 468 0
2 ZwCl 0024+1652 ClG 00 26 36.0 +17 08 36     18.35     ~ 597 1
3 2MASX J00274579+2616264 ClG 00 27 45.90 +26 16 25.0           ~ 32 0
4 PSZ2 G167.66-65.59 ClG 01 59 49.4 -08 50 00           ~ 59 0
5 ClG 0303+1658 ClG 03 05 31.6 +17 10 02     20.13     ~ 89 0
6 1RXS J040438.5+110921 ClG 04 04 37.4 +11 09 57           ~ 27 0
7 RXC J0417.5-1154 ClG 04 17 34.6 -11 54 32           ~ 54 0
8 ClG J0542-4100 ClG 05 42 49.9 -40 59 58           ~ 51 0
9 ClG J0647+7015 ClG 06 47 50.0 +70 14 55           ~ 121 0
10 ClG 0657-56 ClG 06 58 29.6 -55 56 39           ~ 777 1
11 ClG J0744+3927 ClG 07 44 52.5 +39 27 30           ~ 152 0
12 ClG J0849+4452 ClG 08 48 56.3 +44 52 16           ~ 101 1
13 [SHR2002] 23 GiC 09 10 48.3 +54 22 30           ~ 6 0
14 ClG J0956+4107 ClG 09 56 03.4 +41 07 14           ~ 38 0
15 ACO 907 ClG 09 58 21.84 -11 03 47.5           ~ 111 0
16 ClG 1008-12 ClG 10 10 34.1 -12 39 48     18.0     ~ 141 0
17 ClG 1054-03 ClG 10 57 00.2 -03 37 27     22     ~ 448 0
18 ClG J1113-2615 ClG 11 13 05.7 -26 15 36           ~ 33 0
19 SC 1120-12.0 ClG 11 20.0 -12 02           ~ 3 0
20 ClG 1137+66 ClG 11 40 23.3 +66 09 01     21.0     ~ 134 0
21 MCS J1149.5+2223 ClG 11 49 35.8 +22 23 55           ~ 291 0
22 MCS J1206.2-0847 ClG 12 06 12.2 -08 48 02           ~ 169 0
23 ClG J1221+4918 ClG 12 21 25.0 +49 18 07           ~ 54 0
24 ClG J1226+3332 ClG 12 26 57.7 +33 32 50           ~ 190 0
25 ClG J1252-2927 ClG 12 52 54.4 -29 27 17           ~ 150 0
26 ClG J1311-0311 ClG 13 11 01.7 -03 10 38           ~ 82 0
27 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1003 0
28 ClG J1317+2911 ClG 13 17 21.70 +29 11 18.1           ~ 30 0
29 ClG J1350+6007 ClG 13 50 48.55 +60 07 06.7           ~ 40 0
30 ZwCl 1358+6245 ClG 13 59 54.3 +62 30 36     18.5     ~ 346 0
31 ClG J1415+3611 ClG 14 15 11.1 +36 12 03           ~ 67 1
32 ClG J1416+4446 ClG 14 16 28.1 +44 46 38           ~ 41 0
33 ClG J1423+2404 ClG 14 23 47.7 +24 04 40           ~ 167 0
34 ACO 1995 ClG 14 52 55.0 +58 02 59           ~ 117 0
35 ClG J1524+0957 ClG 15 24 40.3 +09 57 35           ~ 55 0
36 ClG J1641+4001 ClG 16 41 52.3 +40 01 29           ~ 36 0
37 ClG J1701+6414 ClG 17 01 22.6 +64 14 09           ~ 63 0
38 ClG J1716+6708 ClG 17 16 49.6 +67 08 30           ~ 112 0
39 ClG J1720+3536 ClG 17 20 16.8 +35 36 27           ~ 105 1
40 1RXS J182418.7+430954 ClG 18 24 19.0 +43 09 49           ~ 20 0
41 ClG 2053-04 ClG 20 56 21.2 -04 37 46   21.0       ~ 160 0
42 ClG J2129-0741 ClG 21 29 26.0 -07 41 28           ~ 122 0
43 ClG 2137-2353 ClG 21 40 12.8 -23 39 27     18.5     ~ 337 0
44 1RXS J222834.4+203647 ClG 22 28 37.1 +20 36 31           ~ 98 0
45 ClG J2235-2557 ClG 22 35 20.6 -25 57 42           ~ 135 0
46 ClG J2302+0844 ClG 23 02 48.1 +08 43 50           ~ 39 0

    Equat.    Gal    SGal    Ecl

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2019.11.16-03:51:53

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