2017A&A...599A.138Z


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.09CEST05:32:59

2017A&A...599A.138Z - Astronomy and Astrophysics, volume 599A, 138-138 (2017/3-1)

HIFLUGCS: X-ray luminosity-dynamical mass relation and its implications for mass calibrations with the SPIDERS and 4MOST surveys.

ZHANG Y.-Y., REIPRICH T.H., SCHNEIDER P., CLERC N., MERLONI A., SCHWOPE A., BORM K., ANDERNACH H., CARETTA C.A. and WU X.-P.

Abstract (from CDS):

We present the relation of X-ray luminosity versus dynamical mass for 63 nearby clusters of galaxies in a flux-limited sample, the HIghest X-ray FLUx Galaxy Cluster Sample (HIFLUGCS, consisting of 64 clusters). The luminosity measurements are obtained based on ∼1.3Ms of clean XMM-Newton data and ROSAT pointed observations. The masses are estimated using optical spectroscopic redshifts of 13647 cluster galaxies in total. We classify clusters into disturbed and undisturbed based on a combination of the X-ray luminosity concentration and the offset between the brightest cluster galaxy and X-ray flux-weighted center. Given sufficient numbers (i.e., ≥45) of member galaxies when the dynamical masses are computed, the luminosity versus mass relations agree between the disturbed and undisturbed clusters. The cool-core clusters still dominate the scatter in the luminosity versus mass relation even when a core-corrected X-ray luminosity is used, which indicates that the scatter of this scaling relation mainly reflects the structure formation history of the clusters. As shown by the clusters with only few spectroscopically confirmed members, the dynamical masses can be underestimated and thus lead to a biased scaling relation. To investigate the potential of spectroscopic surveys to follow up high-redshift galaxy clusters or groups observed in X-ray surveys for the identifications and mass calibrations, we carried out Monte Carlo resampling of the cluster galaxy redshifts and calibrated the uncertainties of the redshift and dynamical mass estimates when only reduced numbers of galaxy redshifts per cluster are available. The resampling considers the SPIDERS and 4MOST configurations, designed for the follow-up of the eROSITA clusters, and was carried out for each cluster in the sample at the actual cluster redshift as well as at the assigned input cluster redshifts of 0.2, 0.4, 0.6, and 0.8. To follow up very distant clusters or groups, we also carried out the mass calibration based on the resampling with only ten redshifts per cluster, and redshift calibration based on the resampling with only five and ten redshifts per cluster, respectively. Our results demonstrate the power of combining upcoming X-ray and optical spectroscopic surveys for mass calibration of clusters. The scatter in the dynamical mass estimates for the clusters with at least ten members is within 50%.

Abstract Copyright: © ESO, 2017

Journal keyword(s): cosmology: observations - methods: data analysis - galaxies: kinematics and dynamics - X-rays: galaxies: clusters - galaxies: clusters: intracluster medium - surveys - surveys

Simbad objects: 66

goto Full paper

goto View the reference in ADS

Number of rows : 66

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 ACO 2 ClG 00 08 27 -19 38.3           ~ 15 1
2 ACO 85 ClG 00 41 37.8 -09 20 33           ~ 790 0
3 ACO 119 ClG 00 56 16.8 -01 15 00           ~ 518 2
4 ACO 133 ClG 01 02 39.0 -21 57 15           ~ 336 1
5 NGC 507 BiC 01 23 39.950 +33 15 22.22   13.0       ~ 395 3
6 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 652 1
7 ACO 400 ClG 02 57 37.4 +06 00 45           ~ 386 3
8 ACO 399 ClG 02 57 56.4 +13 00 59           ~ 347 0
9 ACO 401 ClG 02 58 56.9 +13 34 56           ~ 519 0
10 ACO 3112 ClG 03 17 52.4 -44 14 35           ~ 290 1
11 NGC 1339 GiG 03 28 06.582 -32 17 10.16   12.63   11.18   ~ 152 0
12 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 344 1
13 2MASX J03411752+1523477 BiC 03 41 17.5325964402 +15 23 47.585740854   17.5       ~ 41 1
14 ACO 3158 ClG 03 42 39.6 -53 37 50           ~ 271 0
15 ACO 478 ClG 04 13 20.7 +10 28 35           ~ 467 0
16 NGC 1550 BiC 04 19 37.921 +02 24 35.58   14.0       ~ 151 1
17 ClG 0422-09 ClG 04 25 51.02 -08 33 38.5           ~ 85 0
18 ACO 3266 ClG 04 31 11.9 -61 24 23           ~ 372 0
19 ACO 496 ClG 04 33 30.3838 -13 14 21.584           ~ 661 2
20 ACO 3376 ClG 06 01 42.1521 -39 59 06.227           ~ 271 0
21 ACO 3391 ClG 06 26 15.4 -53 40 52           ~ 170 1
22 [HJ96] A3395S ClG 06 26 46.1 -54 32 43           ~ 4 0
23 ACO 576 ClG 07 21 24.1 +55 44 20           ~ 284 1
24 ACO 754 ClG 09 08 50.1 -09 38 12           ~ 631 1
25 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 909 1
26 ACO 780 ClG 09 18 30 -12 15.7           ~ 430 0
27 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 774 1
28 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 995 1
29 NAME NGC 4073 Group GrG 12 04 21.7 +01 50 19     13.53     ~ 245 0
30 ZwCl 1215+0400 ClG 12 17 40.6 +03 39 45           ~ 105 0
31 NGC 4636 LIN 12 42 49.867 +02 41 16.01   12.62 11.84     ~ 1041 1
32 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 973 2
33 ACO 1644 ClG 12 57 11.6 -17 24 34           ~ 335 1
34 ACO 1650 ClG 12 58 36.76 -01 43 34.2           ~ 271 0
35 ACO 1651 ClG 12 59 22.43 -04 11 47.1           ~ 274 0
36 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4223 2
37 NGC 5044 BiC 13 15 23.969 -16 23 08.00   11.9   10.74   ~ 452 0
38 ACO 1736 ClG 13 26 52.1 -27 06 33           ~ 238 2
39 ACO 3558 ClG 13 27 54.8 -31 29 32           ~ 407 2
40 ACO 3562 ClG 13 33 31.8 -31 40 23           ~ 284 1
41 ACO 3571 ClG 13 47 28.9 -32 51 57           ~ 265 2
42 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1156 0
43 ACO 3581 ClG 14 07 29.8 -27 01 04           ~ 165 3
44 NAME NGC 5718 Group ClG 14 40 38.5 +03 28 20     14.31     ~ 105 0
45 2MASX J15040752-0248161 Sy1 15 04 07.519415 -02 48 16.65402   18.53 18.08     ~ 45 1
46 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 855 0
47 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 676 1
48 NAME NGC 5920 Group ClG 15 21 50.7 +07 42 18     15.13     ~ 288 0
49 ACO 2065 ClG 15 22 42.6 +27 43 21           ~ 344 0
50 ACO 2063 ClG 15 23 01.8 +08 38 22           ~ 371 2
51 ACO 2142 ClG 15 58 20.00 +27 14 00.3           ~ 673 0
52 ACO 2147 ClG 16 02 17.2 +15 53 43           ~ 375 0
53 ACO 2163 ClG 16 15 34.1 -06 07 26           ~ 520 0
54 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1102 1
55 ACO 2204 ClG 16 32 45.7 +05 34 43           ~ 398 0
56 ACO 2244 ClG 17 02 34.01 +34 04 41.1           ~ 247 0
57 ACO 2256 ClG 17 03 43.5 +78 43 03           ~ 830 1
58 ACO 2255 ClG 17 12 50.04 +64 03 10.6           ~ 503 0
59 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 567 1
60 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 233 1
61 ACO 2589 ClG 23 24 00.5 +16 49 29           ~ 297 1
62 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 493 0
63 ACO 2634 ClG 23 38 18.4 +27 01 37           ~ 480 2
64 ACO 2657 ClG 23 44 51.0 +09 08 40           ~ 261 3
65 ACO 4038 ClG 23 47 31.1 -28 12 10           ~ 314 3
66 ACO 4059 ClG 23 56 40.7 -34 40 18           ~ 352 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2017A&A...599A.138Z and select 'bookmark this link' or equivalent in the popup menu


2020.08.09-05:32:59

© Université de Strasbourg/CNRS

    • Contact