2012ApJ...755..116L

Query : 2012ApJ...755..116L

2012ApJ...755..116L - Astrophys. J., 755, 116 (2012/August-3)

Constraining cluster physics with the shape of X-ray clusters: comparison of local X-ray clusters versus ΛCDM clusters.

LAU E.T., NAGAI D., KRAVTSOV A.V., VIKHLININ A. and ZENTNER A.R.

Abstract (from CDS):

Recent simulations of cluster formation have demonstrated that condensation of baryons into central galaxies during cluster formation can drive the shape of the gas distribution in galaxy clusters significantly rounder out to their virial radius. These simulations generally predict stellar fractions within cluster virial radii that are ∼2-3 times larger than the stellar masses deduced from observations. In this paper, we compare ellipticity profiles of simulated clusters performed with varying input physics (radiative cooling, star formation, and supernova feedback) to the cluster ellipticity profiles derived from Chandra and ROSAT observations, in an effort to constrain the fraction of gas that cools and condenses into the central galaxies within clusters. We find that local relaxed clusters have an average ellipticity of ε radii r > 0.1r500, the observed ellipticity profiles agree well with the predictions of non-radiative simulations. In contrast, the ellipticity profiles of simulated clusters that include dissipative gas physics deviate significantly from the observed ellipticity profiles at all radii. The dissipative simulations overpredict (underpredict) ellipticity in the inner (outer) regions of galaxy clusters. By comparing simulations with and without dissipative gas physics, we show that gas cooling causes the gas distribution to be more oblate in the central regions, but makes the outer gas distribution more spherical. We find that late-time gas cooling and star formation are responsible for the significantly oblate gas distributions in cluster cores, but the gas shapes outside of cluster cores are set primarily by baryon dissipation at high redshift (z ≥ 2). Our results indicate that the shapes of X-ray emitting gas in galaxy clusters, especially at large radii, can be used to place constraints on cluster gas physics, making it potential probes of the history of baryonic cooling in galaxy clusters.

Abstract Copyright: ∼

Journal keyword(s): galaxies: clusters: general - X-rays: galaxies: clusters

Simbad objects: 45

goto Full paper

goto View the references in ADS

Number of rows : 45
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 ACO 85 ClG 00 41 36.21 -09 19 30.4           ~ 909 0
2 ACO 119 ClG 00 56 08.57 -01 12 00.8           ~ 555 2
3 ACO 133 ClG 01 02 41.5 -21 52 53           ~ 368 1
4 ACO 399 ClG 02 57 56.4 +13 00 59           ~ 396 0
5 ACO 401 ClG 02 58 56.9 +13 34 56           ~ 566 0
6 ACO 3112 ClG 03 17 52.4 -44 14 35           ~ 311 1
7 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 383 1
8 ACO 3158 ClG 03 42 39.6 -53 37 50           ~ 304 0
9 ClG 0422-09 ClG 04 25 51.02 -08 33 38.5           ~ 91 0
10 ACO 3266 ClG 04 31 11.9 -61 24 23           ~ 410 0
11 ACO 496 ClG 04 33 38.8 -13 15 59           ~ 694 2
12 ACO 3376 ClG 06 01 25.000 -39 59 51.00           ~ 305 0
13 ACO 3391 ClG 06 26 15.4 -53 40 52           ~ 202 1
14 ACO 3395 ClG 06 27 31.1 -54 23 58           ~ 209 0
15 ACO 576 ClG 07 21 24.1 +55 44 20           ~ 297 1
16 NAME Hya A LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 1011 1
17 ZwCl 1215+0400 ClG 12 17 43.62 +03 38 51.5           ~ 153 0
18 ACO 1644 ClG 12 57 11.6 -17 24 34           ~ 366 1
19 ACO 1650 ClG 12 58 42.0 -01 45 45           ~ 304 0
20 ACO 1651 ClG 12 59 22.43 -04 11 47.1           ~ 290 0
21 ACO 1736 ClG 13 26 52.1 -27 06 33           ~ 249 2
22 ACO 3558 ClG 13 27 54.8 -31 29 32           ~ 442 2
23 ACO 3562 ClG 13 33 31.8 -31 40 23           ~ 314 1
24 ACO 3571 ClG 13 47 28.9 -32 51 57           ~ 284 2
25 ClG J1504-0248 ClG 15 04 07.4 -02 48 15           ~ 175 0
26 ACO 2052 ClG 15 16 41.64 +07 01 45.5           ~ 730 1
27 ACT-CL J1521.8+0742 ClG 15 21 55.14 +07 41 27.2     15.13     ~ 311 0
28 ACO 2065 ClG 15 22 29.3 +27 42 22           ~ 374 0
29 ACO 2063 ClG 15 23 01.8 +08 38 22           ~ 397 2
30 ACO 2142 ClG 15 58 14.38 +27 12 57.8           ~ 768 0
31 ACO 2147 ClG 16 02 11.96 +15 55 11.5           ~ 403 0
32 ACO 2151 ClG 16 05 15.0 +17 44 55           ~ 578 3
33 ACO 2163 ClG 16 15 46.1 -06 08 50           ~ 562 0
34 ACO 2199 ClG 16 28 43.31 +39 34 07.6           ~ 1171 1
35 ACO 2204 ClG 16 32 45.7 +05 34 43           ~ 436 0
36 ACO 2244 ClG 17 02 40.33 +34 02 58.7           ~ 281 0
37 ACO 2256 ClG 17 03 09.4 +78 39 36           ~ 885 1
38 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 627 1
39 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 258 1
40 ACO 2589 ClG 23 24 00.5 +16 49 29           ~ 316 1
41 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 539 0
42 ACO 2634 ClG 23 38 18.4 +27 01 37           ~ 503 2
43 ACO 2657 ClG 23 44 51.0 +09 08 40           ~ 269 3
44 ACO 4038 ClG 23 47 31.1 -28 12 10           ~ 335 3
45 ACO 4059 ClG 23 57 02.2 -34 45 58           ~ 380 1

To bookmark this query, right click on this link: simbad:objects in 2012ApJ...755..116L and select 'bookmark this link' or equivalent in the popup menu