2015MNRAS.453....2L

Query : 2015MNRAS.453....2L

2015MNRAS.453....2L - Mon. Not. R. Astron. Soc., 453, 2-13 (2015/October-2)

Non-virialized clusters for detection of dark energy-dark matter interaction.

LE DELLIOU M., MARCONDES R.J.F., LIMA NETO G.B. and ABDALLA E.

Abstract (from CDS):

The observation of galaxy and gas distributions, as well as cosmological simulations in a ΛCDM cold dark matter universe, suggests that clusters of galaxies are still accreting mass and are not expected to be in equilibrium. In this work, we investigate the possibility to evaluate the departure from virial equilibrium in order to detect, in that balance, effects from a dark matter-dark energy interaction. We continue, from previous works, using a simple model of interacting dark sector, the Layzer-Irvine equation for dynamical virial evolution, and employ optical observations in order to obtain the mass profiles through weak-lensing and X-ray observations giving the intracluster gas temperatures. Through a Monte Carlo method, we generate, for a set of clusters, measurements of observed virial ratios, interaction strength, rest virial ratio and departure from equilibrium factors. We found a compounded interaction strength of -1.99^+2.56_-16.00, compatible with no interaction, but also a compounded rest virial ratio of -0.79±0.13, which would entail a 2σ detection. We confirm quantitatively that clusters of galaxies are out of equilibrium but further investigation is needed to constrain a possible interaction in the dark sector.

Abstract Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2015)

Journal keyword(s): Gravitation - Galaxies: clusters: general - Cosmology: theory - dark energy - dark matter - large-scale structure of Universe - X-rays: galaxies: clusters

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 ACO 68 ClG 00 37 06.2 +09 09 33           ~ 195 0
2 ACO 115 ClG 00 55 59 +26 23.2           ~ 295 1
3 ACO 209 ClG 01 31 52.9 -13 36 53           ~ 326 0
4 ACO 267 ClG 01 52 43.016 +00 59 58.90           ~ 241 0
5 ACO 383 ClG 02 48 03.3915 -03 31 45.228           ~ 389 0
6 ACO 521 ClG 04 54 08.6 -10 14 39           ~ 279 0
7 ACO 520 ClG 04 54 10.1 +02 55 38           ~ 465 0
8 ACO 586 ClG 07 32 20.3 +31 37 58           ~ 196 0
9 ACO 611 ClG 08 00 58.7 +36 02 49           ~ 275 0
10 ACO 697 ClG 08 42 57.6 +36 21 45           ~ 277 0
11 ACO 963 ClG 10 17 03.4 +39 02 56           ~ 414 0
12 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1178 0
13 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 727 1
14 ACO 1914 ClG 14 25 57.4 +37 49 54           ~ 338 0
15 ZwCl 1455+2232 ClG 14 57 15.2 +22 20 30     18.62 20.04   ~ 309 0
16 ZwCl 1459+4240 ClG 15 01 23.0 +42 20 47           ~ 61 0
17 ACO 2034 ClG 15 10 03.9 +33 30 57           ~ 248 1
18 ACO 2219 ClG 16 40 22.1 +46 42 20           ~ 381 0
19 ClG J1720+2638 ClG 17 20 09.6 +26 37 35           ~ 284 0
20 ACO 2261 ClG 17 22 26.9 +32 07 58           ~ 370 0
21 ClG J2129+0005 ClG 21 29 40.5 +00 05 47           ~ 308 0
22 ACO 2390 ClG 21 53 37.4 +17 41 46           ~ 732 2
23 ACO 2631 ClG 23 37 40.7 +00 16 35           ~ 183 0

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