Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:1209.2492)
· On-line Data
· References in the article
· Citations to the Article (2) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The three-dimensional geometry and merger history of the massive galaxy cluster MACS J0358.8-2955
Authors:
Hsu, Li-Yen; Ebeling, Harald; Richard, Johan
Affiliation:
AA(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA; ), AB(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA), AC(Centre de Recherche Astrophysique de Lyon, Université Lyon 1, 9 Avenue Charles André, F-69561 Saint Genis Laval Cedex, France)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 429, Issue 1, p.833-848 (MNRAS Homepage)
Publication Date:
02/2013
Origin:
OUP
Astronomy Keywords:
galaxies: clusters: individual: MACS J0358.8-2955
Abstract Copyright:
2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/sts379
Bibliographic Code:
2013MNRAS.429..833H

Abstract

We present results of a combined X-ray/optical analysis of the dynamics of the massive cluster MACS J0358.8-2955 (z = 0.428) based on observations with the Chandra X-ray Observatory, the Hubble Space Telescope and the Keck-I telescope on Mauna Kea. MACS J0358.8-2955 is found to be one of the most X-ray luminous clusters known at z > 0.3, featuring LX, bol( < r500) = 4.24 × 1045 erg s-1, kT = 9.55+ 0.58- 0.37 keV, M3Dgas( < r500) = (9.18 ± 1.45) × 1013 M&sun; and M3Dtot( < r500) = (1.12 ± 0.18) × 1015 M&sun;. The system's high velocity dispersion of 1440+ 130- 110 km s- 1 (890 km s-1 when the correct relativistic equation is used), however, is inflated by infall along the line of sight, as the result of a complex merger of at least three subclusters. One collision proceeds close to head-on, while the second features a significant impact parameter. The temperature variations in the intracluster gas, two tentative cold fronts, the radial velocities measured for cluster galaxies and the small offsets between collisional and non-collisional cluster components all suggest that both merger events are observed close to core passage and along the axes that are greatly inclined with respect to the plane of the sky. A strong-lensing analysis of the system anchored upon three triple-image systems (two of which have spectroscopic redshifts) yields independent constraints on the mass distribution. For a gas fraction of 8.2 per cent, the resulting strong-lensing mass profile is in good agreement with our X-ray estimates, and the details of the mass distribution are fully consistent with our interpretation of the 3D merger history of this complex system.

Underlining yet again the power of X-ray selection, our analysis also resolves earlier confusion about the contribution of the partly superimposed foreground cluster A 3192 (z = 0.168). Based on very faint X-ray emission detected by our Chandra observation and 16 concordant redshifts we identify A 3192 as two groups of galaxies, separated by 700 kpc in the plane of the sky. The X-ray luminosity and mass of the two components of A 3192 combined are <0.5 per cent and <8 per cent of that of MACS J0358.8-2955.


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints