Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321
We observed MS 1054-0321, the highest redshift cluster of galaxies in the Einstein Medium Sensitivity Survey (EMSS), with the Chandra ACIS-S detector. We find the X-ray temperature of the cluster to be 10.4 [+1.7 over -1.5] keV, lower than, but statistically consistent with, the temperature inferred...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | en_US |
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IOP Publishing
2013
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| Online Access: | http://hdl.handle.net/1721.1/76611 https://orcid.org/0000-0002-1379-4482 https://orcid.org/0000-0002-5769-8441 |
| _version_ | 1826203369820127232 |
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| author | Jeltema, Tesla E. Canizares, Claude R. Malm, Michael R. Donahue, Megan Garmire, Gordon P. Bautz, Marshall W. |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Jeltema, Tesla E. Canizares, Claude R. Malm, Michael R. Donahue, Megan Garmire, Gordon P. Bautz, Marshall W. |
| author_sort | Jeltema, Tesla E. |
| collection | MIT |
| description | We observed MS 1054-0321, the highest redshift cluster of galaxies in the Einstein Medium Sensitivity Survey (EMSS), with the Chandra ACIS-S detector. We find the X-ray temperature of the cluster to be 10.4 [+1.7 over -1.5] keV, lower than, but statistically consistent with, the temperature inferred previously. This temperature agrees well with the observed velocity dispersion and that found from weak lensing. We are also able to make the first positive identification of an iron line in this cluster and find a value of 0.26 ± 0.15 for the abundance relative to solar, consistent with early enrichment of the ICM. We confirm significant substructure in the form of two distinct clumps in the X-ray distribution. The eastern clump seems to coincide with the main cluster component. It has a temperature of 10.5[+3.4 over 2.1] keV, approximately the same as the average spectral temperature for the whole cluster. The western clump is cooler, with a temperature of 6.7[+1.7 over -1.2], and may be a subgroup falling into the cluster. Though the presence of substructure indicates that this cluster is not fully relaxed, cluster simulations suggest that we will underestimate the mass, and we can, therefore, use the mass to constrain Ωm. From the overall cluster X-ray temperature we find the virial mass of the cluster to be at least 4.5 × 10[superscript 14] h[superscript -1] M[subscript ☉]. We revisit the cosmological implications of the existence of such a hot, massive cluster at a relatively early epoch. Despite the lower temperature, we still find that the existence of this cluster constrains Ω[subscript m] to be less than one. If Ω[subscript m] = 1 and assuming Gaussian initial perturbations, we find the probability of observing MS 1054 in the EMSS is ~7 × 10[superscript -4]. |
| first_indexed | 2024-09-23T12:35:49Z |
| format | Article |
| id | mit-1721.1/76611 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T12:35:49Z |
| publishDate | 2013 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/766112022-10-01T09:57:53Z Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321 Jeltema, Tesla E. Canizares, Claude R. Malm, Michael R. Donahue, Megan Garmire, Gordon P. Bautz, Marshall W. Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Canizares, Claude R. Jeltema, Tesla E. Canizares, Claude R. Bautz, Mark W. Malm, Michael R. We observed MS 1054-0321, the highest redshift cluster of galaxies in the Einstein Medium Sensitivity Survey (EMSS), with the Chandra ACIS-S detector. We find the X-ray temperature of the cluster to be 10.4 [+1.7 over -1.5] keV, lower than, but statistically consistent with, the temperature inferred previously. This temperature agrees well with the observed velocity dispersion and that found from weak lensing. We are also able to make the first positive identification of an iron line in this cluster and find a value of 0.26 ± 0.15 for the abundance relative to solar, consistent with early enrichment of the ICM. We confirm significant substructure in the form of two distinct clumps in the X-ray distribution. The eastern clump seems to coincide with the main cluster component. It has a temperature of 10.5[+3.4 over 2.1] keV, approximately the same as the average spectral temperature for the whole cluster. The western clump is cooler, with a temperature of 6.7[+1.7 over -1.2], and may be a subgroup falling into the cluster. Though the presence of substructure indicates that this cluster is not fully relaxed, cluster simulations suggest that we will underestimate the mass, and we can, therefore, use the mass to constrain Ωm. From the overall cluster X-ray temperature we find the virial mass of the cluster to be at least 4.5 × 10[superscript 14] h[superscript -1] M[subscript ☉]. We revisit the cosmological implications of the existence of such a hot, massive cluster at a relatively early epoch. Despite the lower temperature, we still find that the existence of this cluster constrains Ω[subscript m] to be less than one. If Ω[subscript m] = 1 and assuming Gaussian initial perturbations, we find the probability of observing MS 1054 in the EMSS is ~7 × 10[superscript -4]. Contract SAO SV1-61010 United States. National Aeronautics and Space Administration (Contracts NAS 8-3907) United States. National Aeronautics and Space Administration (Contracts NAS 8-37716) United States. National Aeronautics and Space Administration (Contracts NAS 8-38252) HST Grant GO-6668 NAG 5-6236 2013-01-25T19:03:45Z 2013-01-25T19:03:45Z 2001-11 2001-05 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/76611 Jeltema, Tesla E. et al. “Chandra X‐Ray Observatory Observation of the High‐Redshift Cluster MS 1054−0321.” The Astrophysical Journal 562.1 (2001): 124–132. https://orcid.org/0000-0002-1379-4482 https://orcid.org/0000-0002-5769-8441 en_US http://dx.doi.org/10.1086/323435 Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf IOP Publishing arXiv link from Prof. Canizares |
| spellingShingle | Jeltema, Tesla E. Canizares, Claude R. Malm, Michael R. Donahue, Megan Garmire, Gordon P. Bautz, Marshall W. Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321 |
| title | Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321 |
| title_full | Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321 |
| title_fullStr | Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321 |
| title_full_unstemmed | Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321 |
| title_short | Chandra X-Ray Observatory Observation of the High-Redshift Cluster MS 1054–0321 |
| title_sort | chandra x ray observatory observation of the high redshift cluster ms 1054 0321 |
| url | http://hdl.handle.net/1721.1/76611 https://orcid.org/0000-0002-1379-4482 https://orcid.org/0000-0002-5769-8441 |
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