Chandra Observations of the W51C Supernova Remnant

We present the results of Chandra ACIS observations of the supernova remnant (SNR) W51C. The remnant is located in the cross section of the Sagittarius arm, and the Chandra images present a superb X-ray view of this complex region including the massive star-forming region W51B. The properties of the...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2005-11, Vol.633 (2), p.946-952
Main Authors: Koo, Bon-Chul, Lee, Jae-Joon, Seward, Frederick D, Moon, Dae-Sik
Format: Article
Language:English
Subjects:
Astronomy
Earth, ocean, space
Exact sciences and technology
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by cdi_FETCH-LOGICAL-c421t-cd251cc16df17583224c968db83eea095531865ca50613f49d363fd9bbd8e9fb3
cites cdi_FETCH-LOGICAL-c421t-cd251cc16df17583224c968db83eea095531865ca50613f49d363fd9bbd8e9fb3
container_end_page 952
container_issue 2
container_start_page 946
container_title The Astrophysical journal
container_volume 633
creator Koo, Bon-Chul
Lee, Jae-Joon
Seward, Frederick D
Moon, Dae-Sik
description We present the results of Chandra ACIS observations of the supernova remnant (SNR) W51C. The remnant is located in the cross section of the Sagittarius arm, and the Chandra images present a superb X-ray view of this complex region including the massive star-forming region W51B. The properties of thermal diffuse SNR emission are consistent with the results of previous studies except that an enhanced abundance of sulfur is required. It is found that the ASCA hard X-ray source CXO J192318.5+1403035, proposed to be a pulsar wind nebula, is composed of a relatively bright core surrounded by an extended (67.0 x 2.5 pc) diffuse envelope. The core contains a compact (
doi_str_mv 10.1086/491468
format article
fullrecord <record><control><sourceid>proquest_iop_p</sourceid><recordid>TN_cdi_iop_primary_10_1086_491468</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>17478331</sourcerecordid><originalsourceid>FETCH-LOGICAL-c421t-cd251cc16df17583224c968db83eea095531865ca50613f49d363fd9bbd8e9fb3</originalsourceid><addsrcrecordid>eNp90U1LAzEQBuAgCtaqv2E9qCCsZjJJNjlK8QsKBT_QW8hmE7rS7q7JtuC_t6WFHkQvMww8vId5CTkFeg1UyRuugUu1RwYgUOUcRbFPBpRSnkssPg7JUUqf65NpPSBsNLVNFW02KZOPS9vXbZOyNmT91GfvAkbZy6LzsWmXNnv288Y2_TE5CHaW_Ml2D8nb_d3r6DEfTx6eRrfj3HEGfe4qJsA5kFWAQihkjDstVVUq9N5SLQSCksJZQSVg4LpCiaHSZVkpr0OJQ3K5ye1i-7XwqTfzOjk_m9nGt4tkCo4ACoGu5MW_EgpeKETYQRfblKIPpov13MZvA9Ssn2c2z1vB822iTc7OQrSNq9NOF0wxTXHlzjaubru_s65-m3UBZt3HaqBhRnNpuirgD6-Rgtw</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>17478331</pqid></control><display><type>article</type><title>Chandra Observations of the W51C Supernova Remnant</title><source>Free E-Journal (出版社公開部分のみ）</source><creator>Koo, Bon-Chul ; Lee, Jae-Joon ; Seward, Frederick D ; Moon, Dae-Sik</creator><creatorcontrib>Koo, Bon-Chul ; Lee, Jae-Joon ; Seward, Frederick D ; Moon, Dae-Sik</creatorcontrib><description>We present the results of Chandra ACIS observations of the supernova remnant (SNR) W51C. The remnant is located in the cross section of the Sagittarius arm, and the Chandra images present a superb X-ray view of this complex region including the massive star-forming region W51B. The properties of thermal diffuse SNR emission are consistent with the results of previous studies except that an enhanced abundance of sulfur is required. It is found that the ASCA hard X-ray source CXO J192318.5+1403035, proposed to be a pulsar wind nebula, is composed of a relatively bright core surrounded by an extended (67.0 x 2.5 pc) diffuse envelope. The core contains a compact (&lt;0.1 pc) source at the center. The X-ray spectrum of CXO J192318.5+1403035 can be fitted by a power-law emission model with = 1.82 super(+) sub(-) super(0) sub(0) super(.) sub(.) super(2) sub(2) super(8) sub(9), and the implied X-ray (0.2-4.0 keV) luminosity is 5 x 10 super(33) ergs s super(-1). The core contributes 620% of the total luminosity. The core-envelope structure and its spectral properties support CXO J192318.5+140305 as a pulsar-wind nebula associated with the SNR W51C. There is also enhanced radio emission coincident with the source. It is conceivable that the central compact source might harbor a pulsar. However, the large extent and the hardening of X-rays at the extreme boundaries need to be explained. We have searched for the Brg line from the ionized gas associated with the source, but no emission was detected.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/491468</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Chicago, IL: IOP Publishing</publisher><subject>Astronomy ; Earth, ocean, space ; Exact sciences and technology</subject><ispartof>The Astrophysical journal, 2005-11, Vol.633 (2), p.946-952</ispartof><rights>2006 INIST-CNRS</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c421t-cd251cc16df17583224c968db83eea095531865ca50613f49d363fd9bbd8e9fb3</citedby><cites>FETCH-LOGICAL-c421t-cd251cc16df17583224c968db83eea095531865ca50613f49d363fd9bbd8e9fb3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&amp;idt=17282903$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Koo, Bon-Chul</creatorcontrib><creatorcontrib>Lee, Jae-Joon</creatorcontrib><creatorcontrib>Seward, Frederick D</creatorcontrib><creatorcontrib>Moon, Dae-Sik</creatorcontrib><title>Chandra Observations of the W51C Supernova Remnant</title><title>The Astrophysical journal</title><description>We present the results of Chandra ACIS observations of the supernova remnant (SNR) W51C. The remnant is located in the cross section of the Sagittarius arm, and the Chandra images present a superb X-ray view of this complex region including the massive star-forming region W51B. The properties of thermal diffuse SNR emission are consistent with the results of previous studies except that an enhanced abundance of sulfur is required. It is found that the ASCA hard X-ray source CXO J192318.5+1403035, proposed to be a pulsar wind nebula, is composed of a relatively bright core surrounded by an extended (67.0 x 2.5 pc) diffuse envelope. The core contains a compact (&lt;0.1 pc) source at the center. The X-ray spectrum of CXO J192318.5+1403035 can be fitted by a power-law emission model with = 1.82 super(+) sub(-) super(0) sub(0) super(.) sub(.) super(2) sub(2) super(8) sub(9), and the implied X-ray (0.2-4.0 keV) luminosity is 5 x 10 super(33) ergs s super(-1). The core contributes 620% of the total luminosity. The core-envelope structure and its spectral properties support CXO J192318.5+140305 as a pulsar-wind nebula associated with the SNR W51C. There is also enhanced radio emission coincident with the source. It is conceivable that the central compact source might harbor a pulsar. However, the large extent and the hardening of X-rays at the extreme boundaries need to be explained. We have searched for the Brg line from the ionized gas associated with the source, but no emission was detected.</description><subject>Astronomy</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2005</creationdate><recordtype>article</recordtype><recordid>eNp90U1LAzEQBuAgCtaqv2E9qCCsZjJJNjlK8QsKBT_QW8hmE7rS7q7JtuC_t6WFHkQvMww8vId5CTkFeg1UyRuugUu1RwYgUOUcRbFPBpRSnkssPg7JUUqf65NpPSBsNLVNFW02KZOPS9vXbZOyNmT91GfvAkbZy6LzsWmXNnv288Y2_TE5CHaW_Ml2D8nb_d3r6DEfTx6eRrfj3HEGfe4qJsA5kFWAQihkjDstVVUq9N5SLQSCksJZQSVg4LpCiaHSZVkpr0OJQ3K5ye1i-7XwqTfzOjk_m9nGt4tkCo4ACoGu5MW_EgpeKETYQRfblKIPpov13MZvA9Ssn2c2z1vB822iTc7OQrSNq9NOF0wxTXHlzjaubru_s65-m3UBZt3HaqBhRnNpuirgD6-Rgtw</recordid><startdate>20051110</startdate><enddate>20051110</enddate><creator>Koo, Bon-Chul</creator><creator>Lee, Jae-Joon</creator><creator>Seward, Frederick D</creator><creator>Moon, Dae-Sik</creator><general>IOP Publishing</general><general>University of Chicago Press</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20051110</creationdate><title>Chandra Observations of the W51C Supernova Remnant</title><author>Koo, Bon-Chul ; Lee, Jae-Joon ; Seward, Frederick D ; Moon, Dae-Sik</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c421t-cd251cc16df17583224c968db83eea095531865ca50613f49d363fd9bbd8e9fb3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2005</creationdate><topic>Astronomy</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Koo, Bon-Chul</creatorcontrib><creatorcontrib>Lee, Jae-Joon</creatorcontrib><creatorcontrib>Seward, Frederick D</creatorcontrib><creatorcontrib>Moon, Dae-Sik</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Koo, Bon-Chul</au><au>Lee, Jae-Joon</au><au>Seward, Frederick D</au><au>Moon, Dae-Sik</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Chandra Observations of the W51C Supernova Remnant</atitle><jtitle>The Astrophysical journal</jtitle><date>2005-11-10</date><risdate>2005</risdate><volume>633</volume><issue>2</issue><spage>946</spage><epage>952</epage><pages>946-952</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>We present the results of Chandra ACIS observations of the supernova remnant (SNR) W51C. The remnant is located in the cross section of the Sagittarius arm, and the Chandra images present a superb X-ray view of this complex region including the massive star-forming region W51B. The properties of thermal diffuse SNR emission are consistent with the results of previous studies except that an enhanced abundance of sulfur is required. It is found that the ASCA hard X-ray source CXO J192318.5+1403035, proposed to be a pulsar wind nebula, is composed of a relatively bright core surrounded by an extended (67.0 x 2.5 pc) diffuse envelope. The core contains a compact (&lt;0.1 pc) source at the center. The X-ray spectrum of CXO J192318.5+1403035 can be fitted by a power-law emission model with = 1.82 super(+) sub(-) super(0) sub(0) super(.) sub(.) super(2) sub(2) super(8) sub(9), and the implied X-ray (0.2-4.0 keV) luminosity is 5 x 10 super(33) ergs s super(-1). The core contributes 620% of the total luminosity. The core-envelope structure and its spectral properties support CXO J192318.5+140305 as a pulsar-wind nebula associated with the SNR W51C. There is also enhanced radio emission coincident with the source. It is conceivable that the central compact source might harbor a pulsar. However, the large extent and the hardening of X-rays at the extreme boundaries need to be explained. We have searched for the Brg line from the ionized gas associated with the source, but no emission was detected.</abstract><cop>Chicago, IL</cop><pub>IOP Publishing</pub><doi>10.1086/491468</doi><tpages>7</tpages></addata></record>
fulltext fulltext
identifier ISSN: 0004-637X
ispartof The Astrophysical journal, 2005-11, Vol.633 (2), p.946-952
issn 0004-637X
1538-4357
language eng
recordid cdi_iop_primary_10_1086_491468
source Free E-Journal (出版社公開部分のみ）
subjects Astronomy
Earth, ocean, space
Exact sciences and technology
title Chandra Observations of the W51C Supernova Remnant
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-06T13%3A20%3A08IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_iop_p&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Chandra%20Observations%20of%20the%20W51C%20Supernova%20Remnant&rft.jtitle=The%20Astrophysical%20journal&rft.au=Koo,%20Bon-Chul&rft.date=2005-11-10&rft.volume=633&rft.issue=2&rft.spage=946&rft.epage=952&rft.pages=946-952&rft.issn=0004-637X&rft.eissn=1538-4357&rft.coden=ASJOAB&rft_id=info:doi/10.1086/491468&rft_dat=%3Cproquest_iop_p%3E17478331%3C/proquest_iop_p%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c421t-cd251cc16df17583224c968db83eea095531865ca50613f49d363fd9bbd8e9fb3%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=17478331&rft_id=info:pmid/&rfr_iscdi=true