Millimeter observations of the candidate soft gamma-ray repeater SGR 1814-13
Identifieur interne : 001A86 ( Istex/Corpus ); précédent : 001A85; suivant : 001A87Millimeter observations of the candidate soft gamma-ray repeater SGR 1814-13
Auteurs : Ph. Durouchoux ; R. Sood ; I. Smith ; S. Corbel ; D. Hannikainen ; R. LoyerSource :
- Advances in Space Research [ 0273-1177 ] ; 2000.
English descriptors
- KwdEn :
- Astrophys, Corbel, Durouchoux, Elsevier science, Galactic, Galactic rotation curve, Hurley, Hydrogen column density, Interstellar extinction, June, Kinematic distances, Kouveliotou, Millimeter observations, Molecular cloud, Mopra millimeter radio telescope, Private communication, Repeater, Second date, September, Sgrs, Soft repeater, Visual absorption.
- Teeft :
- Astrophys, Corbel, Durouchoux, Elsevier science, Galactic, Galactic rotation curve, Hurley, Hydrogen column density, Interstellar extinction, June, Kinematic distances, Kouveliotou, Millimeter observations, Molecular cloud, Mopra millimeter radio telescope, Private communication, Repeater, Second date, September, Sgrs, Soft repeater, Visual absorption.
Abstract
Abstract: A possible new soft Gamma-Ray Repeater, SGR 1814-13, was first detected on 1997 June 29, with a subsequent possible detection on 1997 September 12. We observed this region on 1997 October 28 and 29, with the MOPRA millimeter radio telescope, in the transition CO(1-0) at 115 GHz, and found a molecular cloud in the direction of this source. Assuming that this cloud is associated with SGR 1814-13, we have derived, from the Galactic rotation curve, kinematic distances of 1.3 kpc and 15 kpc to the source. From the CO (1-0) spectrum, we estimate a hydrogen column density of N(H2) = 5 × 1021 cm−2, and a visual absorption of Av = 5.7 mag. We present arguments for the source to be located at 15 kpc.
Url:
DOI: 10.1016/S0273-1177(99)00837-6
Links to Exploration step
ISTEX:8E4DC373B5E56794AEC65355F04DE73E10B87B3ELe document en format XML
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We observed this region on 1997 October 28 and 29, with the MOPRA millimeter radio telescope, in the transition CO(1-0) at 115 GHz, and found a molecular cloud in the direction of this source. Assuming that this cloud is associated with SGR 1814-13, we have derived, from the Galactic rotation curve, kinematic distances of 1.3 kpc and 15 kpc to the source. From the CO (1-0) spectrum, we estimate a hydrogen column density of N(H2) = 5 × 1021 cm−2, and a visual absorption of Av = 5.7 mag. We present arguments for the source to be located at 15 kpc.</div></front></TEI><istex><corpusName>elsevier</corpusName><keywords><teeft><json:string>molecular cloud</json:string><json:string>june</json:string><json:string>durouchoux</json:string><json:string>kouveliotou</json:string><json:string>soft repeater</json:string><json:string>astrophys</json:string><json:string>september</json:string><json:string>corbel</json:string><json:string>sgrs</json:string><json:string>repeater</json:string><json:string>hurley</json:string><json:string>millimeter observations</json:string><json:string>kinematic distances</json:string><json:string>hydrogen column density</json:string><json:string>visual absorption</json:string><json:string>mopra millimeter radio telescope</json:string><json:string>elsevier science</json:string><json:string>private communication</json:string><json:string>second date</json:string><json:string>interstellar extinction</json:string><json:string>galactic rotation curve</json:string><json:string>galactic</json:string></teeft></keywords><author><json:item><name>Ph. 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From the CO (1-0) spectrum, we estimate a hydrogen column density of N(H2) = 5 × 1021 cm−2, and a visual absorption of Av = 5.7 mag. We present arguments for the source to be located at 15 kpc.</abstract><qualityIndicators><score>4.999</score><pdfWordCount>1487</pdfWordCount><pdfCharCount>7751</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>4</pdfPageCount><pdfPageSize>545 x 774 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>126</abstractWordCount><abstractCharCount>709</abstractCharCount><keywordCount>0</keywordCount></qualityIndicators><title>Millimeter observations of the candidate soft gamma-ray repeater SGR 1814-13</title><pii><json:string>S0273-1177(99)00837-6</json:string></pii><genre><json:string>research-article</json:string></genre><serie><title>The Transparent Universe, Proc. 2nd INTEGRAL Workshop</title><language><json:string>unknown</json:string></language><pages><first>331</first></pages></serie><host><title>Advances in Space Research</title><language><json:string>unknown</json:string></language><publicationDate>2000</publicationDate><issn><json:string>0273-1177</json:string></issn><pii><json:string>S0273-1177(00)X0106-8</json:string></pii><volume>25</volume><issue>3–4</issue><pages><first>765</first><last>768</last></pages><genre><json:string>journal</json:string></genre><conference><json:item><name>Broad Band X-Ray Spectra of Cosmic Sources, Nagoya, Japan 19980712 19980719</name></json:item></conference><editor><json:item><name>K. 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Assuming that this cloud is associated with SGR 1814-13, we have derived, from the Galactic rotation curve, kinematic distances of 1.3 kpc and 15 kpc to the source. From the CO (1-0) spectrum, we estimate a hydrogen column density of N(H2) = 5 × 1021 cm−2, and a visual absorption of Av = 5.7 mag. We present arguments for the source to be located at 15 kpc.</p></abstract></profileDesc><revisionDesc><change when="2000">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/8E4DC373B5E56794AEC65355F04DE73E10B87B3E/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Elsevier doc found" wicri:toSee="Elsevier, no converted or simple article"><istex:xmlDeclaration>version="1.0" encoding="utf-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//ES//DTD journal article DTD version 5.0.1//EN//XML" URI="art501.dtd" name="istex:docType"></istex:docType><istex:document><article version="5.0" xml:lang="en" docsubtype="fla"><item-info><jid>JASR</jid><aid>99008376</aid><ce:pii>S0273-1177(99)00837-6</ce:pii><ce:doi>10.1016/S0273-1177(99)00837-6</ce:doi><ce:copyright type="unknown" year="2000">COSPAR</ce:copyright></item-info><head><ce:title>Millimeter observations of the candidate soft gamma-ray repeater SGR 1814-13</ce:title><ce:author-group><ce:author><ce:given-name>Ph.</ce:given-name><ce:surname>Durouchoux</ce:surname><ce:cross-ref refid="aff1"><ce:sup>1</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>R.</ce:given-name><ce:surname>Sood</ce:surname><ce:cross-ref refid="aff2"><ce:sup>2</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>I.</ce:given-name><ce:surname>Smith</ce:surname><ce:cross-ref refid="aff3"><ce:sup>3</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>S.</ce:given-name><ce:surname>Corbel</ce:surname><ce:cross-ref refid="aff1"><ce:sup>1</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>D.</ce:given-name><ce:surname>Hannikainen</ce:surname><ce:cross-ref refid="aff4"><ce:sup>4</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>R.</ce:given-name><ce:surname>Loyer</ce:surname><ce:cross-ref refid="aff5"><ce:sup>5</ce:sup></ce:cross-ref></ce:author><ce:affiliation id="aff1"><ce:label>1</ce:label><ce:textfn>CE Saclay, DSM, DAPNIA, Service d'Astrophysique, 91191 Gif sur Yvette Cedex, France</ce:textfn></ce:affiliation><ce:affiliation id="aff2"><ce:label>2</ce:label><ce:textfn>School of Physics, Australian Defence Force Academy, UNSW, Canberra ACT 2600, Australia</ce:textfn></ce:affiliation><ce:affiliation id="aff3"><ce:label>3</ce:label><ce:textfn>Department of Space Physics and Astronomy, Rice University, MS 108, 6100 South Main Street, Houston, TX 77005-1892, USA</ce:textfn></ce:affiliation><ce:affiliation id="aff4"><ce:label>4</ce:label><ce:textfn>Observatory, PO Box 14, 00014 University of Helsinki, Finland</ce:textfn></ce:affiliation><ce:affiliation id="aff5"><ce:label>5</ce:label><ce:textfn>Ecole Centrale de Paris, Grande Voie des Vignes, 92295 Chatenay-Malabry Cedex, France</ce:textfn></ce:affiliation></ce:author-group><ce:abstract id="ab1" class="author" xml:lang="en"><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>A possible new soft Gamma-Ray Repeater, SGR 1814-13, was first detected on 1997 June 29, with a subsequent possible detection on 1997 September 12. We observed this region on 1997 October 28 and 29, with the MOPRA millimeter radio telescope, in the transition CO(1-0) at 115 GHz, and found a molecular cloud in the direction of this source. Assuming that this cloud is associated with SGR 1814-13, we have derived, from the Galactic rotation curve, kinematic distances of 1.3 kpc and 15 kpc to the source. From the CO (1-0) spectrum, we estimate a hydrogen column density of N<ce:inf>(H2)</ce:inf> = 5 × 10<ce:sup>21</ce:sup> cm<ce:sup>−2</ce:sup>, and a visual absorption of A<ce:inf>v</ce:inf> = 5.7 mag. 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We observed this region on 1997 October 28 and 29, with the MOPRA millimeter radio telescope, in the transition CO(1-0) at 115 GHz, and found a molecular cloud in the direction of this source. Assuming that this cloud is associated with SGR 1814-13, we have derived, from the Galactic rotation curve, kinematic distances of 1.3 kpc and 15 kpc to the source. From the CO (1-0) spectrum, we estimate a hydrogen column density of N(H2) = 5 × 1021 cm−2, and a visual absorption of Av = 5.7 mag. We present arguments for the source to be located at 15 kpc.</abstract><relatedItem type="host"><titleInfo><title>Advances in Space Research</title></titleInfo><titleInfo type="abbreviated"><title>JASR</title></titleInfo><name type="conference"><namePart>Broad Band X-Ray Spectra of Cosmic Sources, Nagoya, Japan</namePart><namePart type="date">19980712</namePart><namePart type="date">19980719</namePart></name><name type="personal"><namePart>K. 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Takahashi</namePart><role><roleTerm type="text">editor</roleTerm></role></name><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><originInfo><publisher>ELSEVIER</publisher><dateIssued encoding="w3cdtf">2000</dateIssued></originInfo><identifier type="ISSN">0273-1177</identifier><identifier type="PII">S0273-1177(00)X0106-8</identifier><part><date>2000</date><detail type="issue"><title>Broad Band X-Ray Spectra of Cosmic Sources, Nagoya, Japan</title></detail><detail type="volume"><number>25</number><caption>vol.</caption></detail><detail type="issue"><number>3–4</number><caption>no.</caption></detail><extent unit="issue-pages"><start>351</start><end>918</end></extent><extent unit="pages"><start>765</start><end>768</end></extent></part></relatedItem><identifier type="istex">8E4DC373B5E56794AEC65355F04DE73E10B87B3E</identifier><identifier type="ark">ark:/67375/6H6-PWJCDX2N-J</identifier><identifier type="DOI">10.1016/S0273-1177(99)00837-6</identifier><identifier type="PII">S0273-1177(99)00837-6</identifier><identifier type="ArticleID">99008376</identifier><accessCondition type="use and reproduction" contentType="copyright">©2000 COSPAR</accessCondition><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-HKKZVM7B-M">elsevier</recordContentSource><recordOrigin>COSPAR, ©2000</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/8E4DC373B5E56794AEC65355F04DE73E10B87B3E/metadata/json</uri></json:item></metadata></istex></record>Pour manipuler ce document sous Unix (Dilib)
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