Detection of gamma-rays around SNR HB9 and its implications for the diffusive shock-acceleration history

Abstract We analyze the GeV gamma-ray emission data from the vicinity of the supernova remnant (SNR) HB9 (G160.9+2.6) from the Fermi-LAT 12 yr observations to quantify the evolution of diffusive shock acceleration (DSA) in the SNR. In the vicinity of HB9, there are molecular clouds whose locations d...

Ausführliche Beschreibung

Gespeichert in:
Bibliographische Detailangaben
Veröffentlicht in:Publications of the Astronomical Society of Japan 2022-06, Vol.74 (3), p.625-638
Hauptverfasser: Oka, Tomohiko, Ishizaki, Wataru
Format: Artikel
Sprache:eng
Online-Zugang:Volltext
Tags: Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
container_end_page 638
container_issue 3
container_start_page 625
container_title Publications of the Astronomical Society of Japan
container_volume 74
creator Oka, Tomohiko
Ishizaki, Wataru
description Abstract We analyze the GeV gamma-ray emission data from the vicinity of the supernova remnant (SNR) HB9 (G160.9+2.6) from the Fermi-LAT 12 yr observations to quantify the evolution of diffusive shock acceleration (DSA) in the SNR. In the vicinity of HB9, there are molecular clouds whose locations do not coincide with the SNR shell in the line of sight. We detect significant gamma-ray emissions above 1 GeV spatially coinciding with the two prominent cloud regions, as well as emission from the SNR shell, the latter of which is consistent with the results of previous studies. The energy spectrum above 1 GeV in each region is fitted with a simple power-law function of dN/dE ∝ E−Γ. The fitting result indicates harder spectra, with power-law indices of Γ = 1.84 ± 0.18 and 1.84 ± 0.14, than that at the SNR shell, with Γ = 2.55 ± 0.10. The observed spectra from the cloud regions are found to be consistent with the theoretically expected gamma-ray emissions originating in the protons that escaped from SNR HB9, where particles can be accelerated up to higher energies than those in the shell at present. The resultant diffusion coefficient in the vicinity of the SNR is comparable to that of the Galactic mean.
doi_str_mv 10.1093/pasj/psac024
format Article
fullrecord <record><control><sourceid>oup_cross</sourceid><recordid>TN_cdi_crossref_primary_10_1093_pasj_psac024</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><oup_id>10.1093/pasj/psac024</oup_id><sourcerecordid>10.1093/pasj/psac024</sourcerecordid><originalsourceid>FETCH-LOGICAL-c305t-828245ac29f8e94fd4ef6899fd26e4fc830c08d26d6c410b1d2f110e1d42eaf33</originalsourceid><addsrcrecordid>eNp9kEtLAzEUhYMoWGp3_oDs3Bh785h0stT6qFAUfIC7Ic3DiXaaIZkK8--d2q5d3XPhO2fxIXRO4YqC4tNW569pm7UBJo7QiEHBCRT04xiNAEAQyaQ4RZOcwwqYVDMqZ3yE6lvXOdOFuMHR40_dNJok3WesU9xuLH59esGLG4X1kEOXcWjadTB6V8jYx4S72mEbvN_m8ONwrqP5JtoYt3bpj8J1yF1M_Rk68Xqd3eRwx-j9_u5tviDL54fH-fWSGA5FR0pWMlFow5QvnRLeCudlqZS3TDrhTcnBQDk8VhpBYUUt85SCo1Ywpz3nY3S53zUp5pycr9oUGp36ikK1E1XtRFUHUQN-scfjtv2f_AVlKGx1</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>Detection of gamma-rays around SNR HB9 and its implications for the diffusive shock-acceleration history</title><source>Oxford University Press Journals All Titles (1996-Current)</source><source>Open Access Titles of Japan</source><creator>Oka, Tomohiko ; Ishizaki, Wataru</creator><creatorcontrib>Oka, Tomohiko ; Ishizaki, Wataru</creatorcontrib><description>Abstract We analyze the GeV gamma-ray emission data from the vicinity of the supernova remnant (SNR) HB9 (G160.9+2.6) from the Fermi-LAT 12 yr observations to quantify the evolution of diffusive shock acceleration (DSA) in the SNR. In the vicinity of HB9, there are molecular clouds whose locations do not coincide with the SNR shell in the line of sight. We detect significant gamma-ray emissions above 1 GeV spatially coinciding with the two prominent cloud regions, as well as emission from the SNR shell, the latter of which is consistent with the results of previous studies. The energy spectrum above 1 GeV in each region is fitted with a simple power-law function of dN/dE ∝ E−Γ. The fitting result indicates harder spectra, with power-law indices of Γ = 1.84 ± 0.18 and 1.84 ± 0.14, than that at the SNR shell, with Γ = 2.55 ± 0.10. The observed spectra from the cloud regions are found to be consistent with the theoretically expected gamma-ray emissions originating in the protons that escaped from SNR HB9, where particles can be accelerated up to higher energies than those in the shell at present. The resultant diffusion coefficient in the vicinity of the SNR is comparable to that of the Galactic mean.</description><identifier>ISSN: 0004-6264</identifier><identifier>EISSN: 2053-051X</identifier><identifier>DOI: 10.1093/pasj/psac024</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Publications of the Astronomical Society of Japan, 2022-06, Vol.74 (3), p.625-638</ispartof><rights>The Author(s) 2022. Published by Oxford University Press on behalf of the Astronomical Society of Japan. 2022</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c305t-828245ac29f8e94fd4ef6899fd26e4fc830c08d26d6c410b1d2f110e1d42eaf33</citedby><cites>FETCH-LOGICAL-c305t-828245ac29f8e94fd4ef6899fd26e4fc830c08d26d6c410b1d2f110e1d42eaf33</cites><orcidid>0000-0002-9924-9978</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,1578,27903,27904</link.rule.ids></links><search><creatorcontrib>Oka, Tomohiko</creatorcontrib><creatorcontrib>Ishizaki, Wataru</creatorcontrib><title>Detection of gamma-rays around SNR HB9 and its implications for the diffusive shock-acceleration history</title><title>Publications of the Astronomical Society of Japan</title><description>Abstract We analyze the GeV gamma-ray emission data from the vicinity of the supernova remnant (SNR) HB9 (G160.9+2.6) from the Fermi-LAT 12 yr observations to quantify the evolution of diffusive shock acceleration (DSA) in the SNR. In the vicinity of HB9, there are molecular clouds whose locations do not coincide with the SNR shell in the line of sight. We detect significant gamma-ray emissions above 1 GeV spatially coinciding with the two prominent cloud regions, as well as emission from the SNR shell, the latter of which is consistent with the results of previous studies. The energy spectrum above 1 GeV in each region is fitted with a simple power-law function of dN/dE ∝ E−Γ. The fitting result indicates harder spectra, with power-law indices of Γ = 1.84 ± 0.18 and 1.84 ± 0.14, than that at the SNR shell, with Γ = 2.55 ± 0.10. The observed spectra from the cloud regions are found to be consistent with the theoretically expected gamma-ray emissions originating in the protons that escaped from SNR HB9, where particles can be accelerated up to higher energies than those in the shell at present. The resultant diffusion coefficient in the vicinity of the SNR is comparable to that of the Galactic mean.</description><issn>0004-6264</issn><issn>2053-051X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNp9kEtLAzEUhYMoWGp3_oDs3Bh785h0stT6qFAUfIC7Ic3DiXaaIZkK8--d2q5d3XPhO2fxIXRO4YqC4tNW569pm7UBJo7QiEHBCRT04xiNAEAQyaQ4RZOcwwqYVDMqZ3yE6lvXOdOFuMHR40_dNJok3WesU9xuLH59esGLG4X1kEOXcWjadTB6V8jYx4S72mEbvN_m8ONwrqP5JtoYt3bpj8J1yF1M_Rk68Xqd3eRwx-j9_u5tviDL54fH-fWSGA5FR0pWMlFow5QvnRLeCudlqZS3TDrhTcnBQDk8VhpBYUUt85SCo1Ywpz3nY3S53zUp5pycr9oUGp36ikK1E1XtRFUHUQN-scfjtv2f_AVlKGx1</recordid><startdate>20220602</startdate><enddate>20220602</enddate><creator>Oka, Tomohiko</creator><creator>Ishizaki, Wataru</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0002-9924-9978</orcidid></search><sort><creationdate>20220602</creationdate><title>Detection of gamma-rays around SNR HB9 and its implications for the diffusive shock-acceleration history</title><author>Oka, Tomohiko ; Ishizaki, Wataru</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c305t-828245ac29f8e94fd4ef6899fd26e4fc830c08d26d6c410b1d2f110e1d42eaf33</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Oka, Tomohiko</creatorcontrib><creatorcontrib>Ishizaki, Wataru</creatorcontrib><collection>CrossRef</collection><jtitle>Publications of the Astronomical Society of Japan</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Oka, Tomohiko</au><au>Ishizaki, Wataru</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Detection of gamma-rays around SNR HB9 and its implications for the diffusive shock-acceleration history</atitle><jtitle>Publications of the Astronomical Society of Japan</jtitle><date>2022-06-02</date><risdate>2022</risdate><volume>74</volume><issue>3</issue><spage>625</spage><epage>638</epage><pages>625-638</pages><issn>0004-6264</issn><eissn>2053-051X</eissn><abstract>Abstract We analyze the GeV gamma-ray emission data from the vicinity of the supernova remnant (SNR) HB9 (G160.9+2.6) from the Fermi-LAT 12 yr observations to quantify the evolution of diffusive shock acceleration (DSA) in the SNR. In the vicinity of HB9, there are molecular clouds whose locations do not coincide with the SNR shell in the line of sight. We detect significant gamma-ray emissions above 1 GeV spatially coinciding with the two prominent cloud regions, as well as emission from the SNR shell, the latter of which is consistent with the results of previous studies. The energy spectrum above 1 GeV in each region is fitted with a simple power-law function of dN/dE ∝ E−Γ. The fitting result indicates harder spectra, with power-law indices of Γ = 1.84 ± 0.18 and 1.84 ± 0.14, than that at the SNR shell, with Γ = 2.55 ± 0.10. The observed spectra from the cloud regions are found to be consistent with the theoretically expected gamma-ray emissions originating in the protons that escaped from SNR HB9, where particles can be accelerated up to higher energies than those in the shell at present. The resultant diffusion coefficient in the vicinity of the SNR is comparable to that of the Galactic mean.</abstract><pub>Oxford University Press</pub><doi>10.1093/pasj/psac024</doi><tpages>14</tpages><orcidid>https://orcid.org/0000-0002-9924-9978</orcidid><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 0004-6264
ispartof Publications of the Astronomical Society of Japan, 2022-06, Vol.74 (3), p.625-638
issn 0004-6264
2053-051X
language eng
recordid cdi_crossref_primary_10_1093_pasj_psac024
source Oxford University Press Journals All Titles (1996-Current); Open Access Titles of Japan
title Detection of gamma-rays around SNR HB9 and its implications for the diffusive shock-acceleration history
url https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-25T10%3A40%3A07IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-oup_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Detection%20of%20gamma-rays%20around%20SNR%20HB9%20and%20its%20implications%20for%20the%20diffusive%20shock-acceleration%20history&rft.jtitle=Publications%20of%20the%20Astronomical%20Society%20of%20Japan&rft.au=Oka,%20Tomohiko&rft.date=2022-06-02&rft.volume=74&rft.issue=3&rft.spage=625&rft.epage=638&rft.pages=625-638&rft.issn=0004-6264&rft.eissn=2053-051X&rft_id=info:doi/10.1093/pasj/psac024&rft_dat=%3Coup_cross%3E10.1093/pasj/psac024%3C/oup_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rft_oup_id=10.1093/pasj/psac024&rfr_iscdi=true