Identification of an X-Ray Pulsar in the BeXRB System IGR J18219−1347
We report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219−1347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin perio...
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| Veröffentlicht in: | The Astrophysical journal 2022-03, Vol.927 (2), p.139 |
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| creator | O’Connor, B. Göğüş, E. Huppenkothen, D. Kouveliotou, C. Gorgone, N. Townsend, L. J. Calamida, A. Fruchter, A. Buckley, D. A. H. Baring, M. G. Kennea, J. A. Younes, G. Arzoumanian, Z. Bellm, E. Cenko, S. B. Gendreau, K. Granot, J. Hailey, C. Harrison, F. Hartmann, D. Kaper, L. Kutyrev, A. Slane, P. O. Stern, D. Troja, E. van der Horst, A. J. Wijers, R. A. M. J. Woudt, P. |
| description | We report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219−1347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin period of a neutron star with
P
spin
= 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10–15 kpc for the source. The broadband X-ray spectrum (1.5–50 keV) of the source is described by an absorbed power law with a photon index Γ ∼ 0.5 and a cutoff energy at ∼13 keV. |
| doi_str_mv | 10.3847/1538-4357/ac5032 |
| format | Article |
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P
spin
= 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10–15 kpc for the source. The broadband X-ray spectrum (1.5–50 keV) of the source is described by an absorbed power law with a photon index Γ ∼ 0.5 and a cutoff energy at ∼13 keV.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ac5032</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Broadband ; High mass x-ray binary stars ; Neutron stars ; Orbits ; Outbursts ; Pulsars ; Spectral energy distribution ; Spectroscopic telescopes ; X ray binaries ; X ray spectra ; X ray stars ; X ray telescopes ; X-ray astronomy ; X-rays</subject><ispartof>The Astrophysical journal, 2022-03, Vol.927 (2), p.139</ispartof><rights>2022. The Author(s). Published by the American Astronomical Society.</rights><rights>2022. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c380t-1c697e9286191f14d0042e920e537b3e5e8af1bae52ffa855ffdca012308371a3</citedby><cites>FETCH-LOGICAL-c380t-1c697e9286191f14d0042e920e537b3e5e8af1bae52ffa855ffdca012308371a3</cites><orcidid>0000-0001-9788-3345 ; 0000-0002-6896-1655 ; 0000-0002-3101-1808 ; 0000-0002-3681-145X ; 0000-0001-9149-6707 ; 0000-0002-6745-4790 ; 0000-0001-7115-2819 ; 0000-0003-4433-1365 ; 0000-0002-9700-0036 ; 0000-0003-1673-970X ; 0000-0002-1869-7817 ; 0000-0002-1169-7486 ; 0000-0002-6652-9279 ; 0000-0001-8018-5348 ; 0000-0001-8530-8941 ; 0000-0003-2992-8024 ; 0000-0002-7991-028X ; 0000-0002-5274-6790 ; 0000-0003-1443-593X ; 0000-0002-7004-9956 ; 0000-0002-6986-6756 ; 0000-0002-1653-6411 ; 0000-0002-2715-8460 ; 0000-0003-2686-9241 ; 0000-0002-0882-7702 ; 0000-0002-8028-0991</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ac5032/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,27901,27902,38867,53842</link.rule.ids></links><search><creatorcontrib>O’Connor, B.</creatorcontrib><creatorcontrib>Göğüş, E.</creatorcontrib><creatorcontrib>Huppenkothen, D.</creatorcontrib><creatorcontrib>Kouveliotou, C.</creatorcontrib><creatorcontrib>Gorgone, N.</creatorcontrib><creatorcontrib>Townsend, L. J.</creatorcontrib><creatorcontrib>Calamida, A.</creatorcontrib><creatorcontrib>Fruchter, A.</creatorcontrib><creatorcontrib>Buckley, D. A. H.</creatorcontrib><creatorcontrib>Baring, M. G.</creatorcontrib><creatorcontrib>Kennea, J. A.</creatorcontrib><creatorcontrib>Younes, G.</creatorcontrib><creatorcontrib>Arzoumanian, Z.</creatorcontrib><creatorcontrib>Bellm, E.</creatorcontrib><creatorcontrib>Cenko, S. B.</creatorcontrib><creatorcontrib>Gendreau, K.</creatorcontrib><creatorcontrib>Granot, J.</creatorcontrib><creatorcontrib>Hailey, C.</creatorcontrib><creatorcontrib>Harrison, F.</creatorcontrib><creatorcontrib>Hartmann, D.</creatorcontrib><creatorcontrib>Kaper, L.</creatorcontrib><creatorcontrib>Kutyrev, A.</creatorcontrib><creatorcontrib>Slane, P. O.</creatorcontrib><creatorcontrib>Stern, D.</creatorcontrib><creatorcontrib>Troja, E.</creatorcontrib><creatorcontrib>van der Horst, A. J.</creatorcontrib><creatorcontrib>Wijers, R. A. M. J.</creatorcontrib><creatorcontrib>Woudt, P.</creatorcontrib><title>Identification of an X-Ray Pulsar in the BeXRB System IGR J18219−1347</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219−1347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin period of a neutron star with
P
spin
= 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10–15 kpc for the source. The broadband X-ray spectrum (1.5–50 keV) of the source is described by an absorbed power law with a photon index Γ ∼ 0.5 and a cutoff energy at ∼13 keV.</description><subject>Astrophysics</subject><subject>Broadband</subject><subject>High mass x-ray binary stars</subject><subject>Neutron stars</subject><subject>Orbits</subject><subject>Outbursts</subject><subject>Pulsars</subject><subject>Spectral energy distribution</subject><subject>Spectroscopic telescopes</subject><subject>X ray binaries</subject><subject>X ray spectra</subject><subject>X ray stars</subject><subject>X ray telescopes</subject><subject>X-ray astronomy</subject><subject>X-rays</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><recordid>eNp9kL1OwzAUhS0EEqWwM1pCbIT6-saxPVIEpagSqIDUzXITW6RqkxCnQ9-AmUfkSUgUBAtiujpX59yfj5BTYJeoYjkCgSqKUciRTQVDvkcGP619MmCMxVGCcnFIjkJYdZJrPSCTaeaKJvd5apu8LGjpqS3oIprbHX3croOtaV7Q5tXRsVvMx_RpFxq3odPJnN6D4qA_3z8AY3lMDrxdB3fyXYfk5fbm-foumj1MptdXsyhFxZoI0kRLp7lKQIOHOOvuaDVzAuUSnXDKelhaJ7j3VgnhfZZaBhyZQgkWh-Ssn1vV5dvWhcasym1dtCsNT-L2Lc0xaV2sd6V1GULtvKnqfGPrnQFmOlymY2M6NqbH1UYu-kheVr8z_7Gf_2G31cpoLg03gNpUmccvfMd0Yw</recordid><startdate>20220301</startdate><enddate>20220301</enddate><creator>O’Connor, B.</creator><creator>Göğüş, E.</creator><creator>Huppenkothen, D.</creator><creator>Kouveliotou, C.</creator><creator>Gorgone, N.</creator><creator>Townsend, L. 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B.</au><au>Gendreau, K.</au><au>Granot, J.</au><au>Hailey, C.</au><au>Harrison, F.</au><au>Hartmann, D.</au><au>Kaper, L.</au><au>Kutyrev, A.</au><au>Slane, P. O.</au><au>Stern, D.</au><au>Troja, E.</au><au>van der Horst, A. J.</au><au>Wijers, R. A. M. J.</au><au>Woudt, P.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Identification of an X-Ray Pulsar in the BeXRB System IGR J18219−1347</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2022-03-01</date><risdate>2022</risdate><volume>927</volume><issue>2</issue><spage>139</spage><pages>139-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219−1347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin period of a neutron star with
P
spin
= 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10–15 kpc for the source. The broadband X-ray spectrum (1.5–50 keV) of the source is described by an absorbed power law with a photon index Γ ∼ 0.5 and a cutoff energy at ∼13 keV.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ac5032</doi><tpages>13</tpages><orcidid>https://orcid.org/0000-0001-9788-3345</orcidid><orcidid>https://orcid.org/0000-0002-6896-1655</orcidid><orcidid>https://orcid.org/0000-0002-3101-1808</orcidid><orcidid>https://orcid.org/0000-0002-3681-145X</orcidid><orcidid>https://orcid.org/0000-0001-9149-6707</orcidid><orcidid>https://orcid.org/0000-0002-6745-4790</orcidid><orcidid>https://orcid.org/0000-0001-7115-2819</orcidid><orcidid>https://orcid.org/0000-0003-4433-1365</orcidid><orcidid>https://orcid.org/0000-0002-9700-0036</orcidid><orcidid>https://orcid.org/0000-0003-1673-970X</orcidid><orcidid>https://orcid.org/0000-0002-1869-7817</orcidid><orcidid>https://orcid.org/0000-0002-1169-7486</orcidid><orcidid>https://orcid.org/0000-0002-6652-9279</orcidid><orcidid>https://orcid.org/0000-0001-8018-5348</orcidid><orcidid>https://orcid.org/0000-0001-8530-8941</orcidid><orcidid>https://orcid.org/0000-0003-2992-8024</orcidid><orcidid>https://orcid.org/0000-0002-7991-028X</orcidid><orcidid>https://orcid.org/0000-0002-5274-6790</orcidid><orcidid>https://orcid.org/0000-0003-1443-593X</orcidid><orcidid>https://orcid.org/0000-0002-7004-9956</orcidid><orcidid>https://orcid.org/0000-0002-6986-6756</orcidid><orcidid>https://orcid.org/0000-0002-1653-6411</orcidid><orcidid>https://orcid.org/0000-0002-2715-8460</orcidid><orcidid>https://orcid.org/0000-0003-2686-9241</orcidid><orcidid>https://orcid.org/0000-0002-0882-7702</orcidid><orcidid>https://orcid.org/0000-0002-8028-0991</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2022-03, Vol.927 (2), p.139 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_crossref_primary_10_3847_1538_4357_ac5032 |
| source | IOP Publishing Free Content; DOAJ Directory of Open Access Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; Alma/SFX Local Collection |
| subjects | Astrophysics Broadband High mass x-ray binary stars Neutron stars Orbits Outbursts Pulsars Spectral energy distribution Spectroscopic telescopes X ray binaries X ray spectra X ray stars X ray telescopes X-ray astronomy X-rays |
| title | Identification of an X-Ray Pulsar in the BeXRB System IGR J18219−1347 |
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