IGR J17062-6143 Is an Accreting Millisecond X-Ray Pulsar

We present the discovery of 163.65 Hz X-ray pulsations from IGR J17062−6143 in the only observation obtained from the source with the Rossi X-ray Timing Explorer. This detection makes IGR J17062−6143 the lowest-frequency accreting millisecond X-ray pulsar presently known. The pulsations are detected...

Full description

Saved in:
Bibliographic Details
Published in:Astrophysical journal. Letters 2017-02, Vol.836 (2), p.L23-L23
Main Authors: Strohmayer, Tod, Keek, Laurens
Format: Article
Language:English
Subjects:
Accretion
AMPLITUDES
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Circular orbits
DETECTION
Intervals
KEV RANGE
MASS
NEUTRON STARS
ORBITS
OSCILLATIONS
PULSARS
Pulsation
PULSATIONS
ROTATION
stars: neutron
stars: oscillations
stars: rotation
Time measurements
X RADIATION
X rays
X-rays: binaries
X-rays: individual (IGR J17062-6143)
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-c513t-756be54247c7c9e38a3b03cda866d04a9760fc738b7283cf3f947b89055a1d73
cites cdi_FETCH-LOGICAL-c513t-756be54247c7c9e38a3b03cda866d04a9760fc738b7283cf3f947b89055a1d73
container_end_page L23
container_issue 2
container_start_page L23
container_title Astrophysical journal. Letters
container_volume 836
creator Strohmayer, Tod
Keek, Laurens
description We present the discovery of 163.65 Hz X-ray pulsations from IGR J17062−6143 in the only observation obtained from the source with the Rossi X-ray Timing Explorer. This detection makes IGR J17062−6143 the lowest-frequency accreting millisecond X-ray pulsar presently known. The pulsations are detected in the 2-12 keV band with an overall significance of 4.3 and an observed pulsed amplitude of 5.54% 0.67% (in this band). Both dynamic power spectral and coherent phase timing analysis indicate that the pulsation frequency is decreasing during the 1.2 ks observation in a manner consistent with orbital motion of the neutron star. Because the observation interval is short, we cannot precisely measure the orbital period; however, periods shorter than 17 minutes are excluded at 90% confidence. For the range of acceptable circular orbits the inferred binary mass function substantially overlaps the observed range for the AMXP population as a whole.
doi_str_mv 10.3847/2041-8213/aa5e51
format article
fullrecord <record><control><sourceid>proquest_osti_</sourceid><recordid>TN_cdi_osti_scitechconnect_22654537</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1893902676</sourcerecordid><originalsourceid>FETCH-LOGICAL-c513t-756be54247c7c9e38a3b03cda866d04a9760fc738b7283cf3f947b89055a1d73</originalsourceid><addsrcrecordid>eNqNkE1Lw0AQhhdRsFbvHgOCeDB2d2e_ciyitVJRSg_els1moylpEneTQ_-9CZGeRDzNy_C8w_AgdEnwHSgmZxQzEitKYGYMd5wcoclhdXzImJ-isxC2GFMsiJogtVyso2cisaCxIAyiZYhMFc2t9a4tqo_opSjLIjhbV1n0Hq_NPnrrymD8OTrJTRncxc-cos3jw-b-KV69Lpb381VsOYE2llykjjPKpJU2caAMpBhsZpQQGWYmkQLnVoJKJVVgc8gTJlOVYM4NySRM0dV4tg5toYMtWmc_-2cqZ1tNqeCMw0DdjFTj66_OhVbvimBdWZrK1V3QRCWQYCqk-AcqpaKcEdKjeEStr0PwLteNL3bG7zXBepCuB6t6MKxH6X3ldqwUdaO3deer3s1f-PUvuGm2pVYgNNUrCrrJcvgGAWKKLQ</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1877825411</pqid></control><display><type>article</type><title>IGR J17062-6143 Is an Accreting Millisecond X-Ray Pulsar</title><source>EZB Electronic Journals Library</source><creator>Strohmayer, Tod ; Keek, Laurens</creator><creatorcontrib>Strohmayer, Tod ; Keek, Laurens</creatorcontrib><description>We present the discovery of 163.65 Hz X-ray pulsations from IGR J17062−6143 in the only observation obtained from the source with the Rossi X-ray Timing Explorer. This detection makes IGR J17062−6143 the lowest-frequency accreting millisecond X-ray pulsar presently known. The pulsations are detected in the 2-12 keV band with an overall significance of 4.3 and an observed pulsed amplitude of 5.54% 0.67% (in this band). Both dynamic power spectral and coherent phase timing analysis indicate that the pulsation frequency is decreasing during the 1.2 ks observation in a manner consistent with orbital motion of the neutron star. Because the observation interval is short, we cannot precisely measure the orbital period; however, periods shorter than 17 minutes are excluded at 90% confidence. For the range of acceptable circular orbits the inferred binary mass function substantially overlaps the observed range for the AMXP population as a whole.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/aa5e51</identifier><language>eng</language><publisher>United States: The American Astronomical Society</publisher><subject>Accretion ; AMPLITUDES ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; Circular orbits ; DETECTION ; Intervals ; KEV RANGE ; MASS ; NEUTRON STARS ; ORBITS ; OSCILLATIONS ; PULSARS ; Pulsation ; PULSATIONS ; ROTATION ; stars: neutron ; stars: oscillations ; stars: rotation ; Time measurements ; X RADIATION ; X rays ; X-rays: binaries ; X-rays: individual (IGR J17062-6143)</subject><ispartof>Astrophysical journal. Letters, 2017-02, Vol.836 (2), p.L23-L23</ispartof><rights>2017. The American Astronomical Society. All rights reserved.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c513t-756be54247c7c9e38a3b03cda866d04a9760fc738b7283cf3f947b89055a1d73</citedby><cites>FETCH-LOGICAL-c513t-756be54247c7c9e38a3b03cda866d04a9760fc738b7283cf3f947b89055a1d73</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,780,784,885,27924,27925</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/22654537$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Strohmayer, Tod</creatorcontrib><creatorcontrib>Keek, Laurens</creatorcontrib><title>IGR J17062-6143 Is an Accreting Millisecond X-Ray Pulsar</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>We present the discovery of 163.65 Hz X-ray pulsations from IGR J17062−6143 in the only observation obtained from the source with the Rossi X-ray Timing Explorer. This detection makes IGR J17062−6143 the lowest-frequency accreting millisecond X-ray pulsar presently known. The pulsations are detected in the 2-12 keV band with an overall significance of 4.3 and an observed pulsed amplitude of 5.54% 0.67% (in this band). Both dynamic power spectral and coherent phase timing analysis indicate that the pulsation frequency is decreasing during the 1.2 ks observation in a manner consistent with orbital motion of the neutron star. Because the observation interval is short, we cannot precisely measure the orbital period; however, periods shorter than 17 minutes are excluded at 90% confidence. For the range of acceptable circular orbits the inferred binary mass function substantially overlaps the observed range for the AMXP population as a whole.</description><subject>Accretion</subject><subject>AMPLITUDES</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>Circular orbits</subject><subject>DETECTION</subject><subject>Intervals</subject><subject>KEV RANGE</subject><subject>MASS</subject><subject>NEUTRON STARS</subject><subject>ORBITS</subject><subject>OSCILLATIONS</subject><subject>PULSARS</subject><subject>Pulsation</subject><subject>PULSATIONS</subject><subject>ROTATION</subject><subject>stars: neutron</subject><subject>stars: oscillations</subject><subject>stars: rotation</subject><subject>Time measurements</subject><subject>X RADIATION</subject><subject>X rays</subject><subject>X-rays: binaries</subject><subject>X-rays: individual (IGR J17062-6143)</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNqNkE1Lw0AQhhdRsFbvHgOCeDB2d2e_ciyitVJRSg_els1moylpEneTQ_-9CZGeRDzNy_C8w_AgdEnwHSgmZxQzEitKYGYMd5wcoclhdXzImJ-isxC2GFMsiJogtVyso2cisaCxIAyiZYhMFc2t9a4tqo_opSjLIjhbV1n0Hq_NPnrrymD8OTrJTRncxc-cos3jw-b-KV69Lpb381VsOYE2llykjjPKpJU2caAMpBhsZpQQGWYmkQLnVoJKJVVgc8gTJlOVYM4NySRM0dV4tg5toYMtWmc_-2cqZ1tNqeCMw0DdjFTj66_OhVbvimBdWZrK1V3QRCWQYCqk-AcqpaKcEdKjeEStr0PwLteNL3bG7zXBepCuB6t6MKxH6X3ldqwUdaO3deer3s1f-PUvuGm2pVYgNNUrCrrJcvgGAWKKLQ</recordid><startdate>20170220</startdate><enddate>20170220</enddate><creator>Strohmayer, Tod</creator><creator>Keek, Laurens</creator><general>The American Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20170220</creationdate><title>IGR J17062-6143 Is an Accreting Millisecond X-Ray Pulsar</title><author>Strohmayer, Tod ; Keek, Laurens</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c513t-756be54247c7c9e38a3b03cda866d04a9760fc738b7283cf3f947b89055a1d73</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Accretion</topic><topic>AMPLITUDES</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>Circular orbits</topic><topic>DETECTION</topic><topic>Intervals</topic><topic>KEV RANGE</topic><topic>MASS</topic><topic>NEUTRON STARS</topic><topic>ORBITS</topic><topic>OSCILLATIONS</topic><topic>PULSARS</topic><topic>Pulsation</topic><topic>PULSATIONS</topic><topic>ROTATION</topic><topic>stars: neutron</topic><topic>stars: oscillations</topic><topic>stars: rotation</topic><topic>Time measurements</topic><topic>X RADIATION</topic><topic>X rays</topic><topic>X-rays: binaries</topic><topic>X-rays: individual (IGR J17062-6143)</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Strohmayer, Tod</creatorcontrib><creatorcontrib>Keek, Laurens</creatorcontrib><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><collection>OSTI.GOV</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Strohmayer, Tod</au><au>Keek, Laurens</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>IGR J17062-6143 Is an Accreting Millisecond X-Ray Pulsar</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2017-02-20</date><risdate>2017</risdate><volume>836</volume><issue>2</issue><spage>L23</spage><epage>L23</epage><pages>L23-L23</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>We present the discovery of 163.65 Hz X-ray pulsations from IGR J17062−6143 in the only observation obtained from the source with the Rossi X-ray Timing Explorer. This detection makes IGR J17062−6143 the lowest-frequency accreting millisecond X-ray pulsar presently known. The pulsations are detected in the 2-12 keV band with an overall significance of 4.3 and an observed pulsed amplitude of 5.54% 0.67% (in this band). Both dynamic power spectral and coherent phase timing analysis indicate that the pulsation frequency is decreasing during the 1.2 ks observation in a manner consistent with orbital motion of the neutron star. Because the observation interval is short, we cannot precisely measure the orbital period; however, periods shorter than 17 minutes are excluded at 90% confidence. For the range of acceptable circular orbits the inferred binary mass function substantially overlaps the observed range for the AMXP population as a whole.</abstract><cop>United States</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/aa5e51</doi><tpages>5</tpages><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 2041-8205
ispartof Astrophysical journal. Letters, 2017-02, Vol.836 (2), p.L23-L23
issn 2041-8205
2041-8213
language eng
recordid cdi_osti_scitechconnect_22654537
source EZB Electronic Journals Library
subjects Accretion
AMPLITUDES
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Circular orbits
DETECTION
Intervals
KEV RANGE
MASS
NEUTRON STARS
ORBITS
OSCILLATIONS
PULSARS
Pulsation
PULSATIONS
ROTATION
stars: neutron
stars: oscillations
stars: rotation
Time measurements
X RADIATION
X rays
X-rays: binaries
X-rays: individual (IGR J17062-6143)
title IGR J17062-6143 Is an Accreting Millisecond X-Ray Pulsar
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-07T13%3A37%3A32IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_osti_&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=IGR%20J17062-6143%20Is%20an%20Accreting%20Millisecond%20X-Ray%20Pulsar&rft.jtitle=Astrophysical%20journal.%20Letters&rft.au=Strohmayer,%20Tod&rft.date=2017-02-20&rft.volume=836&rft.issue=2&rft.spage=L23&rft.epage=L23&rft.pages=L23-L23&rft.issn=2041-8205&rft.eissn=2041-8213&rft_id=info:doi/10.3847/2041-8213/aa5e51&rft_dat=%3Cproquest_osti_%3E1893902676%3C/proquest_osti_%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c513t-756be54247c7c9e38a3b03cda866d04a9760fc738b7283cf3f947b89055a1d73%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=1877825411&rft_id=info:pmid/&rfr_iscdi=true