A new symbiotic low mass X-ray binary system: 4U 1954+319
4U 1954+319 was discovered 25 years ago, but only recently has a clear picture of its nature begun to emerge. We present for the first time a broad-band spectrum of the source and a detailed timing study using more than one year of monitoring data. The timing and spectral analysis was done using pub...
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| creator | Mattana, F Gotz, D Falanga, M Senziani, F De Luca, A Esposito, P Caraveo, P. A |
| description | 4U 1954+319 was discovered 25 years ago, but only recently has a clear
picture of its nature begun to emerge. We present for the first time a
broad-band spectrum of the source and a detailed timing study using more than
one year of monitoring data. The timing and spectral analysis was done using
publicly available Swift, INTEGRAL, BeppoSAX, and RXTE/ASM data in the 0.7-150
keV energy band. The source spectrum is described well by a highly absorbed
(N_H~10^23 cm^-2) power law with a high-energy exponential cutoff around 15
keV. An additional black body component is needed below 3 keV to account for a
soft excess. The derived ~5 hr periodicity, with a spin-up timescale of ~25
years, could be identified as the neutron star spin period. The spectral and
timing characteristics indicate that we are dealing both with the slowest
established wind-accreting X-ray pulsar and with the second confirmed member of
the emerging class dubbed "symbiotic low mass X-ray binaries" to host a neutron
star. |
| doi_str_mv | 10.48550/arxiv.astro-ph/0610158 |
| format | Article |
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picture of its nature begun to emerge. We present for the first time a
broad-band spectrum of the source and a detailed timing study using more than
one year of monitoring data. The timing and spectral analysis was done using
publicly available Swift, INTEGRAL, BeppoSAX, and RXTE/ASM data in the 0.7-150
keV energy band. The source spectrum is described well by a highly absorbed
(N_H~10^23 cm^-2) power law with a high-energy exponential cutoff around 15
keV. An additional black body component is needed below 3 keV to account for a
soft excess. The derived ~5 hr periodicity, with a spin-up timescale of ~25
years, could be identified as the neutron star spin period. The spectral and
timing characteristics indicate that we are dealing both with the slowest
established wind-accreting X-ray pulsar and with the second confirmed member of
the emerging class dubbed "symbiotic low mass X-ray binaries" to host a neutron
star.</description><identifier>DOI: 10.48550/arxiv.astro-ph/0610158</identifier><language>eng</language><subject>Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Earth and Planetary Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics</subject><creationdate>2006-10</creationdate><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,885</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/astro-ph/0610158$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.1051/0004-6361:20066154$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.astro-ph/0610158$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Mattana, F</creatorcontrib><creatorcontrib>Gotz, D</creatorcontrib><creatorcontrib>Falanga, M</creatorcontrib><creatorcontrib>Senziani, F</creatorcontrib><creatorcontrib>De Luca, A</creatorcontrib><creatorcontrib>Esposito, P</creatorcontrib><creatorcontrib>Caraveo, P. A</creatorcontrib><title>A new symbiotic low mass X-ray binary system: 4U 1954+319</title><description>4U 1954+319 was discovered 25 years ago, but only recently has a clear
picture of its nature begun to emerge. We present for the first time a
broad-band spectrum of the source and a detailed timing study using more than
one year of monitoring data. The timing and spectral analysis was done using
publicly available Swift, INTEGRAL, BeppoSAX, and RXTE/ASM data in the 0.7-150
keV energy band. The source spectrum is described well by a highly absorbed
(N_H~10^23 cm^-2) power law with a high-energy exponential cutoff around 15
keV. An additional black body component is needed below 3 keV to account for a
soft excess. The derived ~5 hr periodicity, with a spin-up timescale of ~25
years, could be identified as the neutron star spin period. The spectral and
timing characteristics indicate that we are dealing both with the slowest
established wind-accreting X-ray pulsar and with the second confirmed member of
the emerging class dubbed "symbiotic low mass X-ray binaries" to host a neutron
star.</description><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2006</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNpjYJA3NNAzsTA1NdBPLKrILNNLLC4pytctyNA3MDM0MDS14GSwdFTISy1XKK7MTcrML8lMVsjJL1fITSwuVojQLUqsVEjKzEssqgTKF5ek5lopmIQqGFqammgbG1ryMLCmJeYUp_JCaW4GVTfXEGcPXbBV8QVFmblAnfFgK-MLMuKhVhoTqw4AGhk6ag</recordid><startdate>20061005</startdate><enddate>20061005</enddate><creator>Mattana, F</creator><creator>Gotz, D</creator><creator>Falanga, M</creator><creator>Senziani, F</creator><creator>De Luca, A</creator><creator>Esposito, P</creator><creator>Caraveo, P. A</creator><scope>GOX</scope></search><sort><creationdate>20061005</creationdate><title>A new symbiotic low mass X-ray binary system: 4U 1954+319</title><author>Mattana, F ; Gotz, D ; Falanga, M ; Senziani, F ; De Luca, A ; Esposito, P ; Caraveo, P. A</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_astro_ph_06101583</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2006</creationdate><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><toplevel>online_resources</toplevel><creatorcontrib>Mattana, F</creatorcontrib><creatorcontrib>Gotz, D</creatorcontrib><creatorcontrib>Falanga, M</creatorcontrib><creatorcontrib>Senziani, F</creatorcontrib><creatorcontrib>De Luca, A</creatorcontrib><creatorcontrib>Esposito, P</creatorcontrib><creatorcontrib>Caraveo, P. A</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Mattana, F</au><au>Gotz, D</au><au>Falanga, M</au><au>Senziani, F</au><au>De Luca, A</au><au>Esposito, P</au><au>Caraveo, P. A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A new symbiotic low mass X-ray binary system: 4U 1954+319</atitle><date>2006-10-05</date><risdate>2006</risdate><abstract>4U 1954+319 was discovered 25 years ago, but only recently has a clear
picture of its nature begun to emerge. We present for the first time a
broad-band spectrum of the source and a detailed timing study using more than
one year of monitoring data. The timing and spectral analysis was done using
publicly available Swift, INTEGRAL, BeppoSAX, and RXTE/ASM data in the 0.7-150
keV energy band. The source spectrum is described well by a highly absorbed
(N_H~10^23 cm^-2) power law with a high-energy exponential cutoff around 15
keV. An additional black body component is needed below 3 keV to account for a
soft excess. The derived ~5 hr periodicity, with a spin-up timescale of ~25
years, could be identified as the neutron star spin period. The spectral and
timing characteristics indicate that we are dealing both with the slowest
established wind-accreting X-ray pulsar and with the second confirmed member of
the emerging class dubbed "symbiotic low mass X-ray binaries" to host a neutron
star.</abstract><doi>10.48550/arxiv.astro-ph/0610158</doi><oa>free_for_read</oa></addata></record> |
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| identifier | DOI: 10.48550/arxiv.astro-ph/0610158 |
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| subjects | Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics |
| title | A new symbiotic low mass X-ray binary system: 4U 1954+319 |
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