Abstract
We report on the Swift monitoring of the candidate supergiant fast X-ray transient (SFXT) IGR J16418-4532, for which both orbital and spin periods are known (~3.7d and ~1250s, respectively). Our observations, for a total of ~43ks, span over three orbital periods and represent the most intense and complete sampling of the light curve of this source with a sensitive X-ray instrument. With this unique set of observations, we can address the nature of this transient. By applying the clumpy wind model for blue supergiants to the observed X-ray light curve, and assuming a circular orbit, the X-ray emission from this source can be explained in terms of the accretion from a spherically symmetric clumpy wind, composed of clumps with different masses, ranging from ~5 × 10 16 to 10 21g. Our data suggest, based on the X-ray behaviour, that this is an intermediate SFXT.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 2695-2702 |
| Number of pages | 8 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 419 |
| Issue number | 3 |
| DOIs | |
| State | Published - Jan 1 2012 |
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All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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Swift/X-ray Telescope monitoring of the candidate supergiant fast X-ray transient IGR J16418-4532. / Romano, P.; Mangano, V.; Ducci, L.; Esposito, P.; Evans, P. A.; Vercellone, S.; Kennea, J. A.; Burrows, D. N.; Gehrels, N.
In: Monthly Notices of the Royal Astronomical Society, Vol. 419, No. 3, 01.01.2012, p. 2695-2702.Research output: Contribution to journal › Article
TY - JOUR
T1 - Swift/X-ray Telescope monitoring of the candidate supergiant fast X-ray transient IGR J16418-4532
AU - Romano, P.
AU - Mangano, V.
AU - Ducci, L.
AU - Esposito, P.
AU - Evans, P. A.
AU - Vercellone, S.
AU - Kennea, J. A.
AU - Burrows, D. N.
AU - Gehrels, N.
PY - 2012/1/1
Y1 - 2012/1/1
N2 - We report on the Swift monitoring of the candidate supergiant fast X-ray transient (SFXT) IGR J16418-4532, for which both orbital and spin periods are known (~3.7d and ~1250s, respectively). Our observations, for a total of ~43ks, span over three orbital periods and represent the most intense and complete sampling of the light curve of this source with a sensitive X-ray instrument. With this unique set of observations, we can address the nature of this transient. By applying the clumpy wind model for blue supergiants to the observed X-ray light curve, and assuming a circular orbit, the X-ray emission from this source can be explained in terms of the accretion from a spherically symmetric clumpy wind, composed of clumps with different masses, ranging from ~5 × 10 16 to 10 21g. Our data suggest, based on the X-ray behaviour, that this is an intermediate SFXT.
AB - We report on the Swift monitoring of the candidate supergiant fast X-ray transient (SFXT) IGR J16418-4532, for which both orbital and spin periods are known (~3.7d and ~1250s, respectively). Our observations, for a total of ~43ks, span over three orbital periods and represent the most intense and complete sampling of the light curve of this source with a sensitive X-ray instrument. With this unique set of observations, we can address the nature of this transient. By applying the clumpy wind model for blue supergiants to the observed X-ray light curve, and assuming a circular orbit, the X-ray emission from this source can be explained in terms of the accretion from a spherically symmetric clumpy wind, composed of clumps with different masses, ranging from ~5 × 10 16 to 10 21g. Our data suggest, based on the X-ray behaviour, that this is an intermediate SFXT.
UR - http://www.scopus.com/inward/record.url?scp=84855355110&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84855355110&partnerID=8YFLogxK
U2 - 10.1111/j.1365-2966.2011.19916.x
DO - 10.1111/j.1365-2966.2011.19916.x
M3 - Article
AN - SCOPUS:84855355110
VL - 419
SP - 2695
EP - 2702
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 3
ER -