Enrico Bozzo, V. Bhalerao, Prajal Pradhan, J. Tomsick, Patrizia Romano, Carlo Ferrigno, S. Chaty, Lida Oskinova, A. Manousakis, R. Walter, M. Falanga, S. Campana, L. Stella, M. Ramolla, R. Chini
- In this paper we report on a long multi-wavelength observational campaign of the supergiant fast X-ray transient prototype IGR J17544-2619. A 150 ks-long observation was carried out simultaneously with XMM-Newton and NuSTAR, catching the source in an initial faint X-ray state and then undergoing a bright X-ray outburst lasting approximately 7 ks. We studied the spectral variability during outburst and quiescence by using a thermal and bulk Comptonization model that is typically adopted to describe the X-ray spectral energy distribution of young pulsars in high mass X-ray binaries. Although the statistics of the collected X-ray data were relatively high, we could neither confirm the presence of a cyclotron line in the broad-band spectrum of the source (0.5-40 keV), nor detect any of the previously reported tentative detections of the source spin period. The monitoring carried out with Swift/XRT during the same orbit of the system observed by XMM-Newton and NuSTAR revealed that the source remained in a low emission state for most of theIn this paper we report on a long multi-wavelength observational campaign of the supergiant fast X-ray transient prototype IGR J17544-2619. A 150 ks-long observation was carried out simultaneously with XMM-Newton and NuSTAR, catching the source in an initial faint X-ray state and then undergoing a bright X-ray outburst lasting approximately 7 ks. We studied the spectral variability during outburst and quiescence by using a thermal and bulk Comptonization model that is typically adopted to describe the X-ray spectral energy distribution of young pulsars in high mass X-ray binaries. Although the statistics of the collected X-ray data were relatively high, we could neither confirm the presence of a cyclotron line in the broad-band spectrum of the source (0.5-40 keV), nor detect any of the previously reported tentative detections of the source spin period. The monitoring carried out with Swift/XRT during the same orbit of the system observed by XMM-Newton and NuSTAR revealed that the source remained in a low emission state for most of the time, in agreement with the known property of all supergiant fast X-ray transients being significantly sub-luminous compared to other supergiant X-ray binaries. Optical and infrared observations were carried out for a total of a few thousand seconds during the quiescence state of the source detected by XMM-Newton and NuSTAR. The measured optical and infrared magnitudes were slightly lower than previous values reported in the literature, but compatible with the known micro-variability of supergiant stars. UV observations obtained with the UVOT telescope on-board Swift did not reveal significant changes in the magnitude of the source in this energy domain compared to previously reported values.…
MetadatenAuthor details: | Enrico BozzoORCiD, V. Bhalerao, Prajal PradhanORCiDGND, J. Tomsick, Patrizia RomanoORCiD, Carlo FerrignoORCiD, S. Chaty, Lida OskinovaORCiDGND, A. Manousakis, R. Walter, M. Falanga, S. Campana, L. Stella, M. Ramolla, R. Chini |
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DOI: | https://doi.org/10.1051/0004-6361/201629311 |
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ISSN: | 1432-0746 |
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Title of parent work (English): | Journal of geophysical research : Earth surface |
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Publisher: | EDP Sciences |
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Place of publishing: | Les Ulis |
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Publication type: | Article |
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Language: | English |
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Year of first publication: | 2016 |
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Publication year: | 2016 |
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Release date: | 2020/03/22 |
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Tag: | X-rays: binaries |
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Volume: | 596 |
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Number of pages: | 12 |
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Funding institution: | NASA [NNG08FD60C]; National Aeronautics and Space Administration; International Space Science Institute in Bern, Switzerland; ISSI; Polish ESA Member States; [ASI-INAFI/004/11/0]; [ASI-INAFI/037/12/0] |
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Organizational units: | Mathematisch-Naturwissenschaftliche Fakultät / Institut für Physik und Astronomie |
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Peer review: | Referiert |
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