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Title:
The Dust-scattering X-ray Rings of the Anomalous X-ray Pulsar 1E 1547.0-5408
Authors:
Tiengo, A.; Vianello, G.; Esposito, P.; Mereghetti, S.; Giuliani, A.; Costantini, E.; Israel, G. L.; Stella, L.; Turolla, R.; Zane, S.; Rea, N.; Götz, D.; Bernardini, F.; Moretti, A.; Romano, P.; Ehle, M.; Gehrels, N.
Affiliation:
AA(INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica-Milano, via E. Bassini 15, 20133 Milano, Italy ), AB(INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica-Milano, via E. Bassini 15, 20133 Milano, Italy ), AC(INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica-Milano, via E. Bassini 15, 20133 Milano, Italy ; INFN—Istituto Nazionale di Fisica Nucleare, Sezione di Pavia, via A. Bassi 6, 27100 Pavia, Italy ), AD(INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica-Milano, via E. Bassini 15, 20133 Milano, Italy ), AE(INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica-Milano, via E. Bassini 15, 20133 Milano, Italy ), AF(SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands ), AG(INAF/Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone, Italy ), AH(INAF/Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone, Italy ), AI(Università degli Studi di Padova, Dipartimento di Fisica, via F. Marzolo 8, 35131 Padova, Italy ; University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK ), AJ(University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK ), AK(Institut de Ciències de l'Espai (CSIC-IEEC), Campus UAB, Facultat de Ciències, Torre C5-parell, 08193 Barcelona, Spain ; Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands ), AL(CEA Saclay, DSM/Irfu/Service d'Astrophysique, Orme des Merisiers, Bât. 709, 91191 Gif-sur-Yvette, France ), AM(INAF/Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone, Italy ), AN(INAF/Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate, Italy ), AO(INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica-Palermo, via U. La Malfa 153, 90146 Palermo, Italy ), AP( XMM-Newton Science Operations Centre, ESAC, ESA, P.O. Box 78, 28691 Villanueva de la Cañada, Spain ), AQ(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA)
Publication:
The Astrophysical Journal, Volume 710, Issue 1, pp. 227-235 (2010). (ApJ Homepage)
Publication Date:
02/2010
Origin:
IOP
ApJ Keywords:
dust, extinction, stars: neutron, X-rays: individual: 1E 1547.0-5408, X-rays: stars
DOI:
10.1088/0004-637X/710/1/227
Bibliographic Code:
2010ApJ...710..227T

Abstract

On 2009 January 22 numerous strong bursts were detected from the anomalous X-ray pulsar 1E 1547.0-5408. Swift/XRT and XMM-Newton/EPIC observations carried out in the following two weeks led to the discovery of three X-ray rings centered on this source. The ring radii increased with time following the expansion law expected for a short impulse of X-rays scattered by three dust clouds. Assuming different models for the dust composition and grain size distribution, we fit the intensity decay of each ring as a function of time at different energies, obtaining tight constraints on the distance of the X-ray source. Although the distance strongly depends on the adopted dust model, we find that some models are incompatible with our X-ray data, restricting to 4-8 kpc the range of possible distances for 1E 1547.0-5408. The best-fitting dust model provides a source distance of 3.91 ± 0.07 kpc, which is compatible with the proposed association with the supernova remnant G327.24-0.13, and implies distances of 2.2 kpc, 2.6 kpc and 3.4 kpc for the dust clouds, in good agreement with the dust distribution inferred by CO line observations toward 1E 1547.0-5408. However, dust distances in agreement with CO data are also obtained for a set of similarly well-fitting models that imply a source distance of ~5 kpc. A distance of ~4-5 kpc is also favored by the fact that these dust models are already known to provide good fits to the dust-scattering halos of bright X-ray binaries. Assuming N H = 1022 cm–2 in the dust cloud responsible for the brightest ring and a bremsstrahlung spectrum with kT = 100 keV, we estimate that the burst producing the X-ray ring released an energy of 1044-1045 erg in the 1-100 keV band, suggesting that this burst was the brightest flare without any long-lasting pulsating tail ever detected from a magnetar.
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