We report on a simultaneous Chandra and RossiXTE observation of the low-mass X-ray binary atoll bursting source MXB 1728-34 performed on 2002 March 3-5. We fit the 1.2-35 keV continuum spectrum with a blackbody plus a Comptonized component. Large residuals at 6-10 keV can be fitted by a broad ({FWHM} ≃ 2 keV) Gaussian emission line or, alternatively, by two absorption edges associated with lowly ionized iron and Fe XXV/XXVI at 7.1 keV and 9 keV, respectively. In this interpretation, we find no evidence of broad emission lines between 6 and 7 keV. We test our alternative model of the iron K shell region by reanalysing a previous BeppoSAX observation of MXB 1728-34, finding a general agreement with our new spectral model.

D'AI' A, DI SALVO T, IARIA R, MENDEZ M, BURDERI L, LAVAGETTO G, et al. (2006). The iron K-shell features of MXB 1728-34 from a simultaneous Chandra-RXTE observation. ASTRONOMY & ASTROPHYSICS, 448, 817-822 [10.1051/0004-6361:20053228].

The iron K-shell features of MXB 1728-34 from a simultaneous Chandra-RXTE observation

D'AI', Antonino;DI SALVO, Tiziana;IARIA, Rosario;LAVAGETTO, Giuseppe;
2006-01-01

Abstract

We report on a simultaneous Chandra and RossiXTE observation of the low-mass X-ray binary atoll bursting source MXB 1728-34 performed on 2002 March 3-5. We fit the 1.2-35 keV continuum spectrum with a blackbody plus a Comptonized component. Large residuals at 6-10 keV can be fitted by a broad ({FWHM} ≃ 2 keV) Gaussian emission line or, alternatively, by two absorption edges associated with lowly ionized iron and Fe XXV/XXVI at 7.1 keV and 9 keV, respectively. In this interpretation, we find no evidence of broad emission lines between 6 and 7 keV. We test our alternative model of the iron K shell region by reanalysing a previous BeppoSAX observation of MXB 1728-34, finding a general agreement with our new spectral model.
D'AI' A, DI SALVO T, IARIA R, MENDEZ M, BURDERI L, LAVAGETTO G, et al. (2006). The iron K-shell features of MXB 1728-34 from a simultaneous Chandra-RXTE observation. ASTRONOMY & ASTROPHYSICS, 448, 817-822 [10.1051/0004-6361:20053228].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10447/12875
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