2002/08/31 by J. M. Mïller, J. M. Miller, R. Wijnands +9 · 39 citations
Engineering · Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black-body radiation #Emission spectrum #Flux (metallurgy) #Mechanics and Biomechanics Studies #Millisecond #Millisecond pulsar #Neutron star #Optics #Physics #Power law #Pulsar #Pulsars and Gravitational Waves Research #Radiation #Spectral line #Spectroscopy #X-ray pulsar #astro-ph
paper · pdf · doi:10.1086/368105
published in The Astrophysical Journal 583(2), L99-L102 (IOP Publishing) · 5 pages, 3 figures (2 color). ApJ Letters, accepted. Uses emulateapj.sty
arxiv created 2003/01/17 · openalex publication_date 2003/01/17 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
We present an analysis of the first high-resolution spectra measured from an accretion-driven millisecond X-ray pulsar in outburst. We observed XTE J1751-305 with XMM-Newton on 2002 April 7 for approximately 35 ks. Using a simple absorbed blackbody plus power-law model, we measure an unabsorbed flux of (6.6 ± 0.1) × 10 -10 ergs cm -2 s -1 (0.5-10.0 keV). A hard power-law component (Γ = 1.44 ± 0.01) contributes 83% of the unabsorbed flux in the 0.5-10.0 keV band, but a blackbody component ( kT = 1.05 ± 0.01 keV) is required. We find no clear evidence for narrow or broad emission or absorption lines in the time-averaged spectra, and the sensitivity of this observation has allowed us to set constraining upper limits on the strength of important features. The lack of line features is at odds with spectra measured from some other X-ray binaries that share some similarities with XTE J1751-305. We discuss the implications of these findings on the accretion flow geometry in XTE J1751-305.