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http://hdl.handle.net/20.500.12386/32115
Titolo: | MAXI and NuSTAR Observations of the Faint X-Ray Transient MAXI J1848-015 in the GLIMPSE-C01 Cluster | Autori: | Pike, Sean N. Negoro, Hitoshi Tomsick, John A. BACHETTI, Matteo Brumback, McKinley Connors, Riley M.T. García, Javier A. Grefenstette, Brian Hare, Jeremy Harrison, Fiona A. Jaodand, Amruta Ludlam, R. M. MASTROSERIO, Guglielmo Mihara, Tatehiro Shidatsu, Megumi Sugizaki, Mutsumi Takagi, Ryohei |
Data pubblicazione: | 2022 | Rivista: | THE ASTROPHYSICAL JOURNAL | Numero: | 927 | Fascicolo: | 2 | Da pagina:: | 190 | Abstract: | We present the results of Monitor of All-sky X-ray Image (MAXI) monitoring and two Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the recently discovered faint X-ray transient MAXI J1848015. Analysis of the MAXI light curve shows that the source underwent a rapid flux increase beginning on 2020 December 20, followed by a rapid decrease in flux after only ∼5 days. NuSTAR observations reveal that the source transitioned from a bright soft state with unabsorbed, bolometric (0.1-100 keV) flux F = 6.9 ± 0.1 × 10-10 erg cm-2 s-1, to a low hard state with flux F = 2.85 ± 0.04 × 10-10 erg cm-2 s-1. Given a distance of 3.3 kpc, inferred via association of the source with the GLIMPSE-C01 cluster, these fluxes correspond to an Eddington fraction of the order of 10-3 for an accreting neutron star (NS) of mass M = 1.4M ⊙, or even lower for a more massive accretor. However, the source spectra exhibit strong relativistic reflection features, indicating the presence of an accretion disk that extends close to the accretor, for which we measure a high spin, a = 0.967 ± 0.013. In addition to a change in flux and spectral shape, we find evidence for other changes between the soft and hard states, including moderate disk truncation with the inner disk radius increasing from R in ≈ 3 R g to R in ≈ 8 R g, narrow Fe emission whose centroid decreases from 6.8 ± 0.1 keV to 6.3 ± 0.1 keV, and an increase in low-frequency (10-3-10-1 Hz) variability. Due to the high spin, we conclude that the source is likely to be a black hole rather than an NS, and we discuss physical interpretations of the low apparent luminosity as well as the narrow Fe emission. | URI: | http://hdl.handle.net/20.500.12386/32115 | URL: | https://api.elsevier.com/content/abstract/scopus_id/85126672845 https://iopscience.iop.org/article/10.3847/1538-4357/ac5258 |
ISSN: | 0004-637X | DOI: | 10.3847/1538-4357/ac5258 | Fulltext: | open |
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