Constraining the mass of the black hole GX 339-4 using spectro-temporal analysis of multiple outbursts. (arXiv:1811.04341v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+H%2E_S/0/1/0/all/0/1">Sreehari H.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iyer_N/0/1/0/all/0/1">Nirmal Iyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+D%2E_R/0/1/0/all/0/1">Radhika D.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nandi_A/0/1/0/all/0/1">Anuj Nandi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandal_S/0/1/0/all/0/1">Samir Mandal</a>
We carried out spectro-temporal analysis of the archived data from multiple
outbursts spanning over the last two decades from the black hole X-ray binary
GX 339-4. In this paper, the mass of the compact object in the X-ray binary
system GX 339-4 is constrained based on three indirect methods. The first
method uses broadband spectral modelling with a two component flow structure of
the accretion around the black hole. The broadband data are obtained from {it
RXTE (Rossi X-ray Timing Explorer)} in the range 3.0 to 150.0 keV and from {it
Swift} and {it NuSTAR (Nuclear Spectroscopic Telescope Array)} simultaneously
in the range 0.5 to 79.0 keV. In the second method, we model the time evolution
of Quasi-periodic Oscillation (QPO) frequencies, considering it to be the
result of an oscillating shock that radially propagates towards or away from
the compact object. The third method is based on scaling a mass dependent
parameter from an empirical model of the photon index ($Gamma$) – QPO ($nu$)
correlation. We compare the results at 90 percent confidence from the three
methods and summarize the mass estimate of the central object to be in the
range $8.28 – 11.89~ M_{odot}$.
We carried out spectro-temporal analysis of the archived data from multiple
outbursts spanning over the last two decades from the black hole X-ray binary
GX 339-4. In this paper, the mass of the compact object in the X-ray binary
system GX 339-4 is constrained based on three indirect methods. The first
method uses broadband spectral modelling with a two component flow structure of
the accretion around the black hole. The broadband data are obtained from {it
RXTE (Rossi X-ray Timing Explorer)} in the range 3.0 to 150.0 keV and from {it
Swift} and {it NuSTAR (Nuclear Spectroscopic Telescope Array)} simultaneously
in the range 0.5 to 79.0 keV. In the second method, we model the time evolution
of Quasi-periodic Oscillation (QPO) frequencies, considering it to be the
result of an oscillating shock that radially propagates towards or away from
the compact object. The third method is based on scaling a mass dependent
parameter from an empirical model of the photon index ($Gamma$) – QPO ($nu$)
correlation. We compare the results at 90 percent confidence from the three
methods and summarize the mass estimate of the central object to be in the
range $8.28 – 11.89~ M_{odot}$.
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