RA [J2000] DEC
|Distance to the plane (z) [kpc]||∼1.3±0.4||CadolleBel2007|
|Orbital period (Porb) [h]||3.244±0.001||Zurita2008|
|Peak X-ray flux [erg s-1 cm-2]
|Outburst magnitude (AB)||R∼15.85||Halpern2005|
|Quiescent magnitude (AB)||V>21.0||CadolleBel2007|
Strictly speaking it is not a dynamical BH but there is either a robust mass function or mass determination suggesting the presence of a BH
|Swift J1753.5-0127 remained in a low/hard X-ray state since its outburst in 2005 until 2016. In June 2015, it reached its lowest flux since its outburst ( Neustroev2015 ). After 11 years in outburst, it started to decay towards its quiescent state around September 2016 ( Russell2016 ). By early November 2016, the source was not detected in X-rays by Swift ( Shaw2016a ).
There is a discrepance between the K2,Porb and M1 measured by Neustroev2014 and Shaw2016 .
The FWHM(Hα) scaling ( Casares2015 ) coupled with the Porb ( Zurita2008 ) strongly indicates a BH ( Shaw2016 ).
Gandhi2019 obtained a distance of 7.15+3.99-2.48 kpc from Gaia DR2.
|Orbital period [h]||3.244±0.001||Zurita2008|
|Star's spectral type||>M2||Zurita2008|
|Star's radial velocity amplitude (K2) [km/s]||>808±76||Shaw2016|
|Mass function 'f(M1)' [M☉]||0.69±0.04||Neustroev2014|
|BH mass (M1) [M☉]||>7.4±1.2||Shaw2016|
|Mass ratio (q=M2/M1)||≥0.04±0.03||Neustroev2014|
|Inclination angle (i) [deg]||≥40||Neustroev2014|
|Rot. broadening (v sini) [km/s]|
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