RA (ICRS) DEC
|
ℓ b
|
Distance [kpc] | 1.72±0.1 | Gelino2006 |
---|---|---|
Distance to the plane (z) [kpc] | 1.52±0.09 | Gelino2006 |
Orbital period (Porb) [h] | 4.0784088±5E-07 | Torres2004GonzalezHernandez2014 |
Peak X-ray flux [erg s-1 cm-2] [keV] |
4.99E-10 [2-10] |
Brockshopp2010 |
Outburst magnitude (AB) | I=13.6±0.1 | Torres2002Zurita2005Hynes2000 |
Quiescent magnitude (AB) | i’=19.0±0.2 | Gelino2006Shahbaz2005 |
E(B-V) [mag] | 0.024 | Garcia2000 |
Dynamically confirmed BH
XTE J1118+480 showed an outburst in 2005 (Zurita2005). The peak X-ray flux is taken from that outburst (Brocksopp2010). Simon2020 detected another outburst ocurred in 1927 analysing photographic plates, also as a double event with a precursor similar to the outburst occurred in 2000. Gandhi2019 obtained a distance of 4.16+3.91-2.12 kpc from Gaia DR2. GonzalezHernandez2012 and GonzalezHernandez2014 reported a period derivative of -1.9±0.6 ms/yr |
Orbital period [h] | 4.0784088±5E-07 | Torres2004GonzalezHernandez2014 |
---|---|---|
Star's spectral type | K7 – M1V | Khargharia2013 |
Star's radial velocity amplitude (K2) [km/s] | 708.8±1.4 | GonzalezHernandez2008 |
Mass function 'f(M1)' [M☉] | 6.27±0.04 | GonzalezHernandez2008 |
BH mass (M1) [M☉] | 6.9 – 8.2 | Khargharia2013 |
Mass ratio (q=M2/M1) | 0.024±0.009 | Calvelo2009 |
Inclination angle (i) [deg] | 68 – 79 | Khargharia2013 |
Rot. broadening (v sini) [km/s] | 96+3-11 | Calvelo2009 |
|
|||
---|---|---|---|
V=13.0±0.3 | R=13.42±0.01 | I=13.6±0.1 | |
J=12.83±0.07 | |||
Gelino2006Shahbaz2005 |
|||
B=20.0 | V=19.61 | g'=21±0.3 | R=19.1 |
i’=19.0±0.2 | |||
J=18.6±0.1 | H=18.0±0.1 | Ks=18.5±0.1 |
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