RA (ICRS) DEC
|
ℓ b
|
Distance [kpc] | ≥6 / >2.29 | Charles2019MataSanchez2015 |
---|---|---|
Distance to the plane (z) [kpc] | ≥4.6 / >1.8 | Charles2019MataSanchez2015 |
Orbital period (Porb) [h] | 2.8±0.3 | Corral-Santana2013MataSanchez2015 |
Peak X-ray flux [erg s-1 cm-2] [keV] |
2.23E-10 [2-10] |
ArmasPadilla2013 |
Outburst magnitude (AB) | r'=16.3±0.05 | Rau2011 |
Quiescent magnitude (AB) | r’=21.71±0.08 | Shahbaz2013MataSanchez2015ArmasPadilla2014a |
E(B-V) [mag] | 0.037 | Schlafly2011 |
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 J1357.2-0933: Strictly speaking is not a dynamical BH because it lacks a detection of the secondary star but it has a robust mass function determination (Corral-Santana2013,MataSanchez2015), also based on the FWHM(Hα) scaling from Casares2015 coupled with Porb (Corral-Santana2018,Mata-Sanchez2015). The distance is still uncertain (see Rau2011,Shahbaz2013,MataSanchez2015,Charles2019). It showed other outbursts in 2017 (Drake2017), 2019 (vanVelzen2019) and 2021 (Bellm2021) |
Orbital period [h] | 2.8±0.3 | Corral-Santana2013MataSanchez2015 |
---|---|---|
Star's spectral type | M2-4V | MataSanchez2015 |
Star's radial velocity amplitude (K2) [km/s] | 967±49 | MataSanchez2015 |
Mass function 'f(M1)' [M☉] | 11±2.1 | MataSanchez2015 |
BH mass (M1) [M☉] | 12.4±3.6 | MataSanchez2015Casares2016 |
Mass ratio (q=M2/M1) | ∼0.04 | MataSanchez2015Casares2016 |
Inclination angle (i) [deg] | ∼90 | Corral-Santana2013MataSanchez2015 |
|
|||
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r'=16.3±0.05 | |||
Shahbaz2013MataSanchez2015ArmasPadilla2014a |
|||
u'=23.12±0.04 | g'=22.29±0.08 | ||
r’=21.71±0.08 | i’=21.2±0.4 | ||
J=20.51±0.06 | H=20.07±0.05 | Ks=20.09±0.05 |
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Orientation: North up, East left.
Object marked
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Finding chart reference: Corral-Santana2013