RA (ICRS) DEC
|
ℓ b
|
Distance [kpc] | 8.6±3.7 | Kuulkers2013 |
---|---|---|
Distance to the plane (z) [kpc] | 2.45±1.05 | Kuulkers2013 |
Orbital period (Porb) [h] | 2.414±0.005 | Kuulkers2013Corral-Santana2018 |
Peak X-ray flux [erg s-1 cm-2] [keV] |
6.80E-09 [2-10] |
Munoz-Darias2011 |
Outburst magnitude (AB) | v=16.5 | Russell2010Kennea2011 |
Quiescent magnitude (AB) | r’=24.20±0.08 | Corral-Santana2018 |
E(B-V) [mag] | 0.34 | DAvanzo2010 |
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
MAXI J1659-152: Strictly speaking is not a dynamical BH because it lacks a detection of the secondary star. However, the FWHM(Hα) scaling from Casares2015 coupled with knowledge of the orbital period (Kuulkers2013,Corral-Santana2018) strongly indicates so. In addition, Yamaoka2012 also suggested a BH from the study of X-ray spectral and timing properties. This values should be taken with caution. |
Orbital period [h] | 2.414±0.005 | Kuulkers2013Corral-Santana2018 |
---|---|---|
Star's spectral type | ~M5V | Kuulkers2013Corral-Santana2018 |
Star's radial velocity amplitude (K2) [km/s] | ||
Mass function 'f(M1)' [M☉] | ||
BH mass (M1) [M☉] | Yamaoka2012 | |
Mass ratio (q=M2/M1) | ||
Inclination angle (i) [deg] | ∼70±10 | Kuulkers2013 |
|
|||
---|---|---|---|
V=16.76 | v=16.5 | ||
Corral-Santana2018 |
|||
r’=24.20±0.08 | I=23.63±0.02 | ||
H=22.1±0.1 |
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Orientation: North up, East left.
Object marked
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Finding chart reference: Corral-Santana2018
r'C1=16.065±0.005 | i'C1=15.21±0.06 |
r'C2=17.069±0.006 | i'C2=16.31±0.06 |
r'C3=18.795±0.006 | i'C3=17.86±0.06 |
r'C4=20.240±0.006 | i'C4=19.54±0.06 |
r'C5=18.256±0.008 | i'C5=17.54±0.06 |
r'C6=18.332±0.006 | i'C6=17.35±0.06 |
r'D1=18.450±0.006 | i'D1=17.72±0.06 |
r'D2=17.629±0.006 | i'D2=16.83±0.06 |
r'D3=19.023±0.006 | i'D3=18.27±0.06 |
r'D4=17.877±0.006 | i'D4=17.13±0.06 |
r'D5=17.532±0.006 | i'D5=16.82±0.06 |
r'D7=20.085±0.006 | i'D7=19.35±0.06 |
r'D8=19.407±0.005 | i'D8=18.66±0.06 |