RA Dec
|
ℓ b
|
Location in Globular Cluster | ||
---|---|---|
Type of accretor | NS | Transient |
Distance [kpc] (other distances) |
<7 (H), <9.1 (He)
|
Galloway2020 Bhattacharyya2006 |
z [kpc] | -0.67 | Galloway2020 |
Orbital period (Porb) [min] | ||
Porb determination method | ||
Thermonuclear X-ray burst | Short-B | Emelyanov2001Bhattacharyya2006 |
Peak X-ray flux [erg s-1 cm-2] (2 - 10 keV) |
1.4E-9 | Gavriil2012 |
NH [x1022 cm-2] | 0.41±0.01 | Gavriil2012 |
E(B-V) [mag] | ||
Magnitude | ||
Proposed companion |
By measuring the spacing between two dip episodes observed by RXTE, Bhattacharyya2006 estimated an orbital period of 97±22 min. However, these dip episodes were separated by a data gap, thus not precluding a shorter period (Gavriil2012). The optical counterpart was identified during the 2004 outburst (Steeghs2004). Burst oscillations were detected at 530 Hz during the 2005 outburst (Bhattacharyya2006). The burst properties suggest H-poor fuel (Galloway2008). |
UV | ||
---|---|---|
Optical | ||
X-ray | Fe emission (~6 keV) and absorption (~8.4 keV) features Fe XXVI absorption line (6.96 keV) |
Bhattacharyya2006b Gavriil2012 |
|
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