RA Dec
|
ℓ b
|
Location in Globular Cluster | NGC 6652 | |
---|---|---|
Type of accretor | NS | Transient |
Distance [kpc] (other distances) |
9.464
+0.139-0.137 |
Baumgardt2021 Kuulkers2003Harris2010Chelovekov2011 |
z [kpc] | -1.87 | Baumgardt2021 |
Orbital period (Porb) [min] | ||
Porb determination method | ||
Thermonuclear X-ray burst | Short-B | Intzand1998 |
Peak X-ray flux [erg s-1 cm-2] (2 - 10 keV) |
7.52E-13 | Stacey2012 |
NH [x1022 cm-2] | 0.05 | Coomber2011 |
E(B-V) [mag] | 0.09±0.01 | Harris2010 |
Magnitude | B = 20.4 | Deutsch1998 |
Proposed companion | - MS (not compatible with Porb) or degenerate (not compatible with colors). - Early to mid G-type star. (- Geometry and observed parameter's arguments. - Optical spectrum) |
Heinke2001 Paduano2021 |
NGC 6652 B can only be separated from NGC 6652 A (XB 1832-330) by Chandra; then, properties such as bursts and activity (transient or persistent), have to be considered carefully, since they could belong to either source. Deutsch1998 identified an optical counterpart with NGC 6652 A and Deutsch2000 estimated an orbital period of 43.6 (+/-0.6) min, based in optical modulation (HST). But later, Heinke2001 associated that counterpart with NGC 6652 B from Chandra data. Engel2012 obtained a light curve that shows a lot of flickering and suggested that the orbital period reported by Deutsch2000 is spurious (this was also suggested by Heinke2001). Radio flux density = 79.2 ± 2.2 μJy (10 GHz; Paduano2021). |
UV | ||
---|---|---|
Optical | H and He emission features (changing to absorption in ~2 hours), G-band, and metallic absorption lines (Fe, Mg, Na, O). | Paduano2021 |
X-ray |
|
|||
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B = 20.4, V > 17.7, I = 18.72 |