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Home All issues Volume 496 / No 1 (March II 2009) A&A, 496 1 (2009) 121-127 Full HTML
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Table 2:

Detected IPs with masses from XSPEC fit with the model from Suleimanov et al. (2005). The temperature is from a bremsstrahlung fit, and is provided for comparison.
Name kT        Mass F14-195    DistanceA L14-195 $\dot{M}$ $\chi^2_{\rm red}$
  (keV)      ($M_{\odot }$) (10-11 erg/cm2/s)   (pc) (1032 erg/s) (1016 g/s)  
FO Aqr 15.2 $\pm$ 1.6 0.61 $\pm$ 0.05 4.7 $\pm$ 0.5 4001 9.00 29.0 1.4
XY Ari 29.1 $\pm$ 6.2 0.96 $\pm$ 0.12 2.3 $\pm$ 0.4 2702 2.01 2.8 1.3
V405 Aur 22.1 $\pm$ 4.2 0.89 $\pm$ 0.13C 2.2 $\pm$ 0.5 - -   0.5
MU Cam 19.6 $\pm$ 4.7 0.74 $\pm$ 0.13 1.3 $\pm$ 0.3 - -   1.7
V709 Cas 30.0 $\pm$ 2.5 0.96 $\pm$ 0.05C 7.2 $\pm$ 0.6 - -   1.0
V1025 Cen 10.8 $\pm$ 7.7 0.46 $\pm$ 0.31 0.4 $\pm$ 0.3 - -   0.6
BG CMi 18.9 $\pm$ 5.5 0.67 $\pm$ 0.19 2.0 $\pm$ 0.4 7003 11.73 32.3 0.7
TV Col 21.6 $\pm$ 2.4 0.78 $\pm$ 0.06 5.0 $\pm$ 0.5 3864 8.92 18.8 0.9
TX Col 17.0 $\pm$ 3.2 0.67 $\pm$ 0.10 1.7 $\pm$ 0.3 5505 6.15 16.9 0.7
V2306 Cyg 20.5 $\pm$ 5.7 0.77 $\pm$ 0.16 1.2 $\pm$ 0.3 - -   1.0
DO Dra 12.0 $\pm$ 2.6 0.50 $\pm$ 0.11C 1.0 $\pm$ 0.3 1556 0.29 1.3 0.7
PQ Gem 16.8 $\pm$ 2.8 0.65 $\pm$ 0.09 2.5 $\pm$ 0.4 - -   1.0
EX Hya 19.4 $\pm$ 4.4 0.66 $\pm$ 0.17 2.1 $\pm$ 0.5 64.57 0.10 0.28 0.4
NY Lup 39.1 $\pm$ 4.3 1.09 $\pm$ 0.07 7.1 $\pm$ 0.6 6908 40.45 25.3 1.1
V2400 Oph 21.1 $\pm$ 2.8 0.81 $\pm$ 0.10 4.3 $\pm$ 0.6 - -   1.0
GK Per 26.2 $\pm$ 5.4 0.90 $\pm$ 0.12B,C$\!\!$ 2.8 $\pm$ 0.5 3409 10.24 16.2 0.8
AO Psc 13.1 $\pm$ 1.9 0.55 $\pm$ 0.06 2.8 $\pm$ 0.4 42010 10.13 38.6 0.7
V1223 Sgr 17.0 $\pm$ 1.3 0.65 $\pm$ 0.04 8.5 $\pm$ 0.8 52711 28.25 82.0 1.0
V1062 Tau 18.3 $\pm$ 5.8 0.72 $\pm$ 0.17 1.6 $\pm$ 0.4 50012 4.79 11.6 0.4
RX J2133 27.1 $\pm$ 2.9 0.91 $\pm$ 0.06 4.6 $\pm$ 0.4 >60013 -   0.6
Swift J0713 21.7 $\pm$ 4.1 0.79 $\pm$ 0.11 2.5 $\pm$ 0.4 - -   0.9
IGR J00234 $\rm 22.8^{+30.0}_{-11.5}$ 0.85 $\pm$ 0.39 0.7 $\pm$ 0.3 - -   0.8
IGR J17303 37.1 $\pm$ 4.4 1.08 $\pm$ 0.07 6.6 $\pm$ 0.6 - -   1.1
A References to the distances: 1. McHardy et al. (1987); 2. Littlefair et al. (2001); 3. Berriman (1987); 4. McArthur et al. (2001); 5. Buckley & Tuohy (1989); 6. Mateo et al. (1991); 7. Beuermann et al. (2003); 8. de Martino et al. (2006); 9. Warner (1987); 10. Hellier et al. (1991); 11. Beuermann et al. (2004); 12. Szkody & Silber (1996); 13 Bonnet-Bidaud et al. (2006).
B All numbers correspond to the measured spectrum during the low-flux period; but see Sect. 3.2.
C The derived mass is likely a lower limit due to the fast rotation of the WD; see Sect. 3.1.

Source LaTeX | All tables | In the text

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