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Table 9

Observed and derived parameters of X-ray detected optical novae in M 31.

Optical measurements X-ray measurements Derived parameters

Namea Brightnessb t2Rc SSS phase LXd k TBBe Ejected mass Burned mass
M31N (mag Filter) (d) Turn on (d) Turn off (d) (1036 erg s-1) (eV) (10-5M) (10-6M)

1995-09b 15.6(Hα) 1653 ± 81 3656 ± 273 16.1 ± 3.6 6.1 ± 0.5
1995-11c 16.3(Hα) 762 ± 725 3609 ± 236 13.8 ± 3.3 6.0 ± 0.4
1996-08b 16.1(Hα) 1831 ± 49  > 3829 5.6 ± 1.0  > 6.4
1997-11a 18.0(R) 2027 ± 566  > 3418 9.5 ± 1.4  > 5.7
1999-10a 17.5(W) 357 ± 496 2203 ± 234 21.2 ± 1.6 3.7 ± 0.4
2000-07a 16.8(R) 22.4 162 ± 8 1904 ± 236 13.4 ± 0.7 6.7 ± 0.7 3.2 ± 0.4
2001-01a 17.1(R)  < 1990  > 2317 2.4 ± 0.5  < 1016  > 3.9
2001-10a 17.0(R) 39.3 1089 ± 70  > 1985 12.0 ± 2.0  > 3.3
2003-11a 16.9(R) 22.0 327 ± 70 709 ± 235 27.6 ± 1.8 1.2 ± 0.4
2003-11b 17.4(R) 42.2 302 ± 70 684 ± 235 10.4 ± 1.3 1.1 ± 0.4
2004-05b 17.2(R) 49.7 213 ± 11  > 1028 45.8 ± 5.4 11.7 ± 1.2  > 1.72
2004-06c 17.1(R) 10.9 94 ± 70 476 ± 234 33.9 ± 2.0 0.8 ± 0.4
2004-11b+ 16.6(R) 32.0 68 ± 16 343 ± 235 16.2 ± 1.6 0.6 ± 0.4
2004-11g 18.0(R) 28.4 16 ± 16 343 ± 235 82.1 ± 3.0 0.6 ± 0.4
2004-11e 17.6(R) 34.6 44 ± 16 319 ± 235 35.9 ± 4.0 0.5 ± 0.4
2005-02a 17.7(W) 236 ± 236  > 751 56.4 ± 4.9  > 1.25
2006-04a 15.9(W) 86 ± 19 132 ± 27 48.9 ± 2.0 0.22 ± 0.05
2006-06a∗+ 17.6(R) 106 ± 26 200 ± 25 10.3 ± 2.1 0.33 ± 0.04

Notes.

(a)

indicates novae with parameters mainly from this paper while the remaining objects are from PHS2007 (their Table 8) and we give updated turn-off times, ejected masses and burned masses, + indicates novae confirmed by optical spectra;

(b)

maximum observed magnitude (not necessarily peak magnitude), “W” indicates unfiltered magnitude;

(c)

time in days the nova R magnitude needs to drop 2 mag below peak magnitude (see Payne-Gaposchkin 1964);

(d)

unabsorbed luminosity in 0.2–1.0 keV band in units of 1036 erg s-1 during observed maximum X-ray brightness assuming a 50 eV blackbody spectrum with Galactic foreground absorption;

(e)

blackbody temperature from spectral fit.

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