γ Cassiopeiae: an X-ray Be star with personality | Astronomy & Astrophysics (A&A)

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Table 3:

Parameters of the strongest emission lines.
	$\lambda_{\rm C}$	EW	Flux^a
	(Å)	(mÅ)	( $\times$ 10^-4)
Ne X Ly $\alpha$ ^c	12.131[11]	125[18]	2.15[31]	(1.26 $\pm$ 0.16)
O VIII Ly $\beta$ ^c	15.997[41]	40[14]	0.55[20]	(0.31 $\pm$ 0.16)
O VIII Ly $\alpha$ ^c	18.9796[49]	360[28]	3.93[31]	(1.71 $\pm$ 0.26)
O VII r^b	21.60[90]	163[19]	1.72[20]	(0.77 $\pm$ 0.28)
O VII i^b	21.78[92]	149[19]	1.58[20]	(0.79 $\pm$ 0.40)
O VII f^b	22.097^d	<32	<0.3	(0.13 $\pm$ 0.16)
N VII Ly $\alpha$ ^c	24.79[99]	296[17]	2.76[16]	(0.61 $\pm$ 0.03)
N VI r^c	28.81[90]	<230	<2	...
N VI i^c	29.09[95]	<169	<1.4	...
N VI f^c	29.531^d	<10	<0.08	...
C VI Ly $\alpha$ ^d	33.736[64]	201[29]	1.37[20]	...

Notes. ^(a) Total flux in line, in units of photons cm^-2 s^-1; in parenthesis are shown the values derived by Smith et al. (2004) from Chandra. ^(b) From RGS1. ^(c) From RGS2. ^(d) Frozen parameter. Quoted errors are at 90% confidence level.

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