An evolved donor star in the long-period cataclysmic variable HS 0218+3229

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Table 4:

Spectral classification and rotational broadening.
Template	Spectral	$v \sin i^{a}$ (km s^-1)	f	$\chi^2_{\nu}$	$v \sin i^{b}$ (km s^-1)
	type	( $\mu=0.5$ )		(d.o.f. = 496)	[ $\mu=0.0$ , $\mu$ at continuum]
HD10780	K0 V	$89.5 \pm 1.2$	$1.20 \pm 0.01$	2.1	[ $84.7 \pm 1.8$ , $91.4 \pm 2.0$ ]
HD10476	K1 V	$89.6 \pm 1.2$	$1.17 \pm 0.01$	1.8	[ $84.8 \pm 1.6$ , $91.2 \pm 4.3$ ]
HD16160	K3 V	$89.0 \pm 1.2$	$0.97 \pm 0.01$	1.0	[ $84.3 \pm 1.2$ , $91.1 \pm 1.3$ ]
HD 6660	K4 V	$87.7 \pm 1.2$	$0.728\pm 0.007$	1.0	[ $83.2 \pm 1.1$ , $90.0 \pm 1.1$ ]
HD10436	K5 V	$86.9 \pm 0.6$	$0.785 \pm 0.008$	0.9	[ $82.4 \pm 1.2$ , $89.4 \pm 1.3$ ]

^a Uncertainties are 1- $\sigma$ corresponding to $\chi^{2}_{\min}+1$ (Lampton et al. 1976); ^b uncertainties are 1- $\sigma$ and were estimated using the Monte-Carlo method by simulating a total of 1 000 000 copies of our target spectrum using the bootstrap technique outlined in Steeghs & Jonker (2007).

Source LaTeX | All tables | In the text

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