The double-peaked 2008 outburst of the accreting milli-second X-ray pulsar, IGR J00291+5934

F. Lewis; D. M. Russell; P. G. Jonker; M. Linares; V. Tudose; P. Roche; J. S. Clark; M. A. P. Torres; D. Maitra; C. G. Bassa; D. Steeghs; A. Patruno; S. Migliari; R. Wijnands; G. Nelemans; L. J. Kewley; V. E. Stroud; M. Modjaz; J. S. Bloom; C. H. Blake; D. Starr

doi:10.1051/0004-6361/201014382

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Volume 517 (July 2010)

A&A, 517 (2010) A72

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Table 8:

Spectra equivalent widths (Å).
Telescope	WHT	Keck I	Keck I
instrument	ISIS	LRIS	LRIS
Date	2004-12-05	2004-12-12	2008-08-28
H $\delta$ 4102	1.2 $\pm$ 0.4	-	-
H $\gamma$ 4341	1.7 $\pm$ 0.3	-	-
He II 4686	2.9 $\pm$ 0.2	0.6	-
H $\beta$ 4861	2.4 $\pm$ 0.3	5.4	-
H $\alpha$ 6563	6.5 $\pm$ 0.4	9.6	29.2 $\pm$ 1.7
He I 6678	-	1.0	-
Reference	1	2	3
R Mag	17.40	18.61	21.10
$L_{\rm X}$ (erg s^-1)	8.6 $\times$ 10³⁵	1.7 $\times$ 10³⁵	<2.6 $\times$ 10³²

Notes. 1 = Torres et al. (2008a), 2 = Reynolds et al. (2006) 3 = this paper. R-band magnitudes and X-ray luminosities are taken within one day of the optical spectra (Torres et al. 2008a, this paper). X-ray luminosities are from RXTE/PCA are based on a distance of 2.8 kpc as adopted in Sect. 10.3 of Torres et al. (2008a).

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