The first outburst of the black-hole candidate MAXI J1836−194 observed by INTEGRAL, Swift, and RXTE

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Volume 537 (January 2012)

A&A, 537 (2012) L7

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Table 1

Quasi-simultaneous Swift /XRT, JEM-X, and IBIS/ISGRI spectral fits.

Data^a	Exposures^b			N_H	Γ	k T_BB		Flux^c			/d.o.f.
	(ks)			(×10²² cm^-2)		(keV)	∝ R_in	(×10^-9 erg cm^-2 s^-1)
	XRT	JEM-X	ISGRI					Bol	2–10 keV	20–100 keV

1088+09	1.5	–	8.6	0.31 ± 0.01	2.2 ± 0.1	0.38 ± 0.01	1.0 ± 0.3	12.1	1.6	0.7	1.13/397
1090+13	0.7	18.0	56.5	0.33 ± 0.01	2.24 ± 0.03	0.37 ± 0.01	1.0	10.6	1.3	0.6	0.99/329
1093+17	0.7	–	8.2	0.24 ± 0.01	1.95 ± 0.04	0.28 ± 0.02	1.1	6.6	0.8	0.9	0.98/239
1094+19	1.0	12.0	67.7	0.23 ± 0.02	1.91 ± 0.02	0.21 ± 0.02	1.3	4.8	0.6	0.8	0.98/287
1095+20	0.6	–	13.2	0.27 ± 0.01	1.84 ± 0.05	0.21 ± 0.04	1.4	5.7	0.7	1.0	0.92/202
1097+23	1.0	–	9.9	0.33	1.85 ± 0.06	0.18 ± 0.03	2	4.2	0.5	0.7	0.94/205
1099+26	1.0	–	10.2	0.26 ± 0.07	1.5 ± 0.1 (E_c > 53 keV)^d	0.25 ± 0.06	0.6	2.9	0.4	0.9	0.90/166

Notes.

^(a)

Indicates the INTEGRAL revolution + the latest two digits XX of the Swift observation 000320870XX.

^(b)

Effective exposure time of XRT, JEM-X (both units), and ISGRI, respectively.

^(c)

Unabsorbed fluxes. “Bol” indicates the model flux in the 0.1–200 keV energy range.

^(d)

This spectrum is modeled by a cut-off power-law with E_c = 150 keV.

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