NuSTAR and NICER reveal IGR J17591–2342 as a new accreting millisecond X-ray pulsar

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Volume 617 (September 2018)

A&A, 617 (2018) L8

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Table 2.

Best-fit spectral parameters of IGR J17591–2342 with uncertainties at the 90% confidence level.

Parameter	Multiple^a	NICER-1,2^a	NICER-3,4^a
N_H (10²²cm⁻²)	3.6 ± 1.1
Γ	1.76 ± 0.02	1.83 ± 0.06	2.23 ± 0.05
kT_e (keV)		22(fixed)	22(fixed)
kT_BB (keV)	0.79 ± 0.09
r_bb (km/D_{10 kpc})²			<5 × 10³
E_Fe (keV)		6.35 ± 0.04	6.37 ± 0.10
N_Fe (10⁻⁵ ph s⁻¹ cm⁻²)	5.2 ± 1.8	3.8 ± 0.9	2.9 ± 1.6
Flux (1–10 keV)^b	^c2.0 ± 0.3	^d1.85 ± 0.09	^e
		^d	^e
Flux (3–20 keV)^b	2.41 ± 0.05	–	–
Flux (20–100 keV)^b		–	–
Flux (0.1–10 keV)^f	1.73	1.31^d	1.57^e
		0.78^d	1.61^e
/d.o.f.	1.09/473	1.11/377	1.13/1129

Notes.

^(a)

“Multiple” indicates the combined fit of the NuSTAR, IBIS/ISGRI, and Swift/XRT observations. NICER-1 and NICER-1,2 are the observations of 2018, August 15 and 18, and NICER-3,4 of August 23 and 24.

^(b)

The flux of the nthComp component is in units of 10⁻¹⁰ erg s⁻¹ cm⁻². The 3–20 and 20–100 keV nthcomp fluxes apply to NuSTAR and IBIS/ISGRI data, respectively. IBIS/ISGRI flux is higher than the others, since the data were obtained earlier, when the source was brighter.

^(c)

This flux applies to Swift/XRT data only.

^(d)

The upper and lower rows refer to the NICER-1 and 2 observations.

^(e)

The upper and lower rows refer to the NICER-3 and 4 observations.

^(f)

Extrapolated absorbed flux derived by the model in units of 10⁻¹⁰ erg s⁻¹ cm⁻². For the multiple observation, we extrapolated the NuSTAR spectrum.

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