2014A&A...566A.131G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST06:52:45

2014A&A...566A.131G - Astronomy and Astrophysics, volume 566A, 131-131 (2014/6-1)

Astrophysical parameters and orbital solution of the peculiar X-ray transient IGR J00370+6122.

GONZALEZ-GALAN A., NEGUERUELA I., CASTRO N., SIMON-DIAZ S., LORENZO J. and VILARDELL F.

Abstract (from CDS):

BD +60°73 is the optical counterpart of the X-ray source IGR J00370+6122, a probable accretion-powered X-ray pulsar. The X-ray light curve of this binary system shows clear periodicity at 15.7d, which has been interpreted as repeated outbursts around the periastron of an eccentric orbit. We aim to characterise the binary system IGR J00370+6122 by deriving its orbital and physical parameters. We obtained high-resolution spectra of BD +60°73 at different epochs. We used the fastwind code to generate a stellar atmosphere model to fit the observed spectrum and obtain physical magnitudes. The synthetic spectrum was used as a template for cross-correlation with the observed spectra to measure radial velocities. The radial velocity curve provided an orbital solution for the system. We also analysed the RXTE/ASM and Swift/BAT light curves to confirm the stability of the periodicity. BD +60°73 is a BN0.7Ib low-luminosity supergiant located at a distance ∼3.1kpc, in the Cas OB4 association. We derive Teff=24000K and loggc=3.0, and chemical abundances consistent with a moderately high level of evolution. The spectroscopic and evolutionary masses are consistent at the 1-σ level with a mass M*≃15M. The recurrence time of the X-ray flares is the orbital period of the system. The neutron star is in a high-eccentricity (e=0.56±0.07) orbit, and the X-ray emission is strongly peaked around orbital phase φ=0.2, though the observations are consistent with some level of X-ray activity happening at all orbital phases. The X-ray behaviour of IGR J00370+6122 is reminiscent of ``intermediate'' supergiant X-ray transients, though its peak luminosity is rather low. The orbit is somewhat wider than those of classical persistent supergiant X-ray binaries, which when combined with the low luminosity of the mass donor, explains the low X-ray luminosity. IGR J00370+6122 will very likely evolve towards a persistent supergiant system, highlighting the evolutionary connection between different classes of wind-accreting X-ray sources.

Abstract Copyright:

Journal keyword(s): binaries: close - stars: evolution - stars: individual: IGR J00370+6122 - pulsars: general - supergiants - X-rays: stars

Simbad objects: 32

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Number of rows : 32

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SH 2-172 HII 00 15 29.1 +61 14 41           ~ 24 0
2 HD 1544 * 00 20 05.5412170692 +62 03 58.697659878 7.51 8.28 8.12     B0.5III(n) 60 0
3 LBN 119.57-00.92 HII 00 21 16 +61 43.5           ~ 36 0
4 Ass Cas OB 4 As* 00 27 +62.4           ~ 41 0
5 SH 2-175 HII 00 27 17.00 +64 42 23.3   12.26 11.37     ~ 40 1
6 SH 2-177 HII 00 31.5 +62 28           ~ 23 0
7 * kap Cas s*b 00 32 59.9911963 +62 55 54.417374 3.50 4.30 4.16 4.02 3.96 B1Ia 445 0
8 BD+60 73 HXB 00 37 09.6358465128 +61 21 36.485521705 9.79 10.14 9.66     B1Ib 62 0
9 BD+63 70 * 00 40 44.5926887855 +63 55 00.029235995 9.52 9.79 9.22     B0Ib 23 0
10 SK 160 HXB 01 17 05.1447530244 -73 26 36.015353425 12.23 13.00 13.15   13.17 O9.7Ia+ 798 0
11 V* V662 Cas HXB 01 18 02.6973905772 +65 17 29.829417242 12.27 11.99 11.14 10.33 9.58 B1Iae 231 0
12 NAME Per Arm PoG 03 30 +45.0           ~ 1247 0
13 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
14 RX J0535.6-6651 HXB 05 35 40.9965654015 -66 51 53.522991468   13.7 13.8     B0.5IIIe 279 0
15 HD 47240 Pu* 06 37 52.7036331811 +04 57 24.007346108 5.65 6.35 6.20 5.98 5.87 B1Ib 149 0
16 V* GP Vel HXB 09 02 06.8610736194 -40 33 16.896402010 6.85 7.37 6.87 6.31 6.05 B0.5Ia 1373 0
17 HD 306414 s*b 11 21 46.8237210288 -59 51 47.969821291 10.12 10.69 10.23 10.00   B1Ia 133 0
18 1E 1145.1-6141 HXB 11 47 28.5595495558 -61 57 13.424380577   13.08       B2Iae 123 0
19 V* BP Cru HXB 12 26 37.5607088371 -62 46 13.259605389   12.70 10.66     B1.5Iaeq 604 0
20 2MASS J16415078-4532253 HXB 16 41 50.7854893198 -45 32 25.452141297           O8.5(sg?) 92 2
21 2MASS J16463526-4507045 HXB 16 46 35.2592332854 -45 07 04.609816032   15.2       O9.5Ia 87 1
22 2MASS J16480656-4512068 HXB 16 48 06.56 -45 12 06.8           O8.5Iab 119 2
23 * zet01 Sco s*b 16 53 59.7270104119 -42 21 43.313745214 4.80 5.31 4.79 4.32 3.86 B1Ia-0ek 347 0
24 NAME OAO 1657-41 HXB 17 00 48.884 -41 39 21.46           Ofpe/WN9 211 0
25 2XMM J172511.3-361658 HXB 17 25 11.392 -36 16 57.53           B0-1Ia 109 2
26 IGR J17544-2619 HXB 17 54 25.2724584579 -26 19 52.578788584   14.71 12.94 12.10 10.38 O9Ib 164 0
27 SAX J1818.6-1703 HXB 18 18 37.8990045305 -17 02 47.970872274     17.4 17.4   ~ 95 0
28 IGR J18483-0311 HXB 18 48 17.2064881183 -03 10 16.876608322 23.702 25.162 21.884 17.888 15.88 B0.5Ia 109 0
29 4U 1907+09 HXB 19 09 37.9 +09 49 49   19.41 16.35 14.40 12.53 O8.5Iab 307 1
30 HD 190603 s*b 20 04 36.1744053423 +32 13 06.952102252 5.73 6.19 5.65 5.13 4.71 B1.5Ia 323 0
31 * omi And Be* 23 01 55.2645930 +42 19 33.533383 3.00 3.53 3.62 3.61 3.69 B6IV/V_sh 411 0
32 NAME Local Arm reg ~ ~           ~ 374 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-06:52:45

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