2008A&A...484..801R


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.03CET11:25:15

2008A&A...484..801R - Astronomy and Astrophysics, volume 484, 801-813 (2008/6-4)

Multi-wavelength observations of Galactic hard X-ray sources discovered by INTEGRAL. II. The environment of the companion star.

RAHOUI F., CHATY S., LAGAGE P.-O. and PANTIN E.

Abstract (from CDS):

The INTEGRAL mission has led to the discovery of a new type of supergiant X-ray binaries (SGXBs), whose physical properties differ from those of previously known SGXBs. Those sources are in the course of being unveiled by means of multi-wavelength X-rays, optical, near- and mid-infrared observations, and two classes are appearing. The first class consists of obscured persistent SGXBs and the second is populated by the so-called supergiant fast X-ray transients (SFXTs). We report here mid-infrared (MIR) observations of the companion stars of twelve SGXBs from these two classes in order to assess the contribution of the star and the material enshrouding the system to the total emission. We used data from observations we carried out at ESO/VLT with VISIR, as well as archival and published data, to perform broad-band spectral energy distributions of the companion stars and fitted them with a combination of two black bodies representing the star and a MIR excess due to the absorbing material enshrouding the star, if there was any. We detect a MIR excess in the emission of IGR J16318-4848, IGR J16358-4726, and perhaps IGR J16195-4945. The other sources do not exhibit any MIR excess even when the intrinsic absorption is very high. Indeed, the stellar winds of supergiant stars are not suitable for dust production, and we show that this behaviour is not changed by the presence of the compact object. Concerning IGR J16318-4848 and probably IGR J16358-4726, the MIR excess can be explained by their sgB[e] nature and the presence of an equatorial disk around the supergiant companion in which dust can be produced. Moreover, our results suggest that some of the supergiant stars in those systems could exhibit an absorption excess compared to isolated supergiant stars, this excess being possibly partly due to the photoionisation of their stellar wind in the vicinity of their atmosphere. We also show that the differences in behaviour between the obscured SGXBs and the SFXTs in the high-energy domain do not exist from optical-to-MIR wavelength. Supergiant stars in SFXTs could nevertheless be most of the time less absorbed than supergiant stars in obscured SGXBs, due to the geometry of the systems. At last, our results confirm a very dense cocoon of material around the compact object as the extinction in the X-ray domain is generally several orders of magnitude higher than the extinction in the visible.

Abstract Copyright:

Journal keyword(s): stars: fundamental parameters - infrared: stars - X-rays: binaries - stars: binaries: general - stars: supergiants

CDS comments: Paragraph 3.4 2MASS J16320215-4752289 is a probable misprint for 2MASS J16320215-4752322. Paragraph 4.4 IGR J16465-4945 is a misprint for IGR J16465-4507 or for IGR J16195-4945.

Simbad objects: 34

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Number of rows : 34

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 144969 s*b 16 10 49.1402832539 -48 47 41.736445891 9.14 9.32 8.39 7.47 6.70 B1Ia 60 0
2 SSTGLMC G333.4590+01.0501 IR 16 16 02.880 -49 18 02.10           ~ 1 0
3 HD 146628 * 16 19 29.5213460341 -49 45 40.716565476 10.23 10.58 10.06 10.02   B1/2Ia 64 1
4 IGR J16195-4945 HXB 16 19 32.1829528980 -49 44 30.564960595   17.4 16.8 15.3 15.6 B1sg 47 0
5 CXOU J162046.2-513006 HXB 16 20 46.2655398336 -51 30 06.046848280   18.9   16.28 13.4 B8IIIe 56 0
6 HD 148422 * 16 30 59.8915188816 -56 29 43.229024439 7.93 8.70 8.65 9.40   B1Ia 67 0
7 IGR J16318-4848 HXB 16 31 48.3102815892 -48 49 00.664215918           ~ 158 0
8 SSTGLMC G335.6260-00.4477 IR 16 31 50.800 -48 48 34.36           ~ 1 0
9 SSTGLMC G336.3293+00.1689 IR 16 32 01.760 -47 52 28.97           ~ 1 0
10 3FHL J1633.0-4746e HXB 16 32 01.87 -47 52 28.3           O8I 151 3
11 2MASS J16320215-4752322 * 16 32 02.1636048300 -47 52 32.294200860   17.3 16.1     K 7 1
12 * mu. Nor s*b 16 34 05.0202815 -44 02 43.128156 4.05 4.99 4.94 6.36   O9.7Iab 261 0
13 2MASS J16355369-4725398 IR 16 35 53.70 -47 25 39.8           ~ 9 1
14 SSTGLMC G337.0994-00.0062 IR 16 35 53.740 -47 25 40.03           ~ 1 0
15 [KRL2007b] 194 Psr 16 36 30 -47 37.5           Be 75 0
16 2MASS J16415078-4532253 HXB 16 41 50.7854893198 -45 32 25.452141297           O8.5(sg?) 95 2
17 SSTGLMC G339.1889+00.4889 IR 16 41 50.820 -45 32 25.65           ~ 1 0
18 2MASS J16463526-4507045 HXB 16 46 35.2592332854 -45 07 04.609816032   15.2       O9.5Ia 87 1
19 SSTGLMC G340.0536+00.1350 IR 16 46 35.300 -45 07 04.58           ~ 1 0
20 2MASS J16480656-4512068 HXB 16 48 06.56 -45 12 06.8           O8.5Iab 123 2
21 SSTGLMC G340.1630-00.1239 IR 16 48 06.590 -45 12 07.01           ~ 1 0
22 USNO-B1.0 0447-00531332 * 16 48 06.8543388749 -45 12 07.981988216           ~ 4 0
23 HD 151804 s*b 16 51 33.7215112148 -41 13 49.928887100 4.45 5.29 5.22     O8Iaf 357 0
24 HD 152235 s*b 16 53 58.8524252928 -41 59 39.573669251 6.47 6.92 6.38 5.84 5.42 B0.5Ia 178 0
25 HD 152234 s*b 16 54 01.8374467 -41 48 23.007764 4.92 5.64 5.45     B0.5Ia 183 0
26 HD 152249 s*b 16 54 11.6391931444 -41 50 57.294733186 5.91 6.65 6.45     OC9Iab 221 0
27 HD 153919 HXB 17 03 56.7728262865 -37 50 38.912077679 6.06 6.78 6.51 6.08 5.90 O6Iafcp 765 1
28 HD 156201 * 17 17 45.5141583820 -35 13 27.019910833 8.34 8.70 8.01 7.31   B0.5Ia/ab 56 0
29 2MASS J17251139-3616575 HXB 17 25 11.392 -36 16 57.53     14.30     B0-1Ia 111 2
30 AX J1739.1-3020 HXB 17 39 11.5521531365 -30 20 37.783172824     14.40 13.91   O8.5Iab(f) 142 1
31 GAL 000.0+00.0 gam 17 45 39.60213 -29 00 22.0000           ~ 12003 0
32 IGR J17544-2619 HXB 17 54 25.2724584579 -26 19 52.578788584   14.71 12.94 12.10 10.38 O9Ib 166 0
33 INTEGRAL1 111 HXB 19 14 04.2269997048 +09 52 58.398334234   18.6 16.4     B0.5I 89 0
34 SSTGLMC G044.2963-00.4688 IR 19 14 04.250 +09 52 58.02           ~ 1 0

    Equat.    Gal    SGal    Ecl

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2021.03.03-11:25:16

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