2017ApJ...844...72W

Query : 2017ApJ...844...72W

2017ApJ...844...72W - Astrophys. J., 844, 72-72 (2017/July-3)

Submilliarcsecond optical interferometry of the high-mass X-ray binary BP Cru with VLTI/GRAVITY.

WAISBERG I., DEXTER J., PFUHL O., ABUTER R., AMORIM A., ANUGU N., BERGER J.P., BLIND N., BONNET H., BRANDNER W., BURON A., CLENET Y., DE WIT W., DEEN C., DELPLANCKE-STROBELE F., DEMBET R., DUVERT G., ECKART A., EISENHAUER F., FEDOU P., FINGER G., GARCIA P., GARCIA LOPEZ R., GENDRON E., GENZEL R., GILLESSEN S., HAUBOIS X., HAUG M., HAUSSMANN F., HENNING T., HIPPLER S., HORROBIN M., HUBERT Z., JOCHUM L., JOCOU L., KERVELLA P., KOK Y., KULAS M., LACOUR S., LAPEYRERE V., LE BOUQUIN J.-B., LENA P., LIPPA M., MERAND A., MULLER E., OTT T., PALLANCA L., PANDURO J., PAUMARD T., PERRAUT K., PERRIN G., RABIEN S., RAMIREZ A., RAMOS J., RAU C., ROHLOFF R.-R., ROUSSET G., SANCHEZ-BERMUDEZ J., SCHEITHAUER S., SCHOLLER M., STRAUBMEIER C., STURM E., VINCENT F., WANK I., WIEPRECHT E., WIEST M., WIEZORREK E., WITTKOWSKI M., WOILLEZ J., YAZICI S. (The GRAVITY Collaboration)

Abstract (from CDS):

We observe the high-mass X-ray binary (HMXB) BP Cru using interferometry in the near-infrared K band with VLTI/GRAVITY. Continuum visibilities are at most partially resolved, consistent with the predicted size of the hypergiant. Differential visibility amplitude (Δ| V| ∼5 % ) and phase (Δφ∼2○) signatures are observed across the He I 2.059 µm and Brγ lines, the latter seen strongly in emission, unusual for the donor star's spectral type. For a baseline B∼100 m, the differential phase rms ∼0○ / . 2 corresponds to an astrometric precision of ∼2 µas. We generalize expressions for image centroid displacements and variances in the marginally resolved limit of interferometry to spectrally resolved data, and use them to derive model-independent properties of the emission such as its asymmetry, extension, and strong wavelength dependence. We propose geometric models based on an extended and distorted wind and/or a high-density gas stream, which has long been predicted to be present in this system. The observations show that optical interferometry is now able to resolve HMXBs at the spatial scale where accretion takes place, and therefore to probe the effects of the gravitational and radiation fields of the compact object on its environment.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): circumstellar matter - techniques: high angular resolution - techniques: interferometric - X-rays: binaries - X-rays: individual: GX 301-2 - X-rays: individual: GX 301-2

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 V* CI Cam HXB 04 19 42.1355996520 +55 59 57.706599192 12.13 12.41 11.77 10.79 9.99 B0/2I[e] 271 0
2 * bet Ori s*b 05 14 32.27210 -08 12 05.8981 -0.56 0.10 0.13 0.13 0.15 B8Ia 786 0
3 1A 0620-00 HXB 06 22 44.5423857312 -00 20 44.290460544           K3V-K7V 1144 0
4 V* GP Vel HXB 09 02 06.8608812864 -40 33 16.899168060 6.85 7.37 6.87 6.31 6.05 B0.5Ia 1588 0
5 HD 97550 * 11 12 56.7155579520 -49 44 09.950038728   7.163 6.109     G8II/III 29 0
6 V* BP Cru HXB 12 26 37.5605188992 -62 46 13.261044684   12.482 10.803 10.304   B1Ia+ 731 0
7 HD 110532 PM* 12 43 28.3215591528 -58 54 09.874004328   7.53 6.42     K0/1III 21 0
8 V* V818 Sco LXB 16 19 55.0692669024 -15 38 25.017666540 11.60 12.40 11.1     Oev 1730 0
9 HD 148688 s*b 16 31 41.7687715992 -41 49 01.732565676 5.16 5.78 5.39 5.05 4.70 B1Iaeqp 170 0
10 V* V5512 Sgr LXB 18 14 31.3 -17 09 23     12.73     K5III 449 0
11 HD 169454 s*b 18 25 15.1937863728 -13 58 42.309359544 7.39 7.61 6.71 5.82 5.13 B1Ia+ 359 1
12 SS 433 HXB 19 11 49.5647697480 +04 58 57.827127648   16.854 14.643     A7Ib 2253 4
13 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4590 0
14 HD 190603 s*b 20 04 36.1742825304 +32 13 06.953333016 5.73 6.19 5.65 5.13 4.71 B1.5Ia+ 357 0

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