2004ApJ...616..376O


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.14CEST14:18:22

2004ApJ...616..376O - Astrophys. J., 616, 376-382 (2004/November-3)

Orbital parameters for the black hole binary XTE J1650-500.

OROSZ J.A., McCLINTOCK J.E., REMILLARD R.A. and CORBEL S.

Abstract (from CDS):

We present R-band photometry of the X-ray transient and candidate black hole binary XTE J1650-500 obtained between 2003 May and August with the 6.5 m Clay telescope. A timing analysis of these data reveals a photometric period of 0.3205±0.0007 days (i.e., 7.63 hr) with a possible alias at 0.3785 days (9.12 hr). Our photometry completely rules out the previously published spectroscopic period of 0.212 days (5.09 hr). Consequently, we reanalyzed the 15 archival ESO VLT spectra (obtained 2002 June by Sanchez-Fernandez et al.) that were the basis of the previously published spectroscopic period. We used a ``rest-frame search'' technique that is well suited for cases in which the signal-to-noise ratio of individual spectra is low. For each of roughly 1.1 million binary ephemerides, we summed all of the spectra in a trial rest frame of the secondary star, and each rest-frame spectrum was cross-correlated against a template spectrum. We then searched for the set of orbital parameters that produced the strongest cross-correlation value. The results confirmed the photometric period of 0.3205 days and ruled out the alias period near 0.38 days. The best value for the velocity semiamplitude of the companion star is K2=435±30 km/s, and the corresponding optical mass function is f(M)=2.73±0.56 M. The spectral type of the companion star is not well constrained because we only have six template spectra available to us. The K4 V template provides the best match; next-best matches are provided by the G5 V and K2 III templates. We also find that the accretion disk dominates the light in the R band where the disk fraction is 80% or higher, although this value should be treated with caution owing to the poor signal-to-noise ratio and the limited number of templates. The amplitude of the phased R-band light curve is 0.2 mag, which gives a lower limit to the inclination of 50°±3° in the limiting case of no contribution to the R-band light curve from the accretion disk. If the mass ratio of XTE J1650-500 is similar to the mass ratios of other black hole binaries, such as A0620-00 or GRS 1124-683 (e.g., Q≳10), then our lower limit to the inclination gives an upper limit to the mass of the black hole in XTE J1650-500 of M1≲7.3 M. However, the mass can be considerably lower if the R-band flux is dominated by the accretion disk. For example, if the accretion disk does contribute 80% of the flux, as our preliminary results suggest, then the black hole mass would be only about 4 M.

Abstract Copyright:

Journal keyword(s): Stars: Binaries: Spectroscopic - Black Hole Physics - Stars: Individual: Alphanumeric: XTE J1650-500 - X-Rays: Binaries - X-Rays: Stars

Simbad objects: 25

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Number of rows : 25

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 11301 * 01 48 11.3511354439 -69 43 45.527886602   9.47 8.31     K2III 7 0
2 V* V518 Per HXB 04 21 42.7231318463 +32 54 26.936934166 13.00 13.50 13.2     M4.5V 626 1
3 X LMC X-3 HXB 05 38 56.6325045489 -64 05 03.321118015   17 17.2     B2.5Ve 637 0
4 X LMC X-1 HXB 05 39 38.8285930597 -69 44 35.533031148   14.8 14.5     O8(f)p 576 2
5 1A 0620-00 HXB 06 22 44.5420315454 -00 20 44.289428950 10.60 11.40 11.2     K3V-K7V 1052 0
6 HD 53706 PM* 07 03 58.9213019817 -43 36 40.869960689 7.978 7.632 6.851 6.427 6.013 K0.5V 131 0
7 V* MM Vel HXB 10 13 36.4107940553 -45 04 32.555813596   14.84 14.71     G5V-M0V 187 0
8 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 737 0
9 V* GU Mus HXB 11 26 26.5947467816 -68 40 32.888148788           K3V-K7V 677 1
10 HD 131977 BY* 14 57 28.0008928545 -21 24 55.726897561 7.89 6.83 5.72 4.74 4.19 K4V 452 0
11 V* IL Lup HXB 15 47 08.2766679321 -47 40 10.284971214     11.96     ~ 426 1
12 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1062 0
13 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 358 0
14 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1751 1
15 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1826 0
16 V* V2107 Oph HXB 17 08 14.520 -25 05 30.15   16.50 15.9     K3V-K7V 213 1
17 V* V4641 Sgr HXB 18 19 21.6342721789 -25 24 25.849323550     13.654   13.092 B9III 407 1
18 V* V406 Vul HXB 18 58 41.580 +22 39 29.40 15.00 15.65 15.31     G5V-K0V 326 0
19 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2361 0
20 HD 181321 PM* 19 21 29.7277723051 -34 59 00.356331012 7.22 7.11 6.48     G2V 128 0
21 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3997 0
22 V* QZ Vul HXB 20 02 49.58 +25 14 11.3   19.64 18.2     K3V-K6V 400 0
23 V* V404 Cyg HXB 20 24 03.820 +33 52 01.90 14.50 14.20 12.7     K0IV 1125 0
24 HD 200011 PM* 21 02 12.7326811665 -43 00 07.578420049 7.49 7.32 6.64     F8/G0V 44 0
25 HD 209290 PM* 22 02 10.2751729794 +01 24 00.830153206 11.838 10.616 9.146 8.213 7.245 M0.5V 197 0

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2021.04.14-14:18:23

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