2012MNRAS.423..590G


Query : 2012MNRAS.423..590G

2012MNRAS.423..590G - Mon. Not. R. Astron. Soc., 423, 590-599 (2012/June-2)

Assessing luminosity correlations via cluster analysis: evidence for dual tracks in the radio/X-ray domain of black hole X-ray binaries.

GALLO E., MILLER B.P. and FENDER R.

Abstract (from CDS):

The radio/X-ray correlation for hard and quiescent state black hole X-ray binaries is critically investigated in this paper. New observations of known sources, along with newly discovered ones (since 2003), have resulted in an increasingly large number of outliers lying well outside the scatter about the quoted best-fitting relation. Most of these outliers tend to cluster below the best-fitting line, possibly indicative of two distinct tracks which might reflect different accretion regimes within the hard state. Here, we employ and compare state of the art data clustering techniques in order to identify and characterize different data groupings within the radio/X-ray luminosity plane for 18 hard and quiescent state black hole X-ray binaries with nearly simultaneous multiwavelength coverage. Linear regression is then carried out on the clustered data to infer the parameters of a relationship of the form lr=α+βlx through a Bayesian approach (where l denotes logarithmic luminosities). We conclude that the two-cluster model, with independent linear fits, is a significant improvement over fitting all points as a single cluster. While the upper track slope (0.63±0.03) is consistent, within the errors, with the fitted slope for the 2003 relation (0.7±0.1), the lower track slope (0.98±0.08) is not consistent with the upper track or with the widely adopted value of ≃ 1.4 for the neutron stars. The two luminosity tracks do not reflect systematic differences in black hole spins as estimated either from reflection- or continuum-fitting method. Additionally, there is evidence for at least two sources (H1743-322 and GRO J1655-500) jumping from the lower to the upper track as they fade towards quiescence, further indicating that black hole spin does not play any major role in defining the radio loudness of compact jets from hard black hole X-ray binaries. The results of the clustering and regression analysis are fairly insensitive to the selection of subsamples, accuracy in the distances and the treatment of upper limits. Besides introducing a further level of complexity in understanding the interplay between synchrotron and Comptonized emission from black hole X-ray binaries, the existence of two tracks in the radio/X-ray domain underscores that a high level of caution must be exercised when employing black hole luminosity-luminosity relations for the purpose of estimating a third parameter, such as distance or mass.

Abstract Copyright: 2012 The Authors Monthly Notices of the Royal Astronomical Society2012 RAS

Journal keyword(s): accretion, accretion discs - black hole physics - methods: statistical - ISM: jets and outflows - radio continuum: general - X-rays: binaries

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* V518 Per HXB 04 21 42.7227473352 +32 54 26.939156184 13.00 13.50 13.2     M4.5V 638 1
2 1A 0620-00 HXB 06 22 44.5423857312 -00 20 44.290460544 10.60 11.40 11.2     K3V-K7V 1073 0
3 V* KV UMa HXB 11 18 10.7930420496 +48 02 12.314730120     12.25     K5V-M1V 769 0
4 V* BW Cir HXB 13 58 09.700 -64 44 05.80 17.90 18.00 16.9     ~ 217 1
5 V* IL Lup HXB 15 47 08.2768672752 -47 40 10.284587760     11.96     ~ 453 1
6 V* V381 Nor HXB 15 50 58.6637920704 -56 28 35.258385000   17.95 16.6     K3III 1103 0
7 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 370 0
8 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1800 1
9 V* V821 Ara HXB 17 02 49.3876391280 -48 47 23.087954544 16.20 16.30 15.5     ~ 1952 0
10 [KRL2007b] 222 LXB 17 09 07.61 -36 24 25.7           ~ 245 1
11 IGR J17177-3656 LXB 17 17 39.0 -36 56 17           ~ 23 0
12 V* V1228 Sco LXB 17 19 58.990 -31 45 01.11           ~ 110 1
13 NAME Great Annihilator LXB 17 43 54.83 -29 44 42.6           ~ 659 1
14 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 677 0
15 XTE J1752-522 X 17 52 -52.2           ~ 2 0
16 2MAXI J1753-013 LXB 17 53 28.2898766424 -01 27 06.256555272 15.30 16.73 16.46 16.15 15.64 ~ 330 0
17 2XMM J180112.4-254436 LXB 18 01 12.40 -25 44 36.1           ~ 376 1
18 [KRL2007b] 353 HXB 19 08 53.080 +09 23 04.84     15.80     ~ 101 0
19 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2464 0
20 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4140 0
21 V* V404 Cyg HXB 20 24 03.8254458776 +33 52 01.962185735           G9/K0III/V 1192 0

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2022.10.07-03:59:20

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