2002A&A...391..923G


Query : 2002A&A...391..923G

2002A&A...391..923G - Astronomy and Astrophysics, volume 391, 923-944 (2002/9-1)

The Milky Way in X-rays for an outside observer. Log(N)-Log(S) and luminosity function of X-ray binaries from RXTE/ASM data.

GRIMM H.-J., GILFANOV M. and SUNYAEV R.

Abstract (from CDS):

We study the Log(N)-Log(S) and X-ray luminosity function in the 2-10 keV energy band, and the spatial (3-D) distribution of bright, LX≥1034-1035erg/s, X-ray binaries in the Milky Way. In agreement with theoretical expectations and earlier results we found significant differences between the spatial distributions of low (LMXB) and high (HMXB) mass X-ray binaries. The volume density of LMXB sources peaks strongly at the Galactic Bulge whereas HMXBs tend to avoid the inner ∼3-4kpc of the Galaxy. In addition HMXBs are more concentrated towards the Galactic Plane (scale heights of ≃150 and ≃410pc for HMXB and LMXB correspondingly) and show clear signatures of the spiral structure in their spatial distribution. The Log(N)-Log(S) distributions and the X-ray luminosity functions are also noticeably different. LMXB sources have a flatter Log(N)-Log(S) distribution and luminosity function. The integrated 2-10keV luminosities of all X-ray binaries in the Galaxy, averaged over 1996-2000, are ∼2-3x1039 (LMXB) and ∼2-3x1038 (HMXB) erg/s. Normalised to the stellar mass and the star formation rate, respectively, these correspond to ∼5x1028erg/s/M for LMXBs and ∼5x1037erg/s/(M/yr) for HMXBs. Due to the shallow slopes of the luminosity functions the integrated emission of X-ray binaries is dominated by the ∼5-10 most luminous sources which determine the appearance of the Milky Way in the standard X-ray band for an outside observer. In particular variability of individual sources or an outburst of a bright transient source can increase the integrated luminosity of the Milky Way by as much as a factor of ∼2. Although the average LMXB luminosity function shows a break near the Eddington luminosity for a 1.4M neutron star, at least 12 sources showed episodes of super-Eddington luminosity during ASM observations. We provide the maps of distribution of X-ray binaries in the Milky Way in various projections, which can be compared to images of nearby galaxies taken by CHANDRA and XMM-Newton.

Abstract Copyright:

Journal keyword(s): X-rays: binaries - X-rays: galaxies - Galaxy: general - Galaxy: structure - galaxies: spiral - stars: luminosity function

Simbad objects: 71

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Number of rows : 71
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 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1135 1
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11880 1
3 SK 160 HXB 01 17 05.1457288392 -73 26 36.014808156 12.23 13.00 13.15   13.17 O9.7Ia+ 827 0
4 NAME PER SUPERCL SCG 02 33.2 +41 37           ~ 389 1
5 NGC 1399 BiC 03 38 29.083 -35 27 02.67 11.05 9.74 9.59 8.12   ~ 1515 1
6 NGC 1553 GiP 04 16 10.4697802536 -55 46 48.072797400 10.76 10.10 9.40 8.74   ~ 366 2
7 X LMC X-2 LXB 05 20 28.04 -71 57 53.3 17.20 18.00 18.0     ~ 176 0
8 X LMC X-4 HXB 05 32 49.5556042296 -66 22 13.202721768   13.9 14.0     O8III 635 0
9 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5060 0
10 M 1 SNR 05 34 32 +22 00.8           ~ 5938 1
11 * tet01 Ori C SB* 05 35 16.4662967280 -05 23 22.921811880 4.20 5.15 5.13 4.91 4.73 O7Vp 1351 1
12 X LMC X-3 HXB 05 38 56.6323605504 -64 05 03.317937504   17 17.2     B2.5Ve 647 0
13 X LMC X-1 HXB 05 39 38.8284304464 -69 44 35.531553624   14.8 14.5     O8(f)p 602 2
14 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1113 1
15 NAME Pup A SNR 08 24 07 -42 59.8           ~ 562 1
16 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2207 1
17 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4201 3
18 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5616 6
19 V* V779 Cen HXB 11 21 15.0920532528 -60 37 25.630264596   14.4 12.27     O9III/Veq 1032 0
20 NAME COMA SUPERCL SCG 11 23 +23.9           ~ 256 0
21 V* GU Mus HXB 11 26 26.5961559600 -68 40 32.877752952           K3V-K7V 690 1
22 NGC 4038 GiP 12 01 53.002 -18 52 03.32   10.91   9.74 11.0 ~ 1304 1
23 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1631 0
24 NGC 4039 GiP 12 01 53.8 -18 53 06   11.08   9.77   ~ 1148 1
25 M 84 Sy2 12 25 03.74333 +12 53 13.1393 12.67 12.09 10.49     ~ 1703 2
26 V* BP Cru HXB 12 26 37.5605188992 -62 46 13.261044684   12.70 10.66     B1.5Iaeq 641 0
27 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6704 3
28 NAME LOCAL SUPERCL SCG 12 31 +12.4           ~ 488 0
29 NGC 4697 GiG 12 48 35.8981498824 -05 48 02.482374564   10.97   9.83   ~ 835 0
30 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 1020 2
31 CPD-63 2495 HXB 13 02 47.6544015048 -63 50 08.626970292 10.34 10.72 9.98 10.03   O9.5Ve 731 0
32 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 1098 2
33 V* BR Cir HXB 15 20 40.85 -57 10 00.1   21.4 21.4     ~ 746 1
34 V* QV Nor HXB 15 42 23.3633146128 -52 23 09.577395960   16.3 14.5     B0.2Ia:e 394 1
35 V* V381 Nor HXB 15 50 58.6637920704 -56 28 35.258385000   17.95 16.6     K3III 1098 0
36 V* QX Nor LXB 16 12 43.0 -52 25 23           ~ 872 1
37 V* V818 Sco LXB 16 19 55.0692669024 -15 38 25.017666540 11.60 12.40 11.1     Oev 1577 0
38 4U 1624-49 LXB 16 28 05.5318788600 -49 12 40.011095160           ~ 214 0
39 SNR G337.0-00.1 SNR 16 35 06.9 -47 47 25           ~ 126 1
40 4U 1642-45 LXB 16 45 47.7 -45 36 40     14.30     ~ 394 1
41 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1793 1
42 V* HZ Her LXB 16 57 49.8110126616 +35 20 32.486555472 11.90 14.89 13.63 13.88   B3/6ep 1994 0
43 NAME OAO 1657-41 HXB 17 00 48.884 -41 39 21.46           Ofpe/WN9 225 0
44 V* V1101 Sco LXB 17 05 44.4916006152 -36 25 23.049324480   20.10 18.6     ~ 420 0
45 V* V2107 Oph HXB 17 08 14.520 -25 05 30.15   16.50 15.9     K3V-K7V 216 1
46 4U 1705-44 LXB 17 08 54.470 -44 06 07.35           ~ 372 0
47 PSR J1713+0447 Psr 17 13 49.53053 +07 47 37.5264           ~ 412 1
48 V* V2116 Oph Sy* 17 32 02.1532435416 -24 44 44.129169096   20.78 18.4     M6IIIe 669 1
49 KS 1731-260 LXB 17 34 13.46 -26 05 18.6       22.8 20.9 ~ 405 0
50 V* V926 Sco LXB 17 38 58.3 -44 27 00 16.90 17.70 17.5     ~ 443 0
51 3FHL J1746.2-2852 LXB 17 44 33.09 -28 44 27.0           ~ 513 0
52 4U 1758-25 LXB 18 01 09.7308060816 -25 04 44.120221284     11.08     ~ 631 1
53 X Sgr X-3 LXB 18 01 32.3 -20 31 44           ~ 226 1
54 V* V5512 Sgr LXB 18 14 31.55 -17 09 26.7     12.73     K5III 371 0
55 V* NP Ser LXB 18 16 01.389 -14 02 10.62   18.8       K 619 2
56 V* V4641 Sgr HXB 18 19 21.6343259256 -25 24 25.849595952     13.654   13.092 B9III 436 1
57 NGC 6624 GlC 18 23 40.51 -30 21 39.7           ~ 827 1
58 V* MM Ser LXB 18 39 57.56 +05 02 09.6   19.2 19.2     ~ 336 0
59 2MASS J18453684+0051474 HXB 18 45 36.8356591776 +00 51 47.437790184     20.6     B0-2IV-Ve 104 0
60 2MASS J18553040-0236167 HXB 18 55 30.4058947392 -02 36 16.737653700           B0Iaep 84 0
61 XTE J1906+090 HXB 19 04 47.491 +09 02 41.40           Be? 25 0
62 4U 1908+075 HXB 19 10 48.2133201408 +07 35 51.707133960           O7.5-9.5sg 110 0
63 SS 433 HXB 19 11 49.5647697480 +04 58 57.827127648   16.3 13.0     A7Ib: 2028 4
64 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2453 0
65 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4122 0
66 PSR J1959+2048 Psr 19 59 36.7480 +20 48 14.599   20.4       ~ 750 2
67 V* QZ Vul HXB 20 02 49.58 +25 14 11.3   19.64 18.2     K3V-K6V 408 0
68 V* V404 Cyg HXB 20 24 03.8254458776 +33 52 01.962185735           G9/K0III/V 1186 0
69 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1868 2
70 V* V1341 Cyg LXB 21 44 41.1544345272 +38 19 17.066570988 15.00 15.13 14.68 15.00   A9III 1108 1
71 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2619 1

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2022.08.10-07:20:58

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