2010ApJ...719..143T


Query : 2010ApJ...719..143T

2010ApJ...719..143T - Astrophys. J., 719, 143-150 (2010/August-2)

Fading hard X-ray emission from the galactic center molecular cloud Sgr B2.

TERRIER R., PONTI G., BELANGER G., DECOURCHELLE A., TATISCHEFF V., GOLDWURM A., TRAP G., MORRIS M.R. and WARWICK R.

Abstract (from CDS):

The center of our Galaxy harbors a four million solar mass black hole that is unusually quiet: its present X-ray luminosity is more than 10 orders of magnitude less than its Eddington luminosity. The observation of iron fluorescence and hard X-ray emission from some of the massive molecular clouds surrounding the Galactic center has been interpreted as an echo of a past 1039 erg/s flare. Alternatively, low-energy cosmic rays propagating inside the clouds might account for the observed emission, through inverse bremsstrahlung of low-energy ions or bremsstrahlung emission of low-energy electrons. Here, we report the observation of a clear decay of the hard X-ray emission from the molecular cloud Sgr B2 during the past seven years, thanks to more than 20 Ms of INTEGRAL exposure. This confirms the decay previously observed comparing the 6.4 keV line fluxes measured by various X-ray instruments, but without intercalibration effects. The measured decay time is 8.2±1.7 yr, compatible with the light crossing time of the molecular cloud core. Such a short timescale rules out inverse bremsstrahlung by cosmic-ray ions as the origin of the X ray emission. We also obtained 2-100 keV broadband X-ray spectra by combining INTEGRAL and XMM-Newton data and compared them with detailed models of X-ray emission due to irradiation of molecular gas by (1) low-energy cosmic-ray electrons and (2) hard X-rays. Both models can reproduce the data equally well, but the time variability constraints and the huge cosmic-ray electron luminosity required to explain the observed hard X-ray emission strongly favor the scenario in which the diffuse emission of Sgr B2 is scattered and reprocessed radiation emitted in the past by Sgr A*. The spectral index of the illuminating power-law source is found to be Γ ∼ 2 and its luminosity 1.5-5x1039 erg/s, depending on the relative positions of Sgr B2 and Sgr A*. Using recent parallax measurements that place Sgr B2 in front of Sgr A*, we find that the period of intense activity of Sgr A* ended between 75 and 155 years ago.

Abstract Copyright: ∼

Journal keyword(s): Galaxy: center - ISM: clouds - X-rays: ISM

Simbad objects: 27

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Number of rows : 27
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 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
2 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
3 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4725 3
4 BAX 258.1082-23.3759 ClG 17 12 26.3 -23 21 38           ~ 303 0
5 2E 3938 HXB 17 43 54.7 -29 44 44           ~ 693 1
6 NAME Sgr C MoC 17 44 36.3 -29 28 13           ~ 400 0
7 KS 1741-293 LXB 17 44 51.63 -29 20 42.8           ~ 106 0
8 NAME Sgr A Region reg 17 45 12 -28 48.3           ~ 955 0
9 [KRL2007b] 270 gam 17 45 38.5 -29 01 15           ~ 27 0
10 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
11 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 4970 3
12 NAME Sgr A East SNR 17 45 41 -29 00.8           ~ 523 2
13 2E 3943 LXB 17 46 05.3 -29 30 52           ~ 217 1
14 2E 3944 LXB 17 46 21.1 -28 43 39     12.50     ~ 126 0
15 CO 000.13-00.13 MoC 17 46.4 -28 54           ~ 24 0
16 NAME Sgr B MoC 17 47 02 -28 25.4           ~ 241 0
17 [KRL2007b] 275 LXB 17 47 02.60 -28 52 58.9     14.20     ~ 182 0
18 NAME Sgr B2 (North) Rad 17 47 20.2 -28 22 21           ~ 742 1
19 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 2443 1
20 NAME Sgr B2 (South) HII 17 47 20.430 -28 23 45.06           ~ 106 0
21 NAME Sgr B2 Main Rad 17 47 20.5 -28 23 06           ~ 436 1
22 AX J1747.4-3000 LXB 17 47 26.0 -30 00 02           ~ 119 0
23 CXOGCS J174742.4-282228 MoC 17 47 42.41 -28 22 28.1           ~ 49 1
24 GCM +0.74 -0.09 Cld 17 47.7 -28 21           ~ 5 0
25 [CHM2006] Candidate 1b LXB 17 49 38.039 -28 21 17.50           ~ 82 0
26 IGR J17511-3057 LXB 17 51 08.55 -30 57 41.7           ~ 114 1
27 GCM +0.66 -0.04 MoC ~ ~           ~ 2 0

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