FADING HARD X-RAY EMISSION FROM THE GALACTIC CENTER MOLECULAR CLOUD Sgr B2
- Astroparticule et Cosmologie, Universite Paris7/CNRS/CEA, Batiment Condorcet, 75013 Paris (France)
- European Space Agency, ESAC, P.O. Box 78, 28691, Villanueva de la Canada, Madrid (Spain)
- Service d'Astrophysique (SAp)/IRFU/DSM/CEA Saclay, Bt. 709, 91191 Gif-sur-Yvette Cedex (France)
- Centre de Spectrometrie Nucleaire et de Spectrometrie de Masse, CNRS/IN2P3 and Univ Paris-Sud, 91405 Orsay (France)
- Department of Physics and Astronomy, University of California, Los Angeles, CA 90095-1547 (United States)
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)
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 10{sup 39} erg s{sup -1} 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 {Gamma} {approx} 2 and its luminosity 1.5-5 x 10{sup 39} erg s {sup -1}, 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.
- OSTI ID:
- 21455018
- Journal Information:
- Astrophysical Journal, Vol. 719, Issue 1; Other Information: DOI: 10.1088/0004-637X/719/1/143; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
COSMOLOGY AND ASTRONOMY
BLACK HOLES
BREMSSTRAHLUNG
COSMIC RADIATION
FLUORESCENCE
GALAXIES
HARD X RADIATION
LUMINOSITY
X-RAY SPECTRA
ELECTROMAGNETIC RADIATION
EMISSION
IONIZING RADIATIONS
LUMINESCENCE
OPTICAL PROPERTIES
PHOTON EMISSION
PHYSICAL PROPERTIES
RADIATIONS
SPECTRA
X RADIATION