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Title:
Multiwavelength Monitoring of Sgr A* During Chandra Observations of Multiple X-ray Flares
Authors:
Baganoff, F. K.; Bautz, M. W.; Ricker, G. R.; Morris, M.; Becklin, E. E.; Ghez, A. M.; Hornstein, S. D.; Tanner, A. M.; Brandt, W. N.; Chartas, G.; Feigelson, E. D.; Garmire, G. P.; Cotera, A. S.; Hinz, P. M.; Hoffmann, W. F.; Meyer, M. R.; Eckart, A.; Genzel, R.; Zhao, J.-H.; Herrnstein, R. M.; Hora, J. L.; Macquart, J.-P.; Maeda, Y.; Sault, R. J.; Taylor, G. B.; Walter, F.
Affiliation:
AA(MIT), AB(MIT), AC(MIT), AD(UCLA), AE(UCLA), AF(UCLA), AG(UCLA), AH(UCLA), AI(PSU), AJ(PSU), AK(PSU), AL(PSU), AM(Steward Obs.), AN(Steward Obs.), AO(Steward Obs.), AP(Steward Obs.), AQ(U. Cologne), AR(MPE), AS(CfA), AT(CfA), AU(CfA), AV(U. Groningen), AW(ISAS), AX(ATNF), AY(NRAO), AZ(Caltech)
Publication:
American Astronomical Society, 201st AAS Meeting, #31.08; Bulletin of the American Astronomical Society, Vol. 34, p.1153
Publication Date:
12/2002
Origin:
AAS
Abstract Copyright:
(c) 2002: American Astronomical Society
Bibliographic Code:
2002AAS...201.3108B

Abstract

Sgr A* was observed with the ACIS-I instrument on the Chandra X-Ray Observatory for 0.5 Ms during the period 22 May 2002 to 4 June 2002. Three X-ray flares with amplitudes in excess of a factor of 10 and several flares of lower amplitude were detected. The flare durations ranged from half an hour to several hours with rise and fall times of a few hundred seconds, similar to the original X-ray flare discovered with Chandra in 2000. These observations confirm that rapid X-ray flaring of Sgr A* is common. Averaging over all Chandra observations from 1999-2002, a total of 0.6 Ms, the mean rate of factor-of-10 flares is 0.6 +\- 0.3 per day. During the Chandra observations, a network of ground-based telescopes were employed for simultaneous observations for varying amounts of time and at various wavelengths: the Keck-I Telescope at 2 and 10 microns; the VLT at 2 to 5 microns; the Magellan-Baade Telescope at 10 microns; the SMA at 1 mm; the ATCA and the Owens Valley Millimeter Array at 3 mm; the VLBA at 7 mm; and the VLA at 0.7, 1.3 and 2 cm. We compare the variability properties in the X-ray and longer wavelength bands to assess models for the origin of the X-ray flares from Sgr A*. This research was supported by NASA grant NAS8-39073.
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