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Coordinated NIR/mm observations of flare emission from Sagittarius A*

Kunneriath, D. and Mauerhan, J. (2010) Coordinated NIR/mm observations of flare emission from Sagittarius A*. Astronomy and Astrophysics, 517 . A46. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20100902-133626460

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Abstract

Context. We report on a successful, simultaneous observation and modelling of the millimeter (mm) to near-infrared (NIR) flare emission of the Sgr A* counterpart associated with the supermassive (4 × 10^6 M_☉) black hole at the Galactic centre (GC). We present a mm/sub-mm light curve of Sgr A* with one of the highest quality continuous time coverages. Aims. We study and model the physical processes giving rise to the variable emission of Sgr A*. Methods. Our non-relativistic modelling is based on simultaneous observations carried out in May 2007 and 2008, using the NACO adaptive optics (AO) instrument at the ESO's VLT and the mm telescope arrays CARMA in California, ATCA in Australia, and the 30 m IRAM telescope in Spain. We emphasize the importance of multi-wavelength simultaneous fitting as a tool for imposing adequate constraints on the flare modelling. We present a new method for obtaining concatenated light curves of the compact mm-source Sgr A* from single dish telescopes and interferometers in the presence of significant flux density contributions from an extended and only partially resolved source. Results. The observations detect flaring activity in both the mm domain and the NIR. Inspection and modelling of the light curves show that in the case of the flare event on 17 May 2007, the mm emission follows the NIR flare emission with a delay of 1.5±0.5 h. On 15 May 2007, the NIR flare emission is also followed by elevated mm-emission. We explain the flare emission delay by an adiabatic expansion of source components. For two other NIR flares, we can only provide an upper limit to any accompanying mm-emission of about 0.2 Jy. The derived physical quantities that describe the flare emission give a source component expansion speed of ν_(exp) ~ 0.005c–0.017c, source sizes of about one Schwarzschild radius, flux densities of a few Janskys, and spectral indices of α = 0.6 to 1.3. These source components peak in the THz regime. Conclusions. These parameters suggest that either the adiabatically expanding source components have a bulk motion greater than ν_(exp) or the expanding material contributes to a corona or disk, confined to the immediate surroundings of Sgr A*. Applying the flux density values or limits in the mm- and X-ray domain to the observed flare events constrains the turnover frequency of the synchrotron components that are on average not lower than about 1 THz, such that the optically thick peak flux densities at or below these turnover frequencies do not exceed, on average, about ~1 Jy.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/200913613DOIUNSPECIFIED
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/200913613&Itemid=129PublisherUNSPECIFIED
Additional Information:© 2010 ESO. Received 5 November 2009; Accepted 29 March 2010. Published online 03 August 2010. Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG via grant SFB 494. M. Zamaninasab, D. Kunneriath, and R.-S. Lu, are members of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the MPIfR and the Universities of Bonn and Cologne. R.S. acknowledges support by the Ramón y Cajal programme by the Ministerio de Ciencia y Innovación of the government of Spain. Macarena Garcia-Marin is supported by the German federal department for education and research (BMBF) under the project numbers: 50OS0502 & 50OS0801. N. Sabha is a member of the Bonn Cologne Graduate School (BCGS) of Physics and Astronomy.
Funders:
Funding AgencyGrant Number
Deutsche Forschungsgemeinschaft (DFG), GermanySFB 494
Ministerio de Ciencia y Innovación, SpainUNSPECIFIED
Bundesministerium für Bildung und Forschung (BMBF), Germany50OS0502
Bundesministerium für Bildung und Forschung (BMBF), Germany50OS0801
Subject Keywords:black hole physics; infrared: general; accretion, accretion disks; Galaxy: center; galaxies: nuclei; radio continuum: general
Record Number:CaltechAUTHORS:20100902-133626460
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20100902-133626460
Official Citation:Coordinated NIR/mm observations of flare emission from Sagittarius A* D. Kunneriath, G. Witzel, A. Eckart, M. Zamaninasab, R. Gießübel, R. Schödel, F. K. Baganoff, M. R. Morris, M. Dovčiak, W. J. Duschl, M. García-Marín, V. Karas, S. König, T. P. Krichbaum, M. Krips, R.-S. Lu, J. Mauerhan, J. Moultaka, K. Mužić, N. Sabha, F. Najarro, J.-U. Pott, K. F. Schuster, L. O. Sjouwerman, C. Straubmeier, C. Thum, S. N. Vogel, P. Teuben, A. Weiss, H. Wiesemeyer and J. A. Zensus A&A 517 A46 (2010) DOI: 10.1051/0004-6361/200913613
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:19772
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:08 Sep 2010 15:32
Last Modified:26 Dec 2012 12:23

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