Flares and variability from Sagittarius A*: five nights of simultaneous multi-wavelength observations⋆
X. Haubois1,4, K. Dodds-Eden2, A. Weiss3, T. Paumard1, G. Perrin1, Y. Clénet1, S. Gillessen2, P. Kervella1, F. Eisenhauer2, R. Genzel2 and D. Rouan1
1 LESIA-Observatoire de Paris, CNRS UMR 8109, UPMC Univ. Paris 6, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France
2 MPE, Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
3 MPIfR, Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53321 Bonn, Germany
4 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, São Paulo, 05508-900, Brazil
Received: 18 July 2011
Accepted: 11 January 2012
Aims. We report on simultaneous observations and modeling of mid-infrared (MIR), near-infrared (NIR), and submillimeter (sub-mm) emission of the source Sgr A* associated with the supermassive black hole at the center of our Galaxy. Our goal was to monitor the activity of Sgr A* at different wavelengths in order to constrain the emitting processes and gain insight into the nature of the close environment of Sgr A*.
Methods. We used the MIR instrument VISIR in the BURST imaging mode, the adaptive optics assisted NIR camera NACO, and the sub-mm antenna APEX to monitor Sgr A* over several nights in July 2007.
Results. The observations reveal remarkable variability in the NIR and sub-mm during the five nights of observation. No source was detected in the MIR, but we derived the lowest upper limit for a flare at 8.59 μm (22.4 mJy with A8.59 μm = 1.6 ± 0.5). This observational constraint makes us discard the observed NIR emission as coming from a thermal component emitting at sub-mm frequencies. Moreover, comparison of the sub-mm and NIR variability shows that the highest NIR fluxes (flares) are coincident with the lowest sub-mm levels of our five-night campaign involving three flares. We explain this behavior by a loss of electrons to the system and/or by a decrease in the magnetic field, as might conceivably occur in scenarios involving fast outflows and/or magnetic reconnection.
Key words: accretion, accretion disks / black hole physics / Galaxy: center / Galaxy: nucleus
© ESO, 2012