Limits on the Short Term Variability of Sagittarius A* in the Near-Infrared

Abstract

The detection of X-ray flares by the Chandra X-ray Observatory and XMM-Newton has raised the possibility of enhanced emission over a broad range of wavelengths from Sagittarius A*, the suspected 2.6 × 106 M⊙ black hole at the Galactic center, during a flaring event. We have, therefore, reconstructed 3–4 hr data sets from 2 μm speckle and adaptive optics images (θcore = 50–100 mas) obtained with the W. M. Keck 10 m telescopes between 1995 and 2002. The results for 25 of these observations were reported by Hornstein et al. (2002) and an additional 11 observations are presented here. In the 36 separate observations, no evidence of any significant excess emission associated with Sgr A* was detected. The lowest of our detection limits gives an observed limit for the quiescent state of Sgr A* of 0.09 ± 0.005 mJy, or, equivalently, a dereddened value of 2.0 ± 0.1 mJy. Under the assumption that there are random 3 hr flares producing both enhanced X-ray and near-infrared emission, our highest limit constrains the variable state of Sgr A* to ≲0.8 mJy (observed) or 19 mJy (dereddened). These results suggest that the early model favored by Markoff et al. (2002), in which the flare is produced through local heating of relativistic particles surrounding Sgr A* (e.g., a sudden magnetic reconnection event), is unlikely because it predicts peak 2 μm emission of ∼300 mJy, well above our detection limit.

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