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2011A&A...532A..83S - Astronomy and Astrophysics, volume 532A, 83-83 (2011/8-1)

The mean infrared emission of Sagittarius A*.

SCHOEDEL R., MORRIS M.R., MUZIC K., ALBERDI A., MEYER L., ECKART A. and GEZARI D.Y.

Abstract (from CDS):

The massive black hole at the center of the Milky Way, SagittariusA* (SgrA*) is, in relative terms, the weakest accreting black hole accessible to observations. It has inspired the theoretical models of radiatively inefficient accretion. Unfortunately, our knowledge of the mean SED and source structure of SgrA* is very limited owing to numerous observational difficulties. At the moment, the mean SED of SgrA* is only known reliably in the radio to mm regimes. The goal of this paper is to provide constraints on the mean emission from SgrA* in the near-to-mid infrared. Sensitive images of the surroundings of SgrA* at 8.6µm, 4.8µm, and 3.8µm were produced by combining large quantities of imaging data. Images were produced for several observing epochs. Excellent imaging quality was reached in the MIR by using speckle imaging combined with holographic image reconstruction, a novel technique for this kind of data. No counterpart of SgrA* is detected at 8.6 µm. At this wavelength, SgrA* is located atop a dust ridge, which considerably complicates the search for a potential point source. An observed 3σ upper limit of ∼10mJy is estimated for the emission of SgrA* at 8.6µm, a tighter limit at this wavelength than in previous work. The de-reddened 3σ upper limit, including the uncertainty of the extinction correction, is ∼84mJy . Based on the available data, it is argued that, with currently available instruments, SgrA* cannot be detected in the MIR, not even during flares. At 4.8µm and 3.8µm, on the other hand, SgrA* is detected at all times, at least when considering timescales of a few up to 13 min. We derive well-defined time-averaged, de-reddened flux densities of 3.8±1.3mJy at 4.8µm and 5.0±0.6mJy at 3.8µm. Observations with NIRC2/Keck and NaCo/VLT from the literature provide good evidence that SgrA* also has a fairly well-defined de-reddened mean flux of 0.5-2.5mJy at wavelengths of 2.1-2.2µm. We present well-constrained anchor points for the SED of SgrA* on the high-frequency side of the Terahertz peak. The new data are in general agreement with published theoretical SEDs of the mean emission from SgrA*, but we expect them to have an appreciable impact on the model parameters in future theoretical work.

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Journal keyword(s): black hole physics - instrumentation: high angular resolution - instrumentation: adaptive optics - Galaxy: center

Simbad objects: 25

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2020.10.26-19:31:39

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