A New 20 microns Upper Limit for SGR A*

Details A New 20 microns Upper Limit for SGR A* A New 20 microns Upper Limit for SGR A*

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...184.5801g&link_type=abstract

American Astronomical Society, 184th AAS Meeting, #58.01; Bulletin of the American Astronomical Society, Vol. 26, p.954

Astronomy and Astrophysics

Astronomy

Scientific paper

We have made 20.0 microns imaging array observations of the core of the Sgr A West complex with the 58 times 62 pixel array camera system developed at NASA/Goddard. The image was analyzed using four methods: 1) adding and subtracting a set of synthetic point sources of decreasing brightness at the position of Sgr A* to determine a threshold of detection, 2) subtracting a smoothed version of the same image to remove the extended source component, 3) subtracting a version of the same image with the position of Sgr A* patched over by two-dimensional interpolation, and 4) deconvolution of the image using the Richardson-Lucy algorithm. As a result of this analysis, we conclude that no contribution can be attributed to Sgr A* at 20 microns above an observed brightness upper limit of 0.3 Jy arcsec(-2) , or a total observed point source flux density upper limit of 1.0 Jy, with an uncertainty estimated at about +/-0.5 Jy. Among possible implications of the present observations, our result clearly constrains models for either thermal dust emission or self-absorbed synchrotron emission. Our upper limit of ~ 1 Jy could eliminate temperatures T > 2 times 10(4) K in accretion disk models of Sgr A*.

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