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IRAS observations of NGC 1052

Neugebauer, G. and Soifer, B. T. and Rice, W. and Rowan-Robinson, M. (1984) IRAS observations of NGC 1052. Publications of the Astronomical Society of the Pacific, 96 (586). pp. 973-976. ISSN 0004-6280. http://resolver.caltech.edu/CaltechAUTHORS:20170307-102730603

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Abstract

The galaxy NGC 1052 has been observed with the IRAS satellite. The infrared emission at 100 microns is substantially larger than a smooth extrapolation of the radio data. Because of the large diaphragm size of IRAS, it is impossible to decide uniquely if the infrared radiation represents a self-absorbed nonthermal spectrum or thermal reradiation by heated dust.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/131461DOIArticle
http://iopscience.iop.org/article/10.1086/131461PublisherArticle
Additional Information:© 1984 Astronomical Society of the Pacific. Received 9 August 1984. The Infrared Astronomical Satellite (IRAS) was developed and operated by the Netherlands Agency for Aerospace Programs (NIVR), the United States National Aeronautics and Space Administration (NASA), and the United Kingdom Science and Engineering Research Council (SERC). We thank all our colleagues on the ZRAS team for making the mission a success. In particular, we thank E. Kopan and C. Oken for their help in reducing the observations. D. Heeschen, Η. and M. Aller, and T. Haddock kindly provided us with concurrent radio measurements of NGC 1052 and of the radio sources. Conversations with C. Impey were most helpful as well as discussions with T. dejong, H. Habing, J. Wrobel, and G. Wynn-Williams.
Subject Keywords:galaxies—infrared emission
Record Number:CaltechAUTHORS:20170307-102730603
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170307-102730603
Official Citation:G. Neugebauer et al 1984 PASP 96 973
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74843
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:07 Mar 2017 18:33
Last Modified:07 Mar 2017 18:33

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