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Issue A&A
Volume 381, Number 1, January I 2002
Page(s) L1 - L4
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20011520



A&A 381, L1-L4 (2002)
DOI: 10.1051/0004-6361:20011520

Letter

ISOCAM mid-infrared detection of HR 10: A distant clone of Arp 220 at ${\vec z}$ = 1.44

D. Elbaz1, 2, 3, H. Flores1, P. Chanial1, I. F. Mirabel1, 4, D. Sanders5, P.-A. Duc1, C. J. Cesarsky6 and H. Aussel5

1  CEA Saclay/DSM/DAPNIA/Service d'Astrophysique, Orme des Merisiers, 91191 Gif-sur-Yvette Cedex, France
2  Department of Physics, University of California, Santa Cruz, CA 95064, USA
3  Department of Astronomy & Astrophysics, University of California, Santa Cruz, CA 95064, USA
4  Instituto de Astronomía y Física del Espacio, CONICET, 1428 Ciudad Universitaria, Buenos Aires, Argentina
5  Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, 96822 Honolulu, USA
6  European Southern Observatory, Karl-Schwarzchild-Strasse 2, 85748 Garching bei München, Germany

(Received 13 August 2001 / Accepted 30 October 2001 )

Abstract
We report the detection of the extremely red object (ERO), HR 10 ( $I-K\sim 6.5$, z=1.44), at 4.9 and 6.1 $\mu$m (rest-frame) with ISOCAM, the mid-infrared (MIR) camera onboard the Infrared Space Observatory (ISO). HR 10 is the first ERO spectroscopically identified to be associated with an ultra-luminous IR galaxy (ULIG) detected in the radio, MIR and sub-millimeter. The rest-frame spectral energy distribution (SED) of HR 10 is amazingly similar to the one of Arp 220, scaled by a factor $3.8\pm1.3$. The corresponding 8-1000 $\mu$m luminosity (~7 $\times$10 $^{12}~h_{70}^{-2}~L_{\odot}$) translates into a star formation rate of about $1200~h_{70}^{-2}~M_{\odot}$ yr -1 if HR 10 is mostly powered by star formation. We address the key issue of the origin of the powerful luminosity of HR 10, i.e. starburst versus active galactic nucleus (AGN), by using the similarity with its closeby clone, Arp 220.


Key words: galaxies: evolution -- infrared: galaxies

Offprint request: D. Elbaz, delbaz@cea.fr

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© ESO 2002


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