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Astron. Astrophys. 364, 348 (2000)


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Erratum

Sub-mm and X-ray background: Two unrelated phenomena?

P. Severgnini 1, R. Maiolino 2, M. Salvati 2, D. Axon 3, A. Cimatti 2, F. Fiore 4, R. Gilli 1,5, F. La Franca 6, A. Marconi 2, G. Matt 6, G. Risaliti 1 and C. Vignali 7,8

1 Università di Firenze, Dipartimento di Astronomia, Largo E. Fermi 5, 50125 Firenze, Italy
2 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
3 University of Hertfordshire, Department of Physical Sciences, College Lane, Hatfield, Herts AL10 8 AB, UK
4 Osservatorio Astronomico di Roma, Via Frascati 33, 00044 Monteporzio Catone, Italy
5 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Postsdam, Germany
6 Università degli Studi "Roma Tre", Dipartimento di Fisica, Via della Vasca Navale 84, 00146 Roma, Italy
7 Università di Bologna, Dipartimento di Astronomia, Via Ranzani 1, 40127 Bologna, Italy
8 Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy

Astron. Astrophys. 360, 457-462 (2000)


Due to an unfortunate printing error figure 1 has not been printed in colour. Following this text please find the coloured version of Fig. 1.

[FIGURE] Fig. 1. Distribution of the observed sub-mm to hard X-ray spectral indices [FORMULA] as a function of redshift. Filled squares are the HELLAS sources observed by us. Empty squares are the sources reported by F00. The filled circles are Chandra hard-X sources detected by M00 in the SSA13 field. The shaded areas give the distribution of lower limits for the SCUBA sources detected by B99 in the SSA13 field but undetected by Chandra. The empty circles are sources in the HDFN reported by H00. Dark and light blue symbols indicate 2-10 keV sources detected in different ranges of flux (see legend), while red symbols indicate SCUBA sources which were not detected by Chandra in the 2-10 keV band. Templates derived from various types of known active galaxies are shown (see text). Stars are high-z QSOs detected by SCUBA. The thick horizontal segments give the [FORMULA] of the cosmic background and of sources having a factor of 10 lower sub-mm flux relative to the 5 keV flux.


Send offprint requests to: P. Severgnini (paolas@arcetri.astro.it)


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© European Southern Observatory (ESO) 2000

Online publication: December 15, 2000
helpdesk.link@springer.de


© European Southern Observatory (ESO) 2000

Online publication: December 15, 2000

helpdesk.link@springer.de