SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 363, 253-268 (2000)

Next Section Table of Contents

The ISO-LWS map of the Serpens cloud core

I. The SEDs of the IR/SMM sources *

B. Larsson 1, R. Liseau 1, A.B. Men'shchikov 1, G. Olofsson 1, E. Caux 2, C. Ceccarelli 3, D. Lorenzetti 4, S. Molinari 5, B. Nisini 4, L. Nordh 1, P. Saraceno 6, F. Sibille 7, L. Spinoglio 6 and G.J. White 1,8,9

1 Stockholm Observatory, 133 36 Saltsjöbaden, Sweden (bem@astro.su.se)
2 CESR CNRS-UPS, B.P. 4346, 31028 Toulouse Cedex 04, France
3 Observatoire Grenoble, 414 rue de la Piscine, B.P. 53X, 38041 Grenoble Cedex, France
4 Osservatorio Astronomico di Roma, Via Osservatorio 2, 00040 Monteporzio, Italy
5 IPAC/Caltech, MS 100-22, Pasadena, California, USA
6 Istituto di Fisica dello Spazio Interplanetario CNR, Tor Vergata, Via Fosso del Cavaliere, 00133 Roma, Italy
7 Observatoire de Lyon, 69230 St. Genis-Laval, France
8 Queen Mary and Westfield College, Department of Physics, University of London, Mile End Road, London E1-4NS, UK
9 Astrophysics Group, The Cavendish Laboratory, University of Cambridge, Madingly Road, Cambridge CB3 OHE, UK

Received 6 March 2000 / Accepted 14 July 2000

Abstract

ISO -LWS mapping observations of the Serpens molecular cloud core are presented. The spectral range is [FORMULA] µm and the map size is 8´ [FORMULA] 8´. These observations suffer from severe source confusion at FIR wavelengths and we employ a Maximum Likelihood Method for the spectro-spatial deconvolution. The strong and fairly isolated source SMM 1/FIRS 1 presented a test case, whose modelled spectral energy distribution (SED), within observational errors, is identical to the observed one. The model results for the other infrared and submillimetre sources are therefore likely to represent their correct SEDs. Simulations demonstrating the reliability and potential of the developed method support this view.

It is found that some sources do not exhibit significant FIR emission and others are most likely not pointlike at long wavelengths. In contrast, the SEDs of a number of SMMs are well fit by modified single-temperature blackbodies over the entire accessible spectral range. For the majority of sources the peak of the SEDs is found within the spectral range of the LWS and derived temperatures are generally higher ([FORMULA] K) than have been found by earlier deconvolution attempts using IRAS data. SMM sizes are found to be only a few arcsec in diameter. In addition, the SMMs are generally optically thick even at LWS wavelengths, i.e. estimated [FORMULA] are in the range 160-270 µm.

The Rayleigh-Jeans tails are less steep than expected for optically thin dust emission. This indicates that the SMMs are optically thick out to longer wavelengths than previously assumed, an assertion confirmed by self-consistent radiative transfer calculations. Models were calculated for five sources, for which sufficient data were available, viz. SMM 1, 2, 3, 4 and 9. These models are optically thick out to millimetre wavelengths (wavelength of unit optical depth 900 to 1 400 µm). Envelope masses for these SMMs are in the range 2-6 [FORMULA], which is of course considerably more massive than estimates based on the optically thin assumption. The luminosities are in the range 10-70 [FORMULA], suggesting the formation of low-mass to intermediate mass stars, so that the existence of such massive envelopes argues for extreme youth of the SMMs in the [FORMULA].

Finally, we present, for the first time, the full infrared SEDs for the outburst source DEOS, both at high and low intensity states.

Key words: ISM: individual objects: Serpens cloud core – ISM: clouds – ISM: general – ISM: dust, extinction – stars: formation

* Based on observations with Iso, an Esa project with instruments funded by Esa Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of Isas and Nasa.

Send offprint requests to: B. Larsson (bem@astro.su.se)

SIMBAD Objects

Contents

Next Section Table of Contents

© European Southern Observatory (ESO) 2000

Online publication: December 5, 2000
helpdesk.link@springer.de