Multi-wavelength observations of the star forming region in L1616

Creators: Alcalá, J. M.; Wachter, S.; Covino, E.; Sterzik, M. F.; Durisen, R. H.; Freyberg, M. J.; Hoard, D. W.; Cooksey, K.

Abstract

We present the results of a multi-wavelength study of the star forming region in L1616. Our observations include ROSAT All-Sky Survey (RASS) and High Resolution Imager (HRI) X-ray observations, optical wide-field imaging and near-IR imaging data and optical long-slit and multi-object spectroscopic follow-up. 22 new low-mass pre-main sequence (PMS) stars are found to be distributed mainly to the East of the L1616 cometary cloud, in about a one-square-degree field. We find that the class-III infrared sources outnumber the class-II infrared sources by a factor of about three. The X-ray properties of the PMS stars in L1616 are quite similar to those of PMS stars detected in the Orion Nebula Cluster. The comparison of the position of the L1616 PMS stars in the HR diagram with theoretical PMS evolutionary tracks yields an average age of 1–2 Myr, with a very small age spread of about 1 Myr. Unlike the fossil star forming regions in Orion, L1616 appears to be a region of on-going star formation relatively far from the Orion A and B clouds. Given the small age spread, the spatial distribution of the PMS stars relative to the head of the cloud, as well as its cometary shape and high star formation efficiency, we conclude that the star formation in L1616 was most likely induced by a single event, the impact of the winds of the massive stars of the Orion OB association or a supernova explosion being the possible triggers. The Initial Mass Function (IMF) in L1616 is roughly consistent with that of the field in the mass range 0.3 < M/M_⊙ < 2.5. Several faint objects, detected in our optical images, are good candidates for young Brown Dwarfs (BDs). We might expect the number of BDs in L1616 to be intermediate between Taurus and the Trapezium.

Additional Information

© 2014 ESO. Received: 10 October 2003. Accepted: 28 November 2003. We thank the anonymous referee for his/her comments. We thank F. Palla, L. Testi and A. Natta for discussions. We also thank the Calar Alto staff, in particular F. Hoyo, M. Alises and A. Aguirre for their technical support. We also thank the WIYN telescope staff, in particular Gillian Rosenstein and Wendy Shook for their technical support during the observations. We also acknowledge A. Mejia for her assistantship during the HYDRA observations. We thank the ESO 2.2 m telescope team for their support during the WFI observations. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research was conducted in part during the 2001 Research Experiences for Undergraduates (REU) Program at Cerro Tololo Inter-American Observatory (CTIO). The CTIO REU Program is funded by the National Science Foundation (NSF). CTIO is operated by AURA, Inc., under cooperative agreement with the NSF. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

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