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Hα emission-line stars in molecular clouds: II. The M42 region
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy.
Univ Fed Sergipe, Dept Fis, BR-49100000 Sao Cristovao, SE, Brazil.
Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA;Univ Hawaii Manoa, NASA Astrobiol Inst, Hilo, HI 96720 USA.
2014 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 570, A30Article in journal (Refereed) Published
Abstract [en]

We present a deep survey of Hα emission-line stars in the M 42 region using wide-field objective prism films. A total of 1699 Hαemission-line stars were identified, of which 1025 were previously unknown, within an area of 5.̊5 × 5.̊5 centred on the Trapezium Cluster. We present Hα strength estimates, positions, and JHKs photometry extracted from 2MASS, and comparisons to previous surveys. The spatial distribution of the bulk of the stars follows the molecular cloud as seen in CO and these stars are likely to belong to the very young population of stars associated with the Orion Nebula Cluster. Additionally, there is a scattered population of Hα emission-line stars distributed all over the region surveyed, which may consist partly of foreground stars associated with the young NGC 1980 cluster, as well as some foreground and background dMe or Be stars. The present catalogue adds a large number of candidate low-mass young stars belonging to the Orion population, selected independently of their infrared excess or X-ray emission.

Place, publisher, year, edition, pages
EDP Sciences , 2014. Vol. 570, A30
Keyword [en]
stars: emission-line, Be / stars: formation / stars: pre-main sequence
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy with specialization in Astrophysics
URN: urn:nbn:se:uu:diva-233874DOI: 10.1051/0004-6361/201423594ISI: 000344158500028OAI: diva2:754718

Erratum in: Astronomy and Astrophysics, Vol. 2015:573, C2, doi: 10.1051/0004-6361/201423594e

Available from: 2014-10-12 Created: 2014-10-12 Last updated: 2016-11-24Bibliographically approved

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