The nature of the infrared cluster in the R Coronae Australis cloud core

Details The nature of the infrared cluster in the R Coronae Australis cloud core The nature of the infrared cluster in the R Coronae Australis cloud core

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986aj.....92..103w&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 92, July 1986, p. 103-110. Research supported by the University of Missouri.

Astronomy and Astrophysics

Astronomy

51

Infrared Astronomy, Molecular Clouds, Nebulae, Star Clusters, A Stars, B Stars, Cosmic Dust, Spectral Energy Distribution, T Tauri Stars

Scientific paper

Evidence is presented which suggests that a gravitationally bound stellar subgroup is forming within the dense core of the R Coronae Australis molecular cloud. Using new 1.6-20-micron photometry of 2-micron photometry of 2 solar luminosities sources observed toward the core, it becomes possible to distinguish between field stars and association members, estimate the bolometric luminosities for embedded sources, and estimate the total cloud extinction from background field stars. Thirteen embedded sources are found within a 0.08-sq pc area of the core which display a wide variety of evolutionary states. Their bolometric luminosities range from 1-130 solar luminosities; the B8-A0 stars R Cr A and TY Cr A are the dominant luminosity sources. A total mass for this embedded cluster of 19 solar masses implies a star-formation efficiency of about 45 percent in this localized region of the cloud. The significance of this high efficiency is discussed through the comparison of the R Cr A cluster with theoretical models for bound cluster formation and with other low-mass infrared clusters in nearby clouds.

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