Deep Infrared Imaging of the R Coronae Australis Cloud Core

Details Deep Infrared Imaging of the R Coronae Australis Cloud Core Deep Infrared Imaging of the R Coronae Australis Cloud Core

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aj....114.2029w&link_type=abstract

Astronomical Journal v.114, p.2029

Astronomy and Astrophysics

Astronomy

67

Ism: Clouds, Ism: Individual: R Coronae Australis, Infrared: Ism: Lines And Bands

Scientific paper

Infrared images of the R Coronae Australis molecular core in broad-band J, H, and K' filters and in narrow-band [Fe II] and H2 filters are used to investigate star formation in this nearby cloud. Broad-band images with completeness limits of J=17.5, H=17.0, and K'=16.5 mag have revealed a total of 253,482, and 692 sources, respectively. Color-color and color-magnitude diagrams are used to identify sources associated with the cloud and their evolutionary states. Assuming an age of 3X106 years, our H and K observations have completely sampled young stellar objects with M>0.1 Mmsun through about 80% of the depth of the molecular core. As few as 22, and as many as 40, sources are associated with the cloud. In addition, there are five brown dwarf candidates. The large number of background stars in our sample is the key to the proper interpretation of our color-color diagram. As a result, only 8 sources are observed to have infrared excesses at K', implying a disk frequency for the association members between 16% and 35%. A focus of our study is the Coronet cluster, a compact group of ˜10 young stellar objects associated with the star R Cr A. We find that these objects are associated with extensive reflection nebulae, dust-free cavities, and Herbig-Haro (HH) objects. Detailed study of the HH complexes 99A & B and 104C & D suggests they are associated with winds from cluster members IRS 9 and IRS 5 and/or IRS 6, respectively. The true position of the most deeply embedded cluster member, IRS 7, is established through 10 μm imaging. It appears that young stellar objects in this cluster have formed nearly simultaneously and undoubtedly influenced the formation and evolution of their nearest neighbors.

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