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Star formation in the southern complex region NGC 3576

Published online by Cambridge University Press:  04 August 2017

P. Persi ,
M. Perrari-Toniolo  and
L. Spinoglio
P. Persi
Affiliation:
Istituto di Astrofisica Spaziale, CNR, P.O. Box 67 00044 Frascati Italy
M. Perrari-Toniolo
Affiliation:
Istituto di Astrofisica Spaziale, CNR, P.O. Box 67 00044 Frascati Italy
L. Spinoglio
Affiliation:
Istituto di Astrofisica Spaziale, CNR, P.O. Box 67 00044 Frascati Italy

Extract

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NGC 3576 (RCW 57) is a very bright optically visible nebula (~10' in size) located near the galactic plane at a distance of 3.6kpc. The region is associated with the HII region G291.28–0.71 (Retallack & Goss), and with a giant molecular cloud of M≃9×104 M⊙ (Cheung et al.1980) The source is reported in the IRAS Small Scale Structure Catalog. From the observed far-IR fluxes we derive a total luminosity of L(FIR)≃7×105 L⊙, suggesting that at least seven possible 07–09 stars could ionize the entire observed region. A cluster of five IR sources and extended 10μm emission were found by Frogel & Persson (1974). IRS 1 is a very compact object (<3'), while IRS 2–5 show diffuse infrared emission. In addition IRS 2, very close to IRS 1, is coincident with the radio emission peak. An H2O maser source and NH3 emission are present in the complex region.

We present multidiaphragm photometry from 1 to 20μm of 1RS 1, IRS 3 and IRS 4 and CVF observations between 2-μm and 8–13μm of IRS 1, collected at the 1m and 3.6m ESO telescopes.

Type
Bipolar Flows, Jets and Protostars
Information
Symposium - International Astronomical Union , Volume 122: Circumstellar Matter , 1987 , pp. 93 - 94
Copyright
Copyright © Reidel 1987 

References

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