Detection of radio emission from MWC957

Journal Article · Mon Sep 17 04:00:00 EDT 1973 · Nature (London) Phys. Sci., v. 245, no. 142, p. 39

DOI:https://doi.org/10.1038/physci245039a0· OSTI ID:4367364

Feldman, P A; Purton, C R; Marsh, K A

MCW957 is an early-type emission line object with an infrared excess, and is a stellar object that has been described as a B/sub 0/ star and as a planetary nebula. Radio emission was detected at 2.8 cm. (10.63 GHz) using the 46m. telescope of the Algonquin Radio Cbservatory, between June 30 and July 5, 1973. The observed mean flux density was 68 plus or minus 10mfu. It was found that the predicted flux density at 2.8 cm was greater than that actually observed by a factor of ~2. Assuming that the bremsstrahlung mechanism is responsible for the infrared emission, it can be concluded that the object is optically thick at 2.8 cm. The maximum flux density is expected to be ~100 mfu at ~30 GHz. (UK)

• Research Organization: York Univ., Toronto
• NSA Number: NSA-29-013469
• OSTI ID: 4367364
• Journal Information: Nature (London) Phys. Sci., v. 245, no. 142, p. 39, Journal Name: Nature (London) Phys. Sci., v. 245, no. 142, p. 39; ISSN NPSCA
• Country of Publication: United Kingdom
• Language: English

Related Subjects

*STARS-- RADIOWAVE RADIATION
COSMIC RADIO SOURCES
FLUX DENSITY
GHZ RANGE 01-100
INFRARED RADIATION
N56200* --Physics (Astrophysics & Cosmology)--Stars
PLANETARY NEBULAE