H and K maps of two star-forming regions: S 140 and CEP A OB3

Details H and K maps of two star-forming regions: S 140 and CEP A OB3 H and K maps of two star-forming regions: S 140 and CEP A OB3

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986inpr.conf...31g&link_type=abstract

In NASA. Ames Research Center Summer School on Interstellar Processes: Abstracts of Contributed Papers p 31-32 (SEE N87-15043 0

Astronomy and Astrophysics

Astronomy

Astronomical Maps, Cepheus Constellation, Infrared Radiation, Luminosity, Molecular Clouds, Radio Emission, Spectral Emission, Star Formation, Protostars, Space Observations (From Earth)

Scientific paper

The molecular clouds near S 140 and Cep A OB3 both contain regions that emit strongly in the infrared but which have relatively little or no emission in radio wavelengths. The lack of radio emission is usually interpreted to mean that little ionization has taken place, and that the IR emission comes from dust heated by a central pre-main sequence object. We have made high resolution maps of these two areas with H and K broadband filters with the 2.3m telescope of the Wyoming Infrared Observatory (WIRO). Our observations were made with an InSb detector using the standard WIRO mapping technique of multiple scanning to construct a series of 64x64 pictures. Our scanning was made in one arcsec steps with a 7 inch aperture to produce a resolution of about 6 sec FWHM. Observations of S 140 by Blair et al (1978) with moderate resolution in J, H, and K, revealed a prominent IR source that they called S 140IR. We have scanned an area surrounding their S 140IR region and have obtained total IR fluxes which are in close agreement with Blair et al. Additional detail corresponds to that seen by Dinerstein et al (1979) at 0.9 microns and Campbell (1986) at 1.0 microns. The large (H-K) values for all components of S 140IR indicates that they are probably embedded in the parent molecular cloud with A(v) = 25 mag and A(K) = 2.2 mag. Recent radio studies of Cep A by Hughes and Wouterloot (1984) and FIR studies by Evans et al (1981) have shown the similarity of Cep A to S 140. There is, however, some emission detected from ionized regions by the radio observations, indicating a slightly more advanced stage of evolution for Cep A. We observed an area around the strongest source in Cep A in both H and K, and the K map is presented. We have identified three sources separate from the main source.

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