Observations of H2 emission from molecular clouds and Herbig-Haro objects

Details Observations of H2 emission from molecular clouds and Herbig-Haro objects Observations of H2 emission from molecular clouds and Herbig-Haro objects

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...265..864s&link_type=abstract

Astrophysical Journal, Part 1, vol. 265, Feb. 15, 1983, p. 864-876.

Other

55

Herbig-Haro Objects, Hydrogen Clouds, Interstellar Matter, Main Sequence Stars, Molecular Clouds, Carbon Monoxide, Emission Spectra, Interstellar Masers, Line Spectra, Luminosity, Water Masers

Scientific paper

Using a CVF spectrometer with a spectral resolution of ∼2%, we have searched a group of molecular clouds, HH sources, and related objects for emission in the v = 1 → O S(l) line of H2 at λ0 = 2.122 μm. Included in this survey were H2O masers with high-velocity components as well as CO hotspots with broad radio emission lines indicative of high-speed molecular flows. Generally our 3 σ detection limit for the integrated S(1) line flux corresponded to 7 × 10-20 W cm-2 in our 34" diameter beam. We present results for six sources that we detected and mapped in the S (1) line (NGC 1333, HH 12, NGC 2071, S255, Sl40, and Cep A), and we report limits for another 18 regions that were searched but not detected (e.g., Ll 551). In the H2 sources that were mapped, we observed line emission over an extended area > 0.2 pc in diameter. For NGC 1333 and Cep A, whose high velocity CO gas appears to be channeled into bipolar flows, we detected H2 emission from the blueshifted CO lobe but not from the redshifted radio lobe. If the redshifted gas lies relatively deeper within the molecular cloud, then differential 2 μm extinction from dust within the cloud might be sufficient to reduce the H2 emission from this part of the flow below our detection limit. By comparison with the Orion H2 source, the surface brightness and luminosity in the S(l) line of the regions detected in this survey are weaker by an order of magnitude or more.

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