A high density molecular fragment in the Rho OPH cloud

Details A high density molecular fragment in the Rho OPH cloud A high density molecular fragment in the Rho OPH cloud

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...141..127z&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 141, no. 1, Dec. 1984, p. 127-130.

Astronomy and Astrophysics

Astrophysics

23

Ammonia, Interstellar Gas, Molecular Clouds, Radial Velocity, Spatial Distribution, Spectral Line Width, Stellar Evolution, Temperature Distribution

Scientific paper

Ammonia observations of the high density (n/H2/ is greater than or equal to 1,000,000 per cu cm) fragment Rho Oph B (Loren et al., 1980; Martin-Pintado et al., 1983) and the HCO(+) and Rho Oph A peaks (Loren et al., 1982, 1983) are presented. In Rho Oph B, the ammonia emission appears to be formed in the high density region, since the linewidth, radial velocity and spatial distribution agree with that of the dense gas. With the employed 40 sec resolution, the object begins to break up into two peaks of angular size approximately 50 sec (after correction for the beam). At the intensity peak, TK is approximately 18 K; toward the edges of the NH3 cloud, TK = 19 K. There is no hint of collapse motions from the spatial variations of linewidths or velocities. This suggests that no high mass stars have yet formed in this region. Over the whole region, the widths (FWHP) are approximately 1.2 km/s and the average radial velocity is 3.6 km/s. Toward the NH3 peak, the total optical depth is aproximately 2.7 + or - 0.5, while averaged over the edges of the cloud, it is 0.9 + or - 0.4. There are NH3 peaks, extended over approximately 90 sec x 90 sec toward Rho Oph A and the HCO(+) peak. The value of TK is approximately 45 K and the total optical depth in the (1,1) line is approximately 0.4.

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