The nature and distribution of carbon recombination-line emission in the rho Ophiuchi dark cloud

1974 ◽  
Vol 192 ◽  
pp. 607 ◽  
Author(s):  
R. L. Brown ◽  
R. H. Gammon ◽  
G. R. Knapp ◽  
B. Balick
Keyword(s):  
Line Emission ◽  
Recombination Line ◽  
Dark Cloud ◽  
Rho Ophiuchi

scholarly journals Two New Recombination-Line Results

1974 ◽  
Vol 60 ◽  
pp. 81-85
Author(s):  
F. J. Kerr ◽  
P. D. Jackson ◽  
G. R. Knapp ◽  
R. L. Brown
Keyword(s):  
Line Emission ◽  
Recombination Line ◽  
Ionized Gas ◽  
Dark Cloud ◽  
Hydrogen Recombination

This paper reports two new recombination-line results. The first is the detection of carbon line emission from the dark cloud near ϱ Ophiuchi, and the second discusses the origin of hydrogen recombination line emission associated with ionized gas outside known discrete continuum sources.

scholarly journals Contagious B Star Formation in the Rho Ophiuchi Dark Cloud

1980 ◽  
Vol 87 ◽  
pp. 183-184
Author(s):  
E. Falgarone
Keyword(s):  
Star Formation ◽  
Line Emission ◽  
Hii Regions ◽  
Young Stars ◽  
Dark Cloud ◽  
Continuum Source ◽  
Rho Ophiuchi ◽  
Co Emission ◽  
The Continuum ◽  
Compact Hii Regions

Three young stars are still embedded in the small (0.7 pc wide) and densest region of the Rho Ophiuchi dark cloud. One of these stars coincides with the continuum source Oph 4 (Brown and Zuckerman, 1975). Their existence is indicated by the following: i) thermal continuum sources detected at 21 cm and 6 cm with the Westerbork Synthesis Radiotelescope (Netherlands) which display the presence of compact HII regions surrounding each of three stars; ii) peaks of CO emission (J = 1 → 0 transition) detected with the MWO antenna of MacDonald (Texas) which are associated with asymmetrically shaped lines; iii) C 158α (and S 158α for Oph 4) line emission mapped with the Nancay Radiotelescope. All these observations imply that the three stars have B3 - B2 spectral types.

scholarly journals A Remarkable Bipolar Flow in the Center of the Rho Ophiuchi Cloud

1989 ◽  
Vol 120 ◽  
pp. 300-300
Author(s):  
Ph. Andre ◽  
J. Martin-Pintado ◽  
D. Despois ◽  
T. Montmerle
Keyword(s):  
Mass Loss Rate ◽  
Extreme Case ◽  
Width Ratio ◽  
Dark Cloud ◽  
Molecular Outflow ◽  
Ir Sources ◽  
Near Ir ◽  
Exciting Source ◽  
Rho Ophiuchi ◽  
Cloud Core

Using the IRAM 30-m telescope in August and December 1988, we have discovered the first molecular outflow in the central part (L1688) of the nearby ρ Ophiuchi dark cloud. This outflow, found in the J = 2 — 1 line of 12CO near the cloud core A, is an extreme case, weak (outflow mass-loss rate ≈ 5 x 10−8M⊙yr−1) and highly collimated (lenght to width ratio > 14), which explains why it has escaped previous detections with smaller telescopes. The high-velocity molecular gas is hot and optically thin, making the J = 2 — 1 line of 12CO ≈ 3-4 times stronger than the J = 1 — 0 line. Unexpectedly, this outflow does not appears to be driven by any of the embedded near-IR sources known in this region previous deep VLA surveys of the cloud (André, Montmerle, and Feigelson, 1987; Stine et al., 1988; André et al., in prep.). The outflow exciting source is thus probably a very low-luminosity ((L < 0.1L⊙) young stellar object. Using the 30-m equipped with the MPIfIR bolometer, we have very recently found (March 1989) that this object is the strongest continuum point source of L1688 at 1.3 mm. By analogy with L1551-IRS5 and HL Tau, the radio properties of this source suggest that it possesses a weak, possibly collimated, ionized wind and a relatively massive, cold circumstellar disk (Mdisk ≈0.1M⊙).

An investigation of grain properties in the Rho Ophiuchi dark cloud

1993 ◽  
Vol 105 ◽  
pp. 1010 ◽  
Author(s):  
Frederick J. Vrba ◽  
George V. Coyne ◽  
Santiago Tapia
Keyword(s):  
Dark Cloud ◽  
Rho Ophiuchi ◽  
Grain Properties

/C-13/O self-absorption in the Rho Ophiuchi dark cloud

1980 ◽  
Vol 238 ◽  
pp. 620 ◽  
Author(s):  
C. J. Lada ◽  
B. A. Wilking
Keyword(s):  
Dark Cloud ◽  
Rho Ophiuchi
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