High-resolution IRAS observations of the Rho Ophiuchi cloud core

1986 ◽  
Vol 304 ◽  
pp. L45 ◽  
Author(s):  
E. T. Young ◽  
C. J. Lada ◽  
B. A. Wilking
Keyword(s):  
High Resolution ◽  
Rho Ophiuchi ◽  
Cloud Core

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⊙).

scholarly journals Dense core structure and fragmentation in the Rho Ophiuchi molecular cloud

1991 ◽  
Vol 147 ◽  
pp. 229-233
Author(s):  
Alwyn Wootten
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Molecular Cloud ◽  
Surface Density ◽  
Core Structure ◽  
Dense Core ◽  
Dense Cores ◽  
Rho Ophiuchi ◽  
Very High ◽  
Taurus Molecular Cloud

About a dozen distinct dense cores have been identified in the Rho Ophiuchi molecular cloud. The properties of these cores are summarized and compared to the properties of cores in the Taurus molecular cloud, a less efficient region of star formation, and in DR21(OH), a more massive region of star formation. The data are consistent with a picture in which more massive clouds have a higher surface density of cores, which in turn are more massive. The adjacent cores in L1689N have been studied with very high resolution; one has formed stars and one never has. The structure of these cores shows a tendency for duplicity of structures from the largest scales (1 pc) to the smallest (50 AU).

ROSAT X-ray sources embedded in the rho Ophiuchi cloud core

1995 ◽  
Vol 439 ◽  
pp. 752 ◽  
Author(s):  
Sophie Casanova ◽  
Thierry Montmerle ◽  
Eric D. Feigelson ◽  
Philippe Andre
Keyword(s):  
X Ray ◽  
Rho Ophiuchi ◽  
Cloud Core

scholarly journals Small-Scale Structure of the Mon R2 Cloud Core

1994 ◽  
Vol 140 ◽  
pp. 266-267
Author(s):  
TH. Henning ◽  
R. Chini ◽  
W. Pfau
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Formation Process ◽  
Molecular Clouds ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure ◽  
Ir Sources ◽  
Cloud Core

High-resolution mm continuum observations are especially well suited to detect clumpy structures in molecular clouds. In this paper we concentrate on the Mon R2 cloud core which is associated with a cluster of IR sources. Walker et al. (1990) made a 1.3 mm map with 30″ resolution. They found an unresolved and elongated structure extending from NE to SW. Here, we discuss high-resolution continuum maps at 870 and 1300 µm showing a rich clumpy structure on the scale of several 10 arcsec. The clumps are probably intimately linked to the star formation process in Mon R2.

scholarly journals Dense core structure and fragmentation in the Rho Ophiuchi molecular cloud

1991 ◽  
Vol 147 ◽  
pp. 229-233
Author(s):  
Alwyn Wootten
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Molecular Cloud ◽  
Surface Density ◽  
Core Structure ◽  
Dense Core ◽  
Dense Cores ◽  
Rho Ophiuchi ◽  
Very High ◽  
Taurus Molecular Cloud

About a dozen distinct dense cores have been identified in the Rho Ophiuchi molecular cloud. The properties of these cores are summarized and compared to the properties of cores in the Taurus molecular cloud, a less efficient region of star formation, and in DR21(OH), a more massive region of star formation. The data are consistent with a picture in which more massive clouds have a higher surface density of cores, which in turn are more massive. The adjacent cores in L1689N have been studied with very high resolution; one has formed stars and one never has. The structure of these cores shows a tendency for duplicity of structures from the largest scales (1 pc) to the smallest (50 AU).

Self-gravitational collapse of a magnetized cloud core: high resolution simulations with three-dimensional MHD nested grid

2004 ◽  
Vol 164 (1-3) ◽  
pp. 229-236 ◽  
Author(s):  
Tomoaki Matsumoto ◽  
Masahiro N. Machida ◽  
Kohji Tomisaka ◽  
Tomoyuki Hanawa
Keyword(s):  
High Resolution ◽  
Gravitational Collapse ◽  
Three Dimensional ◽  
Nested Grid ◽  
Cloud Core

The evolutionary status of the stellar population in the rho Ophiuchi cloud core

1995 ◽  
Vol 438 ◽  
pp. 813 ◽  
Author(s):  
Karen M. Strom ◽  
Jeremy Kepner ◽  
Stephen E. Strom
Keyword(s):  
Stellar Population ◽  
Evolutionary Status ◽  
Rho Ophiuchi ◽  
Cloud Core

scholarly journals High-Resolution Molecular Line Observations of the Core and Outflow in Orion B

1989 ◽  
Vol 120 ◽  
pp. 339-339
Author(s):  
J.S. Richer ◽  
R.E. Hills ◽  
R. Padman
Keyword(s):  
High Resolution ◽  
Central Axis ◽  
Molecular Gas ◽  
Kinetic Temperature ◽  
Excitation Temperature ◽  
Molecular Line ◽  
Core Mass ◽  
The Core ◽  
Molecular Outflow ◽  
Cloud Core

High-resolution CO J → 1 → 2 observations of the Orion B molecular outflow show that the outflow is unipolar, and that there is evidence of acceleration of molecular gas at up to 0.5pc from the driving star. The highest-velocity material, as well as being furthest from the source, seems to lie close to the central axis of the flow, and is presumably being accelerated by entrainment in the flow or jet emanating from the star. We have also mapped the HCO+J = 3 → 2 emission at 19-arcsec resolution. We derive an excitation temperature of around 25 K in the cloud core, and a core mass of about 75 M⊙, this estimate is in accord with a model in which the core has a kinetic temperature of 30-50 K, with no molecular depletion on to grains. This is in contrast to the recent suggestion that the core contains cold isothermal protostars.

Observations of the spatial structure of interstellar hydrogen

1967 ◽  
Vol 31 ◽  
pp. 45-46
Author(s):  
Carl Heiles
Keyword(s):  
High Resolution ◽  
Spatial Structure ◽  
Velocity Dispersion ◽  
Temperature Variations

High-resolution 21-cm line observations in a region aroundlII= 120°,b11= +15°, have revealed four types of structure in the interstellar hydrogen: a smooth background, large sheets of density 2 atoms cm-3, clouds occurring mostly in groups, and ‘Cloudlets’ of a few solar masses and a few parsecs in size; the velocity dispersion in the Cloudlets is only 1 km/sec. Strong temperature variations in the gas are in evidence.

Combining integrated systems-biology approaches with intervention-based experimental design provides a higher-resolution path forward for microbiome research

2019 ◽  
Vol 42 ◽  
Author(s):  
J. Alfredo Blakeley-Ruiz ◽  
Carlee S. McClintock ◽  
Ralph Lydic ◽  
Helen A. Baghdoyan ◽  
James J. Choo ◽  
...  
Keyword(s):  
Systems Biology ◽  
High Resolution ◽  
Experimental Design ◽  
Integrated Systems ◽  
Microbiome Research ◽  
Constructive Criticism

Abstract The Hooks et al. review of microbiota-gut-brain (MGB) literature provides a constructive criticism of the general approaches encompassing MGB research. This commentary extends their review by: (a) highlighting capabilities of advanced systems-biology “-omics” techniques for microbiome research and (b) recommending that combining these high-resolution techniques with intervention-based experimental design may be the path forward for future MGB research.

Sign in / Sign up

Export Citation Format

Share Document