scholarly journals Evidence for triggered star formation in the Carina Flare supershell

2006 ◽  
Vol 2 (S237) ◽  
pp. 406-406 ◽  
Author(s):  
Joanne Dawson ◽  
A. Kawamura ◽  
N. Mizuno ◽  
T. Onishi ◽  
Y. Fukui
Keyword(s):  
Molecular Clouds ◽  
Large Scale ◽  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Star Forming Regions ◽  
Active Intermediate ◽  
Ambient Gas ◽  
Hi Shells ◽  
Intermediate Mass Star

AbstractTheory predicts the triggered formation of molecular clouds stars through the fragmentation and collapse of swept-up ambient gas. Yet the majority of Galactic HI shells show no more than a scattering of small molecular clouds. The Carina Flare supershell (Fukui et al. 1999) is a rare example of an HI shell with a striking molecular component. Here we present the large-scale morphology of the molecular and atomic gas and the location of YSO candidates. A detailed look at two molecular clumps in the shell walls reveals active, intermediate mass star forming regions at various stages of early evolution.

scholarly journals AN EXTENSIVE, SENSITIVE SEARCH FOR SiO MASERS IN HIGH- AND INTERMEDIATE-MASS STAR-FORMING REGIONS

2009 ◽  
Vol 691 (1) ◽  
pp. 332-341 ◽  
Author(s):  
Luis A. Zapata ◽  
Karl Menten ◽  
Mark Reid ◽  
Henrik Beuther
Keyword(s):  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Star Forming Regions ◽  
Intermediate Mass Star

scholarly journals A SAMPLE OF INTERMEDIATE-MASS STAR-FORMING REGIONS: MAKING STARS AT MASS COLUMN DENSITIES <1 g cm–2

2010 ◽  
Vol 140 (2) ◽  
pp. 462-479 ◽  
Author(s):  
K. Arvidsson ◽  
C. R. Kerton ◽  
M. J. Alexander ◽  
H. A. Kobulnicky ◽  
B. Uzpen
Keyword(s):  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Star Forming Regions ◽  
Intermediate Mass Star

scholarly journals Survey observations of large-scale molecular outflows associated with intermediate-mass protostar candidates in the OMC-2/3 region

2006 ◽  
Vol 2 (S237) ◽  
pp. 479-479
Author(s):  
Satoko Takahashi ◽  
Y. Shimajiri ◽  
S. Takakuwa ◽  
M. Saito ◽  
R. Kawabe
Keyword(s):  
Large Scale ◽  
Driving Mechanism ◽  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Molecular Outflows ◽  
Star Forming Regions ◽  
North East ◽  
The North ◽  
Molecular Outflow

AbstractWe have newly performed millimeter- and submillimeter-wave observations in the nearest GMC: the Orion Molecular Cloud -2/3 region (OMC-2/3). Here, we report results of our large-scale (22' × 14') outflow survey with the Atacama Submillimeter Telescope Experiment (ASTE) in the CO(3-2) emission. The OMC-2/3 region is one of the famous intermediate-mass star-forming regions and harbors several sources diagnosed as Class0 protostars (Chini et al. 1997). With the intensive ASTE observations, we totally identified the 8 clear, 5 probable and 6 marginal outflows in OMC-2/3. 8 clear outflows from them, MMS 2, MMS 5, MMS7, MMS9, FIR-2, FIR 3, VLA 13, and FIR 6b are associated with mm and SPITZER 24 μm sources. The others are more or less complicated, and two of which, VLA 13 and FIR 6, are newly identified. We found the interaction between the molecular outflows and the dust condensations at least in four regions. In addition, we confirmed the increment of the velocity width of the dense gas toward some of these condensations (i.e. at the termination of the outflow lobes). These results suggest that (i) the interaction between the outflows and the dense condensation occurs commonly in the OMC-2/3 region, (ii) the dense condensations in this region are compressed ubiquitously by these outflows and are receiving a part of the momentum from them. Particularly, one of the strongest millimeter sources, and hence protostar candidates, FIR4, is strongly compressed by a molecular outflow driven by FIR3 located at the north-east of FIR 4. These results suggest that the molecular outflows play an important role in the formation and evolution of stars and that the outflows are a driving mechanism of turbulence in the OMC-2/3 region.

scholarly journals AN ALL-SKY SAMPLE OF INTERMEDIATE-MASS STAR-FORMING REGIONS

2014 ◽  
Vol 784 (2) ◽  
pp. 111 ◽  
Author(s):  
Michael J. Lundquist ◽  
Henry A. Kobulnicky ◽  
Michael J. Alexander ◽  
Charles R. Kerton ◽  
Kim Arvidsson
Keyword(s):  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Star Forming Regions ◽  
Intermediate Mass Star

A13CO SURVEY OF INTERMEDIATE-MASS STAR-FORMING REGIONS

2015 ◽  
Vol 806 (1) ◽  
pp. 40 ◽  
Author(s):  
Michael J. Lundquist ◽  
Henry A. Kobulnicky ◽  
Charles R. Kerton ◽  
Kim Arvidsson
Keyword(s):  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Star Forming Regions ◽  
Intermediate Mass Star

scholarly journals The atomic hydrogen/molecular cloud association: an unavoidable relationship

1991 ◽  
Vol 147 ◽  
pp. 37-40
Author(s):  
G. Joncas
Keyword(s):  
Atomic Hydrogen ◽  
Molecular Clouds ◽  
Large Scale ◽  
Young Stars ◽  
Physical Processes ◽  
Star Forming ◽  
Dark Clouds ◽  
Star Forming Regions ◽  
The Impact

The presence of HI in the interstellar medium is ubiquitous. HI is the principal actor in the majority of the physical processes at work in our Galaxy. Restricting ourselves to the topics of this symposium, atomic hydrogen is involved with the formation of molecular clouds and is one of the byproducts of their destruction by young stars. HI has different roles during a molecular cloud's life. I will discuss here a case of coexisting HI and H2 at large scale and the origin of HI in star forming regions. For completeness' sake, it should be mentionned that there are at least three other aspects of HI involvement: HI envelopes around molecular clouds, the impact of SNRs (see work on IC 443), and the role of HI in quiescent dark clouds (see van der Werf's work).

scholarly journals Warm gas in protostellar outflows

2019 ◽  
Vol 629 ◽  
pp. A77
Author(s):  
A. I. Gómez-Ruiz ◽  
A. Gusdorf ◽  
S. Leurini ◽  
K. M. Menten ◽  
S. Takahashi ◽  
...  
Keyword(s):  
Radiative Transfer ◽  
High Velocity ◽  
The Other ◽  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Physical Conditions ◽  
Star Forming Regions ◽  
Low Mass ◽  
Kinematic Properties

Context. OMC-2/3 is one of the nearest embedded cluster-forming regions that includes intermediate-mass protostars at early stages of evolution. A previous CO (3–2) mapping survey towards this region revealed outflow activity related to sources at different evolutionary phases. Aims. The present work presents a study of the warm gas in the high-velocity emission from several outflows found in CO (3–2) emission by previous observations, determines their physical conditions, and makes a comparison with previous results in low-mass star-forming regions. Methods. We used the CHAMP+ heterodyne array on the APEX telescope to map the CO (6–5) and CO (7–6) emission in the OMC-2 FIR 6 and OMC-3 MMS 1-6 regions, and to observe 13CO (6–5) at selected positions. We analyzed these data together with previous CO (3–2) observations. In addition, we mapped the SiO (5–4) emission in OMC-2 FIR 6. Results. The CO (6–5) emission was detected in most of the outflow lobes in the mapped regions, while the CO (7–6) was found mostly in the OMC-3 outflows. In the OMC-3 MMS 5 outflow, a previously undetected extremely high-velocity gas was found in CO (6–5). This extremely high-velocity emission arises from the regions close to the central object MMS 5. Radiative transfer models revealed that the high-velocity gas from MMS 5 outflow consists of gas with nH2 = 104–105 cm−3 and T > 200 K, similar to what is observed in young Class 0 low-mass protostars. For the other outflows, values of nH2 > 104 cm−3 were found. Conclusions. The physical conditions and kinematic properties of the young intermediate-mass outflows presented here are similar to those found in outflows from Class 0 low-mass objects. Due to their excitation requirements, mid − J CO lines are good tracers of extremely high-velocity gas in young outflows likely related to jets.

scholarly journals THE INTERMEDIATE-MASS STAR-FORMING REGION LYNDS 1340. AN OPTICAL VIEW

2016 ◽  
Vol 822 (2) ◽  
pp. 79 ◽  
Author(s):  
Mária Kun ◽  
Attila Moór ◽  
Elza Szegedi-Elek ◽  
Bo Reipurth
Keyword(s):  
Mass Star ◽  
Intermediate Mass ◽  
Star Forming ◽  
Intermediate Mass Star

scholarly journals The atomic hydrogen/molecular cloud association: an unavoidable relationship

1991 ◽  
Vol 147 ◽  
pp. 37-40
Author(s):  
G. Joncas
Keyword(s):  
Atomic Hydrogen ◽  
Molecular Clouds ◽  
Large Scale ◽  
Young Stars ◽  
Physical Processes ◽  
Star Forming ◽  
Dark Clouds ◽  
Star Forming Regions ◽  
The Impact

The presence of HI in the interstellar medium is ubiquitous. HI is the principal actor in the majority of the physical processes at work in our Galaxy. Restricting ourselves to the topics of this symposium, atomic hydrogen is involved with the formation of molecular clouds and is one of the byproducts of their destruction by young stars. HI has different roles during a molecular cloud's life. I will discuss here a case of coexisting HI and H2 at large scale and the origin of HI in star forming regions. For completeness' sake, it should be mentionned that there are at least three other aspects of HI involvement: HI envelopes around molecular clouds, the impact of SNRs (see work on IC 443), and the role of HI in quiescent dark clouds (see van der Werf's work).

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