A Multiwavelength Study of Young Massive Star‐forming Regions. I. The Ionized Gas Content

2006 ◽  
Vol 651 (2) ◽  
pp. 914-932 ◽  
Author(s):  
Guido Garay ◽  
Kate J. Brooks ◽  
Diego Mardones ◽  
Ray P. Norris
Keyword(s):  
Massive Star ◽  
Gas Content ◽  
Ionized Gas ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals DECIPHERING THE IONIZED GAS CONTENT IN THE MASSIVE STAR-FORMING COMPLEX G75.78+0.34

2013 ◽  
Vol 766 (2) ◽  
pp. 114 ◽  
Author(s):  
Álvaro Sánchez-Monge ◽  
Stan Kurtz ◽  
Aina Palau ◽  
Robert Estalella ◽  
Debra Shepherd ◽  
...  
Keyword(s):  
Massive Star ◽  
Gas Content ◽  
Ionized Gas ◽  
Star Forming

scholarly journals IONIZED GAS TOWARD MOLECULAR CLUMPS: PHYSICAL PROPERTIES OF MASSIVE STAR-FORMING REGIONS

2009 ◽  
Vol 707 (1) ◽  
pp. 283-309 ◽  
Author(s):  
Katharine G. Johnston ◽  
Debra S. Shepherd ◽  
James E. Aguirre ◽  
Miranda K. Dunham ◽  
Erik Rosolowsky ◽  
...  
Keyword(s):  
Physical Properties ◽  
Massive Star ◽  
Ionized Gas ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals The Circumstellar Environment of Embedded Massive Stars

2002 ◽  
Vol 12 ◽  
pp. 143-145 ◽  
Author(s):  
Lee G. Mundy ◽  
Friedrich Wyrowski ◽  
Sarah Watt
Keyword(s):  
Massive Star ◽  
Massive Stars ◽  
Low Mass Stars ◽  
Submillimeter Wavelength ◽  
Star Forming ◽  
Star Forming Regions ◽  
Low Mass ◽  
Circumstellar Environments ◽  
Near Future

Millimeter and submillimeter wavelength images of massive star-forming regions are uncovering the natal material distribution and revealing the complexities of their circumstellar environments on size scales from parsecs to 100’s of AU. Progress in these areas has been slower than for low-mass stars because massive stars are more distant, and because they are gregarious siblings with different evolutionary stages that can co-exist even within a core. Nevertheless, observational goals for the near future include the characterization of an early evolutionary sequence for massive stars, determination if the accretion process and formation sequence for massive stars is similar to that of low-mass stars, and understanding of the role of triggering events in massive star formation.

scholarly journals Millimetre wavelength methanol masers survey towards massive star forming regions

2007 ◽  
Vol 3 (S242) ◽  
pp. 234-235
Author(s):  
T. Umemoto ◽  
N. Mochizuki ◽  
K. M. Shibata ◽  
D.-G. Roh ◽  
H.-S. Chung
Keyword(s):  
Detection Rate ◽  
Massive Star ◽  
Molecular Line ◽  
Maser Emission ◽  
Star Forming ◽  
Methanol Maser ◽  
Physical Conditions ◽  
Star Forming Regions ◽  
Methanol Masers ◽  
Maser Sources

AbstractWe present the results of a mm wavelength methanol maser survey towards massive star forming regions. We have carried out Class II methanol maser observations at 86.6 GHz, 86.9 GHz and 107.0 GHz, simultaneously, using the Nobeyama 45 m telescope. We selected 108 6.7 GHz methanol maser sources with declinations above −25 degrees and fluxes above 20 Jy. The detection limit of maser observations was ~3 Jy. Of the 93 sources surveyed so far, we detected methanol emission in 25 sources (27%) and “maser” emission in nine sources (10%), of which thre “maser” sources are new detections. The detection rate for maser emission is about half that of a survey of the southern sky (Caswell et al. 2000). There is a correlation between the maser flux of 107 GHz and 6.7 GHz/12 GHz emission, but no correlation with the “thermal” (non maser) emission. From results of other molecular line observations, we found that the sources with methanol emission show higher gas temperatures and twice the detection rate of SiO emission. This may suggest that dust evaporation and destruction by shock are responsible for the high abundance of methanol molecules, one of the required physical conditions for maser emission.

scholarly journals Infall and outflow motions towards a sample of massive star-forming regions from the RMS survey

2018 ◽  
Vol 477 (2) ◽  
pp. 2455-2469 ◽  
Author(s):  
N Cunningham ◽  
S L Lumsden ◽  
T J T Moore ◽  
L T Maud ◽  
I Mendigutía
Keyword(s):  
Massive Star ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals Water in massive star-forming regions: HIFI observations of W3 IRS5

2010 ◽  
Vol 521 ◽  
pp. L37 ◽  
Author(s):  
L. Chavarría ◽  
F. Herpin ◽  
T. Jacq ◽  
J. Braine ◽  
S. Bontemps ◽  
...  
Keyword(s):  
Massive Star ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals A Multiwavelength Study of Young Massive Star Forming Regions. II. The Dust Environment

2007 ◽  
Vol 666 (1) ◽  
pp. 309-320 ◽  
Author(s):  
Guido Garay ◽  
Diego Mardones ◽  
Kate J. Brooks ◽  
Liza Videla ◽  
Yanett Contreras
Keyword(s):  
Massive Star ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. V. G23.01–0.41 AND G23.44–0.18

2009 ◽  
Vol 693 (1) ◽  
pp. 424-429 ◽  
Author(s):  
A. Brunthaler ◽  
M. J. Reid ◽  
K. M. Menten ◽  
X. W. Zheng ◽  
L. Moscadelli ◽  
...  
Keyword(s):  
Massive Star ◽  
Star Forming ◽  
Star Forming Regions ◽  
Trigonometric Parallaxes

scholarly journals A MULTIWAVELENGTH STUDY OF YOUNG MASSIVE STAR-FORMING REGIONS. III. MID-INFRARED EMISSION

2009 ◽  
Vol 698 (1) ◽  
pp. 488-501 ◽  
Author(s):  
Esteban F. E. Morales ◽  
Diego Mardones ◽  
Guido Garay ◽  
Kate J. Brooks ◽  
Jaime E. Pineda
Keyword(s):  
Massive Star ◽  
Infrared Emission ◽  
Mid Infrared ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals Molecular Gas in the Magellanic Clouds

1999 ◽  
Vol 190 ◽  
pp. 67-73 ◽  
Author(s):  
Mónica Rubio
Keyword(s):  
Line Emission ◽  
Magellanic Clouds ◽  
Gas Content ◽  
Molecular Gas ◽  
Star Forming ◽  
Physical Conditions ◽  
Star Forming Regions ◽  
Hydrogen Column Density ◽  
Spatial Coverage ◽  
Co Emission

The molecular gas content in the Magellanic Clouds has been studied, with different spatial coverage and resolution, through obervations of CO(1-0) line emission. In the LMC and the SMC the molecular gas is dominated by clouds whose properties are different from those of their Galactic counterparts. The relation between the intensity of CO emission and molecular hydrogen column density, or the conversion factor X, is different than that of molecular clouds in our Galaxy and depends on the ambient physical conditions. Studying the molecular gas through observations in the H2 emission line may prove an alternative way to determine the molecular content associated with star forming regions in the Magellanic Clouds. In particular, results obtained towards 30 Doradus in the LMC are presented.

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