scholarly journals Star Formation in the Most Distant Molecular Cloud in the Extreme Outer Galaxy: A Laboratory of Star Formation in an Early Epoch of the Galaxy’s Formation

2008 ◽  
Vol 683 (1) ◽  
pp. 178-188 ◽  
Author(s):  
Naoto Kobayashi ◽  
Chikako Yasui ◽  
Alan T. Tokunaga ◽  
Masao Saito
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Early Epoch

scholarly journals STAR FORMATION AND YOUNG STELLAR CONTENT IN THE W3 GIANT MOLECULAR CLOUD

2011 ◽  
Vol 743 (1) ◽  
pp. 39 ◽  
Author(s):  
Alana Rivera-Ingraham ◽  
Peter G. Martin ◽  
Danae Polychroni ◽  
Toby J. T. Moore
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Stellar Content ◽  
Giant Molecular Cloud

scholarly journals SEQUENTIAL STAR FORMATION IN THE Sh 254-258 MOLECULAR CLOUD: HEINRICH HERTZ TELESCOPE MAPS OF COJ= 2-1 AND 3-2 EMISSION

2009 ◽  
Vol 138 (3) ◽  
pp. 975-985 ◽  
Author(s):  
John H. Bieging ◽  
William L. Peters ◽  
Baltasar Vila Vilaro ◽  
Keith Schlottman ◽  
Craig Kulesa
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Heinrich Hertz

scholarly journals A new distance to the Brick, the dense molecular cloud G0.253+0.016

2021 ◽  
Vol 502 (1) ◽  
pp. 1246-1252
Author(s):  
M Zoccali ◽  
E Valenti ◽  
F Surot ◽  
O A Gonzalez ◽  
A Renzini ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Near Infrared ◽  
Formation Rate ◽  
Dynamical Evolution ◽  
Galactic Centre ◽  
The Galaxy ◽  
Centre Region ◽  
Order Of Magnitude ◽  
Red Clump

ABSTRACT We analyse the near-infrared colour–magnitude diagram of a field including the giant molecular cloud G0.253+0.016 (a.k.a. The Brick) observed at high spatial resolution, with HAWK-I@VLT. The distribution of red clump stars in a line of sight crossing the cloud, compared with that in a direction just beside it, and not crossing it, allow us to measure the distance of the cloud from the Sun to be 7.20, with a statistical uncertainty of ±0.16 and a systematic error of ±0.20 kpc. This is significantly closer than what is generally assumed, i.e. that the cloud belongs to the near side of the central molecular zone, at 60 pc from the Galactic centre. This assumption was based on dynamical models of the central molecular zone, observationally constrained uniquely by the radial velocity of this and other clouds. Determining the true position of the Brick cloud is relevant because this is the densest cloud of the Galaxy not showing any ongoing star formation. This puts the cloud off by one order of magnitude from the Kennicutt–Schmidt relation between the density of the dense gas and the star formation rate. Several explanations have been proposed for this absence of star formation, most of them based on the dynamical evolution of this and other clouds, within the Galactic centre region. Our result emphasizes the need to include constraints coming from stellar observations in the interpretation of our Galaxy’s central molecular zone.

scholarly journals Molecular and ionized gas kinematics in the GC Radio Arc

2016 ◽  
Vol 11 (S322) ◽  
pp. 133-136
Author(s):  
N. Butterfield ◽  
C.C. Lang ◽  
E. A. C. Mills ◽  
D. Ludovici ◽  
J. Ott ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Molecular Clouds ◽  
Radio Continuum ◽  
Molecular Gas ◽  
The South ◽  
Ionized Gas ◽  
Molecular Emission ◽  
Gas Kinematics

AbstractWe present NH3 and H64α+H63α VLA observations of the Radio Arc region, including the M0.20 – 0.033 and G0.10 – 0.08 molecular clouds. These observations suggest the two velocity components of M0.20 – 0.033 are physically connected in the south. Additional ATCA observations suggest this connection is due to an expanding shell in the molecular gas, with the centroid located near the Quintuplet cluster. The G0.10 – 0.08 molecular cloud has little radio continuum, strong molecular emission, and abundant CH3OH masers, similar to a nearby molecular cloud with no star formation: M0.25+0.01. These features detected in G0.10 – 0.08 suggest dense molecular gas with no signs of current star formation.

scholarly journals The Star Formation Region Associated with the Cometary Nebula GM24

1987 ◽  
Vol 115 ◽  
pp. 188-188
Author(s):  
M. Tapia ◽  
M. Roth ◽  
L.F. Rodríguez ◽  
J. Cantó ◽  
P. Persi ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Near Infrared ◽  
Broad Band ◽  
Large Temperature ◽  
Stellar Objects ◽  
Star Formation Region ◽  
The Past ◽  
Visible Part ◽  
H Ii Region

GM24 is a small visible nebulosity in the vicinity of a molecular cloud. In this contribution we present the results of continuum (6-cm) and CO line (J = 1 → 0) radio observations, infrared maps, broad-band photometry and low-resolution spectroscopy as well as long-slit Echelle Ha spectroscopy. We found evidence that the GM24 = PP85 nebula is part of a larger region where star formation occurred in the past 104 years; the region is embedded in a typical molecular cloud with a dimension of ∼ 10 pc and mass of ∼104 M⊙. A compact radio H II region seems to be associated with GM24 and with one of the mid-infrared peaks detected. The nebula is most probably the visible part of an embedded H II region that is starting to emerge from the cloud. The other infrared peaks found in its vicinity (∼ 1 pc) are probably associated with less evolved stellar objects. The complex also shows an extended near-infrared flux which we believe to arise in a reflection nebula. From energy arguments, we found that the luminosity required to power the H II region and keep the cloud at the observed large temperature (TK ≅33 K), is ∼105 L⊙ which is consistent with the infrared total flux from the present measurements and those from IRAS of 4x104 L⊙; this corresponds to the flux of ∼3 BO ZAMS stars. The details of the present work have appeared in the Revista Mexicana de Astronomía y Astrofísica, Volume 11, 83, 1985.

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).

scholarly journals THE PROGRESSION OF STAR FORMATION IN THE ROSETTE MOLECULAR CLOUD

2013 ◽  
Vol 769 (2) ◽  
pp. 140 ◽  
Author(s):  
Jason E. Ybarra ◽  
Elizabeth A. Lada ◽  
Carlos G. Román-Zúñiga ◽  
Zoltan Balog ◽  
Junfeng Wang ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Cloud

scholarly journals Molecular cloud regulated star formation in galaxies

2007 ◽  
Vol 376 (4) ◽  
pp. 1588-1610 ◽  
Author(s):  
C. M. Booth ◽  
Tom Theuns ◽  
Takashi Okamoto
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Star Formation In Galaxies
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