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Title = {{From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey}},
Volume = 518,
Year = 2010}
@article{Chabrier2010a,
Author = {{Chabrier}, G. and {Hennebelle}, P.},
Journal = {\apjl},
Month = dec,
Pages = {L79-L83},
Title = {{Star Formation: Statistical Measure of the Correlation between the Prestellar Core Mass Function and the Stellar Initial Mass Function}},
Volume = 725,
Year = 2010}
@article{Hopkins2012b,
Author = {{Hopkins}, P.~F.},
Journal = {\mnras},
Month = jul,
Pages = {2037-2044},
Title = {{The stellar initial mass function, core mass function and the last-crossing distribution}},
Volume = 423,
Year = 2012}
@article{Hennebelle2012a,
Author = {{Hennebelle}, P. and {Falgarone}, E.},
Journal = {ArXiv e-prints},
Month = nov,
Title = {{Turbulent molecular clouds}},
Year = 2012}
@article{Williams1995a,
Author = {{Williams}, J.~P. and {Blitz}, L. and {Stark}, A.~A.},
Journal = {\apj},
Month = sep,
Pages = {252},
Title = {{The Density Structure in the Rosette Molecular Cloud: Signposts of Evolution}},
Volume = 451,
Year = 1995}
@article{Mangum2013a,
Author = {{Mangum}, Jeffrey~G. and {Darling}, Jeremy and {Henkel}, Christian and {Menten}, Karl~M.},
Month = {Feb},
Title = {Formaldehyde Densitometry of Starburst Galaxies: Density-Independent Global Star Formation},
Year = {2013}}
@article{ArayaMaser2007,
title = {First Detection of an {H2CO} 6 cm Maser Flare: A Burst in {IRAS} 18566+0408},
volume = {654},
shorttitle = {First Detection of an {H2CO} 6 cm Maser Flare},
url = {http://adsabs.harvard.edu/abs/2007ApJ...654L..95A},
abstract = {We report the discovery of a short-duration (less than 3 months)
outburst of the {H2CO} 6 cm maser in {IRAS} 18566+0408
{(G37.55+0.20).} During the flare, the peak flux density of the maser
increased by a factor of 4; after less than a month, it decayed to the
preflare value. This is the first detection of a short, burstlike
variability of an {H2CO} 6 cm maser. The maser shows an
asymmetric line profile that is consistent with the superposition of two
Gaussian components. We did not detect a change in the velocity or the
line width of the Gaussian components during the flare. If the two
Gaussian components trace two separate maser regions, then very likely
an event outside the maser gas triggered simultaneous flares at two
different locations.},
journal = {\apj},
author = {E. Araya and P. Hofner and M. Sewiło and H. Linz and S. Kurtz and L. Olmi and C. Watson and E. Churchwell},
year = {2007},
keywords = {{ISM:} H {II} Regions, {ISM:} individual {(IRAS} 18566+0408), {ISM:} Molecules, {MASERS,} {RADIO} {LINES:} {ISM,} Stars: Formation},
pages = {L95--L98}
},
@article{Araya2008,
title = {A Search for {H2CO} 6 cm Emission toward Young Stellar Objects. {III.} {VLA} Observations},
volume = {178},
url = {http://cdsads.u-strasbg.fr/abs/2008ApJS..178..330A},
abstract = {We report the results of our third survey for formaldehyde
{(H2CO)} 6 cm maser emission in the Galaxy. Using the Very
Large Array, we detected two new {H2CO} maser sources
{(G23.01-0.41} and G25.83-0.18), thus increasing the sample of known
{H2CO} maser regions in the Galaxy to seven. We review the
characteristics of the G23.01-0.41 and G25.83-0.18 star-forming regions.
The {H2CO} masers in G23.01-0.41 and G25.83-0.18 share several
properties with the other known H {2CO} masers, in particular,
emission from rich maser environments and close proximity to very young
massive stellar objects.},
journal = {\apjs},
author = {E. D. Araya and P. Hofner and W. M. Goss and H. Linz and S. Kurtz and L. Olmi},
month = oct,
year = {2008},
keywords = {{ISM:} Molecules, {MASERS,} {RADIO} {LINES:} {ISM}},
pages = {330--338}
},
@article{Araya2007,
title = {A Search for Formaldehyde 6 cm Emission toward Young Stellar Objects. {II.} {H2CO} and H110α Observations},
volume = {170},
url = {http://adsabs.harvard.edu/abs/2007ApJS..170..152A},
abstract = {We report the results of our second survey for Galactic {H2CO}
maser emission toward young stellar objects. Using the {GBT} and the {VLA}
in the A configuration we observed 58 star-forming regions and
discovered the fifth {H2CO} 6 cm maser region in the Galaxy
{(G23.71-0.20).} We have discussed the detection toward G23.71-0.20 in a
previous paper. Here we present all the other results from our survey,
including detection of {H2CO} absorption features toward 48
sources, detection of the H110α recombination line toward 29
sources, detection (including tentative detections) of the carbon
recombination line C110α toward 14 sources, subarcsecond angular
resolution images of 6 cm continuum emission toward five sources, and
observations of the {H2CO} masers in {IRAS} 18566+0408 and {NGC}
7538. In the case of {NGC} 7538, we detected the two main {H2CO}
maser components, and our observations confirm variability of the
blueshifted component recently reported by Hoffman et al. The
variability of both maser components in {NGC} 7538 could be caused by a
shock wave that reached the redshifted component approximately 14 yr
before reaching the blueshifted component. If that were the case, we
would expect to detect an increase in the flux density rate of change of
the blueshifted component sometime after the year 2009. Our data also
support the use of {H2CO/H110α} observations as a tool to
resolve the kinematic distance ambiguity of massive star-forming regions
in the Galaxy.},
journal = {\apjs},
author = {E. Araya and P. Hofner and W. M. Goss and H. Linz and S. Kurtz and L. Olmi},
month = may,
year = {2007},
keywords = {{ISM:} clouds, {ISM:} H {II} Regions, {ISM:} Molecules, {RADIO} {LINES:} {ISM,} Stars: Formation},
pages = {152--174}
},
@article{Evans1975,
title = {Interstellar {H2CO.} I - Absorption studies, dark clouds, and the cosmic background radiation},
volume = {196},
url = {http://adsabs.harvard.edu/abs/1975ApJ...196..433E},
abstract = {Abstract image available at:
{http://adsabs.harvard.edu/abs/1975ApJ...196..433E}},
journal = {\apj},
author = {N. J. Evans and G. Morris and T. Sato and B. Zuckerman},
month = mar,
year = {1975},
keywords = {{ABSORPTION} {SPECTRA,} {ASTRONOMICAL} {CATALOGS,} {ASTRONOMICAL} {MODELS,} {BACKGROUND} {RADIATION,} {CLOUDS,} {DENSITY} {DISTRIBUTION,} {ELECTRON} {TRANSITIONS,} {FORMALDEHYDE,} {INTERSTELLAR} {MATTER,} {LINE} {SPECTRA,} {MOLECULAR} {SPECTRA,} {OPTICAL} {PUMPING,} {RADIAL} {VELOCITY,} {TEMPERATURE} {DISTRIBUTION}},
pages = {433--456}
},
@article{ArayaMaser2007b,
title = {An {H2CO} 6 cm Maser Pinpointing a Possible Circumstellar Torus in {IRAS} 18566+0408},
volume = {669},
url = {http://adsabs.harvard.edu/abs/2007ApJ...669.1050A},
abstract = {We report observations of 6 cm, 3.6 cm, 1.3 cm, and 7 mm radio
continuum, conducted with the Very Large Array, toward {IRAS} 18566+0408,
one of the few sources known to harbor {H2CO} 6 cm maser
emission. Our observations reveal that the emission is dominated by an
ionized jet at centimeter wavelengths. Spitzer {IRAC} images from {GLIMPSE}
support this interpretation, given the presence of 4.5 μm excess
emission at approximately the same orientation as the centimeter
continuum. The 7 mm emission is dominated by thermal dust from a
flattened structure almost perpendicular to the ionized jet; thus, the 7
mm emission appears to trace a torus associated with a young massive
stellar object. The {H2CO} 6 cm maser is coincident with the
center of the torus-like structure. Our observations rule out radiative
pumping via radio continuum as the excitation mechanism for the
{H2CO} 6 cm maser in {IRAS} 18566+0408.},
journal = {\apj},
author = {E. Araya and P. Hofner and M. Sewiło and W. M. Goss and H. Linz and S. Kurtz and L. Olmi and E. Churchwell and L. F. Rodríguez and G. Garay},
month = nov,
year = {2007},
keywords = {{ISM:} H {II} Regions, {ISM:} individual {(IRAS} 18566+0408), {ISM:} Molecules, {MASERS,} Stars: Formation},
pages = {1050--1057}
},
@article{Mangum2008,
title = {Formaldehyde Densitometry of Starburst Galaxies},
volume = {673},
url = {http://adsabs.harvard.edu/abs/2008ApJ...673..832M},
abstract = {With a goal toward deriving the physical conditions in external
galaxies, we present a survey of the formaldehyde emission in a sample
of starburst systems. By extending a technique used to derive the
spatial density in star formation regions in our own Galaxy, we show how
the relative intensity of the 110-111 and
211-212 K-doublet transitions of {H2CO}
can provide an accurate densitometer for the active star formation
environments found in starburst galaxies. Relying on an assumed kinetic
temperature and cospatial emission and absorption from both
{H2CO} transitions, our technique is applied to a sample of 19
infrared-bright galaxies which exhibit various forms of starburst
activity. In the five galaxies of our sample where both {H2CO}
transitions were detected, we have derived spatial densities. We also
use {H2CO} to estimate the dense gas mass in our starburst
galaxy sample, finding similar mass estimates for the dense gas-forming
stars in these objects as derived using other dense gas tracers. A
related trend can be seen when one compares {LIR} to our
derived {n(H2)} for the five galaxies within which we have
derived spatial densities. Even though our number statistics are small,
there appears to be a trend toward higher spatial density for galaxies
with higher infrared luminosity. This is likely another representation
of the {LIR-Mdense} correlation.},
journal = {\apj},
author = {Jeffrey G. Mangum and Jeremy Darling and Karl M. Menten and Christian Henkel},
month = feb,
year = {2008},
keywords = {Galaxies: Starburst, {ISM:} Molecules},
pages = {832--846}
},
@article{Zeiger2010,
title = {Formaldehyde {Anti-Inversion} at z = 0.68 in the Gravitational Lens B0218 + 357},
volume = {709},
url = {http://adsabs.harvard.edu/abs/2010ApJ...709..386Z},
abstract = {We report new observations of the 110-111 (6 cm)
and 211-212 (2 cm) transitions of
ortho-formaldehyde {(o-H2CO)} in absorption at z = 0.68466
toward the gravitational lens system B0218 + 357. Radiative transfer
modeling indicates that both transitions are anti-inverted relative to
the 4.6 K microwave background, regardless of the source covering
factor, with excitation temperatures of {\textasciitilde}1 K and 1.5-2 K for the
110-111 and 211-212 lines,
respectively. Using these observations and a large velocity gradient
radiative transfer model that assumes a gradient of 1 km
s–1 pc–1, we obtain a molecular
hydrogen number density of 2 × 103 cm-3 {\textless}
{n(H2)} {\textless} 1 × 104 cm-3 and a
column density of 2.5 × 1013 cm-2 {\textless}
{N(o-H2CO)} {\textless} 8.9 × 1013 cm-2,
where the allowed ranges conservatively include the range of possible
source covering factors in both lines. The measurements suggest that
{H2CO} excitation in the absorbing clouds in the B0218 + 357
lens is analogous to that in Galactic molecular clouds: it would show
{H2CO} absorption against the cosmic microwave background if it
were not illuminated by the background quasar or if it were viewed from
another direction.},
journal = {\apj},
author = {Benjamin Zeiger and Jeremy Darling},
year = {2010},
keywords = {galaxies: individual: B0218\_357, galaxies: {ISM,} quasars: absorption lines, radiation mechanisms: non-thermal, radio lines: galaxies},
pages = {386--395}
},
@article{Araya2004,
title = {A Search for {H2CO} 6 Centimeter Emission toward Young Massive Stellar Objects},
volume = {154},
url = {http://adsabs.harvard.edu/abs/2004ApJS..154..579A},
abstract = {A survey for {H2CO} 6 cm emission toward young massive stellar
objects has been conducted using the 305 m Arecibo Telescope. We report
detection of emission toward {IRAS} 18566+0408, only the fifth source in
the Galaxy known to show {H2CO} 6 cm emission. A cross-scan
shows that the size of the emitting region is smaller than the C-band
Arecibo half-power beamwidth (i.e.,
θs{\textless}1'). We detect extended
{H2CO} 6 cm absorption around and toward the emitter position.
We detect {H2CO} 6 cm absorption features toward all 15 sources
observed. Three of the sources exhibit complex absorption profiles that
could be due to absorption partially filled by emission.},
journal = {\apjs},
author = {E. Araya and P. Hofner and H. Linz and M. Sewilo and C. Watson and E. Churchwell and L. Olmi and S. Kurtz},
month = oct,
year = {2004},
keywords = {{ISM:} clouds, {ISM:} Molecules, {RADIO} {LINES:} {ISM}},
pages = {579--584}
},
@article{Churchwell2002,
title = {{ULTRA-COMPACT} {HII} {REGIONS} {AND} {MASSIVE} {STAR} {FORMATION}},
volume = {40},
issn = {0066-4146},
url = {http://arjournals.annualreviews.org/doi/full/10.1146/annurev.astro.40.060401.093845},
doi = {10.1146/annurev.astro.40.060401.093845},
number = {1},
journal = {Annual Review of Astronomy and Astrophysics},
author = {Ed Churchwell},
year = {2002},
pages = {27--62}
}
@article{Lockman1978,
title = {The analysis of radio emission from H {II} regions - Consequences of improper analytic methods},
volume = {222},
url = {http://adsabs.harvard.edu/abs/1978ApJ...222..153L},
abstract = {The analytic methods and approximations which have been used to deduce
hot cores in H {II} regions and a gradient in nebular temperatures across
the Galaxy from radio recombination-line and continuum emission are
critiqued. In particular, it is shown that standard analyses of
single-dish flux density measurements are vitiated by the effects of
beam convolution and uncertainties in nebula size; other problems arise
when the local thermodynamic equilibrium assumption is applied to
recombination-line emission and when nebulae are considered to be
plane-parallel, isothermal homogeneous objects. These invalid
assumptions lead to an apparent decrease in the average electron density
of nebulae with distance from the sun, and to an increase in their
electron temperature with frequency and distance from the center of a
nebula.},
journal = {\apj},
author = {F. J. Lockman and R. L. Brown},
month = may,
year = {1978},
keywords = {{ASTRONOMICAL} {SPECTROSCOPY,} {CONTINUOUS} {SPECTRA,} {EMISSION} {SPECTRA,} H {II} regions, {LINE} {SPECTRA,} {MILKY} {WAY} {GALAXY,} {NEBULAE,} {RADIO} {EMISSION,} {RADIO} {SPECTRA,} {THERMODYNAMIC} {EQUILIBRIUM}},
pages = {153--164}
}
@article{Quireza2006,
title = {The Electron Temperature Gradient in the Galactic Disk},
volume = {653},
url = {http://adsabs.harvard.edu/abs/2006ApJ...653.1226Q},
abstract = {We derive the electron temperature gradient in the Galactic disk, using
a sample of H {II} regions that spans Galactocentric distances of 0-17
kpc. The electron temperature was calculated using high-precision radio
recombination line and continuum observations for more than 100 H {II}
regions. Nebular Galactocentric distances were calculated in a
consistent manner, using the radial velocities measured by our radio
recombination line survey. The large number of nebulae widely
distributed over the Galactic disk, together with the uniformity of our
data, provide a secure estimate of the present electron temperature
gradient in the Milky Way. Because metals are the main coolants in the
photoionized gas, the electron temperature along the Galactic disk
should be directly related to the distribution of heavy elements in the
Milky Way. Our best estimate of the electron temperature gradient is
derived from a sample of 76 sources for which we have the highest
quality data. The present gradient in electron temperature has a minimum
at the Galactic center and rises at a rate of 287+/-46 K
kpc-1. There are no significant variations in the value of
the gradient as a function of Galactocentric radius or azimuth. The
scatter we find in the H {II} region electron temperatures at a given
Galactocentric radius is not due to observational error, but rather to
intrinsic fluctuations in these temperatures, which are almost certainly
due to fluctuations in the nebular heavy-element abundances. Comparing
the H {II} region gradient with the much steeper gradient found for
planetary nebulae suggests that the electron temperature gradient
evolves with time, becoming flatter as a consequence of the chemical
evolution of the Milky Way's disk.},
journal = {\apj},
author = {Cintia Quireza and Robert T. Rood and T. M. Bania and Dana S. Balser and Walter J. Maciel},
month = dec,
year = {2006},
keywords = {Abundances, {ISM:} Abundances, {ISM:} clouds, {ISM:} evolution, {ISM:} H {II} Regions, {ISM:} lines and bands, {ISM:} structure, Nuclear Reactions, Nucleosynthesis, {RADIO} {LINES:} {ISM}},
pages = {1226--1240}
}
@article{Becker2005,
title = {{MAGPIS:} A {Multi-Array} Galactic Plane Imaging Survey},
volume = {131},
shorttitle = {{MAGPIS}},
url = {http://adsabs.harvard.edu/abs/2006AJ....131.2525H},
abstract = {We present the {Multi-Array} Galactic Plane Imaging Survey {(MAGPIS),} which
maps portions of the first Galactic quadrant with an angular resolution,
sensitivity, and dynamic range that surpass existing radio images of the
Milky Way by more than an order of magnitude. The source detection
threshold at 20 cm is in the range 1-2 {mJy} over the 85\% of the survey
region (5deg{\textless}32deg, {\textbar}b{\textbar}{\textless}0.8d) not
covered by bright extended emission; the angular resolution is {\textasciitilde}6". We
catalog over 3000 discrete sources (diameters mostly {\textless}30") and
present an atlas of {\textasciitilde}400 diffuse emission regions. New and archival data
at 90 cm for the whole survey area are also presented. Comparison of our
catalogs and images with the Midcourse Space Experiment mid-infrared
data allows us to provide preliminary discrimination between thermal and
nonthermal sources. We identify 49 high-probability supernova remnant
candidates, increasing by a factor of 7 the number of known remnants
with diameters smaller than 5' in the survey region; several are pulsar
wind nebula candidates and/or very small diameter remnants
{(D{\textless}45'').} We report the tentative identification of
several hundred H {II} regions based on a comparison with the {mid-IR}
data; they range in size from unresolved ultracompact sources to large
complexes of diffuse emission on scales of half a degree. In several of
the latter regions, cospatial nonthermal emission illustrates the
interplay between stellar death and birth. We comment briefly on plans
for follow-up observations and our extension of the survey; when
complemented by data from ongoing X-ray and {mid-IR} observations, we
expect {MAGPIS} to provide an important contribution to our understanding
of the birth and death of massive stars in the Milky Way.},
journal = {Astronomical Journal},
author = {David J. Helfand and Robert H. Becker and Richard L. White and Adam Fallon and Sarah Tuttle},
month = may,
year = {2006},
keywords = {Catalogs, Galaxy: General, {ISM:} H {II} Regions, {ISM:} Supernova Remnants, Radio Continuum: {ISM,} Surveys},
pages = {2525--2537}
}
@article{Green1991,
title = {Collisional excitation of formaldehyde in 'hot' interstellar molecular regions},
volume = {76},
url = {http://adsabs.harvard.edu/abs/1991ApJS...76..979G},
abstract = {Earlier calculations for rotational excitation of formaldehyde by
collisions with He atoms are extended to include the lowest 81
rotational levels and kinetic temperatures to 300 K. Calculations are
generally based on Green et al. (1978) but coupled differential
equations are solved via a modified log-derivative propagator at low
energies {(Manolopoulos,} 1986) and an R-matrix propagator at higher
energies {(Stechel,} Walker, and Light, 1978). Consideration is given to
the expected accuracy of the rates for excitation of formaldehyde by
collisions with He atoms which are calculated in the present paper and
to the expected differences between these rates and those for excitation
by H2 molecules which comprise a larger fraction of the interstellar
gas. The comparisons performed indicate that, for excitation by He,
calculated state-to-state rates are likely to be 50 percent accurate,
and total excitation rates, better than 20 percent. For excitation by
H2, the rates should be increased by a factor of 2.2.},
journal = {\apjs},
author = {Sheldon Green},
month = jul,
year = {1991},
keywords = {{ATOMIC} {COLLISIONS,} {FORMALDEHYDE,} {HELIUM} {ATOMS,} {INTERSTELLAR} {MATTER,} {KINETIC} {ENERGY,} {MOLECULAR} {ENERGY} {LEVELS,} {MOLECULAR} {EXCITATION,} {ROTATIONAL} {SPECTRA}},
pages = {979--983}
}
@article{Churchwell1974,
title = {Helium Abundance in Galactic H {II} Regions},
volume = {32},
url = {http://adsabs.harvard.edu/abs/1974A%26A....32..283C},
abstract = {Abstract image available at:
{http://adsabs.harvard.edu/abs/1974A\&A....32..283C}},
journal = {Astronomy and Astrophysics},
author = {E. Churchwell and P. G. Mezger and W. Huchtmeier},
month = may,
year = {1974},
pages = {283}
}
@article{Jackson2006,
title = {The Boston {University-Five} College Radio Astronomy Observatory Galactic Ring Survey},
volume = {163},
url = {http://adsabs.harvard.edu/abs/2006ApJS..163..145J},
abstract = {The Boston {University-Five} College Radio Astronomy Observatory Galactic
Ring Survey is a new survey of Galactic {13CO} J=1--{\textgreater}0
emission. The survey used the {SEQUOIA} multipixel array on the Five
College Radio Astronomy Observatory 14 m telescope to cover a longitude
range of l=18deg-55.7d and a latitude range of
{\textbar}b{\textbar}{\textless}1deg, a total of 75.4 deg2. Using both
position-switching and {On-The-Fly} mapping modes, we achieved an angular
sampling of 22", better than half of the telescope's 46" angular
resolution. The survey's velocity coverage is -5 to 135 km
s-1 for Galactic longitudes l{\textless}=40deg and -5 to
85 km s-1 for Galactic longitudes l{\textgreater}40deg. At
the velocity resolution of 0.21 km s-1, the typical rms
sensitivity is {σ(T*A){\textasciitilde}0.13} K. The survey
comprises a total of 1,993,522 spectra. We show integrated intensity
images (zeroth moment maps), channel maps, position-velocity diagrams,
and an average spectrum of the completed survey data set. We also
discuss the telescope and instrumental parameters, the observing modes,
the data reduction processes, and the emission and noise characteristics
of the data set. The Galactic Ring Survey data are available to the
community online or in {DVD} form by request.},
journal = {\apjs},
author = {J. M. Jackson and J. M. Rathborne and R. Y. Shah and R. Simon and T. M. Bania and D. P. Clemens and E. T. Chambers and A. M. Johnson and M. Dormody and R. Lavoie and M. H. Heyer},
month = mar,
year = {2006},
keywords = {Galaxy: Kinematics and Dynamics, {ISM:} clouds, {ISM:} Molecules, Radio Lines: General, Surveys},
pages = {145--159}
}
@ARTICLE{Troscompt2009,
author = {{Troscompt}, N. and {Faure}, A. and {Wiesenfeld}, L. and {Ceccarelli}, C. and
{Valiron}, P.},
title = "{Rotational excitation of formaldehyde by hydrogen molecules: ortho-H\_2CO at low temperature}",
journal = {\aap},
keywords = {molecular data, molecular processes, ISM: molecules},
year = 2009,
month = jan,
volume = 493,
pages = {687-696},
doi = {10.1051/0004-6361:200810712},
adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...493..687T},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Troscompt2009b,
author = {{Troscompt}, N. and {Faure}, A. and {Maret}, S. and {Ceccarelli}, C. and
{Hily-Blant}, P. and {Wiesenfeld}, L.},
title = "{Constraining the ortho-to-para ratio of H$_{2}$ with anomalous H\_2CO absorption}",
journal = {\aap},
keywords = {astrochemistry, ISM: molecules, ISM: abundances, ISM:, individual objects: Barnard 68},
year = 2009,
month = nov,
volume = 506,
pages = {1243-1247},
doi = {10.1051/0004-6361/200912770},
adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...506.1243T},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Reid2010,
author = {{Reid}, M.~A. and {Wadsley}, J. and {Petitclerc}, N. and {Sills}, A.
},
title = "{Measuring the Clump Mass Function in the Age of SCUBA2, Herschel, and ALMA}",
journal = {\apj},
archivePrefix = "arXiv",
eprint = {1006.4320},
primaryClass = "astro-ph.GA",
keywords = {ISM: structure, methods: data analysis, stars: formation, stars: luminosity function, mass function, submillimeter: ISM},
year = 2010,
month = aug,
volume = 719,
pages = {561-575},
doi = {10.1088/0004-637X/719/1/561},
adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...719..561R},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{henkel1980,
author = {{Henkel}, C. and {Walmsley}, C.~M. and {Wilson}, T.~L.},
title = "{Formaldehyde in giant molecular clouds - H2 densities and corrections to the C-12/C-13 ratios}",
journal = {\aap},
keywords = {ABUNDANCE, CARBON ISOTOPES, FORMALDEHYDE, GALACTIC STRUCTURE, HYDROGEN CLOUDS, MOLECULAR GASES, DATA REDUCTION, GALACTIC NUCLEI, ISOTOPE EFFECT, LINE SPECTRA, MICROWAVE SPECTRA, RADIO ASTRONOMY},
year = 1980,
month = feb,
volume = 82,
pages = {41-47},
adsurl = {http://adsabs.harvard.edu/abs/1980A%26A....82...41H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Turner1993,
author = {{Turner}, B.~E.},
title = "{The nature of the molecular cores in high-altitude cirrus clouds. IV - The electron distribution and the abundance and chemistry of H2CO}",
journal = {\apj},
keywords = {ABUNDANCE, CIRRUS CLOUDS, ELECTRON DISTRIBUTION, FORMALDEHYDE, INTERSTELLAR CHEMISTRY, MOLECULAR CLOUDS, ASTRONOMICAL MODELS, ATOMIC EXCITATIONS, COSMIC DUST, INTERSTELLAR EXTINCTION, RADIATION DISTRIBUTION, STELLAR INTERIORS},
year = 1993,
month = jun,
volume = 410,
pages = {140-156},
doi = {10.1086/172733},
adsurl = {http://adsabs.harvard.edu/abs/1993ApJ...410..140T},
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%% Created for IRAS 05358 Ginsburg et al. paper: 14 Aug 2008
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adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{heyer:w345:1998,
author = {{Heyer}, M.~H. and {Terebey}, S.},
title = "{The Anatomy of the Perseus Spiral Arm: 12CO and IRAS Imaging Observations of the W3-W4-W5 Cloud Complex}",
journal = {\apj},
keywords = {GALAXY: STRUCTURE, GALAXY: GENERAL, ISM: CLOUDS, ISM: MOLECULES, ISM: KINEMATICS AND DYNAMICS, ISM: STRUCTURE},
year = 1998,
month = jul,
volume = 502,
pages = {265-+},
doi = {10.1086/305881},
adsurl = {http://adsabs.harvard.edu/abs/1998ApJ...502..265H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{heyer:ogs:1998,
author = {{Heyer}, M.~H. and {Brunt}, C. and {Snell}, R.~L. and {Howe}, J.~E. and
{Schloerb}, F.~P. and {Carpenter}, J.~M.},
title = "{The Five College Radio Astronomy Observatory CO Survey of the Outer Galaxy}",
journal = {\apjs},
keywords = {GALAXY: STRUCTURE, ISM: CLOUDS, ISM: GENERAL, ISM: KINEMATICS AND DYNAMICS, ISM: MOLECULES, SURVEYS},
year = 1998,
month = apr,
volume = 115,
pages = {241-+},
doi = {10.1086/313086},
adsurl = {http://adsabs.harvard.edu/abs/1998ApJS..115..241H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{oka:gc:2007,
author = {{Oka}, T. and {Nagai}, M. and {Kamegai}, K. and {Tanaka}, K. and
{Kuboi}, N.},
title = "{A CO J = 3-2 Survey of the Galactic Center}",
journal = {\pasj},
eprint = {arXiv:astro-ph/0701843},
keywords = {galaxies: nuclei -- Galaxy: center -- ISM: clouds -- ISM: molecules},
year = 2007,
month = feb,
volume = 59,
pages = {15-23},
adsurl = {http://cdsads.u-strasbg.fr/abs/2007PASJ...59...15O},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{wilking:formation:1984,
author = {{Wilking}, B.~A. and {Doering}, C.~R. and {Harvey}, P.~M. and
{Lada}, C.~J. and {Joy}, M.},
title = "{The formation of massive stars along the W5 ionization front}",
journal = {\apj},
keywords = {INFRARED ASTRONOMY, MOLECULAR CLOUDS, NEBULAE, STELLAR EVOLUTION, STELLAR MASS, CARBON MONOXIDE, FAR INFRARED RADIATION, GAS DENSITY, H II REGIONS, VISIBLE SPECTRUM},
year = 1984,
month = apr,
volume = 279,
pages = {291-303},
doi = {10.1086/161890},
adsurl = {http://adsabs.harvard.edu/abs/1984ApJ...279..291W},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{karr:triggered:2003,
title = {Triggered Star Formation in the W5 H {II} Region},
volume = {595},
url = {http://adsabs.harvard.edu/abs/2003ApJ...595..900K},
journal = {Astrophysical Journal},
author = {J. L. Karr and P. G. Martin},
month = oct,
year = {2003},
keywords = {{ISM:} H {II} Regions, {ISM:} Individual: Alphanumeric: W5, Stars: Formation},
pages = {900--912}
},
@article{koenig:clustered:2008,
title = {Clustered and Triggered Star Formation in W5: Observations with Spitzer},
volume = {688},
shorttitle = {Clustered and Triggered Star Formation in W5},
journal = {Astrophysical Journal},
author = {Xavier P. Koenig and Lori E. Allen and Robert A. Gutermuth and Joseph L. Hora and Christopher M. Brunt and James Muzerolle},
month = dec,
year = {2008},
keywords = {Infrared: Stars, {ISM:} Globules, {ISM:} H {II} Regions, Stars: {Early-Type,} Stars: Formation, Stars: {Pre-Main-Sequence}},
pages = {1142--1158}
},
@article{margulis:young:1989,
title = {Young stellar objects in the Monoceros {OB1} molecular cloud},
volume = {345},
url = {http://adsabs.harvard.edu/abs/1989ApJ...345..906M},
journal = {Astrophysical Journal},
author = {Michael Margulis and Charles J. Lada and Erick T. Young},
month = oct,
year = {1989},
keywords = {{ASTRONOMICAL} {MAPS,} {FAR} {INFRARED} {RADIATION,} {INFRARED} {ASTRONOMY} {SATELLITE,} {INFRARED} {SOURCES} {(ASTRONOMY),} {MOLECULAR} {CLOUDS,} {MOLECULAR} {GASES,} {NEBULAE,} {PRE-MAIN} {SEQUENCE} {STARS,} {SPECTRAL} {ENERGY} {DISTRIBUTION,} {STAR} {FORMATION}},
pages = {906--917}
},
@article{thompson:searching:2004,
title = {Searching for signs of triggered star formation toward {IC} 1848},
volume = {414},
url = {http://adsabs.harvard.edu/abs/2004A%26A...414.1017T},
journal = {Astronomy and Astrophysics},
author = {M. A. Thompson and G. J. White and L. K. Morgan and J. Miao and C. V. M. Fridlund and M. {Huldtgren-White}},
month = feb,
year = {2004},
keywords = {{ISM:} clouds, {ISM:} dust, {ISM:} {HII} regions, {ISM:} individual objects: {IC} 1848, {ISM:} molecules, stars: formation},
pages = {1017--1041}
}
@ARTICLE{seal:symbiotic:1995,
author = {{Seal}, P.},
title = "{Infrared Measurements of Faint Symbiotic Stars}",
journal = {\apss},
year = 1995,
month = dec,
volume = 234,
pages = {223-232},
doi = {10.1007/BF00627668},
adsurl = {http://cdsads.u-strasbg.fr/abs/1995Ap%26SS.234..223S},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{wenzel:fuori:1983,
author = {{Wenzel}, W. and {Fuhrmann}, B.},
title = "{Remark on the Nature of the Eruptive Object Lw-Cassiopeiae}",
journal = {Zentralinstitut fuer Astrophysik Sternwarte Sonneberg Mitteilungen ueber Veraenderliche Sterne},
year = 1983,
volume = 9,
pages = {143-+},
adsurl = {http://cdsads.u-strasbg.fr/abs/1983MitVS...9..143W},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{kauffmann2008,
title = {{MAMBO} mapping of Spitzer c2d small clouds and cores},
volume = {487},
url = {http://adsabs.harvard.edu/abs/2008A%26A...487..993K},
abstract = {Aims. To study the structure of nearby ({\textless}500 pc) dense starless and
star-forming cores with the particular goal to identify and understand
evolutionary trends in core properties, and to explore the nature of
Very Low Luminosity Objects (≤0.1 Lȯ; {VeLLOs).}
Methods: Using the {MAMBO} bolometer array, we create maps unusually
sensitive to faint (few {mJy} per beam) extended (≈5 arcmin) thermal
dust continuum emission at 1.2 mm wavelength. Complementary information
on embedded stars is obtained from Spitzer, {IRAS,} and {2MASS.} Results:
Our maps are very rich in structure, and we characterize extended
emission features (“subcores”) and compact intensity peaks
in our data separately to pay attention to this complexity. We derive,
e.g., sizes, masses, and aspect ratios for the subcores, as well as
column densities and related properties for the peaks. Combination with
archival infrared data then enables the derivation of bolometric
luminosities and temperatures, as well as envelope masses, for the young
embedded stars. Conclusions: Starless and star-forming cores occupy
the same parameter space in many core properties; a picture of dense
core evolution in which any dense core begins to actively form stars
once it exceeds some fixed limit in, e.g., mass, density, or both, is
inconsistent with our data. A concept of necessary conditions for star
formation appears to provide a better description: dense cores
fulfilling certain conditions can form stars, but they do not need to,
respectively have not done so yet. Comparison of various evolutionary
indicators for young stellar objects in our sample (e.g., bolometric
temperatures) reveals inconsistencies between some of them, possibly
suggesting a revision of some of these indicators. Finally, we challenge
the notion that {VeLLOs} form in cores not expected to actively form
stars, and we present a first systematic study revealing evidence for
structural differences between starless and candidate {VeLLO} cores.
Based on observations with the {IRAM} 30-m telescope. Figure 1, Tables 3-5
and Appendices A, B are only available in electronic form at
http://www.aanda.org Data used for the maps {(FITS} files) are only
available in electronic form at the {CDS} via anonymous ftp to
cdsarc.u-strasbg.fr (130.79.128.5), or via
{http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/487/993}},
journal = {Astronomy and Astrophysics},
author = {J. Kauffmann and F. Bertoldi and T. L. Bourke and N. J. Evans and C. W. Lee},
month = sep,
year = {2008},
keywords = {extinction, {ISM:} clouds, {ISM:} dust, {ISM:} evolution, {ISM:} structure, stars: formation},
pages = {993--1017}
}
@article{lada:embedded:2003,
title = {Embedded Clusters in Molecular Clouds},
volume = {41},
url = {http://adsabs.harvard.edu/abs/2003ARA%26A..41...57L},
abstract = {Stellar clusters are born embedded within giant molecular clouds {(GMCs)}
and during their formation and early evolution are often only visible at
infrared wavelengths, being heavily obscured by dust. Over the past 15
years advances in infrared detection capabilities have enabled the first
systematic studies of embedded clusters in galactic molecular clouds. In
this article we review the current state of empirical knowledge
concerning these extremely young protocluster systems. From a survey of
the literature we compile the first extensive catalog of galactic
embedded clusters. We use the catalog to construct the mass function and
estimate the birthrate for embedded clusters within 2 kpc of the sun. We
find that the embedded cluster birthrate exceeds that of visible open
clusters by an order of magnitude or more indicating a high infant
mortality rate for protocluster systems. Less than 4-7\% of embedded
clusters survive emergence from molecular clouds to become bound
clusters of Pleiades age. The vast majority (90\%) of stars that form in
embedded clusters form in rich clusters of 100 or more members with
masses in excess of 50 Mȯ. Moreover, observations of
nearby cloud complexes indicate that embedded clusters account for a
significant (70-90\%) fraction of all stars formed in {GMCs.} We review the
role of embedded clusters in investigating the nature of the initial
mass function {(IMF)} that, in one nearby example, has been measured over
the entire range of stellar and substellar mass, from {OB} stars to
substellar objects near the deuterium burning limit. We also review the
role embedded clusters play in the investigation of circumstellar disk
evolution and the important constraints they provide for understanding
the origin of planetary systems. Finally, we discuss current ideas
concerning the origin and dynamical evolution of embedded clusters and
the implications for the formation of bound open clusters.},
journal = {Annual Review of Astronomy and Astrophysics},
author = {Charles J. Lada and Elizabeth A. Lada},
year = {2003},
pages = {57--115}
},
@inproceedings{bretherton:unbiased:2002,
title = {An Unbiased Survey for Outflows in the W3 and W5 Star-Formation Regions},
volume = {267},
url = {http://adsabs.harvard.edu/abs/2002ASPC..267..347B},
abstract = {Preliminary results from a new {12CO} survey of the W3 and W5
molecular clouds are presented.},
author = {D. E. Bretherton and T. J. T. Moore and N. A. Ridge},
booktitle = {Hot Star Workshop III: The Earliest Phases of Massive Star Birth},
month = oct,
year = {2002},
pages = {347}
},
@article{rosolowsky:bolocam:2009,
title = {The Bolocam Galactic Plane Survey -- {II.} Catalog of the Image Data},
url = {http://arxiv.org/abs/0909.2871},
abstract = {We present a catalog of 8358 sources extracted from images produced by the Bolocam Galactic Plane Survey {(BGPS).} The {BGPS} is a survey of the millimeter dust continuum emission from the northern Galactic plane. The catalog sources are extracted using a custom algorithm, Bolocat, which was designed specifically to identify and characterize objects in the large-area maps generated from the Bolocam instrument. The catalog products are designed to facilitate follow-up observations of these relatively unstudied objects. The catalog is 98\% complete from 0.4 Jy to 60 Jy over all object sizes for which the survey is sensitive ({\textless}3.5'). We find that the sources extracted can best be described as molecular clumps -- large dense regions in molecular clouds linked to cluster formation. We find the flux density distribution of sources follows a power law with {dN/dS} {{\textasciitilde}S{\textasciicircum}(-2.4} +/- 0.1) and that the mean Galactic latitude for sources is significantly below the midplane: {\textless}b{\textgreater}=(-0.095 +/- 0.001) deg.},
journal = {0909.2871},
author = {Erik Rosolowsky and Miranda K Dunham and Adam Ginsburg and Eric Todd Bradley and James Aguirre and John Bally and Cara Battersby and Claudia Cyganowski and Darren Dowell and Meredith Drosback and Neal J Evans {II} and Jason Glenn and Paul Harvey and Guy S Stringfellow and Josh Walawender and Jonathan P Williams},
month = sep,
year = {2009},
keywords = {Astrophysics - Galaxy Astrophysics}
},
@article{hillwig:binary:2006,
title = {Binary and Multiple {O-Type} Stars in the Cassiopeia {OB6} Association},
volume = {639},
url = {http://adsabs.harvard.edu/abs/2006ApJ...639.1069H},
abstract = {We present the results of time-resolved spectroscopy of 13 O-type stars
in the Cas {OB6} stellar association. We conducted a survey for radial
velocity variability in search of binary systems, which are expected to
be plentiful in young {OB} associations. Here we report the discovery of
two new single-lined binaries, and we present new orbital elements for
three double-lined binaries (including one in the multiple-star system
{HD} 17505). One of the double-lined systems is the eclipsing binary
system {DN} Cas, and we present a preliminary light-curve analysis that
yields the system inclination, masses, and radii. We compare the spectra
of the single stars and the individual components of the binary stars
with model synthetic spectra to estimate the stellar effective
temperatures, gravities, and projected rotational velocities. We also
make fits of the spectral energy distributions to derive {E(B-V),}
{R=AV/E(B-V),} and angular diameter. A distance of 1.9 kpc
yields radii that are consistent with evolutionary models. We find that
7 of 14 systems with spectroscopic data are probable binaries,
consistent with the high binary frequency found for other massive stars
in clusters and associations.},
journal = {Astrophysical Journal},
author = {Todd C. Hillwig and Douglas R. Gies and William G. Bagnuolo and Wenjin Huang and M. Virginia {McSwain} and David W. Wingert},
month = mar,
year = {2006},
keywords = {open clusters and associations: individual {(Cassiopeia} {OB6),} open clusters and associations: individual {(IC} 1805), open clusters and associations: individual {(IC} 1848), Stars: Binaries: Close, Stars: {Early-Type,} stars: individual {(BD} +60 497), stars: individual {(BD} +60 594), stars: individual {(DN} Cassiopeiae), stars: individual {(HD} 17505), stars: individual {(HD} 17520)},
pages = {1069--1080}
},
@article{vacca:lyman-continuum:1996,
title = {The {Lyman-Continuum} Fluxes and Stellar Parameters of O and Early {B-Type} Stars},
volume = {460},
url = {http://adsabs.harvard.edu/abs/1996ApJ...460..914V},
abstract = {Using the results of the most recent stellar atmosphere models applied
to a sample of hot stars, we construct calibrations of effective
temperature {(Teff),} and gravity (log g) with a spectral type
and luminosity class for Galactic O-type and early B-type stars. From
the model results we also derive an empirical relation between the
bolometric correction and Teff and log g. Using a sample of
stars with known distances located in {OB} associations in the Galaxy and
the Large Magellanic Cloud, we derive a new calibration of
Mυ with spectral class. With these new calibrations and
the stellar atmosphere models of Kurucz, we calculate the physical
parameters and ionizing photon luminosities in the H0 and
He0 continua for O and early B-type stars. We find
substantial differences between our values of the Lyman- continuum
luminosity and those reported in the literature. We also discuss the
systematic discrepancy between O-type stellar masses derived from
spectroscopic models and those derived from evolutionary tracks. Most
likely, the cause of this "mass discrepancy" lies primarily in the
atmospheric models, which are plane parallel and hydrostatic and
therefore do not account for an extended atmosphere and the velocity
fields in a stellar wind. Finally, we present a new computation of the
Lyman-continuum luminosity from 429 known O stars located within 2.5 kpc
of the Sun. We find the total ionizing luminosity from this population
{(Q0Tot} = 7.0 × 1051 photons
s-1) to be 47\% larger than that determined using the Lyman
continuum values tabulated by Panagia.},
journal = {Astrophysical Journal},
author = {William D. Vacca and Catharine D. Garmany and J. Michael Shull},
month = apr,
year = {1996},
keywords = {{STARS:} {ATMOSPHERES,} Stars: {Early-Type,} {STARS:} {FUNDAMENTAL} {PARAMETERS,} {ULTRAVIOLET:} {STARS}},
pages = {914}
},
@article{karr:triggered:2003-4,
title = {Triggered Star Formation in the W5 H {II} Region},
volume = {595},
url = {http://adsabs.harvard.edu/abs/2003ApJ...595..900K},
abstract = {Young, massive stars can have a profound effect on the surrounding
interstellar medium. The triggering of star formation by an H {II} region
expanding into nearby molecular material is an example of this type of
interaction. This paper presents a multiwavelength study of the W5
star-forming region investigating the possibility of triggered star
formation. The ionizing sources and the morphologies of the ionized and
molecular gas and the dust are examined. A population of {YSOs} is
identified. Statistical evidence for triggering of these {YSOs} is
discussed in terms of the spatial dependence of the star formation
efficiency and the clustering and correlation of the {YSO} sources with
respect to the molecular gas and the H {II} region. Evidence for direct
interactions between the components is discussed, on both large scales
and the scale of individual objects. Timescales for the expansion of the
H {II} region, triggering processes, and the ages of the {YSOs} are compared
to establish a plausible sequence of events.},
journal = {Astrophysical Journal},
author = {J. L. Karr and P. G. Martin},
month = oct,
year = {2003},
keywords = {{ISM:} H {II} Regions, {ISM:} Individual: Alphanumeric: W5, Stars: Formation},
pages = {900--912}
},
@article{lefloch:cometary:1997,
title = {Cometary globules. {III.} Triggered star formation in {IC} 1848.},
volume = {324},
url = {http://adsabs.harvard.edu/abs/1997A%26A...324..249L},
abstract = {We present a multiwavelength study from molecular and continuum
observations of the cometary globule {CG5} in the {HII} region {IC1848.} {CG5}
is associated with the luminous {IRAS} point source 02252+6120
{(L=1100Lsun\_)} and shows evidence for an energetic outflow and
ongoing star formation (a cluster of low-mass stars has formed inside
the cloud). {CG5} is presently undergoing a second episode of
photo-ionisation from a cluster of O stars in the nebula, characterised
by a shock at the surface of the cloud; the shock was detected in
several millimeter lines {(CO,} {CS)} and in the thermal continuum dust
emission. Photo-ionisation conditions at the surface of the globule were
estimated from measurements of the {VLA} free-free continuum emission. A
virial analysis suggests that {CG5} is probably permeated by a static
magnetic field of strength {={\textasciitilde}125μG} and is subject to an outer
pressure 4 times as large as its inner pressure. It is in a globally
magnetically subcritical state whereas its core is close to virial
equilibrium. Photo-ionisation is found to play a key role in the
evolution of {CG5} because a) it confines the molecular gas and contains
the gas dispersal favored by the energy injection from the outflow while
evaporating the superficial layers at the same time, b) the overpressure
of the compressed gas ahead of the ionisation front is sufficient to
trigger the collapse of initially (sub)critical condensations inside the
cloud and initiate star formation. We find that the outflow contains
enough momentum to have contributed to this star-formation process. In
addition, the energy of the outflow is sufficient to sustain turbulence
in the cloud and maintain it in a magnetically subcritical state, i.e.
it tends to stabilize the cloud against collapse and regulate star
formation.},
journal = {Astronomy and Astrophysics},
author = {B. Lefloch and B. Lazareff and A. Castets},
month = aug,
year = {1997},
keywords = {{ISM:} clouds, {ISM:} {GENERAL,} {ISM:} {KINEMATICS} {AND} {DYNAMICS,} {ISM:} Molecules, {ISM:} {STAR} {FORMATION}},
pages = {249--262}
},
@article{krumholz:formation:2009,
title = {The Formation of Massive Star Systems by Accretion},
volume = {323},
url = {http://adsabs.harvard.edu/abs/2009Sci...323..754K},
abstract = {Massive stars produce so much light that the radiation pressure they
exert on the gas and dust around them is stronger than their
gravitational attraction, a condition that has long been expected to
prevent them from growing by accretion. We present three-dimensional
radiation-hydrodynamic simulations of the collapse of a massive
prestellar core and find that radiation pressure does not halt
accretion. Instead, gravitational and {Rayleigh-Taylor} instabilities
channel gas onto the star system through nonaxisymmetric disks and
filaments that self-shield against radiation while allowing radiation to
escape through optically thin bubbles. Gravitational instabilities cause
the disk to fragment and form a massive companion to the primary star.
Radiation pressure does not limit stellar masses, but the instabilities
that allow accretion to continue lead to small multiple systems.},
journal = {Science},
author = {Mark R. Krumholz and Richard I. Klein and Christopher F. {McKee} and Stella S. R. Offner and Andrew J. Cunningham},
month = feb,
year = {2009},
pages = {754}
},
@article{bonnell:star:2006,
title = {Star formation through gravitational collapse and competitive accretion},
volume = {370},
url = {http://adsabs.harvard.edu/abs/2006MNRAS.370..488B},
abstract = {Competitive accretion, a process to explain the origin of the initial
mass function {(IMF),} occurs when stars in a common gravitational
potential accrete from a distributed gaseous component. Stars located
near the centre of the potential benefit from the gravitational
attraction of the full potential and accrete at much higher rates than
do isolated stars. We show that concerns recently raised on the
efficiency of competitive accretion are incorrect as they use globally
averaged properties which are inappropriate for the detailed physics of
a forming stellar cluster. A full treatment requires a realistic
treatment of the cluster potential, the distribution of turbulent
velocities and gas densities. Accreting gas does not travel at the
global virial velocity of the system due to the velocity-sizescale
relation inherent in turbulent gas and due to the lower velocity
dispersion of {small-N} clusters in which much of the accretion occurs.
Accretion occurs due to the effect of the local potential in funnelling
gas down to the centre. Stars located in the gas-rich centres of such
systems initially accrete from low relative velocity gas attaining
larger masses before needing to accrete the higher velocity gas. Stars
not in the centres of such potentials, or that enter the cluster later
when the velocity dispersion is higher, do not accrete significantly and
thus retain their low masses. In competitive accretion, most stars do
not continue to accrete significantly such that their masses are set
from the fragmentation process. It is the few stars which continue to
accrete that become higher-mass stars. Competitive accretion is
therefore likely to be responsible for the formation of higher-mass
stars and can explain the mass distribution, mass segregation and binary
frequency of these stars. Global kinematics of competitive accretion
models include large-scale mass infall, with mean inflow velocities of
the order of {\textasciitilde}0.5 kms-1 at scales of 0.5pc, but infalling
signatures are likely to be confused by the large tangential velocities
and the velocity dispersion present. Finally, we discuss potential
limitations of competitive accretion and conclude that competitive
accretion is currently the most likely model for the origin of the
high-mass end of the {IMF.}},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Ian A. Bonnell and Matthew R. Bate},
month = jul,
year = {2006},
keywords = {globular clusters: general, mass function, Stars: Formation, stars: luminosity function},
pages = {488--494}
}
@article{oey:hierarchical:2005,
title = {Hierarchical Triggering of Star Formation by Superbubbles in {W3/W4}},
volume = {129},
url = {http://adsabs.harvard.edu/abs/2005AJ....129..393O},
abstract = {It is generally believed that expanding superbubbles and mechanical
feedback from massive stars trigger star formation, because there are
numerous examples of superbubbles showing secondary star formation at
their edges. However, although these systems show an age sequence, they
do not provide strong evidence of a causal relationship. The {W3/W4}
Galactic star-forming complex suggests a three-generation hierarchy: the
supergiant shell structures correspond to the oldest generation; these
triggered the formation of {IC} 1795 in W3, the progenitor of a molecular
superbubble that in turn triggered the current star-forming episodes in
the embedded regions {W3-North,} {W3-Main,} and {W3-OH.} We present {UBV}
photometry and spectroscopic classifications for {IC} 1795, which show an
age of 3-5 Myr. This age is intermediate between the reported 6-20 Myr
age of the supergiant shell system and the extremely young ages
(104-105 yr) for the embedded knots of the
ultracompact H {II} regions, {W3-North,} {W3-Main,} and {W3-OH.} Thus, an age
sequence is indeed confirmed for the entire {W3/W4} hierarchical system.
This therefore provides some of the first convincing evidence that
superbubble action and mechanical feedback are indeed a triggering
mechanism for star formation.},
journal = {Astronomical Journal},
author = {M. S. Oey and Alan M. Watson and Katie Kern and Gregory L. Walth},
year = {2005},
keywords = {{ISM:} Bubbles, {ISM:} clouds, {ISM:} Individual: Alphanumeric: W3, {ISM:} Individual: Alphanumeric: W4, {ISM:} structure, open clusters and associations: individual {(IC} 1795), open clusters and associations: individual {(IC} 1805), Stars: Formation},
pages = {393--401}
}
@article{sugitani:catalog:1991,
title = {A catalog of bright-rimmed clouds with {IRAS} point sources: Candidates for star formation by radiation-driven implosion. I - The Northern Hemisphere},
volume = {77},
shorttitle = {A catalog of bright-rimmed clouds with {IRAS} point sources},
url = {http://cdsads.u-strasbg.fr/abs/1991ApJS...77...59S},
abstract = {Forty-four bright-rimmed clouds associated with {IRAS} sources have been
selected from the Palomar Sky Survey prints. They are good candidates
for the sites of star formation induced by radiation-driven implosions;
three well-established cases of radiation-driven implosions in
bright-rimmed globules have been reported by Sugitani et al. (1989).
Nine of the bright-rimmed clouds are known to be associated with
molecular outflows and two (including one with an outflow) with {HH}
objects. Most of their sizes are not more than 1 pc, similar to those of
Bok globules. The luminosities of the associated {IRAS} sources are
relatively large, about 10 to 10,000 solar luminosities, compared to
those of the {IRAS} sources associated with dark globules or dense cores
in dark cloud complexes. {IRAS} luminosity to cloud mass ratios are
significantly greater than those in dark globules or in dense cores of
dark cloud complexes.},
journal = {Astrophysical Journal Supplement Series},
author = {Koji Sugitani and Yasuo Fukui and Katsuo Ogura},
month = sep,
year = {1991},
keywords = {{ASTRONOMICAL} {CATALOGS,} H {II} regions, {HYDROGEN} {CLOUDS,} {INFRARED} {ASTRONOMY} {SATELLITE,} {INFRARED} {SOURCES} {(ASTRONOMY),} {NEBULAE,} {NORTHERN} {HEMISPHERE,} {STAR} {FORMATION}},
pages = {59--66}
},
@article{niwa:millimeter-wave:2009,
title = {Millimeter-wave survey of molecular clouds around the {W5-East} triggered star-forming region},
volume = {500},
url = {http://cdsads.u-strasbg.fr/abs/2009A%26A...500.1119N},
abstract = {Aims. We examined the physical properties of molecular clouds
(morphology, column density, number density, mass) to investigate the
mechanism of triggered star formation by {UV} radiation from a massive
star. Methods: We made extensive, high-resolution maps of molecular
clouds associated and interacting with the {W5-East} H
ii region using the 45-m telescope at the Nobeyama Radio Observatory
{(HPBW} = 15.6 arcsec) in {13CO} {(J} = 1-0) and {C18O} {(J}
= 1-0) to reveal details in the high-density regions of the molecular
clouds. In addition, to investigate the spatial distributions of young
stellar objects {(YSOs)} in the {W5-East} H ii region, we
mapped the spatial distributions of Class I and {II} candidates. Results:
We identified eight {13CO} molecular clouds (three of them are
known bright-rimmed clouds) and nine {18O} clumps. The masses
of the clouds and clumps range from 460 to 36 000 Mȯ and
from 55 to 740 Mȯ, respectively. The peak
{13CO} column densities of the clouds facing the H ii region
are twice as large as the others. They have steep density gradients
toward the H ii region, indicating interactions with the H ii region. We
selected 55 Class I candidates and 778 Class {II} candidates associated
with the {W5-East} H ii region from the previous
Spitzer {IRAC/MIPS} survey. Most Class I candidates are located around
integrated intensity peaks of {13CO,} whereas most Class {II}
candidates are distributed along the front sides of the {BRC} arcs close
to the exciting star. Conclusions: The alignments of the {YSO} candidates
and the molecular clouds in order of age indicate that triggered star
formation occurs in the {W5-East} H ii region as a
result of gas compression by strong {UV} radiation. Based on the column
densities of {13CO} and the spatial distribution of {YSO}
candidates, we identified a new bright-rimmed cloud candidate on the
west side of the {W5-East} H ii region.},
journal = {Astronomy and Astrophysics},
author = {T. Niwa and K. Tachihara and Y. Itoh and Y. Oasa and K. Sunada and K. Sugitani and T. Mukai},
month = jun,
year = {2009},
keywords = {{ISM:} clouds, {ISM:} H {II} Regions, {RADIO} {LINES:} {ISM,} stars: evolution, Stars: Formation},
pages = {1119--1129}
}
@article{dewit2009,
title = {Resolved 24.5 micron emission from massive young stellar objects},
volume = {494},
url = {http://adsabs.harvard.edu/abs/2009A%26A...494..157D},
abstract = {Context: Massive young stellar objects {(MYSO)} are surrounded by massive
dusty envelopes, whose physical structure and geometry are determined by
the star formation process. Aims: Our principal aim is to establish the
density structure of {MYSO} envelopes on scales of {\textasciitilde}1000 {AU.} This
constitutes an increase of a factor {\textasciitilde}10 in angular resolution compared
to similar studies performed in the (sub)mm. Methods: We have obtained
diffraction-limited (0.6´´) 24.5 μm images (field of view
of 40 arcsec×30 arcsec) of 14 well-known massive star formation
regions with the {COMICS} instrument mounted on the 8.2 m Subaru
telescope. We construct azimuthally averaged intensity profiles of the
resolved {MYSO} envelopes and build spectral energy distributions {(SEDs)}
from archival data and the {COMICS} 24.5 μm flux density. The {SEDs}
range from near-infrared to millimeter wavelengths. Self-consistent {1-D}
radiative transfer models described by a density dependence of the form
n(r) ∝ r-p are used to simultaneously compare the
intensity profiles and {SEDs} to model predictions. Results: The images
reveal the presence of discrete {MYSO} sources which are resolved on
arcsecond scales, and, to first-order, the observed emission is circular
on the sky. For many sources, the spherical models are capable of
satisfactorily reproducing the 24.5 μm intensity profile, the 24.5
μm flux density, the 9.7 μm silicate absorption feature, and the
submm emission. They are described by density distributions with p
=1.0±0.25. Such distributions are shallower than those found on
larger scales probed with single-dish (sub)mm studies. Other sources
have density laws that are shallower/steeper than p=1.0 and there is
evidence that these are viewed near edge-on or near face-on
respectively. In these cases spherical models fail to provide good fits
to the data. The images also reveal a diffuse component tracing somewhat
larger scale structures, particularly visible in the regions S 140, {AFGL}
2136, {IRAS} 20126+4104, Mon R2, and Cep A. Conclusions: We find a
flattening of the {MYSO} density law going from scales probed with
single-dish submm observations down to scales of {\textasciitilde}1000 {AU} probed with
the observations presented here. We propose that this may be evidence of
rotational support of the envelope. This finding will be explored
further in a future paper using {2-D} axisymmetric radiative transfer
models.
Based on data collected at the Subaru telescope, which is operated by
the National Astronomical Observatory of Japan.},
journal = {Astronomy and Astrophysics},
author = {W. J. de Wit and M. G. Hoare and T. Fujiyoshi and R. D. Oudmaijer and M. Honda and H. Kataza and T. Miyata and Y. K. Okamoto and T. Onaka and S. Sako and T. Yamashita},
year = {2009},
keywords = {Infrared: Stars, {ISM:} clouds, Stars: {Early-Type,} Stars: Formation, stars: imaging},
pages = {157--178}
}
@article{bontemps1996,
title = {Evolution of outflow activity around low-mass embedded young stellar objects},
volume = {311},
url = {http://adsabs.harvard.edu/abs/1996A%26A...311..858B},
abstract = {We present a detailed study of outflow activity in a sample of 45
low-luminosity embedded young stellar objects {(YSOs).} We use maps in the
J=2-1 line of {{\textasciicircum}12{\textasciicircum}CO} to characterize this activity for {YSOs} that are
still sufficiently embedded to show molecular outflows. Our {CO} outflow
survey benefits from coordinated millimeter continuum measurements of
circumstellar masses which allow us to estimate the evolutionary states
of the central driving sources. Our sample comprises 36 {near-IR} {(Class}
I) protostars and 9 {far-IR/submm} {(Class} 0) protostars, and should be
representative of the ``self-embedded'' phase of (low-mass) protostellar
evolution characterizing young stars still surrounded by significant
circumstellar envelopes. We find that virtually all the objects in our
sample have detectable {CO} outflow activity. We make homogeneous
estimates of the outflow momentum flux deposited in the close
environment of the driving sources in order to assess the dynamical
properties of the underlying driving winds/jets. As is well-known, a
tight correlation between outflow energetics and driving source
luminosity is found for Class I sources. However, Class 0 sources lie a
factor of {\textasciitilde}10 above this correlation, suggesting they have qualitatively
different (e.g., more powerful) {CO} outflows. In addition, we find that
the outflow momentum flux correlates well with the circumstellar
envelope mass of the exciting source for both Class I and Class 0
sources. We show that this new correlation is independent of the
{F\_CO\_-L\_bol\_} correlation and most likely results from a more or less
continuous decrease of outflow power with time during the accretion
phase. For a young star of final mass {{\textasciitilde}0.6Msun\_,} the outflow
momentum flux is typically {F\_CO\_{\textasciitilde}10{\textasciicircum}-4{\textasciicircum}Msun\_.km/s/yr} at the
early Class 0 stage and {F\_CO\_{\textasciitilde}2x10{\textasciicircum}-6{\textasciicircum}Msun\_.km/s/yr} at the
late Class I stage. We suggest that this decrease of outflow energetics
reflects a corresponding decay in the mass accretion/infall rate.},
journal = {Astronomy and Astrophysics},
author = {S. Bontemps and P. Andre and S. Terebey and S. Cabrit},
month = jul,
year = {1996},
keywords = {{ISM:} {JETS} {AND} {OUTFLOWS,} {RADIO} {LINES:} {ISM,} {RADIO} {LINES:} {STARS,} Stars: Formation, {STARS:} {PRE-MAIN} {SEQUENCE}},
pages = {858--872}
}
@ARTICLE{young1991,
author = {{Young}, J.~S. and {Scoville}, N.~Z.},
title = "{Molecular gas in galaxies}",
journal = {\araa},
keywords = {GALACTIC EVOLUTION, INTERSTELLAR GAS, MOLECULAR GASES, SPIRAL GALAXIES, ACTIVE GALACTIC NUCLEI, CARBON MONOXIDE, GALACTIC STRUCTURE, INTERACTING GALAXIES, LOCAL GROUP (ASTRONOMY), STAR FORMATION},
year = 1991,
volume = 29,
pages = {581-625},
doi = {10.1146/annurev.aa.29.090191.003053},
adsurl = {http://adsabs.harvard.edu/abs/1991ARA%26A..29..581Y},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@INPROCEEDINGS{elmegreen1998,
author = {{Elmegreen}, B.~G.},
title = "{Observations and Theory of Dynamical Triggers for Star Formation}",
booktitle = {Origins},
year = 1998,
series = {Astronomical Society of the Pacific Conference Series},
volume = 148,
editor = "{C.~E.~Woodward, J.~M.~Shull, \& H.~A.~Thronson Jr.}",
pages = {150-+},
adsurl = {http://adsabs.harvard.edu/abs/1998ASPC..148..150E},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{adams1996,
author = {{Adams}, F.~C. and {Fatuzzo}, M.},
title = "{A Theory of the Initial Mass Function for Star Formation in Molecular Clouds}",
journal = {\apj},
eprint = {arXiv:astro-ph/9601139},
keywords = {ISM: CLOUDS, STARS: FORMATION, STARS: LUMINOSITY FUNCTION, MASS FUNCTION},
year = 1996,
month = jun,
volume = 464,
pages = {256-+},
doi = {10.1086/177318},
adsurl = {http://adsabs.harvard.edu/abs/1996ApJ...464..256A},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{elmegreen:sequential:1977,
author = {{Elmegreen}, B.~G. and {Lada}, C.~J.},
title = "{Sequential formation of subgroups in OB associations}",
journal = {\apj},
keywords = {B STARS, LYMAN SPECTRA, NEBULAE, O STARS, STAR CLUSTERS, STELLAR EVOLUTION, INTERSTELLAR GAS, PROTOSTARS, SHOCK FRONTS, STELLAR MODELS, STELLAR STRUCTURE},
year = 1977,
month = jun,
volume = 214,
pages = {725-741},
doi = {10.1086/155302},
adsurl = {http://adsabs.harvard.edu/abs/1977ApJ...214..725E},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{bertoldi:cometary:1990,
author = {{Bertoldi}, F. and {McKee}, C.~F.},
title = "{The photoevaporation of interstellar clouds. II - Equilibrium cometary clouds}",
journal = {\apj},
keywords = {COMETS, H II REGIONS, INTERSTELLAR MAGNETIC FIELDS, INTERSTELLAR MATTER, NEBULAE, STAR FORMATION, ASTRONOMICAL MODELS, CONTINUOUS RADIATION, EARLY STARS, GRAVITATIONAL EFFECTS, STELLAR EVOLUTION},
year = 1990,
month = may,
volume = 354,
pages = {529-548},
doi = {10.1086/168713},
adsurl = {http://adsabs.harvard.edu/abs/1990ApJ...354..529B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{klein:implosion:1983,
author = {{Klein}, R.~I. and {Sandford}, II, M.~T. and {Whitaker}, R.~W.
},
title = "{Star formation within OB subgroups - Implosion by multiple sources}",
journal = {\apjl},
keywords = {B STARS, O STARS, PLASMA COMPRESSION, STAR FORMATION, GRAVITATIONAL COLLAPSE, H II REGIONS, IMPLOSIONS, JEANS THEORY, SHOCK WAVE PROPAGATION, STELLAR RADIATION},
year = 1983,
month = aug,
volume = 271,
pages = {L69-L73},
doi = {10.1086/184097},
adsurl = {http://adsabs.harvard.edu/abs/1983ApJ...271L..69K},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{Arce2010,
Author = {{Arce}, H.~G. and {Borkin}, M.~A. and {Goodman}, A.~A. and {Pineda}, J.~E. and {Halle}, M.~W.},
Journal = {\apj},
Month = jun,
Pages = {1170-1190},
Title = {{The COMPLETE Survey of Outflows in Perseus}},
Volume = 715,
Year = 2010}
@ARTICLE{hatchell2009,
author = {{Hatchell}, J. and {Dunham}, M.~M.},
title = "{Star formation in Perseus. V. Outflows detected by HARP}",
journal = {\aap},
archivePrefix = "arXiv",
eprint = {0904.1163},
primaryClass = "astro-ph.GA",
keywords = {star: formation, stars: evolution, submillimeter, ISM: jets and outflows},
year = 2009,
month = jul,
volume = 502,
pages = {139-153},
doi = {10.1051/0004-6361/200911818},
adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...502..139H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{davis:jcmt:2010,
title = {The {JCMT} Legacy Survey of the Gould Belt: a first look at Taurus with {HARP}},
volume = {405},
shorttitle = {The {JCMT} Legacy Survey of the Gould Belt},
url = {http://adsabs.harvard.edu/abs/2010MNRAS.405..759D},
abstract = {{ABSTRACT} As part of a James Clerk Maxwell Telescope {(JCMT)} Legacy Survey
of star formation in the Gould Belt, we present early science results
for Taurus. {CO} J = 3 -2 maps have been secured along the north-west
ridge and bowl, collectively known as L 1495, along with deep
{13CO} and {C18O} J = 3 -2 maps in two subregions.
With these data, we search for molecular outflows, and use the
distribution of flows, {Herbig-Haro} {(HH)} objects and shocked
H2 line-emission features, together with the population of
young stars, protostellar cores and starless condensations to map star
formation across this extensive region. In total, 21 outflows are
identified. It is clear that the bowl is more evolved than the ridge,
harbouring a greater population of T Tauri stars and a more diffuse,
more turbulent ambient medium. By comparison, the ridge contains a much
younger, less widely distributed population of protostars which, in
turn, is associated with a greater number of molecular outflows. We
estimate the ratio of the numbers of pre-stellar to protostellar cores
in L 1495 to be {\textasciitilde}1.3-2.3, and of gravitationally unbound starless cores
to (gravitationally bound) pre-stellar cores to be {\textasciitilde}1. If we take
previous estimates of the protostellar lifetime of {\textasciitilde}5 ×
105 yr, this indicates a pre-stellar lifetime of 9(+/-3)
× 105 yr. From the number of outflows, we also crudely
estimate the star formation efficiency in L 1495, finding it to be
compatible with a canonical value of 10-15 per cent. We note that
molecular outflow-driving sources have redder near-infrared colours than
their {HH} jet-driving counterparts. We also find that the smaller, denser
cores are associated with the more massive outflows, as one might expect
if mass build-up in the flow increases with the collapse and contraction
of the protostellar envelope.},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {C. J. Davis and A. Chrysostomou and J. Hatchell and J. G. A. Wouterloot and J. V. Buckle and D. Nutter and M. Fich and C. Brunt and H. Butner and B. Cavanagh and E. I. Curtis and A. {Duarte-Cabral} and J. di Francesco and M. Etxaluze and P. Friberg and R. Friesen and G. A. Fuller and S. Graves and J. S. Greaves and M. R. Hogerheijde and D. Johnstone and B. Matthews and H. Matthews and J. M. C. Rawlings and J. S. Richer and J. Roberts and S. Sadavoy and R. J. Simpson and N. Tothill and Y. Tsamis and S. Viti and D. {Ward-Thompson} and Glenn J. White and J. Yates},
month = jun,
year = {2010},
keywords = {{ISM:} individual: Taurus, {ISM:} {JETS} {AND} {OUTFLOWS,} {ISM:} {KINEMATICS} {AND} {DYNAMICS,} Stars: Formation},
pages = {759--776}
},
@article{graves:jcmt:2010,
title = {The {JCMT} Legacy Survey of the Gould Belt: a first look at Serpens with {HARP}},
shorttitle = {The {JCMT} Legacy Survey of the Gould Belt},
url = {http://arxiv.org/abs/1006.0891},
abstract = {The Gould Belt Legacy Survey {(GBS)} on the {JCMT} has observed a region of 260 square arcminutes in {12CO} J=3--2 emission, and a 190 square arcminute subset of this in {13CO} and {C18O} towards the Serpens molecular cloud. We examine the global velocity structure of the non-outflowing gas, and calculate excitation temperatures and opacities. The large scale mass and energetics of the region are evaluated, with special consideration for high velocity gas. We find the cloud to have a mass of 203 solar masses, and to be gravitationally bound, and that the kinetic energy of the outflowing gas is approximately seventy percent of the turbulent kinetic energy of the cloud. We identify compact outflows towards some of the submillimetre Class {0/I} sources in the region},
journal = {1006.0891},
author = {S. F Graves and J. S Richer and J. V Buckle and A. {Duarte-Cabral} and G. A Fuller and M. R Hogerheijde and J. E Owen and C. Brunt and H. M Butner and B. Cavanagh and A. Chrysostomou and E. I Curtis and C. J Davis and M. Etxaluze and J. Di Francesco and P. Friberg and R. K Friesen and J. S Greaves and J. Hatchell and D. Johnstone and B. Matthews and H. Matthews and C. D Matzner and D. Nutter and J. M. C Rawlings and J. F Roberts and S. Sadavoy and R. J Simpson and N. F. H Tothill and Y. G Tsamis and S. Viti and D. {Ward-Thompson} and G. J White and J. G. A Wouterloot and J. Yates},
month = jun,
year = {2010},
keywords = {Astrophysics - Galaxy Astrophysics}
},
@article{hatchell2007,
title = {Star formation in Perseus. {III.} Outflows},
volume = {472},
url = {http://adsabs.harvard.edu/abs/2007A%26A...472..187H},
abstract = {Context: We present a search for outflows towards 51 submillimetre cores
in the Perseus molecular cloud.
Aims: Our first objective is to
identify the protostellar population through the detection of molecular
outflows. Our second aim is to consistently derive outflow properties
from a large homogeneous dataset within one molecular cloud in order to
investigate further the mass dependence and time evolution of
protostellar mass loss.
Methods: We used the James Clerk Maxwell
Telescope to map 2' × 2' regions around each core in
{12CO} 3-2. Where molecular outflows were detected we derived
momentum fluxes.
Results: Of the 51 cores, 37 show broad
linewings indicative of molecular outflows. In 13 cases, the linewings
could be due to confusion with neighbouring flows but 9 of those sources
also have near-infrared detections confirming their protostellar nature.
The total fraction of protostars in our sample is 65\%. All but four
outflow detections are confirmed as protostellar by Spitzer {IR}
detections and only one Spitzer source has no outflow, showing that
outflow maps at this sensitivity are equally good at identifying
protostars as Spitzer. Outflow momentum flux correlates both with source
luminosity and with core mass but there is considerable scatter even
within this one cloud despite the homogeneous dataset. We fail to
confirm the result of Bontemps et al. (1996) that Class I sources show
lower momentum fluxes on average than Class 0 sources, with a {KS} test
showing a significant probability that the momentum fluxes for both
Class 0s and Class Is are drawn from the same distribution.
Conclusions: We find that outflow power may not show a simple decline
between the Class 0 to Class I stages. Our sample includes low momentum
flux, low-luminosity Class 0 sources, possibly at a very early
evolutionary stage. If the only mass loss from the core were due to
outflows, cores would last for 10{\textasciicircum}5-108 years, longer than
current estimates of 1.5-4 × 105 years for the mean
lifetime for the embedded phase. Additional mechanisms for removing mass
from protostellar cores may be necessary.
Figs. 9 and 10 are only available in electronic form at
http://www.aanda.org Datacube data in {FITS} are only available in
electronic form at the {CDS} via anonymous ftp to cdsarc.u-strasbg.fr
(130.79.128.5) or via
{http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/472/187}},
journal = {Astronomy and Astrophysics},
author = {{Hatchell}, J. and G. A. Fuller and J. S. Richer},
month = sep,
year = {2007},
keywords = {{ISM:} {JETS} {AND} {OUTFLOWS,} stars: evolution, Stars: Formation, Submillimeter},
pages = {187--198}
}
@ARTICLE{Ossenkopf1994,
author = {{Ossenkopf}, V. and {Henning}, T.},
title = "{Dust opacities for protostellar cores}",
journal = {AAP},
keywords = {COAGULATION, DUST, OPACITY, PROTOSTARS, STAR FORMATION, STELLAR CORES, STELLAR MODELS, ABSORPTIVITY, GAS DENSITY, INFRARED ASTRONOMY, INTERSTELLAR EXTINCTION, OPTICAL PROPERTIES, RADIO ASTRONOMY, STELLAR COMPOSITION},
year = 1994,
month = nov,
volume = 291,
pages = {943-959},
adsurl = {http://cdsads.u-strasbg.fr/abs/1994A%26A...291..943O},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@INBOOK{Dionatos2010,
author = {{Dionatos}, O. and {Nisini}, B. and {Giannini}, T. and {Codella}, C. and
{Richer}, J. and {Tafalla}, M.},
title = "{Wide Field JCMT HARP-B CO(3-2) Mapping of the Serpens Cloud Core}",
booktitle = {Protostellar Jets in Context},
year = 2009,
editor = "{Tsinganos, K., Ray, T., \& Stute, M.}",
pages = {535-537},
doi = {10.1007/978-3-642-00576-3_70},
adsurl = {http://adsabs.harvard.edu/abs/2009pjc..book..535D},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Zapata2001,
author = {{Zapata}, L.~A. and {Rodr{\'{\i}}guez}, L.~F. and {Kurtz}, S.~E.
},
title = "{A Subarcsecond Radio Binary Associated with AFGL 4029-IRS1}",
journal = {\rmxaa},
year = 2001,
month = apr,
volume = 37,
pages = {83-86},
adsurl = {http://adsabs.harvard.edu/abs/2001RMxAA..37...83Z},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Taylor2003:CGPS,
author = {{Taylor}, A.~R. and {Gibson}, S.~J. and {Peracaula}, M. and
{Martin}, P.~G. and {Landecker}, T.~L. and {Brunt}, C.~M. and
{Dewdney}, P.~E. and {Dougherty}, S.~M. and {Gray}, A.~D. and
{Higgs}, L.~A. and {Kerton}, C.~R. and {Knee}, L.~B.~G. and
{Kothes}, R. and {Purton}, C.~R. and {Uyaniker}, B. and {Wallace}, B.~J. and
{Willis}, A.~G. and {Durand}, D.},
title = "{The Canadian Galactic Plane Survey}",
journal = {AJ},
keywords = {Galaxy: General, ISM: General, ISM: Structure, Surveys},
year = 2003,
month = jun,
volume = 125,
pages = {3145-3164},
doi = {10.1086/375301},
adsurl = {http://adsabs.harvard.edu/abs/2003AJ....125.3145T},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Felli1987,
author = {{Felli}, M. and {Hjellming}, R.~M. and {Cesaroni}, R.},
title = "{S201 - an H II region produced by an ionization front eroding a molecular cloud}",
journal = {\aap},
keywords = {HYDROGEN CLOUDS, RADIO SOURCES (ASTRONOMY), EARLY STARS, GAS DYNAMICS},
year = 1987,
month = aug,
volume = 182,
pages = {313-323},
adsurl = {http://adsabs.harvard.edu/abs/1987A%26A...182..313F},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Deharveng1997,
author = {{Deharveng}, L. and {Zavagno}, A. and {Cruz-Gonzalez}, I. and
{Salas}, L. and {Caplan}, J. and {Carrasco}, L.},
title = "{AFGL 4029: a cluster of massive young stars.}",
journal = {\aap},
keywords = {STARS: PRE-MAIN-SEQUENCE, ISM: REFLECTION NEBULAE, INFRARED: STARS, ISM: INDIVIDUAL OBJECTS: AFGL 4029},
year = 1997,
month = jan,
volume = 317,
pages = {459-475},
adsurl = {http://adsabs.harvard.edu/abs/1997A%26A...317..459D},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Digel1996,
author = {{Digel}, S.~W. and {Lyder}, D.~A. and {Philbrick}, A.~J. and
{Puche}, D. and {Thaddeus}, P.},
title = "{A Large-Scale CO Survey toward W3, W4, and W5}",
journal = {\apj},
keywords = {GALAXY: STRUCTURE, ISM: CLOUDS, ISM: INDIVIDUAL ALPHANUMERIC: W3, ISM: INDIVIDUAL ALPHANUMERIC: W4, ISM: INDIVIDUAL ALPHANUMERIC: W5, ISM: MOLECULES, RADIO LINES: ISM},
year = 1996,
month = feb,
volume = 458,
pages = {561-+},
doi = {10.1086/176839},
adsurl = {http://cdsads.u-strasbg.fr/abs/1996ApJ...458..561D},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Enoch2006,
author = {{Enoch}, M.~L. and {Young}, K.~E. and {Glenn}, J. and {Evans}, II, N.~J. and
{Golwala}, S. and {Sargent}, A.~I. and {Harvey}, P. and {Aguirre}, J. and
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title = "{SIMBA survey of southern high-mass star forming regions. I. Physical parameters of the 1.2 mm/IRAS sources}",
journal = {\aap},
keywords = {ISM: clouds, stars: formation, ISM: dust, extinction, radio continum: ISM, stars: circumstellar matter, ISM: H II regions},
year = 2004,
month = oct,
volume = 426,
pages = {97-103},
doi = {10.1051/0004-6361:20035755},
adsurl = {http://adsabs.harvard.edu/abs/2004A%26A...426...97F},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Vansevicius2009,
author = {{Vansevi{\v c}ius}, V. and {Kodaira}, K. and {Narbutis}, D. and
{Stonkut{\.e}}, R. and {Brid{\v z}ius}, A. and {Deveikis}, V. and
{Semionov}, D.},
title = "{Compact Star Clusters in the M31 Disk}",
journal = {\apj},
archivePrefix = "arXiv",
eprint = {0909.1912},
primaryClass = "astro-ph.GA",
keywords = {galaxies: individual: M31, galaxies: star clusters, stars: formation},
year = 2009,
month = oct,
volume = 703,
pages = {1872-1883},
doi = {10.1088/0004-637X/703/2/1872},
adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...703.1872V},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Barmby2006,
author = {{Barmby}, P. and {Ashby}, M.~L.~N. and {Bianchi}, L. and {Engelbracht}, C.~W. and
{Gehrz}, R.~D. and {Gordon}, K.~D. and {Hinz}, J.~L. and {Huchra}, J.~P. and
{Humphreys}, R.~M. and {Pahre}, M.~A. and {P{\'e}rez-Gonz{\'a}lez}, P.~G. and
{Polomski}, E.~F. and {Rieke}, G.~H. and {Thilker}, D.~A. and
{Willner}, S.~P. and {Woodward}, C.~E.},
title = "{Dusty Waves on a Starry Sea: The Mid-Infrared View of M31}",
journal = {\apjl},
eprint = {arXiv:astro-ph/0608593},
keywords = {Galaxies: Individual: Messier Number: M31, Galaxies: ISM, Galaxies: Spiral, Galaxies: Stellar Content, Infrared: Galaxies},
year = 2006,
month = oct,
volume = 650,
pages = {L45-L49},
doi = {10.1086/508626},
adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...650L..45B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Chomiuk2011,
author = {{Chomiuk}, L. and {Povich}, M.~S.},
title = "{Toward a Unification of Star Formation Rate Determinations in the Milky Way and Other Galaxies}",
journal = {\aj},
archivePrefix = "arXiv",
eprint = {1110.4105},
primaryClass = "astro-ph.GA",
keywords = {galaxies: star formation, Galaxy: fundamental parameters, H II regions, ISM: supernova remnants },
year = 2011,
month = dec,
volume = 142,
eid = {197},
pages = {197},
doi = {10.1088/0004-6256/142/6/197},
adsurl = {http://adsabs.harvard.edu/abs/2011AJ....142..197C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{LadaLada2003,
author = {{Lada}, C.~J. and {Lada}, E.~A.},
title = "{Embedded Clusters in Molecular Clouds}",
journal = {\araa},
eprint = {arXiv:astro-ph/0301540},
year = 2003,
volume = 41,
pages = {57-115},
doi = {10.1146/annurev.astro.41.011802.094844},
adsurl = {http://adsabs.harvard.edu/abs/2003ARA%26A..41...57L},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Bressert2010,
author = {{Bressert}, E. and {Bastian}, N. and {Gutermuth}, R. and {Megeath}, S.~T. and
{Allen}, L. and {Evans}, II, N.~J. and {Rebull}, L.~M. and {Hatchell}, J. and
{Johnstone}, D. and {Bourke}, T.~L. and {Cieza}, L.~A. and {Harvey}, P.~M. and
{Merin}, B. and {Ray}, T.~P. and {Tothill}, N.~F.~H.},
title = "{The spatial distribution of star formation in the solar neighbourhood: do all stars form in dense clusters?}",
journal = {\mnras},
archivePrefix = "arXiv",
eprint = {1009.1150},
primaryClass = "astro-ph.SR",
keywords = {stars: formation, stars: protostars, open clusters and associations: general, infrared: stars},
year = 2010,
month = nov,
volume = 409,
pages = {L54-L58},
doi = {10.1111/j.1745-3933.2010.00946.x},
adsurl = {http://adsabs.harvard.edu/abs/2010MNRAS.409L..54B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Lada1984,
author = {{Lada}, C.~J. and {Margulis}, M. and {Dearborn}, D.},
title = "{The formation and early dynamical evolution of bound stellar systems}",
journal = {\apj},
keywords = {COMPUTATIONAL ASTROPHYSICS, INTERSTELLAR GAS, STAR CLUSTERS, STELLAR EVOLUTION, STELLAR SYSTEMS, ASTRONOMICAL MODELS, MANY BODY PROBLEM, MOLECULAR CLOUDS, PLEIADES CLUSTER, POSITION (LOCATION)},
year = 1984,
month = oct,
volume = 285,
pages = {141-152},
doi = {10.1086/162485},
adsurl = {http://adsabs.harvard.edu/abs/1984ApJ...285..141L},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Bastian2006,
author = {{Bastian}, N. and {Goodwin}, S.~P.},
title = "{Evidence for the strong effect of gas removal on the internal dynamics of young stellar clusters}",
journal = {\mnras},
eprint = {arXiv:astro-ph/0602465},
keywords = {stellar dynamics: methods: N-body simulations: galaxies: star clusters, stellar dynamics, methods: N-body simulations, galaxies: star clusters},
year = 2006,
month = jun,
volume = 369,
pages = {L9-L13},
doi = {10.1111/j.1745-3933.2006.00162.x},
adsurl = {http://adsabs.harvard.edu/abs/2006MNRAS.369L...9B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Wang2010,
author = {{Wang}, P. and {Li}, Z.-Y. and {Abel}, T. and {Nakamura}, F.
},
title = "{Outflow Feedback Regulated Massive Star Formation in Parsec-Scale Cluster-Forming Clumps}",
journal = {\apj},
archivePrefix = "arXiv",
eprint = {0908.4129},
primaryClass = "astro-ph.SR",
keywords = {ISM: jets and outflows, magnetic fields, methods: numerical, magnetohydrodynamics: MHD, stars: formation, turbulence},
year = 2010,
month = jan,
volume = 709,
pages = {27-41},
doi = {10.1088/0004-637X/709/1/27},
adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...709...27W},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Price2009,
author = {{Price}, D.~J. and {Bate}, M.~R.},
title = "{Inefficient star formation: the combined effects of magnetic fields and radiative feedback}",
journal = {\mnras},
archivePrefix = "arXiv",
eprint = {0904.4071},
primaryClass = "astro-ph.SR",
keywords = {magnetic fields , MHD , stars: formation , stars: low-mass, brown dwarfs , ISM: clouds , galaxies: star clusters},
year = 2009,
month = sep,
volume = 398,
pages = {33-46},
doi = {10.1111/j.1365-2966.2009.14969.x},
adsurl = {http://adsabs.harvard.edu/abs/2009MNRAS.398...33P},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Messineo2011,
author = {{Messineo}, M. and {Davies}, B. and {Figer}, D.~F. and {Kudritzki}, R.~P. and
{Valenti}, E. and {Trombley}, C. and {Najarro}, F. and {Rich}, R.~M.
},
title = "{Massive Stars in the Cl 1813-178 Cluster: An Episode Of Massive Star Formation in the W33 Complex}",
journal = {\apj},
archivePrefix = "arXiv",
eprint = {1103.4975},
primaryClass = "astro-ph.GA",
keywords = {infrared: stars, stars: evolution},
year = 2011,
month = may,
volume = 733,
eid = {41},
pages = {41},
doi = {10.1088/0004-637X/733/1/41},
adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...733...41M},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Schlingman2011,
author = {{Schlingman}, W.~M. and {Shirley}, Y.~L. and {Schenk}, D.~E. and
{Rosolowsky}, E. and {Bally}, J. and {Battersby}, C. and {Dunham}, M.~K. and
{Ellsworth-Bowers}, T.~P. and {Evans}, II, N.~J. and {Ginsburg}, A. and
{Stringfellow}, G.},
title = "{The Bolocam Galactic Plane Survey. V. HCO$^{+}$ and N$_{2}$H$^{+}$ Spectroscopy of 1.1 mm Dust Continuum Sources}",
journal = {\apjs},
archivePrefix = "arXiv",
eprint = {1105.4181},
primaryClass = "astro-ph.GA",
keywords = {Galaxy: kinematics and dynamics, Galaxy: structure, ISM: clouds, ISM: kinematics and dynamics, stars: formation, submillimeter: ISM, surveys},
year = 2011,
month = aug,
volume = 195,
eid = {14},
pages = {14},
doi = {10.1088/0067-0049/195/2/14},
adsurl = {http://adsabs.harvard.edu/abs/2011ApJS..195...14S},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Vacca1996,
author = {{Vacca}, W.~D. and {Garmany}, C.~D. and {Shull}, J.~M.},
title = "{The Lyman-Continuum Fluxes and Stellar Parameters of O and Early B-Type Stars}",
journal = {\apj},
keywords = {STARS: ATMOSPHERES, STARS: EARLY-TYPE, STARS: FUNDAMENTAL PARAMETERS, ULTRAVIOLET: STARS},
year = 1996,
month = apr,
volume = 460,
pages = {914},
doi = {10.1086/177020},
adsurl = {http://adsabs.harvard.edu/abs/1996ApJ...460..914V},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Kroupa2001,
author = {{Kroupa}, P.},
title = "{On the variation of the initial mass function}",
journal = {\mnras},
eprint = {arXiv:astro-ph/0009005},
keywords = {BINARIES: GENERAL, STARS: FORMATION, STARS: KINEMATICS, STARS: LUMINOSITY FUNCTION, MASS FUNCTION, GLOBULAR CLUSTERS: GENERAL, OPEN CLUSTERS AND ASSOCIATIONS: GENERAL},
year = 2001,
month = apr,
volume = 322,
pages = {231-246},
doi = {10.1046/j.1365-8711.2001.04022.x},
adsurl = {http://adsabs.harvard.edu/abs/2001MNRAS.322..231K},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Schuller2009,
author = {{Schuller}, F. and {Menten}, K.~M. and {Contreras}, Y. and {Wyrowski}, F. and
{Schilke}, P. and {Bronfman}, L. and {Henning}, T. and {Walmsley}, C.~M. and
{Beuther}, H. and {Bontemps}, S. and {Cesaroni}, R. and {Deharveng}, L. and
{Garay}, G. and {Herpin}, F. and {Lefloch}, B. and {Linz}, H. and
{Mardones}, D. and {Minier}, V. and {Molinari}, S. and {Motte}, F. and
{Nyman}, L.-{\AA}. and {Reveret}, V. and {Risacher}, C. and
{Russeil}, D. and {Schneider}, N. and {Testi}, L. and {Troost}, T. and
{Vasyunina}, T. and {Wienen}, M. and {Zavagno}, A. and {Kovacs}, A. and
{Kreysa}, E. and {Siringo}, G. and {Wei{\ss}}, A.},
title = "{ATLASGAL - The APEX telescope large area survey of the galaxy at 870 {$\mu$}m}",
journal = {\aap},
archivePrefix = "arXiv",
eprint = {0903.1369},
primaryClass = "astro-ph.GA",
keywords = {surveys, submillimeter, ISM: structure, dust, extinction, stars: formation, Galaxy: disk},
year = 2009,
month = sep,
volume = 504,
pages = {415-427},
doi = {10.1051/0004-6361/200811568},
adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...504..415S},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Bressert2012,
author = {{Bressert}, E. and {Ginsburg}, A. and {Battersby}, C. and {Bally}, J. and
{Longmore}, S. and {Testi}, L.},
title = "{How to Find Young Massive Cluster Progenitors}",
journal = {ArXiv e-prints},
archivePrefix = "arXiv",
eprint = {1208.3472},
primaryClass = "astro-ph.GA",
keywords = {Astrophysics - Galaxy Astrophysics, Astrophysics - Solar and Stellar Astrophysics},
year = 2012,
month = aug,
adsurl = {http://adsabs.harvard.edu/abs/2012arXiv1208.3472B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Clauset2007,
author = {{Clauset}, A. and {Rohilla Shalizi}, C. and {Newman}, M.~E.~J.
},
title = "{Power-law distributions in empirical data}",
journal = {ArXiv e-prints},
archivePrefix = "arXiv",
eprint = {0706.1062},
primaryClass = "physics.data-an",
keywords = {Physics - Data Analysis, Statistics and Probability, Condensed Matter - Disordered Systems and Neural Networks, Statistics - Applications, Statistics - Methodology},
year = 2007,
month = jun,
adsurl = {http://adsabs.harvard.edu/abs/2007arXiv0706.1062C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Lepine2011,
author = {{L{\'e}pine}, J.~R.~D. and {Cruz}, P. and {Scarano}, Jr., S. and
{Barros}, D.~A. and {Dias}, W.~S. and {Pomp{\'e}ia}, L. and
{Andrievsky}, S.~M. and {Carraro}, G. and {Famaey}, B.},
title = "{Overlapping abundance gradients and azimuthal gradients related to the spiral structure of the Galaxy}",
journal = {\mnras},
archivePrefix = "arXiv",
eprint = {1106.3137},
primaryClass = "astro-ph.GA",
keywords = {stars: kinematics and dynamics, Galaxy: abundances, Galaxy: evolution, Galaxy: structure},
year = 2011,
month = oct,
volume = 417,
pages = {698-708},
doi = {10.1111/j.1365-2966.2011.19314.x},
adsurl = {http://adsabs.harvard.edu/abs/2011MNRAS.417..698L},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Kennicutt2012,
author = {{Kennicutt}, Jr., R.~C. and {Evans}, II, N.~J.},
title = "{Star Formation in the Milky Way and Nearby Galaxies}",
journal = {ArXiv e-prints},
archivePrefix = "arXiv",
eprint = {1204.3552},
primaryClass = "astro-ph.GA",
keywords = {Astrophysics - Galaxy Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics},
year = 2012,
month = apr,
adsurl = {http://adsabs.harvard.edu/abs/2012arXiv1204.3552K},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Hillenbrand1997,
author = {{Hillenbrand}, L.~A.},
title = "{On the Stellar Population and Star-Forming History of the Orion Nebula Cluster}",
journal = {\aj},
year = 1997,
month = may,
volume = 113,
pages = {1733-1768},
doi = {10.1086/118389},
adsurl = {http://adsabs.harvard.edu/abs/1997AJ....113.1733H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Wolfire2003,
author = {{Wolfire}, M.~G. and {McKee}, C.~F. and {Hollenbach}, D. and
{Tielens}, A.~G.~G.~M.},
title = "{Neutral Atomic Phases of the Interstellar Medium in the Galaxy}",
journal = {\apj},
eprint = {arXiv:astro-ph/0207098},
keywords = {ISM: Clouds, ISM: General, ISM: Structure},
year = 2003,
month = apr,
volume = 587,
pages = {278-311},
doi = {10.1086/368016},
adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...587..278W},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Shirley2012,
author = {{Shirley}, Y.},
title = "{BGPS HCO+ follow-up}",
journal = {\apjs},
primaryClass = "astro-ph.GA",
keywords = {ISM: clouds, methods: data analysis, stars: formation, stars: massive, submillimeter: ISM, surveys},
year = {2013},
}
@ARTICLE{Gwinn1992,
author = {{Gwinn}, C.~R. and {Moran}, J.~M. and {Reid}, M.~J.},
title = "{Distance and kinematics of the W49N H2O maser outflow}",
journal = {\apj},
keywords = {GAS FLOW, INTERSTELLAR MATTER, MILKY WAY GALAXY, STAR FORMATION, WATER MASERS, DEGREES OF FREEDOM, DOPPLER EFFECT, GALACTIC ROTATION, H II REGIONS, LINE OF SIGHT},
year = 1992,
month = jul,
volume = 393,
pages = {149-164},
doi = {10.1086/171493},
adsurl = {http://adsabs.harvard.edu/abs/1992ApJ...393..149G},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Sato2010,
author = {M. Sato and M. J. Reid and A. Brunthaler and K. M. Menten},
title = {Trigonometric Parallax of W51 Main/South},
year = {2010},
month = {06},
abstract = {We report measurement of the trigonometric parallax of W51 Main/South
using the Very Long Baseline Array (VLBA). We measure a value of
0.185 +/- 0.010 mas, corresponding to a distance of 5.41 (+0.31/-0.28)
kpc. W51 Main/South is a well-known massive star-forming region near
the tangent point of the Sagittarius spiral arm of the Milky Way.
Our distance to W51 yields an estimate of the distance to the Galactic
center of Ro = 8.3 +/- 0.46 (statistical) +/- 1.0 (systematic) kpc
by simple geometry. Combining the parallax and proper motion measurements
for W51, we obtained the full-space motion of this massive star forming
region. We find W51 is in a nearly circular orbit about the Galactic
center. The H2O masers used for our parallax measurements trace four
powerful bipolar outflows within a 0.4 pc size region, some of which
are associated with dusty molecular hot cores and/or hyper- or ultra-compact
HII regions.},
bdsk-url-1 = {http://arxiv.org/abs/1006.4218v4},
date-added = {2011-08-02 19:50:02 +0000},
date-modified = {2011-08-02 19:50:02 +0000},
eprint = {1006.4218v4},
url = {http://arxiv.org/abs/1006.4218v4}
}
@ARTICLE{Urquhart2012,
author = {{Urquhart}, J.~S. and {Hoare}, M.~G. and {Lumsden}, S.~L. and
{Oudmaijer}, R.~D. and {Moore}, T.~J.~T. and {Mottram}, J.~C. and
{Cooper}, H.~D.~B. and {Mottram}, M. and {Rogers}, H.~C.},
title = "{The RMS survey: resolving kinematic distance ambiguities towards a sample of compact H II regions using H I absorption}",
journal = {\mnras},
archivePrefix = "arXiv",
eprint = {1111.1625},
primaryClass = "astro-ph.GA",
keywords = {stars: early-type, stars: formation, ISM: clouds, Galaxy: kinematics and dynamics},
year = 2012,
month = feb,
volume = 420,
pages = {1656-1672},
doi = {10.1111/j.1365-2966.2011.20157.x},
adsurl = {http://adsabs.harvard.edu/abs/2012MNRAS.420.1656U},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Araya2002,
author = {{Araya}, E. and {Hofner}, P. and {Churchwell}, E. and {Kurtz}, S.},
title = {{Arecibo Observations of Formaldehyde and Radio Recombination Lines
toward Ultracompact H II Regions}},
journal = {\apjs},
year = {2002},
volume = {138},
pages = {63-74},
month = jan,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {http://adsabs.harvard.edu/abs/2002ApJS..138...63A},
bdsk-url-1 = {http://dx.doi.org/10.1086/324021},
date-added = {2011-08-02 19:31:54 +0000},
date-modified = {2011-08-02 19:31:54 +0000},
doi = {10.1086/324021},
keywords = {Galaxy: Structure, ISM: H II Regions, ISM: Molecules, Radio Lines:
ISM}
}
@ARTICLE{Churchwell1990,
author = {{Churchwell}, E. and {Walmsley}, C.~M. and {Cesaroni}, R.},
title = "{A survey of ammonia and water vapor emission from ultracompact HII regions}",
journal = {\aaps},
keywords = {AMMONIA, H II REGIONS, INTERSTELLAR CHEMISTRY, MOLECULAR CLOUDS, WATER VAPOR, INFRARED SPECTRA, INTERSTELLAR MASERS, O STARS, WATER MASERS},
year = 1990,
month = apr,
volume = 83,
pages = {119-144},
adsurl = {http://adsabs.harvard.edu/abs/1990A%26AS...83..119C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Pandian2008,
author = {{Pandian}, J.~D. and {Momjian}, E. and {Goldsmith}, P.~F.},
title = "{Resolving distance ambiguities towards 6.7 GHz methanol masers}",
journal = {\aap},
archivePrefix = "arXiv",
eprint = {0805.2697},
keywords = {Galaxy: kinematics and dynamics, Galaxy: structure, H II regions},
year = 2008,
month = jul,
volume = 486,
pages = {191-208},
doi = {10.1051/0004-6361:200809799},
adsurl = {http://adsabs.harvard.edu/abs/2008A%26A...486..191P},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Vig2008,
author = {{Vig}, S. and {Cesaroni}, R. and {Testi}, L. and {Beltr{\'a}n}, M.~T.
and {Codella}, C.},
title = {{A multiwavelength investigation of G24.78+0.08 A2 using observations
from VLA and VLT-VISIR}},
journal = {\aap},
year = {2008},
volume = {488},
pages = {605-617},
month = sep,
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {http://adsabs.harvard.edu/abs/2008A%26A...488..605V},
bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:200809423},
date-added = {2011-08-02 19:31:03 +0000},
date-modified = {2011-08-02 19:31:03 +0000},
doi = {10.1051/0004-6361:200809423},
keywords = {stars: formation, stars: circumstellar matter, ISM: individual objects:
G24.78+0.08 A2, infrared: ISM, radio lines: ISM}
}
@INPROCEEDINGS{Crossley2008,
author = {{Crossley}, J.~H. and {Sjouwerman}, L.~O. and {Fomalont}, E.~B. and
{Radziwill}, N.~M.},
title = "{NRAO VLA archive survey}",
booktitle = {Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series},
year = 2008,
series = {Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series},
volume = 7016,
month = jul,
doi = {10.1117/12.787890},
adsurl = {http://adsabs.harvard.edu/abs/2008SPIE.7016E..20C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Cesaroni2010,
author = {{Cesaroni}, R. and {Hofner}, P. and {Araya}, E. and {Kurtz}, S.
},
title = "{The structure of hot molecular cores over 1000 AU}",
journal = {\aap},
keywords = {stars: formation, Hii regions, ISM: individual objects: G10.47+0.03, G31.41+0.31, ISM: molecules},
year = 2010,
month = jan,
volume = 509,
eid = {A50},
pages = {A50},
doi = {10.1051/0004-6361/200912877},
adsurl = {http://adsabs.harvard.edu/abs/2010A%26A...509A..50C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{Lucas2008,
author = {{Lucas}, P.~W. and {Hoare}, M.~G. and {Longmore}, A. and {Schr{\"o}der}, A.~C. and
{Davis}, C.~J. and {Adamson}, A. and {Bandyopadhyay}, R.~M. and
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% I've gone through and slowly added the full page range back, because of
% Jason's insistence that NSF requires this
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primaryclass = {astro-ph.GA},
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year = {2011},
pages = {129-134},
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primaryclass = {astro-ph.GA},
year = {2011},
keywords = {dust, extinction, ISM: clouds, ISM: molecules, stars: formation},
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adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...741..110D}
}
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Bieging2011,
author = {{Bieging}, J. H. and {Peters}, W. L.},
doi = {10.1088/0067-0049/196/2/18},
title = {{The Arizona Radio Observatory CO Mapping Survey of Galactic Molecular Clouds. II. The W3 Region in CO J = 2-1, $^{13}$CO J = 2-1, and CO J = 3-2 Emission}},
journal = {\apjs},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {October},
volume = {196},
eid = {18},
key = {2011ApJS..196...18B},
year = {2011},
keywords = {H II regions, ISM: clouds, ISM: individual objects: W3, ISM: kinematics and dynamics, ISM: molecules},
pages = {18},
adsurl = {http://adsabs.harvard.edu/abs/2011ApJS..196...18B}
}
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doi = {10.1088/0004-637X/740/1/40},
key = {2011ApJ...740...40R},
title = {{Evidence for Inflow in High-mass Star-forming Clumps}},
journal = {\apj},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {October},
volume = {740},
eprint = {1107.5343},
eid = {40},
primaryclass = {astro-ph.SR},
year = {2011},
keywords = {ISM: clouds, stars: formation},
archiveprefix = {arXiv},
pages = {40},
adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...740...40R}
}
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doi = {10.1111/j.1365-2966.2011.19056.x},
title = {{Mercer 5: a probable new globular cluster in the Galactic bulge}},
journal = {\mnras},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {September},
volume = {416},
key = {2011MNRAS.416..465L},
year = {2011},
keywords = {stars: abundances, stars: distances, Galaxy: abundances, globular clusters: general, globular clusters: individual: Mercer 5: [MCM2005b] 5},
pages = {465-478},
adsurl = {http://adsabs.harvard.edu/abs/2011MNRAS.416..465L}
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key = {2011AJ....142...94S},
title = {{Testing the Global Star Formation relation: An HCO$^{+}$ (3-2) Mapping Study of Red MSX Sources in the Bolocam Galactic Plane Survey}},
journal = {\aj},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {September},
volume = {142},
eprint = {1109.1246},
eid = {94},
primaryclass = {astro-ph.GA},
year = {2011},
keywords = {galaxies: star formation, radio lines: general, stars: formation},
archiveprefix = {arXiv},
pages = {94},
adsurl = {http://adsabs.harvard.edu/abs/2011AJ....142...94S}
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key = {2011ApJ...736..149G},
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journal = {\apj},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {August},
volume = {736},
eprint = {1106.1430},
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primaryclass = {astro-ph.GA},
year = {2011},
keywords = {H II regions, ISM: molecules, stars: formation},
archiveprefix = {arXiv},
pages = {149},
adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...736..149G}
}
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doi = {10.1088/0067-0049/195/1/1},
key = {2011ApJS..195....1R},
title = {{The Physical Properties of High-mass Star-forming Clumps: A Systematic Comparison of Molecular Tracers}},
journal = {\apjs},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {July},
volume = {195},
eprint = {1104.3899},
eid = {1},
primaryclass = {astro-ph.GA},
year = {2011},
keywords = {dust, extinction, ISM: clouds, stars: formation},
archiveprefix = {arXiv},
pages = {1},
adsurl = {http://adsabs.harvard.edu/abs/2011ApJS..195....1R}
}
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key = {2011A&A...530A..25P},
title = {{Study of the molecular clump associated with the high-energy source HESS J1858+020}},
journal = {\aap},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {June},
volume = {530},
eprint = {1103.5742},
eid = {A25},
primaryclass = {astro-ph.GA},
year = {2011},
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adsurl = {http://adsabs.harvard.edu/abs/2011A%26A...530A..25P}
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journal = {\mnras},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {May},
volume = {413},
eprint = {1012.0782},
primaryclass = {astro-ph.GA},
year = {2011},
keywords = {stars: formation, ISM: individual objects: Galactic Plane, ISM: jets and outflows, ISM: kinematics and dynamics, infrared: stars},
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journal = {\aap},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
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volume = {529},
eprint = {1103.1320},
eid = {A161},
primaryclass = {astro-ph.GA},
year = {2011},
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adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {April},
volume = {731},
eprint = {1102.4610},
eid = {126},
primaryclass = {astro-ph.IM},
year = {2011},
keywords = {methods: data analysis, methods: statistical, techniques: miscellaneous, X-rays: general},
archiveprefix = {arXiv},
pages = {126},
adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...731..126L}
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title = {{A Mid-infrared Census of Star Formation Activity in Bolocam Galactic Plane Survey Sources}},
journal = {\apj},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {April},
volume = {731},
eprint = {1102.1032},
eid = {90},
primaryclass = {astro-ph.GA},
year = {2011},
keywords = {dust, extinction, infrared: stars, ISM: clouds, stars: formation},
archiveprefix = {arXiv},
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adsnote = {Provided by the SAO/NASA Astrophysics Data System},
month = {March},
volume = {193},
eprint = {1101.4072},
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primaryclass = {astro-ph.SR},
year = {2011},
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year = {2010},
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