32 research outputs found
Molecular Gas Around Young Stellar Clusters
We have begun a survey of the molecular gas surrounding 31 young clusters in
order to investigate the link between environment and the resulting cluster. We
present here a preliminary comparison of two clusters in our sample: GGD12-15
and Mon R2. Since both clusters are located in the MonR2 molecular cloud at a
distance of 830 pc, observational biases due to differing sensitivities and
angular resolutions are avoided.Comment: 2 pages, 2 figures, uses newpasp.sty. To appear in "Hot Star Workshop
III: The Earliest Phases of Massive Star Birth" (ed. P.A. Crowther
An Unbiased Survey for Outflows in the W3 and W5 Star-Formation Regions
During their birth all stars undergo periods of copious mass loss, frequently
characterized by the occurrence of bipolar outflows. These outflows are
believed to play a fundamental role in the star formation process. However the
exact outflow generating method is obscure at present. To elucidate this
problem we are investigating whether the flow properties are correlated over
the entire protostellar mass spectrum. Progress in this area requires that we
assemble a statistically valid sample of high-mass outflow systems. This is
necessary since existing catalogues of such objects are heterogeneous and
statistically incomplete.Comment: 2 pages, 1 figure, uses newpasp.sty. To appear in "Hot Star Workshop
III: The Earliest Phases of Massive Star Birth" (ed. P.A. Crowther
The COMPLETE Nature of the Warm Dust Ring in Perseus
The Perseus molecular cloud complex is a ~30pc long chain of molecular clouds
most well-known for the two star-forming clusters NGC1333 and IC348 and the
well-studied outflow source in B5. However, when studied at mid- to
far-infrared wavelengths the region is dominated by a ~10pc diameter shell of
warm dust, likely generated by an HII region caused by the early B-star
HD278942. Using a revised calibration technique the COMPLETE team has produced
high-sensitivity temperature and column-density maps of the Perseus region from
IRAS Sky Survey Atlas (ISSA) 60 and 100um data. In this paper, we combine the
ISSA based dust-emission maps with other observations collected as part of the
COMPLETE Survey, along with archival H-alpha and MSX observations. Molecular
line observations from FCRAO and extinction maps constructed by applying the
NICER method to the 2MASS catalog provide independent estimates of the ``true''
column-density of the shell. H-alpha emission in the region of the shell
confirms that it is most likely an HII region located behind the cloud complex,
and 8um data from MSX indicates that the shell may be interacting with the
cloud. Finally, the two polarisation components previously seen towards
background stars in the region can be explained by the association of the
stronger component with the shell. If confirmed, this would be the first
observation of a parsec-scale swept-up magnetic field.Comment: Accepted by ApJ. Figures have been compressed - full resolution
version available at http://cfa-www.harvard.edu/COMPLETE/results.htm
Turbulence driven by outflow-blown cavities in the molecular cloud of NGC 1333
Outflows from young stellar objects have been identified as a possible source
of turbulence in molecular clouds. To investigate the relationship between
outflows, cloud dynamics and turbulence, we compare the kinematics of the
molecular gas associated with NGC 1333, traced in 13CO(1-0), with the
distribution of young stellar objects (YSOs) within. We find a velocity
dispersion of ~ 1-1.6 km/s in 13CO that does not significantly vary across the
cloud, and is uncorrelated with the number of nearby young stellar outflows
identified from optical and submillimeter observations. However, from velocity
channel maps we identify about 20 cavities or depressions in the 13CO intensity
of scales > 0.1-0.2 pc and velocity widths 1-3 km/s. The cavities exhibit limb
brightened rims in both individual velocity channel maps and position velocity
diagrams, suggesting that they are slowly expanding. We interpret these
cavities to be remnants of past YSO outflow activity: If these cavities are
presently empty, they would fill in on time scales of a million years. This can
exceed the lifetime of a YSO outflow phase, or the transit time of the central
star through the cavity, explaining the the absence of any clear correlation
between the cavities and YSO outflows. We find that the momentum and energy
deposition associated with the expansion of the cavities is sufficient to power
the turbulence in the cloud. In this way we conclude that the cavities are an
important intermediary step between the conversion of YSO outflow energy and
momentum into cloud turbulent motions.Comment: Accepted for publication in ApJ. Check out
http://astro.pas.rochester.edu/~aquillen/coolpics.html for channel map and
PosVel movies of N133
Outflow - Core Interaction in Barnard 1
In order to study how outflows from protostars influence the physical and
chemical conditions of the parent molecular cloud, we have observed Barnard 1
(B1) main core, which harbors four Class 0 and three Class I sources, in the CO
(J=1-0), CH3OH (J_K=2_K-1_K), and the SiO (J=1-0) lines using the Nobeyama 45 m
telescope. We have identified three CO outflows in this region; one is an
elongated (~ 0.3 pc) bipolar outflow from a Class 0 protostar B1-c in the
submillimeter clump SMM 2, another is a rather compact (~ 0.1 pc) outflow from
a Class I protostar B1 IRS in the clump SMM 6, and the other is an extended
outflow from a Class I protostar in SMM 11. In the western lobe of the SMM 2
outflow, both the SiO and CH3OH lines show broad redshifted wings with the
terminal velocities of 25 km/s and 13 km/s, respectively. It is likely that the
shocks caused by the interaction between the outflow and ambient gas enhance
the abundance of SiO and CH3OH in the gas phase. The total energy input rate by
the outflows (1.1x10^{-3} Lsun) is smaller than the energy loss rate
(8.5x10^{-3} Lsun$) through the turbulence decay in B1 main core, which
suggests that the outflows can not sustain the turbulence in this region. Since
the outflows are energetic enough to compensate the dissipating turbulence
energy in the neighboring, more evolved star forming region NGC 1333, we
suggest that the turbulence energy balance depends on the evolutionary state of
the star formation in molecular clouds.Comment: 34 pages, 8 figures, accepted for the publication in Ap
The COMPLETE Survey of Star-Forming Regions: Phase I Data
We present an overview of data available for the Ophiuchus and Perseus
molecular clouds from ``Phase I'' of the COMPLETE Survey of Star-Forming
Regions. This survey provides a range of data complementary to the Spitzer
Legacy Program ``From Molecular Cores to Planet Forming Disks.'' Phase I
includes: Extinction maps derived from 2MASS near-infrared data using the NICER
algorithm; extinction and temperature maps derived from IRAS 60 and 100um
emission; HI maps of atomic gas; 12CO and 13CO maps of molecular gas; and
submillimetre continuum images of emission from dust in dense cores. Not
unexpectedly, the morphology of the regions appears quite different depending
on the column-density tracer which is used, with IRAS tracing mainly warmer
dust and CO being biased by chemical, excitation and optical depth effects.
Histograms of column-density distribution are presented, showing that
extinction as derived from 2MASS/NICER gives the closest match to a log-normal
distribution as is predicted by numerical simulations. All the data presented
in this paper, and links to more detailed publications on their implications
are publically available at the COMPLETE website.Comment: Accepted by AJ. Full resolution version available from:
http://www.cfa.harvard.edu/COMPLETE/papers/complete_phase1.pd
A 13CO and C18O Survey of the Molecular Gas Around Young Stellar Clusters Within 1kpc of the Sun
As the first step of a multi-wavelength investigation into the relationship
between young stellar clusters and their environment we present fully-sampled
maps in the J=1--0 lines of 13CO and C18O and the J=2--1 line of C18O for a
selected group of thirty young stellar groups and clusters within 1kpc of the
Sun. This is the first systematic survey of these regions to date. The clusters
range in size from several stars to a few hundred stars. Thirty fields ranging
in size from 8'x 8' to 60'x 30' were mapped with 47'' resolution simultaneously
in the J=1-0 lines with Five College Radio Observatory. Seventeen sources were
mapped over fields ranging in size from 3'x 3' to 13'x 13' in the J=2--1 line
with 35'' resolution with the Heinrich Hertz Telescope. We compare the cloud
properties derived from each of the three tracers in order to better understand
systematic uncertainties in determing masses and linewidths. Cloud masses are
determined independently using the 13CO and C18O transitions, these masses
range from 30 to 4000 M_sun. Finally, we present a simple morphological
classification scheme which may serve as a rough indicator of cloud evolution.Comment: 52 pages, 29 figures. Accepted for publication in AJ. Some figures
have been reduced in resolution, a full resolution version is available from
http://daisy.astro.umass.edu/~naomi/pubs/pubs.htm
ABCA7 p.G215S as potential protective factor for Alzheimer’s disease
Genome-wide association studies (GWASs) have been effective approaches to dissect common genetic variability underlying complex diseases in a systematic and unbiased way. Recently, GWASs have led to the discovery of over 20 susceptibility loci for Alzheimer’s disease (AD).
Despite the evidence showing the contribution of these loci to AD pathogenesis, their genetic architecture has not been extensively investigated, leaving the possibility that low frequency and rare coding variants may also occur and contribute to the risk of disease. We have used exome and genome sequencing data to analyse the single independent and joint effect of rare and low frequency protein coding variants in 9 AD GWAS loci with the strongest effect sizes after APOE (BIN1, CLU, CR1, PICALM, MS4A6A, ABCA7, EPHA1, CD33, CD2AP) in a cohort of 332 sporadic AD cases and 676 elderly controls of British and North American ancestry. We identified coding variability in ABCA7 as contributing to AD risk. This locus harbors a low frequency coding variant (p.G215S, rs72973581, MAF=4.3%) conferring a modest but statistically significant protection against AD (p-value= 6x10-4, OR=0.57, 95% CI 0.41-0.80). Notably, our results are not driven by an enrichment of loss of function variants in ABCA7, recently reported as main pathogenic factor underlying AD risk at this locus. In summary, our study confirms the role of ABCA7 in AD and provide new insights that should address functional studies