672 research outputs found
Wide field CO J = 3->2 mapping of the Serpens Cloud Core
Context. Outflows provide indirect means to get an insight on diverse star
formation associated phenomena. On scales of individual protostellar cores,
outflows combined with intrinsic core properties can be used to study the mass
accretion/ejection process of heavily embedded protostellar sources. Methods.
An area comprising 460"x230" of the Serpens cloud core has been mapped in 12 CO
J = 3\to 2 with the HARP-B heterodyne array at the James Clerk Maxwell
Telescope; J = 3\to 2 observations are more sensitive tracers of hot outflow
gas than lower J CO transitions; combined with the high sensitivity of the
HARP-B receptors outflows are sharply outlined, enabling their association with
individual protostellar cores. Results. Most of ~20 observed outflows are found
to be associated with known protostellar sources in bipolar or unipolar
configurations. All but two outflow/core pairs in our sample tend to have a
projected orientation spanning roughly NW-SE. The overall momentum driven by
outflows in Serpens lies between 3.2 and 5.1 x 10^(-1) M\odot km s^(-1), the
kinetic energy from 4.3 to 6.7 x 10^(43) erg and momentum flux is between 2.8
and 4.4 x 10^(-4) M\odot km s^(-1) yr^(-1). Bolometric luminosities of
protostellar cores based on Spitzer photometry are found up to an order of
magnitude lower than previous estimations derived with IRAS/ISO data.
Conclusions. We confirm the validity of the existing correlations between the
momentum flux and bolometric luminosity of Class I sources for the homogenous
sample of Serpens, though we suggest that they should be revised by a shift to
lower luminosities. All protostars classified as Class 0 sources stand well
above the known Class I correlations, indicating a decline in momentum flux
between the two classes.Comment: 15 pages, 10 figures, accepted for publication in A&
Molecular ions in the protostellar shock L1157-B1
We perform a complete census of molecular ions with an abundance larger than
1e-10 in the protostellar shock L1157-B1 by means of an unbiased
high-sensitivity survey obtained with the IRAM-30m and Herschel/HIFI. By means
of an LVG radiative transfer code the gas physical conditions and fractional
abundances of molecular ions are derived. The latter are compared with
estimates of steady-state abundances in the cloud and their evolution in the
shock calculated with the chemical model Astrochem. We detect emission from
HCO+, H13CO+, N2H+, HCS+, and, for the first time in a shock, from HOCO+, and
SO+. The bulk of the emission peaks at blueshifted velocity, ~ 0.5-3 km/s with
respect to systemic, has a width of ~ 4-8 km/s, and is associated with the
outflow cavities (T_kin ~ 20-70 K, n(H2) ~ 1e5 cm-3). Observed HCO+ and N2H+
abundances are in agreement with steady-state abundances in the cloud and with
their evolution in the compressed and heated gas in the shock for cosmic rays
ionization rate Z = 3e-16 s-1. HOCO+, SO+, and HCS+ observed abundances,
instead, are 1-2 orders of magnitude larger than predicted in the cloud; on the
other hand they are strongly enhanced on timescales shorter than the shock age
(~2000 years) if CO2, S or H2S, and OCS are sputtered off the dust grains in
the shock. The performed analysis indicates that HCO+ and N2H+ are a fossil
record of pre-shock gas in the outflow cavity, while HOCO+, SO+, and HCS+ are
effective shock tracers and can be used to infer the amount of CO2 and
sulphur-bearing species released from dust mantles in the shock. The observed
HCS+ (and CS) abundance indicates that OCS should be one of the main sulphur
carrier on grain mantles. However, the OCS abundance required to fit the
observations is 1-2 orders of magnitude larger than observed. Further studies
are required to fully understand the chemistry of sulphur-bearing species.Comment: 12 pages, 5 figures, accepted by A&
First evidence for molecular interfaces between outflows and ambient clouds in high-mass star-forming regions?
We present new observations of the Cep A East region of massive star formation and describe an extended and dynamically distinct feature not previously recognized. This feature is present in emission from H2CS, OCS, CH3OH, and HDO at −5.5 km s−1 but is not traced by the conventional tracers of star-forming regions, H2S, SO2, SO, and CS. The feature is extended up to at least 0.1 pc. We show that the feature is neither a hot core nor a shocked outflow. However, the chemistry of the feature is consistent with predictions from a model of an eroding interface between a fast wind and a dense core; mixing between the two media occurs in the interface on a timescale of 10–50 yr. If these observations are confirmed by detailed maps and by detections in species also predicted to be abundant (e.g., HCO+, H2CO, and NH3), this feature would be the first detection of such an interface in regions of massive star formation. An important implication of the model is that a significant reservoir of sulfur in grain mantles is required to be in the form of OCS
BCN20000: dermoscopic lesions in the wild
This article summarizes the BCN20000 dataset, composed of 19424 dermoscopic images of skin lesions captured from 2010 to 2016 in the facilities of the Hospital Clínic in Barcelona. With this dataset, we aim to study the problem of unconstrained classification of dermoscopic images of skin cancer, including lesions found in hard-to-diagnose locations (nails and mucosa), large lesions which do not fit in the aperture of the dermoscopy device, and hypo-pigmented lesions. The BCN20000 will be provided to the participants of the ISIC Challenge 2019 [8], where they will be asked to train algorithms to classify dermoscopic images of skin cancer automatically.Peer ReviewedPreprin
The L1157-B1 astrochemical laboratory: testing the origin of DCN
L1157-B1 is the brightest shocked region of the large-scale molecular
outflow, considered the prototype of chemically rich outflows, being the ideal
laboratory to study how shocks affect the molecular gas. Several deuterated
molecules have been previously detected with the IRAM 30m, most of them formed
on grain mantles and then released into the gas phase due to the shock. We aim
to observationally investigate the role of the different chemical processes at
work that lead to formation the of DCN and test the predictions of the chemical
models for its formation. We performed high-angular resolution observations
with NOEMA of the DCN(2-1) and H13CN(2-1) lines to compute the deuterated
fraction, Dfrac(HCN). We detected emission of DCN(2-1) and H13CN(2-1) arising
from L1157-B1 shock. Dfrac(HCN) is ~4x10 and given the uncertainties, we
did not find significant variations across the bow-shock. Contrary to HDCO,
whose emission delineates the region of impact between the jet and the ambient
material, DCN is more widespread and not limited to the impact region. This is
consistent with the idea that gas-phase chemistry is playing a major role in
the deuteration of HCN in the head of the bow-shock, where HDCO is undetected
as it is a product of grain-surface chemistry. The spectra of DCN and H13CN
match the spectral signature of the outflow cavity walls, suggesting that their
emission result from shocked gas. The analysis of the time dependent gas-grain
chemical model UCL-CHEM coupled with a C-type shock model shows that the
observed Dfrac(HCN) is reached during the post-shock phase, matching the
dynamical timescale of the shock. Our results indicate that the presence of DCN
in L1157-B1 is a combination of gas-phase chemistry that produces the
widespread DCN emission, dominating in the head of the bow-shock, and
sputtering from grain mantles toward the jet impact region.Comment: Accepted for publication in A&A. 7 pages, 5 Figures, 1 Tabl
SiO excitation from dense shocks in the earliest stages of massive star formation
Molecular outflows are a direct consequence of accretion, and therefore they
represent one of the best tracers of accretion processes in the still poorly
understood early phases of high-mass star formation. Previous studies suggested
that the SiO abundance decreases with the evolution of a massive young stellar
object probably because of a decay of jet activity, as witnessed in low-mass
star-forming regions. We investigate the SiO excitation conditions and its
abundance in outflows from a sample of massive young stellar objects through
observations of the SiO(8-7) and CO(4-3) lines with the APEX telescope. Through
a non-LTE analysis, we find that the excitation conditions of SiO increase with
the velocity of the emitting gas. We also compute the SiO abundance through the
SiO and CO integrated intensities at high velocities. For the sources in our
sample we find no significant variation of the SiO abundance with evolution for
a bolometric luminosity-to-mass ratio of between 4 and 50 . We
also find a weak increase of the SiO(8-7) luminosity with the bolometric
luminosity-to-mass ratio. We speculate that this might be explained with an
increase of density in the gas traced by SiO. We find that the densities
constrained by the SiO observations require the use of shock models that
include grain-grain processing. For the first time, such models are compared
and found to be compatible with SiO observations. A pre-shock density of
cm is globally inferred from these comparisons. Shocks with a
velocity higher than 25 km s are invoked for the objects in our sample
where the SiO is observed with a corresponding velocity dispersion. Our
comparison of shock models with observations suggests that sputtering of
silicon-bearing material (corresponding to less than 10% of the total silicon
abundance) from the grain mantles is occurring.Comment: Accepted for publication by A&
Molecules with a peptide link in protostellar shocks: a comprehensive study of L1157
Interstellar molecules with a peptide link -NH-C(=O)-, like formamide
(NHCHO), acetamide (NHCOCH) and isocyanic acid (HNCO) are
particularly interesting for their potential role in pre-biotic chemistry. We
have studied their emission in the protostellar shock regions L1157-B1 and
L1157-B2, with the IRAM 30m telescope, as part of the ASAI Large Program.
Analysis of the line profiles shows that the emission arises from the outflow
cavities associated with B1 and B2. Molecular abundance of
and are derived for
formamide and isocyanic acid, respectively, from a simple rotational diagram
analysis. Conversely, NHCOCH was not detected down to a relative
abundance of a few . B1 and B2 appear to be among the richest
Galactic sources of HNCO and NHCHO molecules. A tight linear correlation
between their abundances is observed, suggesting that the two species are
chemically related. Comparison with astrochemical models favours molecule
formation on ice grain mantles, with NHCHO generated from hydrogenation of
HNCO.Comment: 11 pages, 9 figures. Accepted for publication in MNRAS Main Journal.
Accepted 2014 August 19, in original form 2014 July
Discovery Of A Molecular Outflow in the Haro 6-10 Star-Forming Region
We present high sensitivity 12CO and 13CO (1-0) molecular line maps covering
the full extent of the parsec scale Haro~6-10 Herbig-Haro (HH) flow. We report
the discovery of a molecular CO outflow along the axis of parsec-scale HH flow.
Previous molecular studies missed the identification of the outflow probably
due to their smaller mapping area and the confusing spectral features present
towards the object. Our detailed molecular line study of the full 1.6 pc extent
of the optical flow shows evidence for both blueshifted and redshifted gas set
in motion by Haro~6-10 activity. The molecular outflow is centered at
Haro~6-10, with redshifted gas being clumpy and directed towards the northeast,
while blueshifted gas is in the southwest direction. The molecular gas
terminates well within the cloud, short of the most distant HH objects of the
optical flow. Contamination from an unrelated cloud along the same line of
sight prevents a thorough study of the blueshifted outflow lobe and the mass
distribution at the lowest velocities in both lobes. The cloud core in which
Haro~6-10 is embedded is filamentary and flattened in the east-west direction.
The total cloud mass is calculated from 13CO(1-0) to be ~200Msun. The lower
limit of the mass associated with the outflow is ~0.25Msun.Comment: ApJ Accepted; 9 pages, 8 figures. For high resolution ps file use:
http://www.astro.umass.edu/~irena/haro.p
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