1,348 research outputs found
A High-Mass Protobinary System in the Hot Core W3(H2O)
We have observed a high-mass protobinary system in the hot core W3(H2O) with
the BIMA Array. Our continuum maps at wavelengths of 1.4mm and 2.8mm both
achieve sub-arcsecond angular resolutions and show a double-peaked morphology.
The angular separation of the two sources is 1.19" corresponding to 2.43X10^3
AU at the source distance of 2.04 kpc. The flux densities of the two sources at
1.4mm and 2.8mm have a spectral index of 3, translating to an opacity law of
kappa ~ nu. The small spectral indices suggest that grain growth has begun in
the hot core. We have also observed 5 K components of the CH3CN (12-11)
transitions. A radial velocity difference of 2.81 km/s is found towards the two
continuum peaks. Interpreting these two sources as binary components in orbit
about one another, we find a minimum mass of 22 Msun for the system. Radiative
transfer models are constructed to explain both the continuum and methyl
cyanide line observations of each source. Power-law distributions of both
density and temperature are derived. Density distributions close to the
free-fall value, r^-1.5, are found for both components, suggesting continuing
accretion. The derived luminosities suggest the two sources have equivalent
zero-age main sequence (ZAMS) spectral type B0.5 - B0. The nebular masses
derived from the continuum observations are about 5 Msun for source A and 4
Msun for source C. A velocity gradient previously detected may be explained by
unresolved binary rotation with a small velocity difference.Comment: 38 pages, 9 figures, accepted by The Astrophysical Journa
Submillimeter Observations of The Isolated Massive Dense Clump IRAS 20126+4104
We used the CSO 10.4 meter telescope to image the 350 micron and 450 micron
continuum and CO J=6-5 line emission of the IRAS 20126+4104 clump. The
continuum and line observations show that the clump is isolated over a 4 pc
region and has a radius of ~ 0.5 pc. Our analysis shows that the clump has a
radial density profile propto r ^{-1.2} for r <~ 0.1 pc and has propto r^{-2.3}
for r >~ 0.1 pc which suggests the inner region is infalling, while the infall
wave has not yet reached the outer region. Assuming temperature gradient of
r^{-0.35}, the power law indices become propto r ^{-0.9} for r < ~0.1 pc and
propto r^{-2.0} for r >~ 0.1 pc. Based on a map of the flux ratio of
350micron/450micron, we identify three distinct regions: a bipolar feature that
coincides with the large scale CO bipolar outflow; a cocoon-like region that
encases the bipolar feature and has a warm surface; and a cold layer outside of
the cocoon region. The complex patterns of the flux ratio map indicates that
the clump is no longer uniform in terms of temperature as well as dust
properties. The CO emission near the systemic velocity traces the dense clump
and the outer layer of the clump shows narrow line widths (< ~3 km/s). The
clump has a velocity gradient of ~ 2 km/s pc^{-1}, which we interpret as due to
rotation of the clump, as the equilibrium mass (~ 200 Msun) is comparable to
the LTE mass obtained from the CO line. Over a scale of ~ 1 pc, the clump
rotates in the opposite sense with respect to the >~ 0.03 pc disk associated
with the (proto)star. This is one of four objects in high-mass and low-mass
star forming regions for which a discrepancy between the rotation sense of the
envelope and the core has been found, suggesting that such a complex kinematics
may not be unusual in star forming regions.Comment: 34 pages, 13 figures, Accepted for publication in the Ap
High Resolution Observations of the Massive Protostar in IRAS18566+0408
We report 3 mm continuum, CH3CN(5-4) and 13CS(2-1) line observations with
CARMA, in conjunction with 6 and 1.3 cm continuum VLA data, and 12 and 25
micron broadband data from the Subaru Telescope toward the massive proto-star
IRAS18566+0408. The VLA data resolve the ionized jet into 4 components aligned
in the E-W direction. Radio components A, C, and D have flat cm SEDs indicative
of optically thin emission from ionized gas, and component B has a spectral
index alpha = 1.0, and a decreasing size with frequency proportional to
frequency to the -0.5 power. Emission from the CARMA 3 mm continuum, and from
the 13CS(2-1), and CH3CN(5-4) spectral lines is compact (i.e. < 6700 AU), and
peaks near the position of VLA cm source, component B. Analysis of these lines
indicates hot, and dense molecular gas, typical for HMCs. Our Subaru telescope
observations detect a single compact source, coincident with radio component B,
demonstrating that most of the energy in IRAS18566+0408 originates from a
region of size < 2400 AU. We also present UKIRT near-infrared archival data for
IRAS18566+0408 which show extended K-band emission along the jet direction. We
detect an E-W velocity shift of about 10 km/sec over the HMC in the CH3CN lines
possibly tracing the interface of the ionized jet with the surrounding core
gas. Our data demonstrate the presence of an ionized jet at the base of the
molecular outflow, and support the hypothesis that massive protostars with
O-type luminosity form with a mechanism similar to lower mass stars
A Documentary of High-Mass Star Formation: Probing the Dynamical Evolution of Orion Source I on 10-100 AU Scales using SiO Masers
A comprehensive picture of high-mass star formation has remained elusive, in
part because examples of high-mass YSOs tend to be relatively distant, deeply
embedded, and confused with other emission sources. These factors have impeded
dynamical investigations within tens of AU of high-mass YSOs--scales that are
critical for probing the interfaces where outflows from accretion disks are
launched and collimated. Using observations of SiO masers obtained with the VLA
and the VLBA, the KaLYPSO project is overcoming these limitations by mapping
the structure and dynamical/temporal evolution of the material 10-1000 AU from
the nearest high-mass YSO: Radio Source I in the Orion BN/KL region. Our data
include ~40 epochs of VLBA observations over a several-year period, allowing us
to track the proper motions of individual SiO maser spots and to monitor
changes in the physical conditions of the emitting material with time.
Ultimately these data will provide 3-D maps of the outflow structure over
approximately 30% of the outflow crossing time. Here we summarize recent
results from the KaLYPSO project, including evidence that high-mass star
formation is occurring via disk-mediated accretion.Comment: 5 pages; to appear in the proceedings of IAU Symposium 242,
Astrophysical Masers and their Environments, ed. J. Chapman & W. Baa
IRAS 23385+6053: a candidate protostellar massive object
We present the results of a multi-line and continuum study towards the source
IRAS 23385+6053,performed with the IRAM-30m telescope, the Plateau de Bure
Interferometer, the Very Large Array Interferometer and the James Clerk Maxwell
Telescope. The new results confirm our earlier findings, namely that IRAS
23385+6053 is a good candidate high-mass protostellar object, precursor of an
ultracompact H region. The source is roughly composed of two regions: a
molecular core pc in size, with a temperature of K
and an H volume density of the order of 10 cm, and an
extended halo of diameter 0.4 pc, with an average kinetic temperature of
K and H volume density of the order of 10 cm. The
core temperature is much smaller than what is typically found in molecular
cores of the same diameter surrounding massive ZAMS stars. We deduce that the
core luminosity is between 150 and , and we believe
that the upper limit is near the ``true'' source luminosity. Moreover, by
comparing the H volume density obtained at different radii from the IRAS
source, we find that the halo has a density profile of the type . This suggests that the source is gravitationally
unstable. Finally, we demonstrate that the temperature at the core surface is
consistent with a core luminosity of and conclude that we
might be observing a protostar still accreting material from its parental
cloud, whose mass at present is .Comment: 18 pages, 20 figure
Long and short term changes in abundance and distribution of butterflies: hints from the Lazio database
The DB on the occurrence data of the butterflies (Papilionoidea) of Lazio, at 14th February 2022 consisted of 36244 records including 154 species istributed throughout a total of 6719 sites. The data set included geoeferenced and chrono-referenced data collected from the literature, specialist-validated occurrences from websites (Forum Natura Mediterraneo, iNaturalist, Ornitho), as well as an important amount of original observations included in the database of the Lazio Biodiversity Observatory. All observations were used to create distribution maps. In order to evaluate any change in observations over time for the various species, all records were divided into three different periods: before 1980
(4425 records), 1980-2000 (6498 records) and post 2000 (25321 records). A finer subdivision was then examined within the post-2000 period: 2001-2007 (11888 records), 2008-2014 (4977 records), 2014-2021 (8456 records). Further analyses were carried out to highlight differences in the distribution of species as a function of altitude and / or changes in land use that have occurred in the last decades. The results show that qualitatively the species present in the region before 1980 are all still present today,
however the abundance of related observations in several cases has changed considerably. Observations of an important portion of the species have significantly decreased in recent years. This trend is observed in the majority of mountain species and various habitat-specialist butterflies regardless of altitude. In some other species, often the most common or habitat-generalist butterflies, an increase was observed. The causes of
these trends can be identified in the human land use and climate change, without excluding, however, the differences in data recording over time that could favor the most common species
X-Ray Emission from Young Stars in the Massive Star Forming Region IRAS 20126+4104
We present a ks Chandra observation of the IRAS20126+4104 core
region. In the inner two X-ray sources were detected, which
are coincident with the radio jet source I20S and the variable radio source
I20Var. No X-ray emission was detected from the nearby massive protostar I20N.
The spectra of both detected sources are hard and highly absorbed, with no
emission below keV.
For I20S, the measured keV count rate was ctsks.
The X-ray spectrum was fit with an absorbed 1T APEC model with an energy of
kTkeV and an absorbing column of Ncm.
An unabsorbed X-ray luminosity of about ergs
was estimated. The spectrum shows broad line emission between 6.4 and 6.7\,
keV, indicative of emission from both neutral and highly ionized iron. The
X-ray lightcurve indicates that I20S is marginally variable; however, no flare
emission was observed.
The variable radio source I20Var was detected with a count rate of
ctsks but there was no evidence of X-ray variability. The
best fit spectral model is a 1T APEC model with an absorbing hydrogen column of
Ncm and a plasma energy of kT = 6.0keV.
The unabsorbed X-ray luminosity is about ergs.Comment: 17pages, 4 figures to appear in Astronomical Journa
Radio Continuum and Recombination Line Study of UC HII Regions with Extended Envelopes
We have carried out 21 cm radio continuum observations of 16 UC HII regions
using the VLA (D-array) in search of associated extended emission. We have also
observed H76 recombination line towards all the sources and
He76 line at the positions with strong H76 line emission. The
UC HII regions have simple morphologies and large (>10) ratios of single-dish
to VLA fluxes. Extended emission was detected towards all the sources. The
extended emission consists of one to several compact components and a diffuse
extended envelope. All the UC HII regions but two are located in the compact
components, where the UC HII regions always correspond to their peaks. The
compact components with UC HII regions are usually smaller and denser than
those without UC HII regions. Our recombination line observations indicate that
the ultracompact, compact, and extended components are physically associated.
The UC HII regions and their associated compact components are likely to be
ionized by the same sources on the basis of the morphological relations
mentioned above. This suggests that almost all of the observed UC HII regions
are not `real' UC HII regions and that their actual ages are much greater than
their dynamical age (<10000 yr). We find that most of simple UC HII regions
previously known have large ratios of single-dish to VLA fluxes, similar to our
sources. Therefore, the `age problem' of UC HII regions does not seem to be as
serious as earlier studies argued. We present a simple model that explains
extended emission around UC HII regions. Some individual sources are discussed.Comment: 29 pages, 28 postscript figures, Accepted for publication in Ap
CARPET: a web-based package for the analysis of ChIP-chip and expression tiling data
Summary: CARPET (Collection of Automated Routine Programs for Easy Tiling) is a set of Perl, Python and R scripts, integrated on the Galaxy2 web-based platform, for the analysis of ChIP-chip and expression tiling data, both for standard and custom chip designs. CARPET allows rapid experimental data entry, simple quality control, normalization, easy identification and annotation of enriched ChIP-chip regions, detection of the absolute or relative transcriptional status of genes assessed by expression tiling experiments and, more importantly, it allows the integration of ChIP-chip and expression data. Results can be visualized instantly in a genomic context within the UCSC genome browser as graph-based custom tracks through Galaxy2. All generated and uploaded data can be stored within sessions and are easily shared with other users. Availability: http://bio.ifom-ieo-campus.it/galaxy Contacts: [email protected] lucilla.luzi@if om-ieo-campus.i
Molecular jets driven by high-mass protostars: a detailed study of the IRAS 20126+4104 jet
We present here an extensive analysis of the protostellar jet driven by IRAS
20126+4104, deriving the kinematical, dynamical, and physical conditions of the
H2 gas along the flow. The jet has been investigated by means of near-IR H2 and
[FeII] narrow-band imaging, high resolution spectroscopy of the 1-0S(1) line
(2.12 um), NIR (0.9-2.5 um) low resolution spectroscopy, along with ISO-SWS and
LWS spectra (from 2.4 to 200 um). The flow shows a complex morphology. In
addition to the large-scale jet precession presented in previous studies, we
detect a small-scale wiggling close to the source, that may indicate the
presence of a multiple system. The peak radial velocities of the H2 knots range
from -42 to -14 km s^-1 in the blue lobe, and from -8 to 47 km s^-1 in the red
lobe. The low resolution spectra are rich in H_2 emission, and relatively faint
[FeII] (NIR), [OI] and [CII] (FIR) emission is observed in the region close to
the source. A warm H2 gas component has an average excitation temperature that
ranges between 2000 K and 2500 K. Additionally, the ISO-SWS spectrum reveals
the presence of a cold component (520 K), that strongly contributes to the
radiative cooling of the flow and plays a major role in the dynamics of the
flow. The estimated L(H2) of the jet is 8.2+/-0.7 L_sun, suggesting that
IRAS20126+4104 has an accretion rate significantly increased compared to
low-mass YSOs. This is also supported by the derived mass flux rate from the H2
lines (Mflux(H2)~7.5x10^-4 M_sun yr^-1). The comparison between the H2 and the
outflow parameters strongly indicates that the jet is driving, at least
partially, the outflow. As already found for low-mass protostellar jets, the
measured H2 outflow luminosity is tightly related to the source bolometric
luminosity.Comment: 16 pages, 12 figures. A&A accepte
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