839 research outputs found
A Search for 6.7 GHz Methanol Masers in M33
We report the negative results from a search for 6.7 GHz methanol masers in
the nearby spiral galaxy M33. We observed 14 GMCs in the central 4 kpc of the
Galaxy, and found 3 sigma upper limits to the flux density of ~9 mJy in
spectral channels having a velocity width of 0.069 km/s. By velocity shifting
and combining the spectra from the positions observed, we obtain an effective
3sigma upper limit on the average emission of ~1mJy in a 0.25 km/s channel.
These limits lie significantly below what we would expect based on our
estimates of the methanol maser luminosity function in the Milky Way. The most
likely explanation for the absence of detectable methanol masers appears to be
the metallicity of M33, which is modestly less than that of the Milky Way
Casimir-Polder interaction of fullerene molecules with surfaces
We calculate the thermal Casimir--Polder potential of C60 and C70 fullerene
molecules near gold and silicon nitride surfaces, motivated by their relevance
for molecular matter wave interference experiments. We obtain the coefficients
governing the asymptotic power laws of the interaction in the thermal, retarded
and nonretarded distance regimes and evaluate the full potential numerically.
The interaction is found to be dominated by electronic transitions, and hence
independent of the internal temperature of the molecules. The contributions
from phonon transitions, which are affected by the molecular temperature, give
rise to only a small correction. Moreover, we find that the sizeable molecular
line widths of thermal fullerenes may modify the nonretarded interaction,
depending on the model used. Detailed measurements of the nonretarded potential
of fullerene thus allow one to distinguish between different theories of
incorporating damping.Comment: 9 pages, 8 figures, 9 table
Scintillation in the Circinus Galaxy water megamasers
We present observations of the 22 GHz water vapor megamasers in the Circinus
galaxy made with the Tidbinbilla 70m telescope. These observations confirm the
rapid variability seen earlier by Greenhill et al (1997). We show that this
rapid variability can be explained by interstellar scintillation, based on what
is now known of the interstellar scintillation seen in a significant number of
flat spectrum AGN. The observed variability cannot be fully described by a
simple model of either weak or diffractive scintillation.Comment: 10 pages, 5 figures. AJ accepte
A bilateral shear layer between two parallel Couette flows
We consider a shear layer of a kind not previously studied to our knowledge.
Contrary to the classical free shear layer, the width of the shear zone does
not vary in the streamwise direction but rather exhibits a lateral variation.
Based on some simplifying assumptions, an analytic solution has been derived
for the new shear layer. These assumptions have been justified by a comparison
with numerical solutions of the full Navier-Stokes equations, which accord with
the analytical solution to better than 1% in the entire domain. An explicit
formula is found for the width of the shear zone as a function of wall-normal
coordinate. This width is independent of wall velocities in the laminar regime.
Preliminary results for a co-current laminar-turbulent shear layer in the same
geometry are also presented. Shear-layer instabilities were then developed and
resulted in an unsteady mixing zone at the interface between the two co-current
streams.Comment: 6 pages, 7 figures. Accepted for publication in Phys. Rev.
The Arecibo Methanol Maser Galactic Plane Survey - III: Distances and Luminosities
We derive kinematic distances to the 86 6.7 GHz methanol masers discovered in
the Arecibo Methanol Maser Galactic Plane Survey. The systemic velocities of
the sources were derived from 13CO (J=2-1), CS (J=5-4), and NH3 observations
made with the ARO Submillimeter Telescope, the APEX telescope, and the
Effelsberg 100 m telescope, respectively. Kinematic distance ambiguities were
resolved using HI self-absorption with HI data from the VLA Galactic Plane
Survey. We observe roughly three times as many sources at the far distance
compared to the near distance. The vertical distribution of the sources has a
scale height of ~ 30 pc, and is much lower than that of the Galactic thin disk.
We use the distances derived in this work to determine the luminosity function
of 6.7 GHz maser emission. The luminosity function has a peak at approximately
10^{-6} L_sun. Assuming that this luminosity function applies, the methanol
maser population in the Large Magellanic Cloud and M33 is at least 4 and 14
times smaller, respectively, than in our Galaxy.Comment: Accepted by Ap
Weak and Compact Radio Emission in Early High-Mass Star Forming Regions: I. VLA Observations
We present a high sensitivity radio continuum survey at 6 and 1.3cm using
the Karl G. Jansky Very Large Array towards a sample of 58 high-mass star
forming regions. Our sample was chosen from dust clumps within infrared dark
clouds with and without IR sources (CMC-IRs, CMCs, respectively), and hot
molecular cores (HMCs), with no previous, or relatively weak radio continuum
detection at the mJy level. Due to the improvement in the continuum
sensitivity of the VLA, this survey achieved map rms levels of 3-10
Jy beam at sub-arcsecond angular resolution. We extracted 70
centimeter continuum sources associated with 1.2mm dust clumps. Most
sources are weak, compact, and are prime candidates for high-mass protostars.
Detection rates of radio sources associated with the mm dust clumps for CMCs,
CMC-IRs and HMCs are 6, 53 and 100, respectively. This result is
consistent with increasing high-mass star formation activity from CMCs to HMCs.
The radio sources located within HMCs and CMC-IRs occur close to the dust clump
centers with a median offset from it of 12,000AU and 4,000AU,
respectively. We calculated 5 - 25GHz spectral indices using power law fits
and obtain a median value of 0.5 (i.e., flux increasing with frequency),
suggestive of thermal emission from ionized jets. In this paper we describe the
sample, observations, and detections. The analysis and discussion will be
presented in Paper II.Comment: Accepted for publication in the ApJ
Weak and Compact Radio Emission in Early High-Mass Star Forming Regions: II. The Nature of the Radio Sources
In this study we analyze 70 radio continuum sources associated with dust
clumps and considered to be candidates for the earliest stages of high-mass
star formation. The detection of these sources was reported by Rosero et al.
(2016), who found most of them to show weak (1 mJy) and
compact (0.6) radio emission. Herein, we
used the observed parameters of these sources to investigate the origin of the
radio continuum emission. We found that at least of these radio
detections are most likely ionized jets associated with high-mass protostars,
but for the most compact sources we cannot discard the scenario that they
represent pressure-confined HII regions. This result is highly relevant for
recent theoretical models based on core accretion that predict the first stages
of ionization from high-mass stars to be in the form of jets. Additionally, we
found that properties such as the radio luminosity as a function of the
bolometric luminosity of ionized jets from low and high-mass stars are
extremely well-correlated. Our data improve upon previous studies by providing
further evidence of a common origin for jets independently of luminosity.Comment: Accepted for publication in the Ap
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Only poster shown, no paper in the proceedings.
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Accurate OH maser positions II. the Galactic Center region
We present high spatial resolution observations of ground-state OH masers,
achieved using the Australia Telescope Compact Array (ATCA). These observations
were conducted towards 171 pointing centres, where OH maser candidates were
identified previously in the Southern Parkes Large-Area Survey in Hydroxyl
(SPLASH) towards the Galactic Center region, between Galactic longitudes of
and and Galactic latitudes of and
. We detect maser emission towards 162 target fields and suggest
that 6 out of 9 non-detections are due to intrinsic variability. Due to the
superior spatial resolution of the follow-up ATCA observations, we have
identified 356 OH maser sites in the 162 of the target fields with maser
detections. Almost half (161 of 356) of these maser sites have been detected
for the first time in these observations. After comparing the positions of
these 356 maser sites to the literature, we find that 269 (76\%) sites are
associated with evolved stars (two of which are planetary nebulae), 31 (9\%)
are associated with star formation, four are associated with supernova remnants
and we were unable to determine the origin of the remaining 52 (15\%) sites.
Unlike the pilot region (\citealt{Qie2016a}), the infrared colors of evolved
star sites with symmetric maser profiles in the 1612 MHz transition do not show
obvious differences compared with those of evolved star sites with asymmetric
maser profiles.Comment: 24 pages, 12 figures, accepted by ApJ
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