374 research outputs found
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
Broadband VLA Spectral Line Survey of a Sample of Ionized Jet Candidates
The study of the interaction between ionized jets, molecular outflows and
their environments is critical to understanding high-mass star formation,
especially because jets and outflows are thought to be key in the transfer of
angular momentum outwards from accretion disks. We report a low-spectral
resolution VLA survey for hydrogen radio recombination lines, OH, NH, and
CHOH lines toward a sample of 58 high-mass star forming regions that
contain numerous ionized jet candidates. The observations are from a survey
designed to detect radio continuum; the novel aspect of this work is to search
for spectral lines in broadband VLA data (we provide the script developed in
this work to facilitate exploration of other datasets). We report detection of
25GHz CHOH transitions toward ten sources; five of them also show
NH emission. We found that most of the sources detected in CHOH and
NH have been classified as ionized jets or jet candidates and that the
emission lines are coincident with, or very near ( pc) these
sources, hence, these molecular lines could be used as probes of the
environment near the launching site of jets/outflows. No radio recombination
lines were detected, but we found that the RMS noise of stacked spectra
decreases following the radiometer equation. Therefore, detecting radio
recombination lines in a sample of brighter free-free continuum sources should
be possible. This work demonstrates the potential of broadband VLA continuum
observations as low-resolution spectral line scans.Comment: 38 pages, 19 figures. Accepted for publication in The Astrophysical
Journal Supplement Serie
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
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
Excited Hydroxyl Outflow in the High-Mass Star-Forming Region G34.26+0.15
G34.26+0.15 is a region of high-mass star formation that contains a broad
range of young stellar objects in different stages of evolution, including a
hot molecular core, hyper-compact HII regions and a prototypical cometary
ultra-compact HII region. Previous high-sensitivity single dish observations by
our group resulted in the detection of broad 6035 MHz OH absorption in this
region; the line showed a significant blue-shifted asymmetry indicative of
molecular gas expansion. We present high-sensitivity Karl G. Jansky Very Large
Array (VLA) observations of the 6035 MHz OH line conducted to image the
absorption and investigate its origin with respect to the different star
formation sites in the region. In addition, we report detection of 6030 MHz OH
absorption with the VLA and further observations of 4.7 GHz and 6.0 GHz OH
lines obtained with the Arecibo Telescope. The 6030 MHz OH line shows a very
similar absorption profile as the 6035 MHz OH line. We found that the 6035 MHz
OH line absorption region is spatially unresolved at " scales, and it
is coincident with one of the bright ionized cores of the cometary HII region
that shows broad radio recombination line emission. We discuss a scenario where
the OH absorption is tracing the remnants of a pole-on molecular outflow that
is being ionized inside-out by the ultra-compact HII region.Comment: 19 pages, 6 figures. Accepted for publication in The Astrophysical
Journa
High Resolution, Wide Field, Narrow Band, Snapshot Imaging
We investigate the imaging performance of an interferometric array in the case of wide field, high resolution, narrow band, snapshot imaging. We find that, when uv-cell sizes are sufficiently small (ie. image sizes are sufficiently large), each instantaneous visibility record is gridded into its own uv-cell. This holds even for dense arrays, like the core of the next generation VLA. In this particular, application, Uniform weighting of the gridded visibilities approaches Natural weighting, with its often deleterious consequences on the resulting synthesized beam. For a core-dominated array, we show that the resulting image noise is highly correlated on scales comparable to the spatial frequencies of the core baselines. In general, this study accentuates the fact that, for imaging applications that require high resolution (Plains array and greater), many of the core antennas can be employed as a separate subarray for low resolution science, without sacrificing the quality of the high resolution science
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