884 research outputs found
Massive envelopes and filaments in the NGC 3603 star forming region
The formation of massive stars and their arrival on the zero-age
main-sequence occurs hidden behind dense clouds of gas and dust. In the giant
Hii region NGC 3603, the radiation of a young cluster of OB stars has dispersed
dust and gas in its vicinity. At a projected distance of 2:5 pc from the
cluster, a bright mid-infrared (mid-IR) source (IRS 9A) had been identified as
a massive young stellar object (MYSO), located on the side of a molecular clump
(MM2) of gas facing the cluster. We investigated the physical conditions in
MM2, based on APEX sub-mm observations using the SABOCA and SHFI instruments,
and archival ATCA 3 mm continuum and CS spectral line data. We resolved MM2
into several compact cores, one of them closely associated with IRS 9A. These
are likely infrared dark clouds as they do not show the typical hot-core
emission lines and are mostly opaque against the mid-IR background. The compact
cores have masses of up to several hundred times the solar mass and gas
temperatures of about 50 K, without evidence of internal ionizing sources. We
speculate that IRS 9A is younger than the cluster stars, but is in an
evolutionary state after that of the compact cores
Unveiling the near-infrared structure of the massive-young stellar object NGC 3603 IRS 9A with sparse aperture masking and spectroastrometry
Contemporary theory holds that massive stars gather mass during their initial
phases via accreting disk-like structures. However, conclusive evidence for
disks has remained elusive for the most massive young objects. This is mainly
due to significant observational challenges. Incisive studies, even targeting
individual objects, are therefore relevant to the progression of the field. NGC
3603 IRS 9A* is a young massive stellar object still surrounded by an envelope
of molecular gas. Previous mid-infrared observations with long-baseline
interferometry provided evidence for a disk of 50 mas diameter at its core.
This work aims at a comprehensive study of the physics and morphology of IRS 9A
at near-infrared wavelengths. New sparse aperture masking interferometry data
taken with NACO/VLT at Ks and Lp filters were obtained and analysed together
with archival CRIRES spectra of the H2 and BrG lines. The calibrated
visibilities recorded at Ks and Lp bands suggest the presence of a partially
resolved compact object of 30 mas at the core of IRS 9A, together with the
presence of over-resolved flux. The spectroastrometric signal of the H2 line
shows that this spectral feature proceeds from the large scale extended
emission (300 mas) of IRS 9A, while the BrG line appears to be formed at the
core of the object (20 mas). This scenario is consistent with the brightness
distribution of the source for near- and mid-infrared wavelengths at various
spatial scales. However, our model suffers from remaining inconsistencies
between SED modelling and the interferometric data. Moreover, the BrG
spectroastrometric signal indicates that the core of IRS 9A exhibits some form
of complexity such as asymmetries in the disk. Future high-resolution
observations are required to confirm the disk/envelope model and to flesh out
the details of the physical form of the inner regions of IRS 9A.Comment: Accepted to be published in Astronomy & Astrophysics, 13 pages, 14
figure
Highly Collimated Jets and Wide-Angle Outflows in HH46/47: New Evidence from Spitzer IR Images
We present new details of the structure and morphology of the jets and
outflows in HH46/47 as seen in Spitzer infrared images from IRAC and MIPS,
reprocessed using the ``HiRes'' deconvolution technique. HiRes improves the
visualization of spatial morphology by enhancing resolution (to sub-arcsec
levels in IRAC bands) and removing the contaminating side lobes from bright
sources. In addition to sharper views of previously reported bow shocks, we
have detected: (i) the sharply-delineated cavity walls of the wide-angle
biconical outflow, seen in scattered light on both sides of the protostar, (ii)
several very narrow jet features at distances 400 AU to 0.1 pc from the star,
and, (iii) compact emissions at MIPS 24 micron coincident with the jet heads,
tracing the hottest atomic/ionic gas in the bow shocks.Comment: 11 pages, 4 Figures, Accepted for publication in ApJ(Letters
GRACE AND LEGALISM IN THE PAULINE WRITINGS
Therefore, our procedure will be to examine the various Pauline writings to determine Paul\u27s advocacy of grace and the implications of this in three areas. We will introduce our study with an examination of the background for the problem of Jewish legalism in the early church. This will include a brief appraisal of the constituency of the early church, expansion to the Gentiles, Paul\u27s missionary labors and resultant opposition from the Judaistic party, and a brief preliminary view of Paul\u27s effort to deal with this problem
A mid-IR survey of the L 1641-N region with ISOCAM
We present an analysis of the L 1641 outflow region using broad-band and
narrow-band imaging data at mid-infrared wavelengths from ISOCAM. We detect a
total of 34 sources in the x region covered by
the broad-band filters. Four of these sources have no reported detection in
previous studies of the region. We find that the source previously identified
as the near-IR counter-part to the IRAS detected point-source (IRAS 05338-0624)
is not the brightest source in the wavelength region of the IRAS 12 \micron\
filter. We find instead that a nearby object (within the beam of IRAS and not
detected at near-IR wavelengths) outshines all others sources in the area by a
factor of 2. We submit that this source is likely to be the IRAS detected
point source. A comparison of the near-IR (J-H vs H-K) and mid-IR (J-K vs [6.7
um]-[14 um]) color-color plots shows only four sources with excess emission at
near-IR wavelengths, but atleast 85% of all sources show excess emission at
mid-IR wavelengths. The CVF spectra suggest a range of evolutionary status in
the program stars ranging from embedded YSOs to the young disks. When combined
with optical and near-IR age estimates, these results show active current
star-formation in the region that has been on-going for at least 2 Myr.Comment: Submitted to ApJ. Abstracted edited for arXiv submission Replaced by
version accepted by Ap
The thermal state of molecular clouds in the Galactic Center: evidence for non-photon-driven heating
We used the Atacama Pathfinder Experiment (APEX) 12 m telescope to observe
the J_KaKc=3_03-2_02, 3_22-2_21, and 3_21-2_20 transitions of para-H_2CO at 218
GHz simultaneously to determine kinetic temperatures of the dense gas in the
central molecular zone (CMZ) of our Galaxy. The map extends over approximately
40 arcmin x 8 arcmin (~100x20 pc^2) along the Galactic plane with a linear
resolution of 1.2 pc. The strongest of the three lines, the H_2CO (3_03-2_02)
transition, is found to be widespread, and its emission shows a spatial
distribution similar to ammonia. The relative abundance of para-H_2CO is
0.5-1.2 10^{-9}, which is consistent with results from lower frequency H_2CO
absorption lines. Derived gas kinetic temperatures for individual molecular
clouds range from 50 K to values in excess of 100 K. While a systematic trend
toward (decreasing) kinetic temperature versus (increasing) angular distance
from the Galactic center (GC) is not found, the clouds with highest temperature
(T_kin > 100 K) are all located near the nucleus. For the molecular gas outside
the dense clouds, the average kinetic temperature is 65+/-10 K. The high
temperatures of molecular clouds on large scales in the GC region may be driven
by turbulent energy dissipation and/or cosmic-rays instead of photons. Such a
non-photon-driven thermal state of the molecular gas provides an excellent
template for the more distant vigorous starbursts found in ultraluminous
infrared galaxies (ULIRGs).Comment: 23 pages, 11 figures, A&A in pres
Herschel/PACS Imaging of Protostars in the HH 1-2 Outflow Complex
We present 70 and 160 micron Herschel science demonstration images of a field
in the Orion A molecular cloud that contains the prototypical Herbig-Haro
objects HH 1 and 2, obtained with the Photodetector Array Camera and
Spectrometer (PACS). These observations demonstrate Herschel's unprecedented
ability to study the rich population of protostars in the Orion molecular
clouds at the wavelengths where they emit most of their luminosity. The four
protostars previously identified by Spitzer 3.6-40 micron imaging and
spectroscopy are detected in the 70 micron band, and three are clearly detected
at 160 microns. We measure photometry of the protostars in the PACS bands and
assemble their spectral energy distributions (SEDs) from 1 to 870 microns with
these data, Spitzer spectra and photometry, 2MASS data, and APEX sub-mm data.
The SEDs are fit to models generated with radiative transfer codes. From these
fits we can constrain the fundamental properties of the protostars. We find
luminosities in the range 12-84 L_sun and envelope densities spanning over two
orders of magnitude. This implies that the four protostars have a wide range of
envelope infall rates and evolutionary states: two have dense, infalling
envelopes, while the other two have only residual envelopes. We also show the
highly irregular and filamentary structure of the cold dust and gas surrounding
the protostars as traced at 160 microns.Comment: 6 pages, 4 figures, accepted for publication in the A&A Herschel
special issu
Rate coefficients for rovibrational transitions in H_2 due to collisions with He
We present quantum mechanical and quasiclassical trajectory calculations of
cross sections for rovibrational transitions in ortho- and para-H_2 induced by
collisions with He atoms. Cross sections were obtained for kinetic energies
between 10^-4 and 3 eV, and the corresponding rate coefficients were calculated
for the temperature range 100<T<4000 K. Comparisons are made with previous
calculations.Comment: 21 pages, 2 figures, AAS, eps
Chemistry of dense clumps near moving Herbig-Haro objects
Localised regions of enhanced emission from HCO+, NH3 and other species near
Herbig-Haro objects (HHOs) have been interpreted as arising in a photochemistry
stimulated by the HHO radiation on high density quiescent clumps in molecular
clouds. Static models of this process have been successful in accounting for
the variety of molecular species arising ahead of the jet; however recent
observations show that the enhanced molecular emission is widespread along the
jet as well as ahead. Hence, a realistic model must take into account the
movement of the radiation field past the clump. It was previously unclear as to
whether the short interaction time between the clump and the HHO in a moving
source model would allow molecules such as HCO+ to reach high enough levels,
and to survive for long enough to be observed. In this work we model a moving
radiation source that approaches and passes a clump. The chemical picture is
qualitatively unchanged by the addition of the moving source, strengthening the
idea that enhancements are due to evaporation of molecules from dust grains. In
addition, in the case of several molecules, the enhanced emission regions are
longer-lived. Some photochemically-induced species, including methanol, are
expected to maintain high abundances for ~10,000 years.Comment: 7 pages, 3 figure
Hier ist wahrhaftig ein Loch im Himmel - The NGC 1999 dark globule is not a globule
The NGC 1999 reflection nebula features a dark patch with a size of ~10,000
AU, which has been interpreted as a small, dense foreground globule and
possible site of imminent star formation. We present Herschel PACS far-infrared
70 and 160mum maps, which reveal a flux deficit at the location of the globule.
We estimate the globule mass needed to produce such an absorption feature to be
a few tenths to a few Msun. Inspired by this Herschel observation, we obtained
APEX LABOCA and SABOCA submillimeter continuum maps, and Magellan PANIC
near-infrared images of the region. We do not detect a submillimer source at
the location of the Herschel flux decrement; furthermore our observations place
an upper limit on the mass of the globule of ~2.4x10^-2 Msun. Indeed, the
submillimeter maps appear to show a flux depression as well. Furthermore, the
near-infrared images detect faint background stars that are less affected by
extinction inside the dark patch than in its surroundings. We suggest that the
dark patch is in fact a hole or cavity in the material producing the NGC 1999
reflection nebula, excavated by protostellar jets from the V 380 Ori multiple
system.Comment: accepted for the A&A Herschel issue; 7 page
- âŠ