12 research outputs found
H110alpha recombination-line emission and 4.8-GHz continuum emission in the Carina Nebula
We present results from observations of H110alpha recombination-line emission
at 4.874 GHz and the related 4.8-GHz continuum emission towards the Carina
Nebula using the Australia Telescope Compact Array. These data provide
information on the velocity, morphology and excitation parameters of the
ionized gas associated with the two bright HII regions within the nebula, Car I
and Car II. They are consistent with both Car I and Car II being expanding
ionization fronts arising from the massive star clusters Trumpler 14 and
Trumpler 16, respectively. The overall continuum emission distribution at 4.8
GHz is similar to that at lower frequencies. For Car I, two compact sources are
revealed that are likely to be young HII regions associated with triggered star
formation. These results provide the first evidence of ongoing star formation
in the northern region of the nebula. A close association between Car I and the
molecular gas is consistent with a scenario in which Car I is currently carving
out a cavity within the northern molecular cloud. The complicated kinematics
associated with Car II point to expansion from at least two different centres.
All that is left of the molecular cloud in this region are clumps of dense gas
and dust which are likely to be responsible for shaping the striking morphology
of the Car II components.Comment: 10 pages, 7 figures, accepted for publication in MNRA
The interstellar medium towards the Ara OB1 region
We present high resolution (R ~ 4 km/s) absorption measurements of the
interstellar NaI and CaII lines measured towards 14 early-type stars of
distance 123 pc - 1650 pc, located in the direction of the Ara OB1 stellar
cluster. The line profiles can broadly be split into four distinct groupings of
absorption component velocity, and we have attempted to identify an origin and
distance to each of these interstellar features. For gas with absorption
covering the velocity range -10 km/s < V_helio < +10 km/s, we can identify the
absorbing medium with local gas belonging to the Lupus-Norma interstellar
cavity located between 100 and 485 pc in this galactic direction. Gas with
velocities spanning the range -20 km/s < V_helio < +20 km/s is detected towards
stars with distances of 570-800 pc. We identify a wide-spread interstellar
feature at V_helio ~ -15 km/s with the expanding HI shell called GSH 337+00-05,
which is now placed at a distance of ~530 pc.Comment: 12 pages, 5 figures, accepted for publication in Astrophysics & Space
Scienc
Star Formation and Dynamics in the Galactic Centre
The centre of our Galaxy is one of the most studied and yet enigmatic places
in the Universe. At a distance of about 8 kpc from our Sun, the Galactic centre
(GC) is the ideal environment to study the extreme processes that take place in
the vicinity of a supermassive black hole (SMBH). Despite the hostile
environment, several tens of early-type stars populate the central parsec of
our Galaxy. A fraction of them lie in a thin ring with mild eccentricity and
inner radius ~0.04 pc, while the S-stars, i.e. the ~30 stars closest to the
SMBH (<0.04 pc), have randomly oriented and highly eccentric orbits. The
formation of such early-type stars has been a puzzle for a long time: molecular
clouds should be tidally disrupted by the SMBH before they can fragment into
stars. We review the main scenarios proposed to explain the formation and the
dynamical evolution of the early-type stars in the GC. In particular, we
discuss the most popular in situ scenarios (accretion disc fragmentation and
molecular cloud disruption) and migration scenarios (star cluster inspiral and
Hills mechanism). We focus on the most pressing challenges that must be faced
to shed light on the process of star formation in the vicinity of a SMBH.Comment: 68 pages, 35 figures; invited review chapter, to be published in
expanded form in Haardt, F., Gorini, V., Moschella, U. and Treves, A.,
'Astrophysical Black Holes'. Lecture Notes in Physics. Springer 201
Molecular abundances in the Magellanic Clouds .2. Deuterated species in the LMC
The first definite discoveries of extragalactic deuterium are reported. DCO^+ has been detected in three and DCN has been measured in one star-forming region of the Large Magellanic Cloud (LMC). While the HCO^+/DCO^+ abundance ratios are found to be 19 \pm 3, 24 \pm 4 and 67 \pm 18 for N113, N44BC and N159HW, respectively, a HCN/DCN abundance ratio of 23 \pm 5 is obtained for N113. These results are consistent with a gas temperature of about 20\,K and a D/H ratio of about 1.5 \times 10^{-5}, consistent with that observed in the Galaxy. If the cloud temperature is closer to 30\,K, then a D/H ratio is required to be up to an order of magnitude larger. Because this ratio provides a lower limit to the primordial D/H ratio, it indicates that the baryon mass density alone is unable to close the universe
Molecular abundances in the magellanic clouds III. LIRS 36, a star-forming region in the Small Magellanic Cloud
Molecular abundances in the magellanic clouds .1. A multiline study of five cloud cores
Nine HII regions of the LMC were mapped in 13CO(1--0) and three in 12CO(1--0) to study the physical properties of the interstellar medium in the Magellanic Clouds. For N113 the molecular core is found to have a peak position which differs from that of the associated HII region by 20 arcsec. Toward this molecular core the 12CO and 13CO peak Tmb line temperatures of 7.3\,K and 1.2\,K are the highest so far found in the Magellanic Clouds. The molecular concentrations associated with N113, N44BC, N159HW, and N214DE in the LMC and LIRS\,36 in the SMC were investigated in a variety of molecular species to study the chemical properties of the interstellar medium. I(HCO+)/I(HCN) and I(HCN)/I(HNC) intensity ratios as well as lower limits to the I(13CO)/I(C18O) ratio were derived for the rotational 1--0 transitions. Generally, HCO+ is stronger than HCN, and HCN is stronger than HNC. The high relative HCO+ intensities are consistent with a high ionization flux from supernovae remnants and young stars, possibly coupled with a large extent of the HCO+ emission region. The bulk of the HCN arises from relatively compact dense cloud cores. Warm or shocked gas enhances HCN relative to HNC. From chemical model calculations it is predicted that I(HCN)/I(HNC) close to one should be obtained with higher angular resolution (> 30 arcsec) toward the cloud cores. Comparing virial masses with those obtained from the integrated CO intensity provides an H2 mass-to-CO luminosity conversion factor of 1.8 \times 10^{20}\,mol\,cm^{-2}\,(Kkms)^{-1} for N113 and 2.4 \times 10^{20}\,mol\,cm^{-2}\,(Kkms)^{-1} for N44BC. This is consistent with values derived for the Galactic disk
High-resolution ammonia mapping of the very young protostellar core Chamaeleon-MMS1
VK: resolve; Karhunen, J.; ReSoLVEAims. The aim of this study is to investigate the structure and kinematics of the nearby candidate first hydrostatic core Cha-MMS1. Methods. Cha-MMS1 was mapped in the NH3(1,1) line and the 1.2 cm continuum using the Australia Telescope Compact Array (ATCA). The angular resolution of the ATCA observations is 7″ (~1000 AU), and the velocity resolution is 50 m s-1. The core was also mapped with the 64 m Parkes Telescope in the NH3(1,1) and (2,2) lines. Observations from Herschel Space Observatory and Spitzer Space Telescope were used to help interpretation. The ammonia spectra were analysed using Gaussian fits to the hyperfine structure. A two-layer model was applied in the central parts of the core where the ATCA spectra show signs of self-absorption. Results. A compact high column density core with a steep velocity gradient (~20 km s-1 pc-1) is detected in ammonia. We derive a high gas density (~106 cm-3) in this region, and a fractional ammonia abundance compatible with determinations towards other dense cores (~10-8). This suggests that the age of the high density core is comparable to the freeze-out timescale of ammonia in these conditions, on the order of 104 years. The direction of the velocity gradient agrees with previous single-dish observations, and the overall velocity distribution can be interpreted as rotation. The rotation axis goes through the position of a compact far-infrared source detected by Spitzer and Herschel. The specific angular momentum of the core, ~10-3km s-1 pc, is typical for protostellar envelopes. A string of 1.2 cm continuum sources is tentatively detected near the rotation axis. The ammonia spectra suggest the presence of warm embedded gas in its vicinity. An hourglass-shaped structure is seen in ammonia at the cloud’s average LSR velocity, also aligned with the rotation axis. Although this structure resembles a pair of outflow lobes the ammonia spectra show no indications of shocked gas. Conclusions. The observed ammonia structure mainly delineates the inner envelope around the central source. The velocity gradient is likely to originate in the angular momentum of the contracting core, although influence of the outflow from the neighbouring young star IRS4 is possibly visible on one side of the core. The tentative continuum detection and the indications of a warm background component near the rotation axis suggest that the core contains a deeply embedded outflow which may have been missed in previous single-dish CO surveys owing to beam dilution.Peer reviewe