499 research outputs found
Linear dust polarization during the embedded phase of protostar formation
Measuring polarization from thermal dust emission can provide constraints on
the magnetic field structure around embedded protostars. However, interpreting
the observations is challenging without models that consistently account for
both the complexity of the protostellar birth environment and polarization
mechanisms. We aim to provide a better understanding with a focus on
bridge-like structures such as that observed towards the protostellar multiple
IRAS 16293--2422 by comparing synthetic polarization maps of thermal reemission
with observations. We analyze the magnetic field properties associated with the
formation of a protostellar multiple based on ideal MHD 3D zoom-in simulations
carried out with the RAMSES code. To compare with observations, we post-process
a snapshot of a bridge-like structure that is associated with a forming triple
star system with the radiative transfer code POLARIS and produce
multi-wavelength dust polarization maps. In the most prominent bridge of our
sample, the typical density is about 10^(-16) g cm^(-3), and the magnetic field
strength is about 1 to 2 mG. The magnetic field structure has an elongated
toroidal morphology and the dust polarization maps trace the complex
morphology. In contrast, the magnetic field strength associated with the
launching of asymmetric bipolar outflows is significantly more magnetized (~100
mG). At {\lambda}=1.3 mm, the orientation of grains in the bridge is similar
for the case accounting for radiative alignment torques (RATs) compared to
perfect alignment with magnetic field lines. However, the polarization fraction
in the bridge is three times smaller for the RAT scenario compared to assuming
perfect alignment. At shorter wavelengths ({\lambda} < 200 {\mu}m), dust
polarization does not trace the magnetic field because other effects such as
self-scattering and dichroic extinction dominate the orientation of the
polarization.Comment: 18 pages, 12 figures plus 3 figures in the appendix, accepted for
publication in A&
Laboratory Characterization and Astrophysical Detection of Vibrationally Excited States of Vinyl Cyanide in Orion-KL
New laboratory data of CHCHCN (vinyl cyanide) in its ground and
vibrationally excited states at the microwave to THz domain allow searching for
these excited state transitions in the Orion-KL line survey.
Frequency-modulated spectrometers combined into a single broadband 50-1900 GHz
spectrum provided measurements of CHCHCN covering a spectral range of
18-1893 GHz, whose assignments was confirmed by Stark modulation spectra in the
18-40 GHz region and by ab-initio anharmonic force field calculations. For
analyzing the emission lines of CHCHCN species detected in Orion-KL we used
the excitation and radiative transfer code (MADEX) at LTE conditions. The
rotational transitions of the ground state of this molecule emerge from four
cloud components of hot core nature which trace the physical and chemical
conditions of high mass star forming regions in the Orion-KL Nebula. The total
column density of CHCHCN in the ground state is (3.00.9)x10
cm. We report on the first interstellar detection of transitions in the
v10=1/(v11=1,v15=1) dyad in space, and in the v11=2 and v11=3 states in
Orion-KL. The lowest energy vibrationally excited states of vinyl cyanide such
as v11=1 (at 328.5 K), v15=1 (at 478.6 K), v11=2 (at 657.8 K), the
v10=1/(v11=1,v15=1) dyad (at 806.4/809.9 K), and v11=3 (at 987.9 K) are
populated under warm and dense conditions, so they probe the hottest parts of
the Orion-KL source. Column density and rotational and vibrational temperatures
for CHCHCN in their ground and excited states, as well as for the
isotopologues, have been constrained by means of a sample of more than 1000
lines in this survey. Moreover, we present the detection of methyl isocyanide
(CHNC) for the first time in Orion-KL and a tentative detection of vinyl
isocyanide (CHCHNC) and give column density ratios between the cyanide and
isocyanide isomers.Comment: 46 pages, 22 figures, 14 tables, 9 online table
Episodic infall towards a compact disk in B335?
Previous observations of B335 have presented evidence of ongoing infall in
various molecular lines, e.g., HCO, HCN, CO. There have been no confirmed
observations of a rotationally supported disk on scales greater than ~12~au.
The presence of an outflow in B335 suggests that also a disk should be present
or in formation. To constrain the earliest stages of protostellar evolution and
disk formation, we aim to map the region where gas falls inwards and
observationally constrain its kinematics. Furthermore, we aim to put strong
limits on the size and orientation of any disk-like structure in B335. We use
high angular resolution CO data from ALMA, and combine it with
shorter-baseline archival data to produce a high-fidelity image of the infall
in B335. We also revisit the imaging of high-angular resolution Band 6
continuum data to study the dust distribution in the immediate vicinity of
B335. Continuum emission shows an elliptical structure (10 by 7 au) with a
position angle 5 degrees east of north, consistent with the expectation for a
forming disk in B335. A map of the infall velocity (as estimated from the
CO emission), shows evidence of asymmetric infall, predominantly from
the north and south. Close to the protostar, infall velocities appear to exceed
free-fall velocities. 3D radiative transfer models, where the infall velocity
is allowed to vary within the infall region, can explain the observed
kinematics. The data suggests that a disk has started to form in B335 and that
gas is falling towards that disk. However, kinematically-resolved line data
towards the disk itself is needed to confirm the presence of a rotationally
supported disk around this young protostar. The measured high infall velocities
are not easily reconcilable with a magnetic braking scenario and suggest that
there is a pressure gradient that allows the infall velocity to vary in the
region.Comment: 14 pages, 11 figure
The ALMA-PILS survey: complex nitriles towards IRAS 16293-2422
Context. Complex organic molecules are readily detected in the inner regions of the gaseous envelopes of forming protostars. Their detection is crucial to understanding the chemical evolution of the Universe and exploring the link between the early stages of star formation and the formation of solar system bodies, where complex organic molecules have been found in abundance. In particular, molecules that contain nitrogen are interesting due to the role nitrogen plays in the development of life and the compact scales such molecules have been found to trace around forming protostars. Aims. The goal of this work is to determine the inventory of one family of nitrogen-bearing organic molecules, complex nitriles (molecules with a -C N functional group) towards two hot corino sources in the low-mass protostellar binary IRAS 16293-2422. This work explores the abundance differences between the two sources, the isotopic ratios, and the spatial extent derived from molecules containing the nitrile functional group. Methods. Using data from the Protostellar Interferometric Line Survey (PILS) obtained with ALMA, we determine abundances and excitation temperatures for the detected nitriles. We also present a new method for determining the spatial structure of sources with high line density and large velocity gradients-Velocity-corrected INtegrated emission (VINE) maps. Results. We detect methyl cyanide (CH3CN) as well as five of its isotopologues, including CHD2CN, which is the first detection in the interstellar medium (ISM). We also detect ethyl cyanide (C2H5CN), vinyl cyanide (C2H3CN), and cyanoacetylene (HC3N). We find that abundances are similar between IRAS 16293A and IRAS 16293B on small scales except for vinyl cyanide which is only detected towards the latter source. This suggests an important difference between the sources either in their evolutionary stage or warm-up timescales. We also detect a spatially double-peaked emission for the first time in molecular emission in the A source, suggesting that this source is showing structure related to a rotating toroid of material. Conclusions. With high-resolution observations, we have been able to show for the first time a number of important similarities and differences in the nitrile chemistry in these objects. These illustrate the utility of nitriles as potential tracers of the physical conditions in star-forming regions
The ALMA Protostellar Interferometric Line Survey (PILS): First results from an unbiased submillimeter wavelength line survey of the Class 0 protostellar binary IRAS 16293-2422 with ALMA
The inner regions of the envelopes surrounding young protostars are characterised by a complex chemistry, with prebiotic molecules present on the scales where protoplanetary disks eventually may form. This paper introduces a systematic survey, "Protostellar Interferometric Line Survey (PILS)" of the Class 0 protostellar binary IRAS 16293-2422 using the Atacama Large Millimeter/submillimeter Array (ALMA). The survey covers the full frequency range from 329 to 363 GHz (0.8 mm) with additional targeted observations at 3.0 and 1.3 mm. More than 10,000 features are detected toward one component in the protostellar binary. Glycolaldehyde, its isomers, methyl formate and acetic acid, and its reduced alcohol, ethylene glycol, are clearly detected. For ethylene glycol both lowest state conformers, aGg' and gGg', are detected, the latter for the first time in the ISM. The abundance of glycolaldehyde is comparable to or slightly larger than that of ethylene glycol. In comparison to the Galactic Center, these two species are over-abundant relative to methanol, possibly an indication of formation at low temperatures in CO-rich ices. Both 13C and deuterated isotopologues of glycolaldehyde are detected, also for the first time ever in the ISM. For the deuterated species, a D/H ratio of approximately 5% is found with no differences between the deuteration in the different functional groups of glycolaldehyde. Measurements of the 13C-species lead to a 12C:13C ratio of approximately 30, lower than the typical ISM value. This low ratio may reflect an enhancement of 13CO in the ice due to either ion-molecule reactions in the gas before freeze-out or differences in the temperatures where 12CO and 13CO ices sublimate. The results reinforce the importance of low-temperature grain surface chemistry for the formation of prebiotic molecules seen here in the gas after sublimation of the entire ice mantle
The ALMA-PILS survey: gas dynamics in IRAS 16293-2422 and the connection between its two protostars
Context. The majority of stars form in binary or higher order systems. The evolution of each protostar in a multiple system may start at different times and may progress differently. The Class 0 protostellar system IRAS 16293-2422 contains two protostars, "A" and "B", separated by similar to 600 au and embedded in a single, 10(4) au scale envelope. Their relative evolutionary stages have been debated. Aims. We aim to study the relation and interplay between the two protostars A and B at spatial scales of 60 au up to similar to 10(3) au. Methods. We selected molecular gas line transitions of the species CO, H2CO, HCN, CS, SiO, and C2H from the ALMA-PILS spectral imaging survey (329-363 GHz) and used them as tracers of kinematics, density, and temperature in the IRAS 16293-2422 system. The angular resolution of the PILS data set allows us to study these quantities at a resolution of 0.5 \u27\u27 (60 au at the distance of the source). Results. Line-of-sight velocity maps of both optically thick and optically thin molecular lines reveal: (i) new manifestations of previously known outflows emanating from protostar A; (ii) a kinematically quiescent bridge of dust and gas spanning between the two protostars, with an inferred density between 4 x 10(4) cm(-3) and similar to 3 x 10(7) cm(-3); and (iii) a separate, straight filament seemingly connected to protostar B seen only in C2H, with a flat kinematic signature. Signs of various outflows, all emanating from source A, are evidence of high-density and warmer gas; none of them coincide spatially and kinematically with the bridge. Conclusions. We hypothesize that the bridge arc is a remnant of filamentary substructure in the protostellar envelope material from which protostellar sources A and B have formed. One particular morphological structure appears to be due to outflowing gas impacting the quiescent bridge material. The continuing lack of clear outflow signatures unambiguously associated to protostar B and the vertically extended shape derived for its disk-like structure lead us to conclude that source B may be in an earlier evolutionary stage than source A
A Randomized Trial Evaluating Prosaptideâ„¢ for HIV-Associated Sensory Neuropathies: Use of an Electronic Diary to Record Neuropathic Pain
Objectives: To examine the efficacy and safety of Prosaptide™ (PRO) for the treatment of painful HIV-associated sensory neuropathies (HIV-SN). Design: A randomized, double-blind, placebo-controlled, multicenter study in participants with sensory neuropathy. Pain modulating therapy was discontinued prior to baseline. Participants were stratified by sural sensory nerve action potential (SNAP) amplitude. Participants were trained to use an electronic diary (ED) to record pain. Setting: Peripheral neuropathies are common complications of HIV infection. The pathogenesis is unknown and currently treatments are restricted to symptomatic measures. We examined PRO against placebo (PBO) for treatment of painful HIV-SN and performed a post-hoc evaluation of an electronic diary (ED) to record HIV-associated neuropathic pain. Participants: Eligible participants included adults with neurologist-confirmed painful HIV-SN.Interventions 2, 4, 8, or 16 mg/d PRO or PBO administered via subcutaneous (SC) injection for six weeks. Neurotoxic antiretroviral drug usage was held constant.Outcome Measures Changes from baseline in the weekly average of evaluable daily random prompts measuring pain using the Gracely pain scale and adverse events. Results: 237 participants were randomized. The study was stopped after a planned futility analysis. There were no between-group differences in the frequency of adverse events or laboratory toxicities. The 6-week mean (sd) Gracely pain scale changes were −0.12 (0.23), −0.24 (0.35), −0.15 (0.32), −0.18 (0.34), and −0.18 (0.32) for the 2, 4, 8, 16 mg, and PBO arms respectively. A similar variability of pain changes recorded using the ED were noted compared to previous trials that used paper collection methods.Conclusions 6-week treatment with PRO was safe but not effective at reducing HIV-associated neuropathic pain. Use of an ED to record neuropathic pain is novel in HIV-SN, resulted in reasonable compliance in recording pain data, but did not decrease the variability of pain scores compared to historical paper collection methods. Trial Registration: Current Controlled Trials NCT0028637
Tracing the cold and warm physico-chemical structure of deeply embedded protostars: IRAS 16293-2422 vs. VLA 1623-2417
Stars and planetary system
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