106 research outputs found
SOLIS: XII. SVS13-A Class i chemical complexity as revealed by S-bearing species
Context. Recent results in astrochemistry have revealed that some molecules, such as interstellar complex organic species and deuterated species, can serve as valuable tools in the investigation of star-forming regions. Sulphuretted species can also be used to follow the chemical evolution of the early stages of a Sun-like star formation process. Aims. The goal is to obtain a census of S-bearing species using interferometric images towards SVS13-A, a Class I object associated with a hot corino that is rich in interstellar complex organic molecules. Methods. To this end, we used the NGC 1333 SVS13-A data at 3 mm and 1.4 mm obtained with the IRAM-NOEMA interferometer in the framework of the SOLIS (Seeds of Life in Space) Large Program. The line emission of S-bearing species was imaged and analyzed using local thermodynamic equilibrium (LTE) and large velocity gradient (LVG) approaches. Results. We imaged the spatial distribution on =300 au scale of the line emission of 32SO, 34SO, C32S, C34S, C33S, OCS, H2C32S, H2C34S, and NS. The low excitation (9 K) 32SO line traces: (i) the low-velocity SVS13-A outflow and (ii) the fast (up to 100 km s-1 away from the systemic velocity) collimated jet driven by the nearby SVS13-B Class 0 object. Conversely, the rest of the lines are confined in the inner SVS13-A region, where complex organics were previously imaged. More specifically, the non-LTE LVG analysis of SO, SO2, and H2CS indicates a hot corino origin (size in the 60 120 au range). Temperatures between 50 K and 300 K, as well as volume densities larger than 105 cm-3 have been derived. The abundances of the sulphuretted are in the following ranges: 0.3 6 ± 10-6 (CS), 7 ± 10-9 1 ± 10-7 (SO), 1 10 ± 10-7 (SO2), a few 10-10 (H2CS and OCS), and 10-10 10-9 (NS). The N(NS)/N(NS+) ratio is larger than 10, supporting the assessment that the NS+ ion is mainly formed in the extended envelope. Conclusions. The [H2CS]/[H2CO] ratio, once measured at high-spatial resolutions, increases with time (from Class 0 to Class II objects) by more than one order of magnitude (from =10-2 to a few 10-1). This suggests that [S]/[O] changes along the process of Sunlike star formation. Finally, the estimate of the [S]/[H] budget in SVS13-A is 2 17% of the Solar System value (1.8 ± 10-5), which is consistent with what was previously measured towards Class 0 objects (1 8%). This finding supports the notion that the enrichment of the sulphuretted species with respect to dark clouds remains constant from the Class 0 to the Class I stages of low-mass star formation. The present findings stress the importance of investigating the chemistry of star-forming regions using large observational surveys as well as sampling regions on the scale of the Solar System
Moving frames applied to shell elasticity
Exterior calculus and moving frames are used to describe curved elastic
shells. The kinematics follow from the Lie-derivative on forms whereas the
dynamics via stress-forms.Comment: 20 pages, 1 figur
Relating jet structure to photometric variability: the Herbig Ae star HD 163296
Herbig Ae/Be stars are intermediate-mass pre-main sequence stars surrounded
by circumstellar dust disks. Some are observed to produce jets, whose
appearance as a sequence of shock fronts (knots) suggests a past episodic
outflow variability. This "jet fossil record" can be used to reconstruct the
outflow history. We present the first optical to near-infrared (NIR)
VLT/X-shooter spectra of the jet from the Herbig Ae star HD 163296. We
determine physical conditions in the knots, as well as their kinematic "launch
epochs". Knots are formed simultaneously on either side of the disk, with a
regular interval of ~16 yr. The velocity dispersion versus jet velocity and the
energy input are comparable in both lobes. However, the mass loss rate,
velocity, and shock conditions are asymmetric. We find Mjet/Macc ~ 0.01-0.1,
consistent with magneto-centrifugal jet launching models. No evidence for dust
is found in the high-velocity jet, suggesting it is launched within the
sublimation radius (<0.5 au). The jet inclination measured from proper motions
and radial velocities confirms it is perpendicular to the disk. A tentative
relation is found between the structure of the jet and the photometric
variability of the source. Episodes of NIR brightening were previously detected
and attributed to a dusty disk wind. We report for the first time significant
optical fadings lasting from a few days up to a year, coinciding with the NIR
brightenings. These are likely caused by dust lifted high above the disk plane;
this supports the disk wind scenario. The disk wind is launched at a larger
radius than the high-velocity atomic jet, although their outflow variability
may have a common origin. No significant relation between outflow and accretion
variability could be established. Our findings confirm that this source
undergoes periodic ejection events, which may be coupled with dust ejections
above the disk plane.Comment: 20 pages, 11 figures, accepted for publication in Astronomy &
Astrophysic
Herschel -PACS observations of [OI] and H2O in Cha II
Gas plays a major role in the dynamical evolution of protoplanetary discs.
Its coupling with the dust is the key to our understanding planetary formation.
Studying the gas content is therefore a crucial step towards understanding
protoplanetary discs evolution. Such a study can be made through spectroscopic
observations of emission lines in the far-infrared, where some of the most
important gas coolants emit, such as the [OI] 3P1-3 P2 transition at 63.18
microns. We aim at characterising the gas content of protoplanetary discs in
the intermediate-aged Chamaeleon II (Cha II) star forming region. We also aim
at characterising the gaseous detection fractions within this age range, which
is an essential step tracing gas evolution with age in different star forming
regions. We obtained Herschel-PACS line scan spectroscopic observations at 63
microns of 19 Cha II Class I and II stars. The observations were used to trace
[OI] and o-H2O at 63 microns. The analysis of the spatial distribution of [OI],
when extended, can be used to understand the origin of the emission. We have
detected [OI] emission toward seven out of the nineteen systems observed, and
o-H2O emission at 63.32 microns in just one of them, Sz 61. Cha II members show
a correlation between [OI] line fluxes and the continuum at 70 microns, similar
to what is observed in Taurus. We analyse the extended [OI] emission towards
the star DK Cha and study its dynamical footprints in the PACS Integral Field
Unit (IFU). We conclude that there is a high velocity component from a jet
combined with a low velocity component with an origin that may be a combination
of disc, envelope and wind emission. The stacking of spectra of objects not
detected individually in [OI] leads to a marginal 2.6sigma detection that may
indicate the presence of gas just below our detection limits for some, if not
all, of them.Comment: 10 pages, 7 figure
Misaligned Rotations of the Envelope, Outflow, and Disks in the Multiple Protostellar System of VLA 1623-2417: FAUST. III
We report a study of the low-mass Class-0 multiple system VLA 1623AB in the Ophiuchus star-forming region, using H13CO+ (J=3â2), CS (J=5â4), and CCH (N=3â2) lines as part of the ALMA Large Program FAUST. The analysis of the velocity fields revealed the rotation motion in the envelope and the velocity gradients in the outflows (about 2000 au down to 50 au). We further investigated the rotation of the circum-binary VLA 1623A disk as well as the VLA 1623B disk. We found that the minor axis of the circum-binary disk of VLA 1623A is misaligned by about 12 degrees with respect to the large-scale outflow and the rotation axis of the envelope. In contrast, the minor axis of the circum-binary disk is parallel to the large-scale magnetic field according to previous dust polarization observations, suggesting that the misalignment may be caused by the different directions of the envelope rotation and the magnetic field. If the velocity gradient of the outflow is caused by rotation, the outflow has a constant angular momentum and the launching radius is estimated to be 5â16 au, although it cannot be ruled out that the velocity gradient is driven by entrainments of the two high-velocity outflows. Furthermore, we detected for the first time a velocity gradient associated with rotation toward the VLA 16293B disk. The velocity gradient is opposite to the one from the large-scale envelope, outflow, and circum-binary disk. The origin of its opposite gradient is also discussed
FAUST VIII. The protostellar disk of VLA 1623-2417 W and its streamers imaged by ALMA
More than 50% of solar-mass stars form in multiple systems. It is therefore
crucial to investigate how multiplicity affects the star and planet formation
processes at the protostellar stage. We report continuum and CO (2-1)
observations of the VLA 1623-2417 protostellar system at 50 au angular
resolution as part of the ALMA Large Program FAUST. The 1.3 mm continuum probes
the disks of VLA 1623A, B, and W, and the circumbinary disk of the A1+A2
binary. The CO emission reveals, for the first time, the gas in the
disk-envelope of VLA 1623W. We estimate the dynamical mass of VLA 1623W,
M, and the mass of its disk, M. CO also reveals streamers that
extend up to 1000 au, spatially and kinematically connecting the envelope and
outflow cavities of the A1+A2+B system with the disk of VLA 1623W. The presence
of the streamers, as well as the spatial (1300 au) and velocity
(2.2 km/s) offset of VLA 1623W suggest that either sources W and A+B
formed in different cores, interacting between them, or that source W has been
ejected from the VLA 1623 multiple system during its formation. In the latter
case, the streamers may funnel material from the envelope and cavities of VLA
1623AB onto VLA 1623W, thus concurring to set its final mass and chemical
content.Comment: 10 pages, 5 figures, accepted by MNRA
SOLIS: XII. SVS13-A Class I chemical complexity as revealed by S-bearing species
Interstellar matter and star formatio
FAUST X. Multi-band, multi-scale dust study of L1527 IRS. Evidence for dust properties variations within the envelope of a Class 0/I YSO
Early dust grain growth in protostellar envelopes infalling on young discs
has been suggested in recent studies, supporting the hypothesis that dust
particles start to agglomerate already during the Class 0/I phase of young
stellar objects (YSOs). If this early evolution were confirmed, it would impact
the usually assumed initial conditions of planet formation, where only
particles with sizes m are usually considered for
protostellar envelopes. We aim to determine the maximum grain size of the dust
population in the envelope of the Class 0/I protostar L1527 IRS, located in the
Taurus star-forming region (140 pc). We use Atacama Large
millimetre/sub-millimetre Array (ALMA) and Atacama Compact Array (ACA) archival
data and present new observations, in an effort to both enhance the
signal-to-noise ratio of the faint extended continuum emission and properly
account for the compact emission from the inner disc. Using observations
performed in four wavelength bands and extending the spatial range of previous
studies, we aim to place tight constraints on the spectral () and dust
emissivity () indices in the envelope of L1527 IRS. We find a rather
flat 3.0 profile in the range 50-2000 au. Accounting for the
envelope temperature profile, we derive values for the dust emissivity index,
0.9 < < 1.6, and reveal a tentative, positive outward gradient. This
could be interpreted as a distribution of mainly ISM-like grains at 2000 au,
gradually progressing to (sub-)millimetre-sized dust grains in the inner
envelope, where at R=300 au, = 1.1 +/- 0.1. Our study supports a
variation of the dust properties in the envelope of L1527 IRS. We discuss how
this can be the result of in-situ grain growth, dust differential collapse from
the parent core, or upward transport of disc large grains.Comment: Accepted for publication in A&A. Contains 18 pages, 21 figures, 5
table
FAUST: IX. Multiband, multiscale dust study of L1527 IRS. Evidence for variations in dust properties within the envelope of a class 0/I young stellar object
Context. Early dust grain growth in protostellar envelopes infalling on young disks has been suggested in recent studies, supporting the hypothesis that dust particles start to agglomerate already during the class 0/I phase of young stellar objects. If this early evolution were confirmed, it would impact the usually assumed initial conditions of planet formation, where only particles with sizes âČ0.25 ”m are usually considered for protostellar envelopes. /
Aims. We aim to determine the maximum grain size of the dust population in the envelope of the class 0/I protostar L1527 IRS, located in the Taurus star-forming region (140 pc). /
Methods. We use Atacama Large millimeter/submillimeter Array and Atacama Compact Array archival data and present new observations, in an effort to both enhance the signal-to-noise ratio of the faint extended continuum emission and properly account for the compact emission from the inner disk. Using observations performed in four wavelength bands and extending the spatial range of previous studies, we aim to place tight constraints on the spectral (α) and dust emissivity (ÎČ) indices in the envelope of L1527 IRS. /
Results. We find a rather flat α ~ 3.0 profile in the range 50â2000 au. Accounting for the envelope temperature profile, we derived values for the dust emissivity index, 0.9 < ÎČ < 1.6, and reveal a tentative, positive outward gradient. This could be interpreted as a distribution of mainly interstellar medium like grains at 2000 au, gradually progressing to (sub)millimeter-sized dust grains in the inner envelope, where at R = 300 au, ÎČ = 1.1 ± 0.1.
Our study supports a variation of the dust properties in the envelope of L1527 IRS. We discuss how this can be the result of in situ grain growth, dust differential collapse from the parent core, or upward transport of disk large grains
Seeds of Life in Space (SOLIS). III. Zooming Into the Methanol Peak of the Prestellar Core L1544
Toward the prestellar core L1544, the methanol (CH3OH) emission forms an asymmetric ring around the core center, where CH3OH is mostly in solid form, with a clear peak at 4000 au to the northeast of the dust continuum peak. As part of the NOEMA Large Project SOLIS (Seeds of Life in Space), the CH3OH peak has been spatially resolved to study its kinematics and physical structure and to investigate the cause behind the local enhancement. We find that methanol emission is distributed in a ridge parallel to the main axis of the dense core. The centroid velocity increases by about 0.2 km sâ1 and the velocity dispersion increases from subsonic to transonic toward the central zone of the core, where the velocity field also shows complex structure. This could be an indication of gentle accretion of material onto the core or the interaction of two filaments, producing a slow shock. We measure the rotational temperature and show that methanol is in local thermodynamic equilibrium (LTE) only close to the dust peak, where it is significantly depleted. The CH3OH column density, N tot(CH3OH), profile has been derived with non-LTE radiative transfer modeling and compared with chemical models of a static core. The measured N tot(CH3OH) profile is consistent with model predictions, but the total column densities are one order of magnitude lower than those predicted by models, suggesting that the efficiency of reactive desorption or atomic hydrogen tunneling adopted in the model may be overestimated; or that an evolutionary model is needed to better reproduce methanol abundance
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