J/A+A/654/A52 SVS13-A Class I IRAM-NOEMA images (Codella+, 2021)
SOLIS XII. SVS13-A Class I chemical complexity as revealed by S-bearing species.
Codella C., Bianchi E., Podio L., Mercimek S., Ceccarelli C.,
Lopez-Sepulcre A., Bachiller R., Caselli P., Sakai N., Neri R., Fontani F.,
Favre C., Balucani N., Lefloch B., Viti S., Yamamoto S.
<Astron. Astrophys. 654, A52 (2021)>
=2021A&A...654A..52C 2021A&A...654A..52C (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Millimetric/submm sources ; Interferometry
Keywords: stars: formation - ISM: abundances - ISM: molecules -
ISM: individual objects: SVS13-A
Abstract:
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.
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.
To this end, we used the NGC1333 SVS13-A data at 3mm and 1.4mm 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.
We imaged the spatial distribution on ≤300au scale of the line
emission of 32SO, 34SO, C32S, C34S, C33S, OCS, H2C32S,
H2C34S, and NS. The low excitation (9K) 32SO line traces: (i)
the low-velocity SVS13-A outflow and (ii) the fast (up to 100km/s 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 60-120au range).
Temperatures between 50K and 300K, as well as volume densities larger
than 105cm-3 have been derived. The abundances of the sulphuretted
are in the following ranges: 0.3-6x10-6 (CS), 7x10-9-1x10-7
(SO), 1-10x10-7 (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.
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 Sun-like star
formation. Finally, the estimate of the [S]/[H] budget in SVS13-A is
2%-17% of the Solar System value (1.8x10-5), 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 lowmass 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.
Description:
The SVS13-A region was observed at 1.4mm and 3mm in two different
setups (hereafter labelled 5 and 6) with the IRAM NOEMA
interferometer.
Setup 6, at 3mm, was observed in A configuration (1 track) using nine
antennas in March 2018. The frequency ranges are 80.2-88.3GHz and
95.7-103.9GHz.
Setup 5, at 1.4mm, was observed in A and C configurations (three
tracks) using eight antennas in December 2016. The frequency range is
204.0-207.6GHz.
Maps of the S-bearing species analysed in the paper, reported in
Figures 1, 2, 4, 6, 8, 10, and 12. The name of the files report the
S-species as well as the line transition.
Objects:
-------------------------------------------------------------
RA (2000) DE Designation(s)
-------------------------------------------------------------
03 29 03.73 +31 16 03.8 SVS13-A = [SVS76] NGC 1333 13A
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 158 22 List of fits images
fits/* . 22 Individual fits images
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See also:
J/A+A/605/A57 : SOLIS. I. OMC2-FIR4 HC3N and HC5N images (Fontani+, 2017)
J/A+A/605/L3 : SOLIS. II. L1157-B1 NH2CHO image (Codella+, 2017)
J/A+A/637/A63 : SOLIS. VI. NGC 1333-IRAS4A radio images (Taquet+, 2020)
J/A+A/640/A74 : SOLIS. VIII. L1157-B1 spectra (Spezzano+, 2020)
J/A+A/640/A75 : SOLIS. X. NGC 1333 IRAS 4A images (De Simone+, 2020)
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 23 I4 --- Nx Number of pixels along X-axis
25- 28 I4 --- Ny Number of pixels along Y-axis
30- 33 I4 Kibyte size Size of FITS file
35- 56 A22 --- FileName Name of FITS file, in subdirectory fits
58-158 A101 --- Title Title of the FITS file
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Acknowledgements:
Claudio Codella, claudio.codella(at)inaf.it
References:
Fontani et al., Paper I 2017A&A...605A..57F 2017A&A...605A..57F, Cat. J/A+A/605/A57
Codella et al., Paper II 2017A&A...605L...3C 2017A&A...605L...3C, Cat. J/A+A/605/L3
Punanova et al., Paper III 2018ApJ...855..112P 2018ApJ...855..112P
Favre et al., Paper IV 2018ApJ...859..136F 2018ApJ...859..136F
Codella et al., Paper V 2020A&A...635A..17C 2020A&A...635A..17C
Taquet et al., Paper VI 2020A&A...637A..63T 2020A&A...637A..63T, Cat. J/A+A/637/A63
Favre et al., Paper VII 2020A&A...635A.189F 2020A&A...635A.189F
Spezzano et al., Paper VIII 2020A&A...640A..74S 2020A&A...640A..74S, Cat. J/A+A/640/A74
Feng et al., Paper IX 2020ApJ...896...37F 2020ApJ...896...37F
De Simone et al., Paper X 2020A&A...640A..75D 2020A&A...640A..75D, Cat. J/A+A/640/A75
Benedettini et al., Paper XI 2021A&A...645A..91B 2021A&A...645A..91B
(End) Patricia Vannier [CDS] 21-Sep-2021