J/A+A/637/A63 NGC 1333-IRAS4A radio images (Taquet+, 2020)
Seeds of Life in Space (SOLIS).
VI. Chemical evolution of sulfuretted species along the outflows driven by the
low-mass protostellar binary NGC 1333-IRAS4A.
Taquet V., Codella C., De Simone M., Lopez-Sepulcre A., Pineda J.E.,
Segura-Cox D., Ceccarelli C., Caselli P., Gusdorf A., Persson M.V.,
Alves F., Caux E., Favre C., Fontani F., Neri R., Oya Y., Sakai N.,
Vastel C., Yamamoto S., Bachiller R., Balucani N., Bianchi E., Bizzocchi L.,
Chacon-Tanarro A., Dulieu F., Enrique-Romero J., Feng S., Holdship J.,
Lefloch B., Jaber Al-Edhari A., Jimenez-Serra I., Kahane C., Lattanzi V.,
Ospina-Zamudio J., Podio L., Punanova A., Rimola A., Sims I.R., Spezzano S.,
Testi L., Theule P., Ugliengo P., Vasyunin A.I., Vazart F., Viti S.,
Witzel A.
<Astron. Astrophys. 637, A63 (2020)>
=2020A&A...637A..63T 2020A&A...637A..63T (SIMBAD/NED BibCode)
ADC_Keywords: YSOs ; Infrared sources ; Interstellar medium
Keywords: astrochemistry - ISM: abundances - ISM: molecules - stars: formation -
ISM: jets and outflows - ISM: individual objects: NGC1333-IRAS4A
Abstract:
Low-mass protostars drive powerful molecular outflows that can be
observed with millimetre and submillimetre telescopes. Various
sulfuretted species are known to be bright in shocks and could be used
to infer the physical and chemical conditions throughout the observed
outflows.
The evolution of sulfur chemistry is studied along the outflows driven
by the NGC1333-IRAS4A protobinary system located in the Perseus cloud
to constrain the physical and chemical processes at work in shocks.
We observed various transitions from OCS, CS, SO, and SO2 towards
NGC1333-IRAS4A in the 1.3, 2, and 3mm bands using the {IRAM NOrthern
Extended Millimeter Array (NOEMA)} and we interpreted the observations
through the use of the Paris-Durham shock model.
The targeted species clearly show different spatial emission along the
two outflows driven by IRAS4A. OCS is brighter on small and large
scales along the south outflow driven by IRAS4A1, whereas SO2 is
detected rather along the outflow driven by IRAS4A2 that is extended
along the north east - south west (NE-SW) direction. SO is detected at
extremely high radial velocity up to +25km/s relative to the source
velocity, clearly allowing us to distinguish the two outflows on small
scales. Column density ratio maps estimated from a rotational diagram
analysis allowed us to confirm a clear gradient of the OCS/SO2
column density ratio between the IRAS4A1 and IRAS4A2 outflows.
Analysis assuming non Local Thermodynamic Equilibrium of four SO$_2$
transitions towards several SiO emission peaks suggests that the
observed gas should be associated with densities higher than
105cm-3 and relatively warm (T>100K) temperatures in most cases.
The observed chemical differentiation between the two outflows of the
IRAS4A system could be explained by a different chemical history. The
outflow driven by IRAS4A1 is likely younger and more enriched in
species initially formed in interstellar ices, such as OCS, and
recently sputtered into the shock gas. In contrast, the longer and
likely older outflow triggered by IRAS4A2 is more enriched in species
that have a gas phase origin, such as SO2.
Description:
For the SOLIS data, the IRAS4A binary system was observed in three
different Setups (1, 3, and 5) with the IRAM NOEMA interferometer
during several tracks in June and September 2016 (see Table 1 of
Ceccarelli2017). Setup 1, 3, and 5 cover the frequency ranges from
80.8GHz to 84.4GHz, from 95.7GHz to 99.5GHz, and between 204.0 and
207.6GHz, respectively. For Setups 1 and 3, the array was used in
both configurations D and C with baselines from 16m to 240m for
Setup 1 and from 15m to 304m for Setup 3. For Setup 5, the array was
used in configurations A and C. The phase centre is on the IRAS4A1
source, alpha(J2000)=03:29:10.5, delta(J2000)=+31:13:30.9. The
bandpass was calibrated on 3C454.3 and 3C84, the absolute flux was
fixed by observing MWC349, LKHA101, 2013+370, and 2007+659, and
0333+321 was used to set the gains in phase and amplitude. The final
uncertainty on the absolute flux scale is less than 15%. The phase rms
was less than 50 degrees, the typical precipitable water vapour (pwv)
was from 4mm to 15mm, and the system temperatures ranged typically
between 50 and 200K. The data were reduced using the packages CLIC
and MAPPING of the GILDAS software collection. A continuum map was
obtained by averaging line-free channels and self calibrating the
data. The self calibration solutions were then applied to the spectral
cube, which was subsequently cleaned. The resulting synthesised FWHM
beam is 4.5x3.5arcsec (P.A.=27-degrees) for Setup 1, 2.2x1.9arcsec
(P.A.=96-degrees) for Setup 3, and 0.9x0.7-arcsec (P.A.=47-degrees)
for Setup 5. The half power primary beam is 61.4, 59.2, and 24.5arcsec
for Setups 1, 3, and 5 respectively.
We used the CALYPSO data observed with the IRAM-PdBI (Maury et al.,
2019A&A...621A..76M 2019A&A...621A..76M) to extract the interferometric maps from the
SiO(5-4), SO(65-54), and OCS(8-7) transitions at 218GHz. These
observations were carried out between February 2011 and February 2013
as part of the CALYPSO Large Program using the A and C configurations
of the array. The synthesised FWHM beam at 1.4mm is 1.1x0.8arcsec.
More details on the observational properties can be found in
(Santangelo et al., 2015A&A...584A.126S 2015A&A...584A.126S).
IRAS4A was observed with the IRAM PdBI at 145 and 165 GHz on 2010 July
20, 21, August 1, 3, November 24, and 2011 March 10 in the C and D
most compact configurations of the array. The baseline range of the
observations is 25m-140m, allowing us to recover emission on
scales from 10-15arcsec to 2arcsec. The WIDEX backends have been
used at 143.4 and 165.2GHz, providing a bandwidth of 3.6GHz each
with a spectral resolution of 1.95MHz (3.5-4km/s).
High-resolution narrowband backends focused on two CH3OH lines have
also been used. They provide a bandwidth of 80MHz with a spectral
resolution of 0.04MHz (0.08km/s). We decreased the spectral
resolution to 0.40MHz (0.8km/s) to obtain a better signal-to-noise.
More details on the observational dataset can be found in Taquet et
al. (2015ApJ...804...81T 2015ApJ...804...81T). PdBI observations at 225GHz were performed
on 27 and 28 November 2011, on 12, 15, 21, 27 March 2012, and on 2
April 2012 in the B and C configurations of the array. The synthesised
FWHM beam is 1.2"x1.0". A more detailed description of the
observational setups is provided by Persson et al.,
2014A&A...563A..74P 2014A&A...563A..74P. For all datasets, the amplitude calibration
uncertainty is estimated to be 15-20%. Given we map relatively
extended structures such as outflow lobes, we cleaned the images using
the Hogbom method with natural weighting and with a mask containing
all the molecular lobes to minimise artefacts in the cleaned image.
Objects:
--------------------------------------------------------------
RA (2000) DE Designation(s)
--------------------------------------------------------------
03 29 10.49 +31 13 30.8 NGC 1333-IRAS4A = [JCC87] IRAS 4A
--------------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 111 38 List of fits files
fits/* . 38 Individual fits files
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See also:
J/A+A/605/A57 : SOLIS. II. OMC2-FIR4 HC3N and HC5N images (Fontani+, 2017)
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)
21- 24 I4 --- Nx Number of pixels along X-axis
26- 29 I4 --- Ny Number of pixels along Y-axis
31- 34 I4 Kibyte size Size of FITS file
36- 68 A33 --- FileName Name of FITS file, in subdirectory fits
70-111 A42 --- Title Title of the FITS file
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Acknowledgements:
Vianney Taquet, taquet(at)arcetri.astro.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
Punanova et al., Paper III 2018ApJ...855..112P 2018ApJ...855..112P
Ceccarelli et al., Paper IV 2017ApJ...850..176C 2017ApJ...850..176C
Codella et al., Paper V 2020A&A...635A..17C 2020A&A...635A..17C
Favre et al., Paper VII 2020A&A...635A.189F 2020A&A...635A.189F
(End) Patricia Vannier [CDS] 14-Apr-2020