J/A+A/687/A92 Anatomy of L1489 IRS with NOEMA I (Tanious+, 2024)
Anatomy of the Class I protostar L1489 IRS with NOEMA,
I. Disk, streamers, outflow(s) and bubbles at 3mm.
Tanious M., Le Gal R., Neri R., Faure A., Gupta A., Law C.J., Huang J.,
Cuello N., Williams J.P., Menard F.
<Astron. Astrophys. 687, A92 (2024)>
=2024A&A...687A..92T 2024A&A...687A..92T (SIMBAD/NED BibCode)
ADC_Keywords: YSOs ; Protostars ; Molecular clouds; Interferometry
Keywords: astrochemistry - protoplanetary disks - stars: low-mass -
ISM: bubbles - ISM: kinematics and dynamics - ISM: lines and bands
Abstract:
Over the past few years, chemical studies have revealed multiple
structures in the vicinity of young stellar objects (YSOs). It has
become evident that specific physical conditions are associated with
the emission of particular molecular lines, allowing us to use
molecular probes of the YSO physics. Consequently, chemical surveys
are now necessary to fully constrain the origin of the observed
structures. Several surveys have been conducted to explore the
chemistry of YSOs, focusing on Class 0 and Class II objects. However,
our knowledge of intermediate objects, that are Class I objects,
remains limited.
To bridge the gap and establish the relationship between observed
structures and molecular line emission at the Class I evolutionary
stage, we investigate the spatial distribution of key molecular gas
species in the low-mass Class I protostar L1489 IRS (IRAS 04016+2610),
a source part of the ChemYSO survey.
We performed a 3mm line survey at high spatial and high spectral
resolution using the NOEMA interferometer and the IRAM-30m telescope.
For the data analysis, we applied and compared two methods: a
streamline model and the new python package TIPSY.
We present here the ten brightest lines of our survey, in which we
identified a new ∼3000au long streamer in HC3N, C2H, and
c-C3H2 emission, likely associated with more localized accretion
shocks probed in SO. In addition, two ∼10000 au bubbles are seen with
the dense molecular tracers HCO+, CS, and HCN around the YSO. We
retrieve previously identified structures, like an outflow in HCO+ and
another streamer in C2H. Additionally, potential indicators of a
second outflow appear in CS and HCN emission, but its nature remains
to be confirmed.
Description:
We present the original cubes used to obtain the results from the
paper. These include NOEMA data (projects S20AH and W20AJ, PI: R.
Le Gal), and IRAM-30m data (project 184-20, PI: R. Le Gal) at 3mm.
Objects:
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RA (2000) DE Designation(s)
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04 04 43.1 +26 18 56 L1489 IRS = IRAS 04016+2610
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 170 12 List of fits files
fits/* . 12 Individual fits files
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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- 32 I3 --- Nz ? Number of slices for the datacubes
34- 45 F12.2 m/s bVRAD Lower value of VRAD interval or VRAD
47- 54 F8.2 m/s BVRAD ? Upper value of VRAD interval
56- 62 F7.3 m/s dVRAD ? VRAD resolution
64- 70 I7 Kibyte size Size of FITS file
72-107 A36 --- FileName Name of FITS file, in subdirectory fits
109-170 A62 --- Title Title of the FITS file
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Acknowledgements:
Maxime Tanious, maxime.tanious(at)univ-grenoble-alpes.fr
Romane Le Gal, romane.le-gal(at)univ-grenoble-alpes.fr
(End) Patricia Vannier [CDS] 29-Mar-2024