J/A+A/707/A348 AB Aur NOEMA CS 3-2 datacube (Riviere-Marichalar+, 2026)
AB Aur, a Rosetta stone for studies of planet formation.
IV. C/O estimates from CS and SO interferometric observations.
Riviere-Marichalar P., Fuente A., le Gal R., Neri R., Esplugues G.,
Semenov D., Teague R., Santamaria-Miranda A.
<Astron. Astrophys. 707, A348 (2026)>
=2026A&A...707A.348R 2026A&A...707A.348R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, pre-main sequence ; Radio lines ; Abundances
Keywords: astrochemistry - techniques: interferometric - protoplanetary disks -
ISM: abundances - ISM: molecules
Abstract:
Protoplanetary disks are the birthplace of planets. As such, they set
the initial chemical abundances available for planetary
atmosphere formation. Thus, studying elemental abundances, molecular
compositions, and abundance ratios in protoplanetary disks is key to
linking planetary atmospheres to their formation sites.
We aim to derive the sulfur abundance and the C/O ratio in the AB Aur
disk using interferometric observations of CS and SO.
New NOEMA observations of CS 3-2 towards AB Aur are presented. We used
velocity-integrated intensity maps to determine
the inclination and position angles. Keplerian masks were constructed
for all observed species to assess the presence of non-Keplerian
motions. We use the CS/SO ratio to study the C/O ratio. We compare our
present and previous interferometric observations of AB Aur with a
NAUTILUS disk model to gain insight into the S elemental abundance and
C/O ratio.
We derive an observational CS/SO ratio ranging from 1.8 to 2.6. Only
NAUTILUS models with C/O&1 can reproduce such ratios. The comparison
with models points to strong sulfur depletion, with [S/H]=8e-8, but
we note that no single model can simultaneously fit all observed
species.
Description:
The observations were conducted using NOEMA under project W21BA (PI:
P. Riviere-Marichalar) in the AB set of configurations, utilizing all
12 antennas between February 20 and March 5, 2022. Observing
conditions were generally excellent, with stable and favorable weather
throughout the campaign. The atmospheric phase stability ranged
between 10° and 40° RMS, and precipitable water vapor values
were between 0.5 and 5mm.
Objects:
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RA (2000) DE Designation(s)
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04 55 45.84 +30 33 04.2 AB Aur = HD 31293
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 112 1 Information on fits datacube
fits/* . 1 Individual fits datacube
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See also:
J/A+A/589/A60 : CO, SO and H2CO images of AB Aur (Pacheco-Vazquez+, 2016)
J/ApJS/248/19 : High-resolution spectroscopy of TESS stars
(Tautvaisiene+, 2020)
J/A+A/649/A126 : Abundances of neutron-capture elements (Tautvaisiene+, 2021)
J/ApJS/259/45 : Abundances of northern bright TESS stars (Tautvaisiene+, 2022)
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- 22 I3 --- Nx Number of pixels along X-axis
24- 26 I3 --- Ny Number of pixels along Y-axis
28- 30 I3 --- Nz Number of slices
32- 39 F8.1 m/s bVRAD Lower value of bVRAD interval
41- 47 F7.1 m/s BVRAD Upper value of bVRAD interval
49- 55 F7.3 m/s dVRAD bVRAD resolution
57- 61 I5 Kibyte size Size of FITS file
63- 83 A21 --- FileName Name of FITS file, in subdirectory fits
85-112 A28 --- Title Title of the FITS file
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Acknowledgements:
From Pablo Riviere-Marichalar, pablo.riviere.m(at)gmail.com
A.F., G.E., and P.R.M. are members of project PID2022-
137980NB-I00, funded by MCIN/AEI/10.13039/501100011033/FEDER UE. This
project has received funding from the European Research Council (ERC)
under the European Union's Horizon Europe research and innovation
program ERC-AdG-2022 (SUL4LIFE , GA No 101096293). D.S. has received
funding from the European Research Council (ERC) under the European
Union's Horizon 2020 research and innovation programme
(PROTOPLANETS, GA No. 101002188). A.S.M. acknowledges support from
ANID / Fondo 2022 ALMA / 31220025. Part of this work was supported by
the Max-Planck Society. This paper makes use of the following ALMA
data: ADS/JAO.ALMA#2019.1.00579.S and ADS/JAO.ALMA#2021.1.00690.S.
This work is based on observations carried out under project number
W21BA with the IRAM NOEMA Interferometer. IRAM is supported by
INSU/CNRS (France), MPG (Germany), and IGN (Spain).
References:
Tautvaisiene et al,. Paper I 2020ApJS..248...19T 2020ApJS..248...19T, Cat. J/ApJS/248/19
Tautvaisiene et al,. Paper II 2021A&A...649A.126T 2021A&A...649A.126T, Cat. J/A+A/649/A126
Tautvaisiene et al,. Paper III 2022ApJS..259...45T 2022ApJS..259...45T, Cat. J/ApJS/259/45
(End) Patricia Vannier [CDS] 17-Feb-2026