J/A+A/681/A50 ATOMIUM. Molecular inventory (Wallstrom+, 2024)
ATOMIUM: Molecular inventory of 17 oxygen-rich evolved stars observed with ALMA.
Wallstrom S.H.J., Danilovich T., Muller H.S.P., Gottlieb C.A., Maes S.,
Van de Sande M., Decin L., Richards A.M.S., Baudry A., Bolte J.,
Ceulemans T., De Ceuster F., de Koter A., El Mellah I., Esseldeurs M.,
Etoka S., Gobrecht D., Gottlieb E., Gray M., Herpin F., Jeste M., Kee D.,
Kervella P., Khouri T., Lagadec E., Malfait J., Marinho L., McDonald I.,
Menten K.M., Millar T.J., Montarges M., Nuth J.A., Plane J.M.C., Sahai R.,
Waters L.B.F.M., Wong K.T., Yates J., Zijlstra A.
<Astron. Astrophys. 681, A50 (2024)>
=2024A&A...681A..50W 2024A&A...681A..50W (SIMBAD/NED BibCode)
ADC_Keywords: Stars, M-type ; Stars, giant ; Abundances ; Spectroscopy
Keywords: stars: AGB and post-AGB - supergiants - circumstellar matter -
line: identification - instrumentation: interferometers -
astro-chemistry
Abstract:
The dusty winds of cool evolved stars are a major contributor of the
newly synthesised material enriching the Galaxy and future generations
of stars. However, the details of the physics and chemistry behind
dust formation and wind launching have yet to be pinpointed. Recent
spatially resolved observations show the importance of gaining a more
comprehensive view of the circumstellar chemistry, but a comparative
study of the intricate interplay between chemistry and physics is
still difficult because observational details such as frequencies and
angular resolutions are rarely comparable.
Aiming to overcome these deficiencies, ATOMIUM is an ALMA Large
Programme to study the physics and chemistry of the circumstellar
envelopes of a diverse set of oxygen-rich evolved stars under
homogeneous observing conditions at three angular resolutions between
∼0.02"-1.4". Here we summarize the molecular inventory of these
sources, and the correlations between stellar parameters and molecular
content.
Seventeen oxygen-rich or S-type asymptotic giant branch (AGB) and red
supergiant (RSG) stars have been observed in several tunings with ALMA
Band 6, targeting a range of molecules to probe the circumstellar
envelope and especially the chemistry of dust formation close to the
star. We systematically assigned the molecular carriers of the
spectral lines and measured their spectroscopic parameters and the
angular extent of the emission of each line from integrated intensity
maps.
Across the ATOMIUM sample, we detect 291 transitions of 24 different
molecules and their isotopologues. This includes several first
detections in oxygen-rich AGB/RSG stars: PO v=1, SO2 v1=1 and v2=2,
and several high energy H2O transitions. We also find several first
detections in S-type AGB stars: vibrationally excited HCN 32 = 2, 3
and SiS 3 = 4, 5, 6, as well as first detections of the molecules SiC,
AlCl, and AlF in W Aql. Overall, we find strong correlations between
the following molecular pairs: CS and SiS, CS and AlF, NaCl and KCl,
AlO and SO, SO2 and SO, and SO2 and H2O; meaning both molecules tend
to have more detected emission lines in the same sources. The measured
isotopic ratios of Si and S are found to be consistent with previous
measurements, except for an anomalously high 29Si/30Si ratio of 4±1
in the RSG VX Sgr.
This paper presents the overall molecular inventory and an initial
analysis of the large ATOMIUM dataset, laying the groundwork for
future work deriving molecular abundances and abundance profiles using
radiative transfer modeling which will provide more rigorous tests for
chemical models.
Description:
These tables give further details on the identified molecular lines
and derived parameters for the 17 ATOMIUM sources.
Table A.1 gives a full list of identified molecules by source, Table
A.2 gives the maximum radial extent of each molecule in each source,
Table A.3 lists all identified molecular lines with references for
their rest frequencies, and Table A.4 lists all the unidentified
lines. Table A.5 list all detected lines in each source, and gives
measurements taken at each spatial resolution (high, medium, low)
where the line was detected.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 217 17 Full list of identified molecules by source
tablea2.dat 53 517 Maximum radial extent of each molecule in
each source
tablea3.dat 184 260 All identified molecular lines
tablea4.dat 35 27 All unidentified lines
tablea5.dat 129 6597 All detected lines in each source,
and derived parameters
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See also:
https://fys.kuleuven.be/ster/research-projects/aerosol/atomium/atomium :
ATOMIUM Home Page
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Source Star name
13-217 A205 --- Molecules All molecules detected in the given source
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Source Star name
13- 28 A16 --- Molecule Molecule
30 A1 --- l_r Limit flag on r
31- 35 F5.2 arcsec r Max radial extent in arcsec
37 A1 --- l_rcm Limit flag on rcm
38- 45 E8.3 cm rcm Max radial extent in cm
47 A1 --- l_rR* Limit flag on rR*
48- 53 F6.1 --- rR* Max radial extent in units of
the stellar radius R*
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 39 A39 --- Line Full line name
41- 48 F8.4 GHz nu0 Rest frequency (1)
50- 56 F7.2 K Elow Energy of the lower transition level
58- 59 I2 --- N Number of sources showing the line
61 A1 --- Note [bcd] Note (2)
63-184 A122 --- Ref Reference for line parameters
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Note (1): The triples (NNN) for H2O indicate excitations in v1, v2, and
v3. Transitions are within one vibrational state, unless a
difference of two triples is given, indicating a rovibrational transition.
The first one indicates the vibrational state of the upper rovibrational
level, the second one of the lower one. See Section A.1 for more details.
Note (2): Note as follows:
b = The references in this table refer to the origin of this particular rest
frequency. Details on the whole data set are given in Section A.1
as far as applicable.
c = The transition frequency has a large uncertainty.
d = Presumed context of unpublished transition frequency; see Section A.1
for more details.
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 7 F7.3 GHz nu0 Rest frequency (GHz)
9- 33 A25 --- Sources Source(s) containing the given U-line
35 A1 --- n_Sources [*] Note on Sources (1)
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Note (1): U253.973 is blended with SO2 v=0 JKa,Kc=156,10-165,11
at 253.9566 GHz in AH Sco and VX Sgr.
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Source Star name
11- 49 A39 --- Line Full line name
51- 57 F7.3 GHz nu0 Rest frequency
59- 62 A4 --- Res [high med low] Angular resolution of the
observations
64- 68 F5.2 arcsec Ap Aperture diameter
70- 75 F6.3 Jy Fp Peak flux
77- 82 F6.3 Jy e_Fp Uncertainty on peak flux
84- 90 F7.3 Jy.km/s FInt ? Integrated flux
92- 98 F7.3 Jy.km/s e_FInt ? Uncertainty on integrated flux
100-103 F4.1 km/s VRW ? Red wing velocity
105-109 F5.1 km/s VBW ? Blue wing velocity
111-115 F5.1 km/s WVel ? Velocity width
117-119 F3.1 km/s e_WVel ? Uncertainty on velocity width
121-125 F5.2 arcsec r ? Emission radius
127-129 A3 --- Notes [abcd, ] Notes (1)
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Note (1): Notes as follows:
a = Line has no measured emission radius (emission radii are measured from
3σ contours in the integrated intensity maps; see Section 2.2 for
more details), so the given value is an upper limit equal to bmaj/2.
b = Line is blended, so only a peak flux value is given.
c = Line is at the edge of a band, so only a peak flux value is given.
d = Line is in absorption, so no value is given for the emission radius and
the given peak flux is the positive or negative extremum
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Acknowledgements:
Sofia Wallstrom, sofia.wallstrom(at)kuleuven.be
References:
Homan et al., 2020A&A...644A..61H 2020A&A...644A..61H
Homan et al., 2021A&A...651A..82H 2021A&A...651A..82H
Danilovich et al., 2021A&A...655A..80D 2021A&A...655A..80D
Gottlieb et al., 2022A&A...660A..94G 2022A&A...660A..94G
Montarges et al., 2023A&A...671A..96M 2023A&A...671A..96M, Cat. J/A+A/671/A86
Baudry et al., 2023A&A...674A.125B 2023A&A...674A.125B
(End) Patricia Vannier [CDS] 13-Nov-2023