J/A+A/660/A94 Observational properties of the ATOMIUM project (Gottlieb+, 2022)
ATOMIUM: ALMA tracing the origins of molecules in dust forming oxygen rich
M-type stars. Motivation, sample, calibration, and initial results.
Gottlieb C.A., Decin L., Richards A.M.S., De Ceuster F., Homan W.,
Wallstrom S.H.J., Danilovich T., Millar T.J., Montarges M., Wong K.T.,
Mcdonald I., Baudry A., Bolte J., Cannon E., De Beck E., De Koter A.,
El Mellah I., Etoka S., Gobrecht D., Gray M., Herpin F., Jeste M.,
Kervella P., Khouri T., Lagadec E., Maes S., Malfait J., Menten K.M.,
Muller H.S.P., Pimpanuwat B., Plane J.M.C., Sahai R., Van De Sande M.,
Waters L.B.F.M., Yates J., Zijlstra A.
<Astron. Astrophys., 660, A94 (2022)>
=2022A&A...660A..94G 2022A&A...660A..94G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, M-type ; Stars, giant
Keywords: stars: AGB and post-AGB - stars: mass-loss - circumstellar matter -
binaries: general - instrumentation: interferometers - astrochemistry
Abstract:
This overview paper presents ATOMIUM, a Large Programme in Cycle 6
with the Atacama Large Millimeter/submillimeter Array (ALMA). The goal
of ATOMIUM is to understand the dynamics and the gas phase and dust
formation chemistry in the winds of evolved asymptotic giant branch
(AGB) and red supergiant (RSG) stars. A more general aim is to
identify chemical processes applicable to other astrophysical
environments. Seventeen oxygen-rich AGB and RSG stars spanning a range
in (circum)stellar parameters and evolutionary phases were observed in
a homogeneous observing strategy allowing for an unambiguous
comparison. Data were obtained between 213.83 and 269.71 GHz at high
(∼0.025''-0.050''), medium (∼0.13''-0.24''), and low (∼1'') angular
resolution. The sensitivity per ∼1.3 km s-1 channel was 1.5-5 mJy
beam-1, and the line-free channels were used to image the millimetre
wave continuum. Our primary molecules for studying the gas dynamics
and dust formation are CO, SiO, AlO, AlOH, TiO, TiO2, and HCN;
secondary molecules include SO, SO2, SiS, CS, H2O, and NaCl. The
scientific motivation, survey design, sample properties, data
reduction, and an overview of the data products are described. In
addition, we highlight one scientific result - the wind kinematics of
the ATOMIUM sources. Our analysis suggests that the ATOMIUM sources
often have a slow wind acceleration, and a fraction of the gas reaches
a velocity which can be up to a factor of two times larger than
previously reported terminal velocities assuming isotropic expansion.
Moreover, the wind kinematic profiles establish that the radial
velocity described by the momentum equation for a spherical wind
structure cannot capture the complexity of the velocity field. In
fifteen sources, some molecular transitions other than 12CO v=0
J=2-1 reach a higher outflow velocity, with a spatial emission zone
that is often greater than 30 stellar radii, but much less than the
extent of CO. We propose that a binary interaction with a (sub)stellar
companion may (partly) explain the non-monotonic behaviour of the
projected velocity field. The ATOMIUM data hence provide a crucial
benchmark for the wind dynamics of evolved stars in single and binary
star models.
Description:
The ALMA ATOMIUM
(https://fys.kuleuven.be/ster/research-projects/aerosol/atomium/atomium)
Large Programme has been constructed with the specific aim of
understanding the chemistry of dust precursors and dust formation, as
well as the more general aim of identifying chemical processes
applicable to other astrophysical environments (including novae,
supernovae, protoplanetary nebulae, and interstellar shocks).
Here the list of observational properties of the ATOMIUM project
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablee1.dat 117 215 Observational properties of the ATOMIUM project
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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: tablee1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- SB Scheduling Block designation
18 A1 --- n_SB [*] Note on SB (1)
20- 27 A8 --- Config Array configuration
29- 38 A10 --- Source Phase-reference source
40- 41 I2 h RAh Phase-reference source right ascension (ICRS)
43- 44 I2 min RAm Phase-reference source right ascension (ICRS)
46- 54 F9.6 s RAs Phase-reference source right ascension (ICRS)
56 A1 --- DE- Phase-reference source declination sign (ICRS)
57- 58 I2 deg DEd Phase-reference source declination (ICRS)
60- 61 I2 arcmin DEm Phase-reference source declination (ICRS)
63- 70 F8.5 arcsec DEs Phase-reference source declination (ICRS)
72- 76 F5.2 deg Sep Separation between the target and the
phase-reference source
78- 80 F3.1 mm PWV Precipitable water vapour at the date of
the observations (2)
82- 91 A10 "date" Date End date of observation
93-117 A25 --- ASDM ALMA archival name
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Note (1): Owing to initial inconsistent capitalisation, SG marked * were
originally named as follows: pi1grua06TM1, pi1grub06TM1,
vxsgra06TM1, vxsgrb06TM1, Tmica06TM1, Tmicb06TM1.
The SG were subsequently renamed as indicated below in our data products.
Note (2): The PWV values are for the start of each night and vary (usually by
only 10% or less) during observations.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 24-Aug-2022