J/A+A/592/A42 A study of dust nucleation in Mira. Part I. (Kaminski+, 2016)
An observational study of dust nucleation in Mira (o Ceti).
I. Variable features of AlO and of other Al-bearing species.
Kaminski T., Wong K.T., Schmidt M.R., Mueller H.S.P., Gottlieb C.A.,
Cherchneff I., Menten K.M., Keller D., Brunken S., Winters J.M., Patel N.A.
<Astron. Astrophys. 592, A42 (2016)>
=2016A&A...592A..42K 2016A&A...592A..42K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, emission ; Stars, M-type ; Radio lines ; Mass loss
Keywords: stars: AGB and post-AGB - stars: mass-loss - circumstellar matter -
submillimeter: stars - astrochemistry
Abstract:
Dust is efficiently produced by cool giant stars, but the condensation
of inorganic dust is poorly understood. Observations of key aluminum
bearing molecules around evolved stars has enabled us to investigate
the nucleation of alumina (Al2O3) dust in the gas. Aims. We aim to
identify and characterize aluminum bearing species in the
circumstellar gas of Mira (o Ceti) in order to elucidate their role in
the production of Al2O3 dust.
We used multiepoch spectral line observations at (sub-)millimeter,
far-infrared, and optical wavelengths including: maps with ALMA that
probe the gas distribution in the immediate vicinity of the star at
∼30mas; observations with ALMA, APEX, and Herschel in 2013-2015 for
studying cycle and inter-cycle variability of the rotational lines of
Al-bearing molecules; optical records as far back as 1965 to examine
variations in electronic transitions over time spans of days to
decades; and velocity measurements and excitation analysis of the
spectral features that constrain the physical parameters of the gas.
Description:
Files contain ALMA observations of AlO emission in Mira (omicron Ceti)
in two rotational transitions, N=6-5 and 9-8, and obtained at
different epochs. Spectral cubes, moment-zero maps, and spectra of the
entire emission source are provided and correspond directly to those
presented in the paper (Figs. 2, 3, and 5). Complementary continuum
data are also included in separate files.
The data were self-calibrated and therefore their absolute astrometry
is inaccurate. Relative spatial coordinates should be used.
Objects:
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RA (2000) DE Designation(s)
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02 19 20.79 -02 58 39.5 Mira = * omi Cet
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 187 13 List of fits files
fits/* . 13 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 pixels along Z-axis
34- 59 A26 --- Obs.date Observation date (YYYY-MM-DDThh:mm:ss.sssss)
61- 67 F7.3 GHz bFreq Frequency or lower value of frequency interval
69- 75 F7.3 GHz BFreq ? Upper value of frequency interval
77- 87 E11.6 Hz dFreq ? Frequency resolution
89- 95 I7 Kibyte size Size of FITS file
97-108 A12 --- FileName Name of FITS file, in subdirectory fits
109-110 A2 --- sp Link to generate the spectrum
112-187 A76 --- Title Title of the FITS file
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Acknowledgements:
Tomasz Kaminski, tkaminsk(at)eso.org
(End) Patricia Vannier [CDS] 06-Jul-2016