J/A+A/667/A74 Distance catalogue for AGB stars (Andriantsaralaza+, 2022)
Distance estimates for AGB stars from parallax measurements.
Andriantsaralaza M., Ramstedt S., Vlemmings W.H.T, De Beck E.
<Astron. Astrophys. 667, A74 (2022)>
=2022A&A...667A..74A 2022A&A...667A..74A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Stars, giant ; Stars, distances ; Optical
Keywords: stars: AGB and post AGB - stars: distances, parallaxes -
methods: statistical
Abstract:
Estimating the distances to asymptotic giant branch (AGB) stars using
optical measurements of their parallaxes is not straightforward
because of the large uncertainties introduced by their dusty
envelopes, their large angular sizes, and their surface brightness
variability. We compared the parallaxes from Gaia DR3 with parallaxes
measured with maser observations with very long baseline
interferometry (VLBI) to determine a statistical correction factor for
the DR3 parallaxes using a sub-sample of 33 maser-emitting oxygen-rich
nearby AGB stars. We then calculated the distances of a total of about
200 AGB stars in the DEATHSTAR project using a Bayesian statistical
approach on the corrected DR3 parallaxes and a prior based on the
previously determined Galactic distribution of AGB stars. We found
that the derived Gaia distances are associated with significant,
asymmetrical errors for more than 40% of the sources in our sample,
and thus are unreliable for these sources. We performed radiative
transfer modelling of the stellar and dust emission to determine the
luminosity of the sources in the VLBI sub-sample based on the
distances derived from maser parallaxes, and derived a new bolometric
period-luminosity relation for Galactic oxygen-rich Mira variables. A
new distance catalogue based on these results is provided for the
sources in the DEATHSTAR sample.
Description:
The distances presented in this catalogue were estimated in the
following ways. For the AGB stars in the VLBI sample, we estimated the
distances and their errors using the VLBI parallaxes (Type = V),
following a Bayesian approach using the prior based on the Galactic
distribution of AGB stars (AGB prior). For the sources outside the
VLBI sample that have a corrected Gaia DR3 parallax fractional error
below 20%, the best distance estimate is the Gaia DR3 distance
obtained with the AGB prior (Type = G_AGB). For sources with a
corrected Gaia DR3 parallax fractional error above 20%, the distance
was determined using a period-luminosity relation, provided that the
source had a known period and variability type. Our new
period-luminosity relation was used to calculate the distances of the
Miras (Type=PL(M) for periods between 276 and 514, PL(M_out) for
periods outside that range), while the relation by Knapp et al.
(2003A&A...403..993K 2003A&A...403..993K) was used for the semi-regular variables
(Type=PL(SR)).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 72 201 DEATHSTAR distance catalogue (table C1)
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See also:
J/A+A/640/A133 : DEATHSTAR. Nearby AGB stars with ALMA ACA (Ramstedt+, 2020)
J/A+A/653/A53 : DEATHSTAR. II. The S-type (Andriantsaralaza+, 2021)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Name of the source
17- 20 I4 pc rmed Best distance estimate
22- 24 I3 pc e_rmed Lower uncertainty on the distance
26- 28 I3 pc E_rmed Upper uncertainty on the distance
30- 38 A9 --- Type Type of distance based on the distance
determination method (1)
40- 44 A5 --- SpType Spectral type of the source
46- 47 I2 h RAh Right ascension (J2000)
49- 50 I2 min RAm Right ascension (J2000)
52- 58 F7.4 s RAs Right ascension (J2000)
60 A1 --- DE- Declination sign (J2000)
61- 62 I2 deg DEd Declination (J2000)
64- 65 I2 arcmin DEm Declination (J2000)
67- 72 F6.3 arcsec DEs Declination (J2000)
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Note (1): Type of distance as follows:
V = estimated the distances and their errors using the VLBI parallaxes
G_AGB = best distance estimate is the Gaia DR3 distance obtained with
the AGB prior
PL(M) = new period-luminosity relation was used to calculate the distances
of the Miras for periods between 276 and 514
PL(M_out) = new period-luminosity relation was used to calculate the distances
of the Miras for periods outside 276-514 range
PL(SR:) = relation by Knapp et al. (2003A&A...403..993K 2003A&A...403..993K) used for the
semi-regular variables
PL(SRa) = relation by Knapp et al. (2003A&A...403..993K 2003A&A...403..993K) used for the
semi-regular variables
PL(SRb) = relation by Knapp et al. (2003A&A...403..993K 2003A&A...403..993K) used for the
semi-regular variables
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Acknowledgements:
Miora Andriantsaralaza, miora.andriantsaralaza(at)physics.uu.se
References:
Knapp et al., 2003A&A...403..993K 2003A&A...403..993K, Reprocessing the Hipparcos data of
evolved stars. III. Revised Hipparcos period-luminosity relationship for
galactic long-period variable stars.
(End) Patricia Vannier [CDS] 07-Sep-2022