J/MNRAS/493/2996 Characterization of LMC M-stars in the JWST era (Marini+, 2020)
Characterization of M-stars in the LMC in the JWST era.
Marini E., Dell'Agli F., Di Criscienzo M., Garcia-Hernandez D.A.,
Ventura P., Groenewegen M.A.T., Mattsson L., Kamath D., Puccetti S.,
Tailo M., Villaver E.
<Mon. Not. R. Astron. Soc., 493, 2996-3013 (2020)>
=2020MNRAS.493.2996M 2020MNRAS.493.2996M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, giant ; Stars, late-type ; Magellanic Clouds ;
Abundances, peculiar ; Infrared
Keywords: stars: abundances - stars: AGB and post-AGB - Magellanic Clouds
Abstract:
We study the M-type asymptotic giant branch (AGB) population of the
Large Magellanic Cloud (LMC) by characterizing the individual sources
in terms of the main properties of the progenitors and of the dust
present in the circumstellar envelope. To this aim we compare the
combination of the spectroscopic and photometric data collected by
Spitzer, complemented by additional photometric results available in
the literature, with results from AGB modelling that include the
description of dust formation in the wind. To allow the interpretation
of a paucity stars likely evolving through the post-AGB phase, we
extended the available evolutionary sequences to reach the PN phase.
The main motivation of the present analysis is to prepare the future
observations of the evolved stellar populations of Local Group
galaxies that will be done by the James Webb Space Telescope (JWST),
by identifying the combination of filters that will maximize the
possibilities of characterizing the observed sources. The present
results show that for the M-star case the best planes to be used for
this purpose are the colour magnitude ([F770W]-[F2550W], [F770W]) and
(KS-[F770W], [F770W]) planes. In these observational diagrams the
sequences of low-mass stars evolving in the AGB phases before the
achievement of the C-star stage and of massive AGBs experiencing hot
bottom burning are clearly separated and peculiar sources, such as
post-AGB, dual-dust chemistry, and iron-dust stars can be easily
identified.
Description:
In this paper we use the LMC sample of 71 O-rich AGB spectra, observed
using Spitzer IRS (Jones et al. 2012MNRAS.427.3209J 2012MNRAS.427.3209J, Cat.
J/MNRAS/427/3209) and classified according to the decision-tree scheme
proposed by Woods et al. (2011MNRAS.411.1597W 2011MNRAS.411.1597W, Cat. J/MNRAS/411/1597).
The sample includes point sources from the SAGE-Spec legacy survey of
the LMC (Kemper et al. 2010PASP..122..683K 2010PASP..122..683K, Cat. J/PASP/122/683), a
spectroscopic follow-up to the SAGE-LMC project (Meixner et al.
2006AJ....132.2268M 2006AJ....132.2268M, Cat. J/AJ/132/2268) and has been supplemented
from archival Spitzer IRS observation within the SAGE-LMC footprint
(Woods et al. 2011MNRAS.411.1597W 2011MNRAS.411.1597W, Cat. J/MNRAS/411/1597). The
detailed description of the original target selection, the observing
strategy, and the techniques used in the data reduction for the
SAGE-Spec legacy programme are discussed in Kemper et al. (Kemper et
al. 2010PASP..122..683K 2010PASP..122..683K, Cat. J/PASP/122/683).
The list of the stars analysed in this work is reported in Table 2.
When available, in column 3 we report the primary periods obtained by
the OGLE collaboration (Soszynski et al. 2009AcA....59..239S 2009AcA....59..239S, Cat.
J/AcA/59/239), that phases well the temporal sequence of observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 90 62 The summary of the overall interpretation of the
LMC sources analysed in this work, including the
interpretation by Groenewegen & Sloan
(2018A&A...609A.114G 2018A&A...609A.114G, Cat. J/A+A/609/A114)
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See also:
J/A+A/609/A114 : Local Group AGB stars and red supergiants
(Groenewegen+, 2018)
J/MNRAS/427/3209 : Galactic and MC O-AGBs and RSGs stars (Jones+, 2012)
J/MNRAS/440/631 : IR photometry of LMC O-rich evolved stars (Jones+, 2014)
J/PASP/122/683 : SAGE-Spec Spitzer legacy program (Kemper+, 2010)
J/MNRAS/411/1597 : LMC point source classification in SAGE-Spec (Woods+, 2011)
J/AcA/59/239 : VI light curves of LMC long-period variables
(Soszynski+, 2009)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- SSID [1/4791] Unique spectral identification number
6- 11 F6.3 deg RAdeg Right ascension (J2000)
13- 19 F7.3 deg DEdeg Declination (J2000)
21- 24 I4 d Period ? OGLE period
26- 30 I5 Lsun L Luminosity of the source derived in this paper
32- 34 I3 % Sil ? Percentage of silicate grains derived in
this paper
36- 37 I2 % Al2O3 ? Percentage of alumina dust derived in this
paper
39- 40 I2 % Fe ? Percentage of solid iron derived in this
paper
42- 46 F5.3 --- tau10e ? Optical depth at 10 micron of the external,
oxygen-rich layer
48- 50 I3 % C ? Percentage of solid carbon derived in this
paper
52- 53 I2 % SiC ? Percentage of silicon carbide derived in
this paper
55- 59 F5.3 --- tau10i ? Optical depth at 10 micron of the internal,
carbon-rich layer
61- 74 A14 --- Type Evolutionary characterization determined in
this work
76- 80 I5 Lsun LGS18 ? Luminosity of the source determined in
Groenewegen & Sloan (2018A&A...609A.114G 2018A&A...609A.114G,
Cat. J/A+A/609/A114)
82- 84 I3 % SilGS18 ? Percentage of olivine (MgFeSiO4)
determined in Groenewegen & Sloan
(2018A&A...609A.114G 2018A&A...609A.114G, Cat. J/A+A/609/A114)
86- 87 I2 % Al2O3GS18 ? Percentage of corundum (Al2O3)
determined in Groenewegen & Sloan
(2018A&A...609A.114G 2018A&A...609A.114G, Cat. J/A+A/609/A114)
89- 90 I2 % FeGS18 ? Percentage of metallic iron determined in
Groenewegen & Sloan (2018A&A...609A.114G 2018A&A...609A.114G,
Cat. J/A+A/609/A114)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 20-Apr-2023