J/A+A/659/A167 Cepheid Period-Wesenheit-Metallicity relation (Ripepi+, 2022)
Classical Cepheid period-Wesenheit-metallicity relation in the Gaia bands.
Ripepi V., Catanzaro G., Clementini G., De Somma G., Drimmel R., Leccia S.,
Marconi M., Molinaro R., Musella I., Poggio E.
<Astron. Astrophys. 659, A167 (2022)>
=2022A&A...659A.167R 2022A&A...659A.167R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Abundances, [Fe/H] ; Stars, distances ;
Parallaxes, trigonometric ; Photometry ; Milky Way
Keywords: stars: variables: Cepheids - stars: distances - Galaxy: disk -
Galaxy: abundances
Abstract:
Classical Cepheids (DCEPs) represent a fundamental tool to calibrate
the extragalactic distance scale. However, they are also powerful
stellar population tracers, in the context of Galactic studies. The
forthcoming Data Release 3 (DR3) of the Gaia mission will allow us to
study with unprecedented detail the structure, the dynamics and the
chemical properties of the Galactic disc, and in particular of the
spiral arms, where most Galactic DCEPs reside.
In this paper we aim at quantifying the metallicity dependence of the
Galactic DCEPs Period-Wesenheit (PWZ) relation in the Gaia bands. We
adopt a sample of 499 DCEPs with metal abundances from high-resolution
spectroscopy, in conjunction with Gaia Early Data Release 3 parallaxes
and photometry to calibrate a PWZ relation in the Gaia bands.
We find a significant metallicity term, of the order of -0.5mag/dex,
which is larger than the values measured in the NIR bands by different
authors. Our best PWZ relation is
W=(-5.988±0.018)-(3.176±0.044)(logP-1.0)-(0.520±0.090)[Fe/H].
We validate our PWZ relations by using the distance to the Large
Magellanic Cloud as a benchmark, finding a very good agreement with
the geometric distance provided by eclipsing binaries. As an
additional test, we evaluate the metallicity gradient of the young
Galactic disc, finding -0.0527±0.0022dex/kpc, in very good agreement
with previous results.
Description:
Classical Cepheid sample adopted in the paper. The Table reports the
all the data used in the calculation of the
Period-Wesenheit-Metallicity relation in the Gaia bands. See below for
more details.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 147 499 Data used in this paper
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See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
J/A+A/566/A37 : Iron abundances for 42 Galactic Cepheids (Genovali+, 2014)
J/A+A/605/A79 : TGAS Cepheids and RR Lyrae stars (Gaia Collaboration+, 2017)
J/A+A/619/A8 : Cepheid period-luminosity-metallicity relation
(Groenewegen, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaEDR3 Gaia EDR3 identification source_id
21- 46 A26 --- Name Other name
48- 57 F10.6 deg RAdeg Right Ascension (J2000)
59- 68 F10.6 deg DEdeg Declination (J2000)
70- 79 A10 --- Mode Mode of pulsation (1)
81- 89 F9.6 d Per Period of pulsation (2)
91- 96 F6.3 mag Gmag Magnitude in the Gaia G band
98-102 F5.3 mag GBP-GRP Colour in the Gaia GBP-GRP bands
104-110 F7.4 mas plx Original parallax value from GaiaEDR3 catalogue
112-117 F6.4 mas e_plx Error on the original parallax value from
GaiaEDR3 catalogue
119-124 F6.4 mas plxcorr Parallax value corrected according to
Lindegren et al. (2021A&A...649A...4L 2021A&A...649A...4L)
126-131 F6.3 --- RUWE Re-normalised unit weight error from
GaiaEDR3 catalogue
133-137 F5.2 [-] [Fe/H] Adopted iron abundance
139-142 F4.2 [-] e_[Fe/H] Error on the adopted iron abundance
144-147 A4 --- r_[Fe/H] Literature source for the iron abundance (3)
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Note (1): F, 1O, F/1O, 1O/2O indicate the fundamental, first overtone and the
mixed mode pulsation modes, respectively.
Note (2): For mixed mode DCEPs the longest period is listed.
Note (3): References as follows:
G14 = Genovali et al. (2014A&A...566A..37G 2014A&A...566A..37G, Cat. J/A+A/566/A37)
GC17 = Gaia Collaboration et al. (2017A&A...605A..79G 2017A&A...605A..79G, Cat. J/A+A/605/A79)
G18 = Groenewegen (2018A&A...619A...8G 2018A&A...619A...8G. Cat. J/A+A/619/A8)
R21 = Ripepi et al. (2021MNRAS.508.4047R 2021MNRAS.508.4047R)
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Acknowledgements:
Vincenzo Ripepi, vincenzo.ripepi(at)inaf.it
(End) Patricia Vannier [CDS] 06-Jan-2022