J/A+A/640/A113 Cepheids flux weighted gravity-luminosity (Groenewegen, 2020)
The flux weighted gravity-luminosity relation of Galactic Classical Cepheids.
Groenewegen M.A.T
<Astron. Astrophys. 640, A113 (2020)>
=2020A&A...640A.113G 2020A&A...640A.113G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Stars, distances
Keywords: stars: distances - stars: fundamental parameters -
stars: variables: Cepheids
Abstract:
The flux-weighted gravity-luminosity relation (FWGLR) is investigated
for a sample of 477 classical Cepheids (CCs), including stars that
have been classified in the literature as such but are probably not.
The luminosities are taken from the literature, based on the fitting
of the spectral energy distributions (SEDs) assuming a certain
distance and reddening. The flux-weighted gravity (FWG) is taken from
gravity and effective temperature determinations in the literature
based on high-resolution spectroscopy.
There is a very good agreement between the theoretically predicted and
observed FWG versus pulsation period relation that could serve in
estimating the FWG (and logg) in spectroscopic studies with a
precision of 0.1dex.
As was known in the literature, the theoretically predicted FWGLR
relation for CCs is very tight and not very sensitive to metallicity
(at least for LMC and Solar values), rotation rate and crossing of the
instability strip. The observed relation has a slightly different
slope and shows more scatter (0.54dex). This is due both to
uncertainties in the distances and the pulsation phase averaged FWG
values.
Data from future Gaia data releases should reduce these errors, and
then the FWGLR could serve as a powerful tool in Cepheid studies.
Description:
The tabular material describes the fundamental parameters and
flux-weighted gravity for the entire sample.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea3.dat 88 477 FWG data for the entire sample
--------------------------------------------------------------------------------
See also:
J/A+A/635/A33 : Galactic classical Cepheids Per-Lbol-Rad (Groenewegen, 2020)
Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name The variable star name
16- 23 A8 --- Type The classification of the variability (1)
25- 30 F6.3 d Per The pulsation period (1)
32- 37 F6.3 kpc d The distance (1)
39- 43 F5.3 kpc e_d The error in the distance (1)
45- 52 F8.1 Lsun Lum The stellar luminosity (1)
54- 60 F7.1 Lsun e_Lum The error in the stellar luminosity (1)
62- 63 I2 --- Nspec Number of available stellar spectra
65- 69 F5.3 --- FWG The average of the available flux weighted
gravity (FWG) values
71- 74 F4.2 --- e_FWG The error in the FWG values
76- 79 F4.2 --- DeltaFWG The difference between largest and smallest
FWG value
81- 88 A8 --- Ref References for logg and Teff values used
to calculate the FWG (2)
--------------------------------------------------------------------------------
Note (1): From Groenewegen, 2020, Cat. J/A+A/635/A33
Note (2): Numbers between parenthesis indicate references not considered.
References as follows:
1 = Luck. 2018AJ....156..171L 2018AJ....156..171L. Cat. J/AJ/156/171
2 = Andrievsky et al.. 1994A&A...281..465A 1994A&A...281..465A, Cat. J/A+A/281/465
3 = Boyarchuk & Lyubimkov, 1981IzKry..64....3B 1981IzKry..64....3B
4 = Luck et al., 2003A&A...401..939L 2003A&A...401..939L
5 = Schmidt et al., 2011AJ....141...53S 2011AJ....141...53S, Cat. J/AJ/141/53
6 = Andrievsky et al.. 2002A&A...392..491A 2002A&A...392..491A, Cat. J/A+A/392/491
7 = Lemasle et al., 2008A&A...490..613L 2008A&A...490..613L
8 = Andrievsky et al., 2013MNRAS.428.3252A 2013MNRAS.428.3252A, Cat. J/MNRAS/428/3252
9 = Kovtyukh et al., 2005PASP..117.1173K 2005PASP..117.1173K
10 = Luck et al., 2006AJ....132..902L 2006AJ....132..902L, Cat. J/AJ/132/902
11 = Yong et al., 2006AJ....131.2256Y 2006AJ....131.2256Y
12 = Lemasle et al., 2015A&A...579A..47L 2015A&A...579A..47L
13 = Romaniello et al., 2008A&A...488..731R 2008A&A...488..731R
14 = Andrievsky et al., 2004A&A...413..159A 2004A&A...413..159A, Cat. J/A+A/413/159
15 = Lemasle et al., 2007A&A...467..283L 2007A&A...467..283L
16 = Andrievsky et al., 2002A&A...392..491A 2002A&A...392..491A, Cat. J/A+A/392/491
17 = Genovali et al., 2014A&A...566A..37G 2014A&A...566A..37G, Cat. J/A+A/566/A37
18 = Anders et al., 2019A&A...628A..94A 2019A&A...628A..94A, Cat. I/349
19 = Martin et al., 2015MNRAS.449.4071M 2015MNRAS.449.4071M
20 = Andrievsky et al., 2016MNRAS.461.4256A 2016MNRAS.461.4256A
21 = Inno et al., 2019MNRAS.482...83I 2019MNRAS.482...83I
--------------------------------------------------------------------------------
Acknowledgements:
Martin Groenewegen, marting(at)oma.be
References:
Groenewegen, 2020A&A...635A..33G 2020A&A...635A..33G, Cat. J/A+A/635/A33
(End) Martin Groenewegen [OMA, Belgium], Patricia Vannier [CDS] 24-Jun-2020