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 =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. Cat. J/AJ/156/171 2 = Andrievsky et al.. 1994A&A...281..465A, Cat. J/A+A/281/465 3 = Boyarchuk & Lyubimkov, 1981IzKry..64....3B 4 = Luck et al., 2003A&A...401..939L 5 = Schmidt et al., 2011AJ....141...53S, Cat. J/AJ/141/53 6 = Andrievsky et al.. 2002A&A...392..491A, Cat. J/A+A/392/491 7 = Lemasle et al., 2008A&A...490..613L 8 = Andrievsky et al., 2013MNRAS.428.3252A, Cat. J/MNRAS/428/3252 9 = Kovtyukh et al., 2005PASP..117.1173K 10 = Luck et al., 2006AJ....132..902L, Cat. J/AJ/132/902 11 = Yong et al., 2006AJ....131.2256Y 12 = Lemasle et al., 2015A&A...579A..47L 13 = Romaniello et al., 2008A&A...488..731R 14 = Andrievsky et al., 2004A&A...413..159A, Cat. J/A+A/413/159 15 = Lemasle et al., 2007A&A...467..283L 16 = Andrievsky et al., 2002A&A...392..491A, Cat. J/A+A/392/491 17 = Genovali et al., 2014A&A...566A..37G, Cat. J/A+A/566/A37 18 = Anders et al., 2019A&A...628A..94A, Cat. I/349 19 = Martin et al., 2015MNRAS.449.4071M 20 = Andrievsky et al., 2016MNRAS.461.4256A 21 = Inno et al., 2019MNRAS.482...83I -------------------------------------------------------------------------------- Acknowledgements: Martin Groenewegen, marting(at)oma.be References: Groenewegen, 2020A&A...635A..33G, Cat. J/A+A/635/A33 ================================================================================ (End) Martin Groenewegen [OMA, Belgium], Patricia Vannier [CDS] 24-Jun-2020