J/A+A/699/A115 delta Scuti stars catalog (Guo+, 2025)
Investigating the period-luminosity relations of delta Scuti stars:
A pathway to distance and 3-D dust map inference.
Guo F., Bloom J.S., Wang X., Chen L., Lin J., Chen X., Mo J., Zhang J.,
Yan S., Liu Q., Peng H., Jiang X., Ma X., Xiang D., Li W.
<Astron. Astrophys. 699, A115 (2025)>
=2025A&A...699A.115G 2025A&A...699A.115G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Photometry, infrared ; Photometry, SDSS ;
Stars, distances ; Abundances, [Fe/H]
Keywords: stars: oscillations - stars: variables: delta Scuti - dust, extinction
Abstract:
While δ Scuti stars --- intermediate-mass stars pulsating with
periods <0.3d --- are the most numerous class of κ-mechanism
pulsators in the instability strip, the short periods and small
peak-to-peak amplitudes have left them understudied and unreutilized.
Recently, large-scale time-domain surveys have significantly increased
the number of identified δ Scuti stars, allowing for more
comprehensive investigations into their properties. Notably, the
Tsinghua University-Ma Huateng Telescopes for Survey (TMTS), with
its high-cadence observations at 1-minute intervals, has identified
thousands of δ Scuti stars, greatly expanding the sample of
these short-period pulsating variables.
This study makes use of multiband photometric time-series data to
refine the period-luminosity (P-L) relations of δ Scuti stars
and show how observed P-L relations can be used to simultaneously
infer dust obscuration and distance. Using spectroscopy, we also study
the dependence of the P-L relations on metallicity.
Using the δ Scuti stars from the TMTS catalogs of Periodic
Variable Stars, we cross-matched the dataset with Pan-STARRS1, 2MASS,
and WISE to obtain photometric measurements across optical (g, r, i,
z, and y), near-infrared (J, H, Ks) and mid infrared (W1, W2, W3)
bands, respectively. Parallax data, used as Bayesian priors, were
retrieved from Gaia DR3, and line-of-sight dust extinction priors were
estimated from a three-dimensional dust map. Using PyMC, we performed
a simultaneous determination of the 11-band P-L relations of δ
Scuti stars.
The simultaneous determination of multiband P-L relations of δ
Scuti stars not only yields precise measurements of these relations,
but also greatly improves constraints on the distance moduli and color
excesses, as evidenced by the reduced uncertainties in the posterior
distributions. Furthermore, our methodology enables an independent
estimation of the color excess through the P-L relations, offering a
potential complement to existing 3-D dust maps. Moreover, by
cross-matching with LAMOST DR7, we investigated the influence of
metallicity on the P-L relations. Our analysis reveals that
incorporating metallicity might reduce the intrinsic scatter at longer
wavelengths. However, this result does not achieve 3σ
significance, leaving open the possibility that the observed reduction
is attributable to statistical fluctuations.
We introduced an innovative approach to studying the P-L relations of
δ Scuti stars, facilitating more comprehensive investigations
into their utility as distance indicators and their significance in
understanding stellar evolution. Our extensible methodology also
enables the inference of dust extinction using pulsating stars beyond
δ Scuti stars. Although the inclusion of metallicity in the P-L
relations appears to reduce intrinsic scatter at longer wavelengths,
further analysis is required to fully understand the impact of metal
abundance on properties of δ Scuti stars.
Description:
With a cadence of 1 minute, the TMTS has proven to be a powerful tool
for identifying short-period variable stars. Leveraging the dataset of
1864 fundamental mode δ Scuti stars from the TMTS catalogs of
Periodic Variable Stars, we developed an innovative methodology to
simultaneously determine the multiband P-L relations of these
pulsators. By cross-matching TMTS sources with Pan-STARRS1, 2MASS, and
WISE for optical and infrared photometry, our approach has achieved
highly precise P-L relations spanning multiple photometric bands.
Additionally, this methodology facilitates the refinement of the
distance modulus and color excess within the posterior distribution.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 293 1236 Photometric, spectroscopic, and distance inputs
to the model
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See also:
V/156 : LAMOST DR7 catalogs (Luo+, 2019)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+, 2016)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Type Type of the variable
6- 26 A21 --- Name TMTS identifier (TMTSJHHMMSSss+DDMMSss)
28- 39 F12.8 deg RAdeg Right Ascension (J2000)
41- 53 F13.9 deg DEdeg Declination (J2000)
55- 65 F11.9 h Per Period
67- 78 F12.9 mag MOD Distance modulus from Gaia DR3
80- 90 F11.9 mag e_MOD Error of distance modulus
92-103 F12.9 --- [Fe/H] ? [Fe/H] from Lamost
105-115 F11.9 --- e_[Fe/H] ? Error of [Fe/H]
117-127 F11.9 mag E(B-V) Line-of-sight color excess
130-140 F11.9 mag e_E(B-V) Error of color excess
142-148 F7.4 mag gmag ? g band apparent magnitude from Pan-STARRS1 (AB)
150-155 F6.4 mag e_gmag ? Error of g band apparent magnitude (AB)
157-163 F7.4 mag rmag ? r band apparent magnitude from Pan-STARRS1 (AB)
165-170 F6.4 mag e_rmag ? Error of r band apparent magnitude (AB)
172-178 F7.4 mag imag ? i band apparent magnitude from Pan-STARRS1 (AB)
180-185 F6.4 mag e_imag ? Error of i band apparent magnitude (AB)
187-193 F7.4 mag zmag ? z band apparent magnitude from Pan-STARRS1 (AB)
195-200 F6.4 mag e_zmag ? Error of z band apparent magnitude (AB)
202-208 F7.4 mag ymag ? y band apparent magnitude from Pan-STARRS1 (AB)
210-215 F6.4 mag e_ymag ? Error of y band apparent magnitude (AB)
217-222 F6.3 mag Jmag ? J band apparent magnitude from 2MASS
224-228 F5.3 mag e_Jmag ? Error of J band apparent magnitude
230-235 F6.3 mag Hmag ? H band apparent magnitude from 2MASS
237-241 F5.3 mag e_Hmag ? Error of H band apparent magnitude
243-248 F6.3 mag Ksmag ? Ks band apparent magnitude from 2MASS
250-254 F5.3 mag e_Ksmag ? Error of Ks band apparent magnitude
256-261 F6.3 mag W1mag ? W1 band apparent magnitude from WISE
263-267 F5.3 mag e_W1mag ? Error of W1 band apparent magnitude
269-274 F6.3 mag W2mag ? W2 band apparent magnitude from WISE
276-280 F5.3 mag e_W2mag ? Error of W2 band apparent magnitude
282-287 F6.3 mag W3mag ? W3 band apparent magnitude from WISE
289-293 F5.3 mag e_W3mag ? Error of W3 band apparent magnitude
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Acknowledgements:
Fangzhou Guo, fangzhou.guo98(at)gmail.com
(End) Patricia Vannier [CDS] 24-Jun-2025