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Light curve selection: 1.Select shortest cadence 2.Select latest sector 0 -15 -30 -45 210 15° 240 270 Galactic Longitude 300 Target Galactic Latitude δ Scuti candidate Save maximum SNR frequency as LombScargle Periodogram Crossmatched with Gaia DR3 query: L = [3, 33] L , T = [6500, 9000] K, G ≤ 16 ⊙ eff ν as R and logg Estimator max Pulsation Constant Distribution Surface gravity from Gaia against the maximum SNR frequency. Color code is the same as in Fig. 3. Confirmed δ Scuti as per Gaia or VSX within PLR were fitted to the red line, with a R =0.67. 2 Targets obtained from TESS Input Catalogue (TIC) located within PLATO first field of view: LOPS2. Constraining stellar parmeters to range T = [6500K, 9000K], logg = [3.5-4.2]dex and magnitude V≤16, we found 281,232 targets. Thus, they are in the same region as δ Scuti in the HR Diagram and may be observed by PLATO. eff CONCLUSION: Camino Mesa, Carlos C. , García Hernández, A., Suárez, J. C. and Mirouh, G. M. *1 [email protected]1 yes Gaia luminosity as a function of the maximum SNR frequency derived from TESS light curves. The dashed lines indicate the boundaries of the most densely populated region around the central PLR from García Hernández et al. (2024). δ Scuti Selection Criteria Acknowledgements &References Radius from Gaia against the maximum SNR frequency. Filled symbols represent δ Scuti Candidates confirmed by Gaia or listed in VSX. Green markers represent δ Scuti candidates (whether confirmed or not) located within PLR central region determined in Fig. 2 and blue indicates they are above PLR. Confirmed δ Scuti as per Gaia or VSX within PLR were fitted to the red line, with a R =0.73. 2 Pulsation constant (Q) distribution for TESS (left panel) and Gaia (right panel) parameters. For both samples, Q was calculated using mean density, following Aerts et al. (2010), and using L, logg and Teff (Breger, 1990). These two methods leads to the same distribution as shown here. Red dashed lines represent fundamental radial mode (F), first (1), second (2) and third (3) overtone. For stars confirmed as δ Scuti variables by Gaia or listed in the VSX, and which dominant (maximum-SNR) pulsation frequency follows the Period–Luminosity Relation (Fig. 2), we found this frequency scales with surface gravity (Fig. 4) and radius (Fig. 3), using both Gaia and TESS-derived parameters. The dominant mode corresponds predominantly to the fundamental radial mode for δ Scuti stars on the PLR, and to the third overtone for those located above it (Fig. 5), in agreement with previous results (Poro, A et al. 2024). Enrich this δ Scuti catalogue with all the prewhitened pulsation frequencies identified. Refine the δ Scuti classification, identifying if the target is part of a binary system, hybrid pulsator, HADS, LADS, etc. Extend the catalogue with LOPN1, and provide equilibrium and oscillations models from MESA and FILOU. TESS Sample using T and logg eff CCM acknowledges this poster is part of the grant PID2023-149439NB-C43, funded by MCIU/AEI/10.13039/501100011033 and by the ESF+. AGH and JCS acknowledge support from the project PID2023-149439NB-C43 funded by MICIU/AEI/10.13039/501100011033 and by FEDER, UE. GMM acknowledges support from the Junta de Andalucía Emergía program, grant EMEC_2023_00533. R - νmax logg - νmax 10442 confirmed δ Scuti as per Gaia or VSX Nascimbeni, V., Piotto, G., et al (2025). Astronomy & Astrophysics, Volume 694, Id.A313, 19 Pp., 694, A313. https://doi.org/10.1051/0004-6361/202452325 García Hernández, A., Pascual-Granado, J., et al (2024). Proceedings of the International Astronomical Union, 18(S376), 239–249. https://doi.org/10.1017/S1743921323003368 Poro, A., Jafarzadeh, S. J., et al (2024). Research in Astronomy and Astrophysics, 24(2), 025011. https://doi.org/10.1088/1674-4527/AD1B0F Breger, M. (1990). DSSN, 2, 13–16. https://ui.adsabs.harvard.edu/abs/1990DSSN....2...13B/abstract 281,232 stars 48,918 stars 25,171 stars 685,878 stars
