Gaia Data Release 3: Pulsations in main sequence OBAF-type stars. (arXiv:2206.06075v1 [astro-ph.SR])

Gaia Data Release 3: Pulsations in main sequence OBAF-type stars. (arXiv:2206.06075v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Gaia/0/1/0/all/0/1">Gaia Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Gaia/0/1/0/all/0/1">Gaia Collaboration</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ridder_J/0/1/0/all/0/1">J. De Ridder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ripepi_V/0/1/0/all/0/1">V. Ripepi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aerts_C/0/1/0/all/0/1">C. Aerts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palaversa_L/0/1/0/all/0/1">L. Palaversa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eyer_L/0/1/0/all/0/1">L. Eyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holl_B/0/1/0/all/0/1">B. Holl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Audard_M/0/1/0/all/0/1">M. Audard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rimoldini_L/0/1/0/all/0/1">L. Rimoldini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_A/0/1/0/all/0/1">A.G.A. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vallenari_A/0/1/0/all/0/1">A. Vallenari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prusti_T/0/1/0/all/0/1">T. Prusti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruijne_J/0/1/0/all/0/1">J.H.J. de Bruijne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arenou_F/0/1/0/all/0/1">F. Arenou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Babusiaux_C/0/1/0/all/0/1">C. Babusiaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biermann_M/0/1/0/all/0/1">M. Biermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Creevey_O/0/1/0/all/0/1">O.L. Creevey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ducourant_C/0/1/0/all/0/1">C. Ducourant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_D/0/1/0/all/0/1">D.W. Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerra_R/0/1/0/all/0/1">R. Guerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hutton_A/0/1/0/all/0/1">A. Hutton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jordi_C/0/1/0/all/0/1">C. Jordi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klioner_S/0/1/0/all/0/1">S.A. Klioner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lammers_U/0/1/0/all/0/1">U.L. Lammers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lindegren_L/0/1/0/all/0/1">L. Lindegren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luri_X/0/1/0/all/0/1">X. Luri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mignard_F/0/1/0/all/0/1">F. Mignard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Panem_C/0/1/0/all/0/1">C. Panem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pourbaix_D/0/1/0/all/0/1">D. Pourbaix</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Randich_S/0/1/0/all/0/1">S. Randich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sartoretti_P/0/1/0/all/0/1">P. Sartoretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soubiran_C/0/1/0/all/0/1">C. Soubiran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanga_P/0/1/0/all/0/1">P. Tanga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walton_N/0/1/0/all/0/1">N.A. Walton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailer_Jones_C/0/1/0/all/0/1">C.A.L. Bailer-Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bastian_U/0/1/0/all/0/1">U. Bastian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drimmel_R/0/1/0/all/0/1">R. Drimmel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jansen_F/0/1/0/all/0/1">F. Jansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katz_D/0/1/0/all/0/1">D. Katz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lattanzi_M/0/1/0/all/0/1">M.G. Lattanzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leeuwen_F/0/1/0/all/0/1">F. van Leeuwen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakker_J/0/1/0/all/0/1">J. Bakker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cacciari_C/0/1/0/all/0/1">C. Cacciari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castaneda_J/0/1/0/all/0/1">J. Castañeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angeli_F/0/1/0/all/0/1">F. De Angeli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabricius_C/0/1/0/all/0/1">C. Fabricius</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fouesneau_M/0/1/0/all/0/1">M. Fouesneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fremat_Y/0/1/0/all/0/1">Y. Frémat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galluccio_L/0/1/0/all/0/1">L. Galluccio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerrier_A/0/1/0/all/0/1">A. Guerrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heiter_U/0/1/0/all/0/1">U. Heiter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masana_E/0/1/0/all/0/1">E. Masana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Messineo_R/0/1/0/all/0/1">R. Messineo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mowlavi_N/0/1/0/all/0/1">N. Mowlavi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nicolas_C/0/1/0/all/0/1">C. Nicolas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nienartowicz_K/0/1/0/all/0/1">K. Nienartowicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pailler_F/0/1/0/all/0/1">F. Pailler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Panuzzo_P/0/1/0/all/0/1">P. Panuzzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riclet_F/0/1/0/all/0/1">F. Riclet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roux_W/0/1/0/all/0/1">W. Roux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seabroke_G/0/1/0/all/0/1">G.M. Seabroke</a>, et al. (387 additional authors not shown)

The third Gaia data release provides photometric time series covering 34
months for about 10 million stars. For many of those stars, a characterisation
in Fourier space and their variability classification are also provided. This
paper focuses on intermediate- to high-mass (IHM) main sequence pulsators M >=
1.3 Msun) of spectral types O, B, A, or F, known as beta Cep, slowly pulsating
B (SPB), delta Sct, and gamma Dor stars. These stars are often multi-periodic
and display low amplitudes, making them challenging targets to analyse with
sparse time series. All datasets used in this analysis are part of the Gaia DR3
data release. The photometric time series were used to perform a Fourier
analysis, while the global astrophysical parameters necessary for the empirical
instability strips were taken from the Gaia DR3 gspphot tables, and the vsini
data were taken from the Gaia DR3 esphs tables. We show that for nearby
OBAF-type pulsators, the Gaia DR3 data are precise and accurate enough to
pinpoint them in the Hertzsprung-Russell diagram. We find empirical instability
strips covering broader regions than theoretically predicted. In particular,
our study reveals the presence of fast rotating gravity-mode pulsators outside
the strips, as well as the co-existence of rotationally modulated variables
inside the strips as reported before in the literature. We derive an extensive
period-luminosity relation for delta Sct stars and provide evidence that the
relation features different regimes depending on the oscillation period.
Finally, we demonstrate how stellar rotation attenuates the amplitude of the
dominant oscillation mode of delta Sct stars.

http://arxiv.org/icons/sfx.gif