Gaia Data Release 3: Mapping the asymmetric disc of the Milky Way. (arXiv:2206.06207v3 [astro-ph.GA] UPDATED)

Gaia Data Release 3: Mapping the asymmetric disc of the Milky Way. (arXiv:2206.06207v3 [astro-ph.GA] UPDATED)
<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:+Drimmel_R/0/1/0/all/0/1">R. Drimmel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_Gomez_M/0/1/0/all/0/1">M. Romero-Gomez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chemin_L/0/1/0/all/0/1">L. Chemin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramos_P/0/1/0/all/0/1">P. Ramos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poggio_E/0/1/0/all/0/1">E. Poggio</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:+Andrae_R/0/1/0/all/0/1">R. Andrae</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blomme_R/0/1/0/all/0/1">R. Blomme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cantat_Gaudin_T/0/1/0/all/0/1">T. Cantat-Gaudin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castro_Ginard_A/0/1/0/all/0/1">A. Castro-Ginard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clementini_G/0/1/0/all/0/1">G. Clementini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Figueras_F/0/1/0/all/0/1">F. Figueras</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. Fremat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jardine_K/0/1/0/all/0/1">K. Jardine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khanna_S/0/1/0/all/0/1">S. Khanna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lobel_A/0/1/0/all/0/1">A. Lobel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_D/0/1/0/all/0/1">D. J. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muraveva_T/0/1/0/all/0/1">T. Muraveva</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:+Eyer_L/0/1/0/all/0/1">L. Eyer</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:+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:+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>, et al. (394 additional authors not shown)

With the most recent Gaia data release the number of sources with complete 6D
phase space information (position and velocity) has increased to well over 33
million stars, while stellar astrophysical parameters are provided for more
than 470 million sources, in addition to the identification of over 11 million
variable stars. Using the astrophysical parameters and variability
classifications provided in Gaia DR3, we select various stellar populations to
explore and identify non-axisymmetric features in the disc of the Milky Way in
both configuration and velocity space. Using more about 580 thousand sources
identified as hot OB stars, together with 988 known open clusters younger than
100 million years, we map the spiral structure associated with star formation
4-5 kpc from the Sun. We select over 2800 Classical Cepheids younger than 200
million years, which show spiral features extending as far as 10 kpc from the
Sun in the outer disc. We also identify more than 8.7 million sources on the
red giant branch (RGB), of which 5.7 million have line-of-sight velocities,
allowing the velocity field of the Milky Way to be mapped as far as 8 kpc from
the Sun, including the inner disc. The spiral structure revealed by the young
populations is consistent with recent results using Gaia EDR3 astrometry and
source lists based on near infrared photometry, showing the Local (Orion) arm
to be at least 8 kpc long, and an outer arm consistent with what is seen in HI
surveys, which seems to be a continuation of the Perseus arm into the third
quadrant. Meanwhile, the subset of RGB stars with velocities clearly reveals
the large scale kinematic signature of the bar in the inner disc, as well as
evidence of streaming motions in the outer disc that might be associated with
spiral arms or bar resonances. (abridged)

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