<i>Gaia</i>Early Data Release 3

Klioner, Sergei A.; Mignard, F.; Lindegren, L.; Bastian, U.; McMillan, P. J.; Hernández, J.; Hobbs, David; Ramos-Lerate, M.; Biermann, M.; Bombrun, A.; Torres, A. de; Gerlach, E.; Geyer, R.; Hilger, T.; Lammers, U.; Steidelmüller, H.; Stephenson, C. A.; Brown, Anthony G.; Vallenari, A.; Prusti, T.; Bruijne, J. H. J. de; Babusiaux, C.; Creevey, O.; Evans, D. W.; Eyer, L.; Hutton, A.; Jansen, F.; Jordi, C.; Luri, X.; Panem, C.; Pourbaix, Dimitri; Randich, S.; Sartoretti, Paola; Soubiran, C.; Walton, N. A.; Arenou, Frédéric; Bailer‐Jones, C. A. L.; Cropper, Mark; Drimmel, R.; Katz, David; Lattanzi, M. G.; Leeuwen, F. van; Bakker, J.; Castañeda, J.; Angeli, F. De; Ducourant, C.; Fabricius, C.; Fouesneau, M.; Frémat, Y.; Guerra, R.; Guerrier, A.; Guiraud, J.; Piccolo, A. Jean-Antoine; Masana, E.; Messineo, R.; Mowlavï, N.; Nicolas, C.; Nienartowicz, K.; Pailler, F.; Panuzzo, P.; Riclet, F.; Roux, W.; Seabroke, G. M.; Sordo, R.; Tanga, P.; Thévenin, F.; Gracia-Abril, G.; Portell, J.; Teyssier, D.; Altmann, M.; Andrae, R.; Bellas‐Velidis, I.; Benson, K.; Berthier, J.; Blomme, R.; Brugaletta, E.; Burgess, P.; Busso, G.; Carry, B.; Cellino, A.; Cheek, N.; Clementini, G.; Damerdji, Y.; Davidson, M.; Delchambre, L.; Dell’Oro, A.; Fernández-Hernández, J.; Galluccio, L.; García-Lario, P.; Garcia-Reinaldos, M.; González-Núñez, J.; Gosset, Éric; Haigron, R.; Halbwachs, J. L.; Hambly, N. C.; Harrison, D. L.; Hatzidimitriou, D.; Heiter, U.; Hestroffer, Daniel; Hodgkin, S. T.; Holl, B.; Janßen, K.; Fombelle, G. Jévardat de; Jordan, S.; Krone-Martins, A.; Lanzafame, A. C.; Löffler, W.; Lorca, A.; Manteiga, M.; Marchal, Olivier; Marrese, P. M.; Moitinho, A.; Mora, A.; Muinonen, K.; Osborne, P.; Pancino, E.; Pauwels, T.; Recio–Blanco, A.; Richards, P. J.; Riello, M.; Rimoldini, L.; Robin, A. C.; Roegiers, T. G. R.; Rybizki, Jan; Sarro, L. M.; Siopis, C.; Smith, M.; Sozzetti, A.; Ulla, A.; Utrilla, E.; Leeuwen, M. van; Reeven, W. van; Abbas, U.; Aramburu, A. Abreu; Accart, S.; Aerts, C.; Aguado, J. J.; Ajaj, M.; Altavilla, G.; Álvarez, M. A.; Cid-Fuentes, J. Álvarez; Alves, J.; Anderson, Richard I.; Varela, E. Anglada; Antoja, T.; Audard, M.; Baines, D.; Baker, S. G.; Balaguer-Núñez, L.; Balbinot, E.; Balog, Z.; Barache, C.; Barbato, D.; Barros, M.; Barstow, M. A.; Bartolomé, S.; Bassilana, J.-L.; Bauchet, N.; Baudesson-Stella, A.; Becciani, U.; Bellazzini, M.; Bernet, M.; Bertone, Stefano; Bianchi, L.; Blanco-Cuaresma, S.; Boch, T.; Bossini, D.; Bouquillon, S.; Bramante, L.; Breedt, E.; Bressan, A.; Brouillet, N.; Bucciarelli, B.; Burlacu, Alexandru; Busonero, D.; Butkevich, A. G.; Buzzi, R.; Caffau, E.; Cancelliere, R.; Cánovas, H.; Cantat-Gaudin, T.; Carballo, R.; Carlucci, T.; Carnerero, M. I.; Carrasco, J. M.; Casamiquela, L.; Castellani, M.; Castro-Ginard, A.; Sampol, P. Castro; Chaoul, L.; Charlot, P.; Chemin, L.; Chiavassa, A.; Comoretto, G.; Cooper, William; Cornez, T.; Cowell, S.; Crifo, F.; Crosta, M.; Crowley, C.; Dafonte, Carlos; Dapergolas, A.; David, M.; David, Pedro; Laverny, P. de; Luise, F. De; March, R. De; Ridder, J. De; Souza, R. de; Teodoro, P. de; Peloso, E. F. del; Pozo, E. del; Delgado, A.; Delgado, Héctor; Delisle, J.-B.; Matteo, P. Di; Diakité, S.; Diener, C.; Distefano, E.; Dolding, C.; Eappachen, D.; Enke, H.; Esquej, P.; Fabre, C.; Fabrizio, M.; Faigler, S.; Fedorets, Grigori; Fernique, P.; Fienga, A.; Figueras, F.; Fouron, C.; Fragkoudi, Francesca; Fraile, E.; Franke, Florian; Gai, M.; Garabato, D.; Garcia-Gutierrez, A.; García-Torres, Miguel; Garofalo, A.; Gavras, P.; Giacobbe, P.; Gilmore, G.; Girona, S.; Giuffrida, G.; Gómez, A.; González-Santamaría, I.; González–Vidal, J. J.; Granvik, Mikael; Gutiérrez–Sánchez, R.; Guy, L. P.; Hauser, M. G.; Haywood, M.; Helmi, Amina; Hidalgo, S. L.; Hładczuk, N.; Holland, G.; Huckle, H. E.; Jasniewicz, G.; Jonker, P. G.; Campillo, J. Juaristi; Julbé, F.; Karbevska, L.; Kervella, P.; Khanna, Shourya; Kochoska, A.; Kordopatis, G.; Korn, A. J.; Kostrzewa-Rutkowska, Z.; Kruszyńska, K.; Lambert, S.; Lanza, A. F.; Lasne, Y.; Campion, J.-F. Le; Fustec, Y. Le; Lebreton, Y.; Lebzelter, T.; Leccia, S.; Leclerc, Nicolas; Lecœur-Taı̈bi, I.; Liao, S.; Licata, E.; Lindstrøm, H. E. P.; Lister, Tim; Livanou, E.; Lobel, A.; Pardo, P. Madrero; Managau, S.; Mann, R. G.; Marchant, J. M.; Marconi, M.; Santos, M. M. S. Marcos; Marinoni, S.; Marocco, F.; Marshall, D. J.; Polo, L. Martin; Martín–Fleitas, J. M.; Masip, A.; Massari, D.; Mastrobuono-Battisti, Alessandra; Mazeh, T.; Messina, S.; Michalik, D.; Millar, N. R.; Mints, A.; Molina, D.; Molinaro, R.; Molnár, L.; Montegriffo, P.; Mor, R.; Morbidelli, R.; Morel, Thierry; Morris, D.; Mulone, A. F.; Muñoz, Diego J.; Muraveva, T.; Murphy, C. P.; Musella, I.; Noval, L.; Ordénovic, C.; Orrù, Graziella; Osinde, J.; Pagani, C.; Pagano, I.; Palaversa, L.; Palicio, P. A.; Panahi, A.; Pawlak, M.; Esteller, X. Peñalosa; Penttilä, Antti; Piersimoni, A. M.; Pineau, F.-X.; Plachy, E.; Plum, G.; Poggio, E.; Poretti, E.; Poujoulet, E.; Prša, Andrej; Pulone, L.; Racero, E.; Ragaini, S.; Rainer, M.; Raiteri, C. M.; Rambaux, N.; Ramos, P.; Fiorentin, P. Re; Regibo, S.; Reylé, C.; Ripepi, V.; Riva, A.; Rixon, G.; Robichon, N.; Ciardullo, Robin; Roelens, M.; Rohrbasser, L.; Romero-Gómez, M.; Rowell, N.; Royer, F.; Rybicki, K.; Sadowski, G.; Sellés, A. Sagristà; Sahlmann, J.; Salgado, J.; Salguero, E.; Samaras, N.; Gimenez, V. Sanchez; Sanna, N.; Santoveña, R.; Sarasso, M.; Schultheis, M.; Sciacca, Eva; Segol, M.; Segovia, J. C.; Ségransan, D.; Semeux, D.; Siddiqui, H. I.; Siebert, A.; Siltala, L.; Slezak, E.; Smart, R. L.; Solano, E.; Solitro, F.; Souami, D.; Souchay, J.; Spagna, A.; Spoto, F.; Steele, I. A.; Süveges, M.; Szabados, László; Szegedi-Elek, E.; Taris, F.; Tauran, G.; Taylor, M. B.; Teixeira, R.; Thuillot, W.; Tonello, N.; Torra, F.; Torra, J.; Turon, C.; Unger, N.; Vaillant, M.; Dillen, E. van; Vanel, O.; Vecchiato, Alberto; Viala, Y.; Vicente, D.; Voutsinas, S.; Weiler, Michael; Wevers, T.; Wyrzykowski, Ł.; Yoldaş, A.; Yvard, P.; Zhao, H.; Zorec, J.; Zucker, S.; Zurbach, C.; Zwitter, T.

doi:10.1051/0004-6361/202039734

Cited by 76 publications

(14 citation statements)

References 68 publications

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“…with pulsar timing (Chakrabarti et al 2021), and in the future with extreme precision radial velocity measurements (Chakrabarti et al 2020), as the LMC is expected to produce the largest contributor to the measurement of the solar system acceleration (Gaia Collaboration et al 2020). Our fiducial LMC mass is consistent with the measured solar system acceleration from Gaia EDR3 data (Klioner et al 2021). Ultimately, by using pulsar timing observations of pulsars within the Magellanic Clouds, we could directly constrain the potential of the Milky Way out to large distances, e.g., with the planned MeerKAT survey (Titus et al 2020).…”

Section: Discussionsupporting

confidence: 79%

“…This yields a somewhat larger mass than what is used in our fiducial model. The mass selected here is consistent with the estimated solar system acceleration from Gaia EDR3 data (Klioner et al 2021), and our masses are consistent with the selections made there. The LMC is one of the largest contributors to the acceleration of our solar system, and the selected LMC mass produces accelerations that are consistent with measurements of this acceleration.…”

Section: Initial Conditionssupporting

confidence: 87%

See 1 more Smart Citation

A Dynamical Mass Estimate from the Magellanic Stream

Craig¹,

Chakrabarti²,

Baum³

et al. 2021

Preprint

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We present a model for the formation of the Magellanic Stream (MS) due to ram pressure stripping. We model the history of the Small and Large Magellanic Clouds in the recent cosmological past in a static Milky Way potential with diffuse halo gas, using observationally motivated orbits for the Magellanic Clouds derived from HST proper motions within the potential of the Milky Way. This model is able to reproduce the trailing arm but does not reproduce the leading arm feature, which is common for models of the stream formation that include ram pressure stripping effects. Our model produces a good match to observations (including the densities and line-of-sight velocities of the stream, as well as the positions and velocities of the satellites at present day) when we include a diffuse halo component for the Milky Way. From analyzing our grid of models, we find that there is a direct correlation between the observed stream length in our simulations and the mass of the Milky Way. For the observed MS length, the inferred Milky Way mass is 1.5 ± 0.3 × 10 12 𝑀 , which agrees closely with other independent measures of the Milky Way mass. We also discuss the MS in the context of HI streams in galaxy clusters, and find that the MS lies on the low-mass end of a continuum from Hickson groups to the Virgo cluster. As a tracer of the dynamical mass in the outer halo, the MS is a particularly valuable probe of the Milky Way's potential.

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Section: Discussionsupporting

confidence: 79%

Section: Initial Conditionssupporting

confidence: 87%

A Dynamical Mass Estimate from the Magellanic Stream

Craig¹,

Chakrabarti²,

Baum³

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…We have to keep in mind that the Gaia DR2 (Data Release 2) distance to this object is not tightly constrained: 2.70 +1.23 −0.67 kpc (Bailer-Jones et al 2018); 2.27 +0.92 −0.57 kpc (Rate & Crowther 2020). Also, we might expect some appreciable changes in the distance estimates of WR 48a based on the parallax values of 0.3451 ± 0.1082 mas (DR2; Gaia Collaboration et al 2018) and 0.1933 ± 0.0462 mas (Gaia EDR3, Early Data Release 3; Gaia Collaboration et al 2021).…”

Section: 59mentioning

confidence: 96%

Chandra revisits WR48a: testing colliding wind models in massive binaries

Zhekov,

Gagne,

Skinner

2021

Preprint

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We present results of new Chandra High-Energy Transmission Grating (HETG) observations (2019 November -December) of the massive Wolf-Rayet binary WR 48a. Analysis of these high-quality data showed that the spectral lines in this massive binary are broadened (FWHM = 1400 km s −1 ) and marginally blueshifted (∼ −100 km s −1 ). A direct modelling of these high-resolution spectra in the framework of the standard colliding stellar wind (CSW) picture provided a very good correspondence between the shape of the theoretical and observed spectra. Also, the theoretical line profiles are in most cases an acceptable representation of the observed ones. We applied the CSW model to the X-ray spectra of WR 48a from previous observations: Chandra-HETG (2012 October) and XMM-Newton (2008 January). From this expanded analysis, we find that the observed X-ray emission from WR 48a is variable on the long timescale (years) and the same is valid for its intrinsic X-ray emission. This requires variable mass-loss rates over the binary orbital period. The X-ray absorption (in excess of that from the stellar winds in the binary) is variable as well. We note that lower intrinsic X-ray emission is accompanied by higher X-ray absorption. A qualitative explanation could be that the presence of clumpy and non-spherically symmetric stellar winds may play a role.

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“…As demonstration of the high quality astrometry from Gaia EDR3, Gaia Collaboration et al (2021c) used the apparent proper motion of about 1.6 million quasar-like objects, to directly determine that the centripetal acceleration at the Solar System is 𝛼 = 5.05 ± 0.35𝜇as 𝑦𝑟 −1 . Right after, Bovy (2020) neatly combined this result, with typical values for 𝑅 and Ω Sgr (proper motion of Sgr A*), to derive 𝑉 = 8.0 ± 8.4 km s −1 .…”

Section: The Local Standard Of Restmentioning

confidence: 99%

Measuring the Streaming motion in the Milky Way disc with Gaia EDR3 +

Khanna¹,

Sharma²,

Bland-Hawthorn³

et al. 2022

Preprint

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We map the 3D kinematics of the Galactic disc out to 3.5 kpc from the Sun, and within 0.75 kpc from the midplane of the Milky Way. To this end, we combine high quality astrometry from Gaia EDR3, with the radial velocities from Gaia DR2, and from major spectroscopic surveys including APOGEE, GALAH, and LAMOST. We construct an axisymmetric model for the mean velocity field, and then subtract this on a star-by-star basis to obtain the peculiar velocity field in the Galactocentric components, 𝑉 𝜙 , 𝑉 𝑅 , 𝑉 𝑧 , as well as the heliocentric lineof-sight, 𝑉 los . The velocity residuals are quantified using the power spectrum, and we find that the peak power (𝐴) in the midplane (|𝑧| < 0.25 kpc) is (𝐴 𝜙 , 𝐴 R , 𝐴 Z , 𝐴 los )=(4.2, 8.5, 2.6, 4.6), at 0.25 < |𝑧|/[kpc] < 0.5, is (𝐴 𝜙 , 𝐴 R , 𝐴 Z , 𝐴 los )=(4.0, 7.9, 3.6, 5.3), and at 0.5 < |𝑧|/[kpc] < 0.75, is (𝐴 𝜙 , 𝐴 R , 𝐴 Z , 𝐴 los )=(1.9, 6.9, 5.2, 6.4). Our results provide for the first time, a measure of the streaming motion in the disc in the individual components. We find that streaming is most significant in the Galactocentric radial component, and at all heights (|𝑍 |) probed, but is also not negligible in the other components. Additionally, we find that the patterns in the velocity field overlap spatially with models for the Spiral arms in the Milky Way. Finally, we demonstrate using a simulation that phase mixing of disrupting spiral arms can generate such residuals in the velocity field, where the radial component is dominant, just as in the real data. The simulation also suggests that with evolution of time both the amplitude and the physical scale of the peculiar motion decreases.

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GaiaEarly Data Release 3

Cited by 76 publications

References 68 publications

A Dynamical Mass Estimate from the Magellanic Stream

A Dynamical Mass Estimate from the Magellanic Stream

Chandra revisits WR48a: testing colliding wind models in massive binaries

Measuring the Streaming motion in the Milky Way disc with Gaia EDR3 +

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