File Download
There are no files associated with this item.
Links for fulltext
(May Require Subscription)
- Publisher Website: 10.1051/0004-6361/201322531
- Scopus: eid_2-s2.0-84894327080
- WOS: WOS:000332161800084
- Find via
Supplementary
- Citations:
- Appears in Collections:
Article: The RAVE survey: The Galactic escape speed and the mass of the Milky Way
Title | The RAVE survey: The Galactic escape speed and the mass of the Milky Way |
---|---|
Authors | Piffl, TilmannScannapieco, CeciliaBinney, James J.Steinmetz, MatthiasScholz, Ralf DieterWilliams, Mary E KDe Jong, Roelof S.Kordopatis, GeorgesMatijevič, GalBienaymé, OlivierBland-Hawthorn, Joss BlandBoeche, CorradoFreeman, Kenneth C.Gibson, Brad K.Gilmore, Gerard F.Grebel, Eva K.Helmi, AminaMunari, UlisseNavarro, Julio F.Parker, Quentin A.Reid, Warren A.Seabroke, George M.Watson, Fred G.Wyse, Rosemary F GZwitter, Tomaž |
Keywords | Galaxy: halo Galaxy: kinematics and dynamics Galaxy: structure Galaxy: fundamental parameters Galaxy: general |
Issue Date | 2014 |
Citation | Astronomy and Astrophysics, 2014, v. 562 How to Cite? |
Abstract | We made new estimates of the Galactic escape speed at various Galactocentric radii using the latest data release of the RAdial Velocity Experiment (RAVE DR4). Compared to previous studies we have a database that is larger by a factor of 10, as well as reliable distance estimates for almost all stars. Our analysis is based on statistical analysis of a rigorously selected sample of 90 high-velocity halo stars from RAVE and a previously published data set. We calibrated and extensively tested our method using a suite of cosmological simulations of the formation of Milky Way-sized galaxies. Our best estimate of the local Galactic escape speed, which we define as the minimum speed required to reach three virial radii R340, is 533 +54 -41533-41+54 km s-1 (90% confidence), with an additional 4% systematic uncertainty, where R340 is the Galactocentric radius encompassing a mean overdensity of 340 times the critical density for closure in the Universe. From the escape speed we further derived estimates of the mass of the Galaxy using a simple mass model with two options for the mass profile of the dark matter halo: an unaltered and an adiabatically contracted Navarro, Frenk & White (NFW) sphere. If we fix the local circular velocity, the latter profile yields a significantly higher mass than the uncontracted halo, but if we instead use the statistics for halo concentration parameters in large cosmological simulations as a constraint, we find very similar masses for both models. Our best estimate for M340, the mass interiorto R340 (dark matter and baryons), is 1.3+0.4 -0.3 × 1012 M⊙1.3-0. 3+0.4×1012M⊙ (corresponds to M200 = 1.6+0.5 -0.4 × 1012M200=1.6-0.4+0. 5×1012 M⊙). This estimate is in good agreement with recently published, independent mass estimates based on the kinematics of more distant halo stars and the satellite galaxy Leo I. © 2014 ESO. |
Persistent Identifier | http://hdl.handle.net/10722/209022 |
ISSN | 2023 Impact Factor: 5.4 2023 SCImago Journal Rankings: 1.896 |
ISI Accession Number ID |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Piffl, Tilmann | - |
dc.contributor.author | Scannapieco, Cecilia | - |
dc.contributor.author | Binney, James J. | - |
dc.contributor.author | Steinmetz, Matthias | - |
dc.contributor.author | Scholz, Ralf Dieter | - |
dc.contributor.author | Williams, Mary E K | - |
dc.contributor.author | De Jong, Roelof S. | - |
dc.contributor.author | Kordopatis, Georges | - |
dc.contributor.author | Matijevič, Gal | - |
dc.contributor.author | Bienaymé, Olivier | - |
dc.contributor.author | Bland-Hawthorn, Joss Bland | - |
dc.contributor.author | Boeche, Corrado | - |
dc.contributor.author | Freeman, Kenneth C. | - |
dc.contributor.author | Gibson, Brad K. | - |
dc.contributor.author | Gilmore, Gerard F. | - |
dc.contributor.author | Grebel, Eva K. | - |
dc.contributor.author | Helmi, Amina | - |
dc.contributor.author | Munari, Ulisse | - |
dc.contributor.author | Navarro, Julio F. | - |
dc.contributor.author | Parker, Quentin A. | - |
dc.contributor.author | Reid, Warren A. | - |
dc.contributor.author | Seabroke, George M. | - |
dc.contributor.author | Watson, Fred G. | - |
dc.contributor.author | Wyse, Rosemary F G | - |
dc.contributor.author | Zwitter, Tomaž | - |
dc.date.accessioned | 2015-03-23T02:31:11Z | - |
dc.date.available | 2015-03-23T02:31:11Z | - |
dc.date.issued | 2014 | - |
dc.identifier.citation | Astronomy and Astrophysics, 2014, v. 562 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.uri | http://hdl.handle.net/10722/209022 | - |
dc.description.abstract | We made new estimates of the Galactic escape speed at various Galactocentric radii using the latest data release of the RAdial Velocity Experiment (RAVE DR4). Compared to previous studies we have a database that is larger by a factor of 10, as well as reliable distance estimates for almost all stars. Our analysis is based on statistical analysis of a rigorously selected sample of 90 high-velocity halo stars from RAVE and a previously published data set. We calibrated and extensively tested our method using a suite of cosmological simulations of the formation of Milky Way-sized galaxies. Our best estimate of the local Galactic escape speed, which we define as the minimum speed required to reach three virial radii R340, is 533 +54 -41533-41+54 km s-1 (90% confidence), with an additional 4% systematic uncertainty, where R340 is the Galactocentric radius encompassing a mean overdensity of 340 times the critical density for closure in the Universe. From the escape speed we further derived estimates of the mass of the Galaxy using a simple mass model with two options for the mass profile of the dark matter halo: an unaltered and an adiabatically contracted Navarro, Frenk & White (NFW) sphere. If we fix the local circular velocity, the latter profile yields a significantly higher mass than the uncontracted halo, but if we instead use the statistics for halo concentration parameters in large cosmological simulations as a constraint, we find very similar masses for both models. Our best estimate for M340, the mass interiorto R340 (dark matter and baryons), is 1.3+0.4 -0.3 × 1012 M⊙1.3-0. 3+0.4×1012M⊙ (corresponds to M200 = 1.6+0.5 -0.4 × 1012M200=1.6-0.4+0. 5×1012 M⊙). This estimate is in good agreement with recently published, independent mass estimates based on the kinematics of more distant halo stars and the satellite galaxy Leo I. © 2014 ESO. | - |
dc.language | eng | - |
dc.relation.ispartof | Astronomy and Astrophysics | - |
dc.subject | Galaxy: halo | - |
dc.subject | Galaxy: kinematics and dynamics | - |
dc.subject | Galaxy: structure | - |
dc.subject | Galaxy: fundamental parameters | - |
dc.subject | Galaxy: general | - |
dc.title | The RAVE survey: The Galactic escape speed and the mass of the Milky Way | - |
dc.type | Article | - |
dc.description.nature | link_to_OA_fulltext | - |
dc.identifier.doi | 10.1051/0004-6361/201322531 | - |
dc.identifier.scopus | eid_2-s2.0-84894327080 | - |
dc.identifier.volume | 562 | - |
dc.identifier.eissn | 1432-0746 | - |
dc.identifier.isi | WOS:000332161800084 | - |
dc.identifier.issnl | 0004-6361 | - |