The central velocity dispersion of the Milky Way bulge

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dc.contributor.authorValenti E.
dc.contributor.authorZoccali M.
dc.contributor.authorMucciarelli A.
dc.contributor.authorGonzález O.A.
dc.contributor.authorSurot F.
dc.contributor.authorMinniti D.
dc.contributor.authorRejkuba M.
dc.contributor.authorPasquini L.
dc.contributor.authorFiorentino G.
dc.contributor.authorBono G.
dc.contributor.authorRich R.M.
dc.contributor.authorSoto M.
dc.date.accessioned2022-09-09T12:35:51Z
dc.date.available2022-09-09T12:35:51Z
dc.date.issued2018
dc.descriptionIndexación Scopuses
dc.description.abstractContext: Current spectroscopic and photometric surveys are providing a comprehensive view of the Milky Way bulge stellar population properties with unprecedented accuracy. This in turn allows us to explore the correlation between kinematics and stellar density distribution, crucial to constrain the models of Galactic bulge formation. Aims. The Giraffe Inner Bulge Survey (GIBS) revealed the presence of a velocity dispersion peak in the central few degrees of the Galaxy by consistently measuring high velocity dispersion in the three central most fields. Due to the suboptimal distribution of these fields, all being at negative latitudes and close to each other, the shape and extension of the sigma peak is poorly constrained. In this study we address this by adding new observations distributed more uniformly and in particular including fields at positive latitudes that were missing in GIBS. Methods. Observations with Multi Unit Spectroscopic Explorer (MUSE) were collected in four fields at (l, b) = (0◦, +2◦), (0◦, −2◦), (+1◦, −1◦), and (−1◦, +2◦). Individual stellar spectra were extracted for a number of stars comprised between ∼500 and ∼1200, depending on the seeing and the exposure time. Velocity measurements are done by cross-correlating observed stellar spectra in the CaT region with a synthetic template, and velocity errors are obtained through Monte Carlo simulations, cross-correlating synthetic spectra with a range of different metallicities and different noise characteristics. Results. We measure the central velocity dispersion peak within a projected distance from the Galactic center of ∼280 pc, reaching σVGC ∼ 140 km s−1 at b = −1◦. This is in agreement with the results obtained previously by GIBS at negative longitude. The central sigma peak is symmetric with respect to the Galactic plane, with a longitude extension at least as narrow as predicted by GIBS. As a result of the Monte Carlo simulations we present analytical equations for the radial velocity measurement error as a function of metallicity and signal-to-noise ratio for giant and dwarf stars. © ESO 2018.es
dc.description.urihttps://www.aanda.org/articles/aa/full_html/2018/08/aa32905-18/aa32905-18.html
dc.identifier.citationAstronomy and Astrophysics Volume 616 2018 Article number A83es
dc.identifier.doi10.1051/0004-6361/201832905
dc.identifier.issn00046361
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/23817
dc.language.isoenes
dc.publisherEDP Scienceses
dc.rights.licenseCC BY 4.0
dc.subjectGaiaes
dc.subjectBiomechanicses
dc.subjectLAMOSTes
dc.subjectGalaxy: bulgees
dc.subjectTechniques: imaging spectroscopyes
dc.titleThe central velocity dispersion of the Milky Way bulgees
dc.typeArtículoes
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