Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data

Abstract

The availability of the Hipparcos Catalogue triggered many kinematic and dynamical studies of the solar neighbourhood. Nevertheless, those studies generally lacked the third component of the space velocities, i.e., the radial velocities. This work presents the kinematic analysis of 5952 K and 739 M giants in the solar neighbourhood which includes for the first time radial velocity data from a large survey performed with the CORAVEL spectrovelocimeter. It also uses proper motions from the Tycho-2 catalogue, which are expected to be more accurate than the Hipparcos ones. An important by-product of this study is the observed fraction of only 5.7% of spectroscopic binaries among M giants as compared to 13.7% for K giants. After excluding the binaries for which no center-of-mass velocity could be estimated, 5311 K and 719 M giants remain in the final sample. The UV-plane constructed from these data for the stars with precise parallaxes (σ π /π ≤ 20%) reveals a rich small-scale structure, with several clumps corresponding to the Hercules stream, the Sirius moving group, and the Hyades and Pleiades superclusters. A maximum-likelihood method, based on a bayesian approach, has been applied to the data, in order to make full use of all the available stars (not only those with precise parallaxes) and to derive the kinematic properties of these subgroups. Isochrones in the Hertzsprung-Russell diagram reveal a very wide range of ages for stars belonging to these groups. These groups are most probably related to the dynamical perturbation by transient spiral waves (as recently modelled by De Simone et al. 2004) rather than to cluster remnants. A possible explanation for the presence of young group/clusters in the same area of the UV-plane is that they have been put there by the spiral wave associated with their formation, while the kinematics of the older stars of our sample has also been disturbed by the same wave. The emerging picture is thus one of dynamical streams pervading the solar neighbourhood and travelling in the Galaxy with similar space velocities. The term dynamical stream is more appropriate than the traditional term supercluster since it involves stars of different ages, not born at the same place nor at the same time. The position of those streams in the UV-plane is responsible for the vertex deviation of 16.2 • ± 5.6 • for the whole sample. Our study suggests that the vertex deviation for younger populations could in fact have the same dynamical origin. The underlying velocity ellipsoid, extracted by the maximum-likelihood method after removal of the streams, is not centered on the value commonly accepted for the radial antisolar motion: it is centered on U = −2.78 ± 1.07 km s −1 . However, the full data set (including the various streams) does yield the usual value for the radial solar motion, when properly accounting for the biases inherent to this kind of analysis (namely, U = −10.25 ± 0.15 km s −1 ). This discrepancy clearly raises the essential question of how to derive the solar motion in the presence o...

Rotation and Granulation of the K2 Giant Α Ser

“…Surprisingly, few measurements of αSerʼs radial velocity have been published since the advent of electronic detectors. Among these are 2.63±0.16 by Famaey et al (2005) and 3.03±0.26 by Massarotti et al (2008). The first is consistent with Figure 8 and approximately with Gray (2009).…”

“…Beavers et al (1979) list 2.5±0.4 km s −1 in their table of standard stars, while Barnes et al (1986) found 6.6±0.3 km s −1 . In their catalog, de Medeiros & Mayor (1999) fixed the velocity at 2.13±0.16 km s −1 using the CORAVEL spectrometer, while Famaey et al (2005) find 2.63±0.16 km s −1 using the same instrument. Massarotti et al (2008), also using a correlation technique, give a mean of 3.03±0.26 km s −1 for three observations taken over an interval of 117 days.…”

Constraining the Milky Way assembly history with Galactic Archaeology

“…The numerical work of Dehnen (1999Dehnen ( , 2000, Fux (2001), , and more recently Antoja et al (2012), has shown that this stream can be explained as the effect of the Milky Way central bar if the Sun is placed just outside the 2:1 Outer Lindblad Resonance (OLR). Due to the inhomogeneity in age and metallicity of Hercules stars, a number of works (e.g., Bensby et al 2007;Famaey et al 2005Famaey et al , 2007 have concluded that a dynamical effect, such as the influence of the bar, is a more likely explanation than a dispersed cluster. Most estimates agree on a bar orientation 2 of φ b = 30 • ± 10 and a pattern speed of Ω b /Ω 0 = 1.9 ± 0.1, where Ω 0 is the local standard of rest (LSR) rotation rate.…”

Spiral- and bar-driven peculiar velocities in Milky Way-sized galaxy simulations

“…Dehnen & Binney 1998;Chereul et al 1998Chereul et al , 1999Famaey et al 2005;Antoja et al 2008;Bovy et al 2009;Antoja et al 2015), which have been attributed to the gravitational perturbations provided by non-axisymmetric structure. In particular, it has been reported that the local moving group known as the 'Hercules' stream is likely caused by the constant periodic perturbations supplied by the outer Lindblad resonance of the bar (e.g., Dehnen 2000;Fux 2001;, which is thought to be close to the solar radius.…”