New nearby white dwarfs from Gaia DR1 TGAS and UCAC5/URAT

Using an accurate Gaia TGAS 25pc sample, nearly complete for GK stars, and selecting common proper motion (CPM) candidates from UCAC5, we search for new white dwarf (WD) companions around nearby stars with relatively small proper motions. For investigating known CPM systems in TGAS and for selecting CPM candidates in TGAS+UCAC5, we took into account the expected effect of orbital motion on the proper motion as well as the proper motion catalogue errors. Colour-magnitude diagrams (CMDs) $M_J/J-K_s$ and $M_G/G-J$ were used to verify CPM candidates from UCAC5. Assuming their common distance with a given TGAS star, we searched for candidates that occupied similar regions in the CMDs as the few known nearby WDs (4 in TGAS) and WD companions (3 in TGAS+UCAC5). CPM candidates with colours and absolute magnitudes corresponding neither to the main sequence nor to the WD sequence were considered as doubtful or subdwarf candidates. With a minimum proper motion of 60mas/yr, we selected three WD companion candidates, two of which are also confirmed by their significant parallaxes measured in URAT data, whereas the third may also be a chance alignment of a distant halo star with a nearby TGAS star (angular separation of about 465arcsec). One additional nearby WD candidate was found from its URAT parallax and $GJK_s$ photometry. With HD 166435 B orbiting a well-known G1 star at ~24.6pc with a projected physical separation of ~700AU, we discovered one of the hottest WDs, classified by us as DA2.0$\pm$0.2, in the solar neighbourhood. We also found TYC 3980-1081-1 B, a strong cool WD companion candidate around a recently identified new solar neighbour with a TGAS parallax corresponding to a distance of ~8.3pc and our photometric classification as ~M2 dwarf. This raises the question whether previous assumptions on the completeness of the WD sample to a distance of 13pc were correct.Comment: 9 pages, 6 figures, accepted for publication in Astronomy and Astrophysic

The kinematics of late type stars in the solar cylinder studied with SDSS data

We study the velocity distribution of Milky Way disk stars in a kiloparsec-sized region around the Sun, based on ~ 2 million M-type stars from DR7 of SDSS, which have newly re-calibrated absolute proper motions from combining SDSS positions with the USNO-B catalogue. We estimate photometric distances to all stars, accurate to ~ 20 %, and combine them with the proper motions to derive tangential velocities for this kinematically unbiased sample of stars. Based on a statistical de-projection method we then derive the vertical profiles (to heights of Z = 800 pc above the disk plane) for the first and second moments of the three dimensional stellar velocity distribution. We find that = -7 +/- 1 km/s and = -9 +/- 1 km/s, independent of height above the mid-plane, reflecting the Sun's motion with respect to the local standard of rest. In contrast, changes distinctly from -20 +/- 2 km/s in the mid-plane to = -32 km/s at Z = 800 pc, reflecting an asymmetric drift of the stellar mean velocity that increases with height. All three components of the M-star velocity dispersion show a strong linear rise away from the mid-plane, most notably \sigma_{ZZ}, which grows from 18 km/s (Z = 0) to 40 km/s (at Z = 800 pc). We determine the orientation of the velocity ellipsoid, and find a significant vertex deviation of 20 to 25 degrees, which decreases only slightly to heights of Z = 800 pc. Away from the mid-plane, our sample exhibits a remarkably large tilt of the velocity ellipsoid towards the Galactic plane, which reaches 20 deg. at Z = 800 pc and which is not easily explained. Finally, we determine the ratio \sigma^2_{\phi\phi}/\sigma^2_{RR} near the mid-plane, which in the epicyclic approximation implies an almost perfectly flat rotation curve at the Solar radius.Comment: 18 pages, 9 figures, accepted to Astron.

The Fifth Catalogue of Nearby Stars (CNS5)

Context. We present the compilation of the Fifth Catalogue of Nearby Stars (CNS5), based on astrometric and photometric data from Gaia EDR3 and HIPPARCO