- ID:
- ivo://CDS.VizieR/J/AJ/158/181
- Title:
- Radial velocities and S-index values for HR 5183
- Short Name:
- J/AJ/158/181
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Based on two decades of radial velocity (RV) observations using Keck/High Resolution Echelle Spectrometer (HIRES) and McDonald/Tull, and more recent observations using the Automated Planet Finder, we found that the nearby star HR 5183 (HD 120066) hosts a 3 M_J_ minimum mass planet with an orbital period of 74_-22_^+43^ yr. The orbit is highly eccentric (e~0.84), shuttling the planet from within the orbit of Jupiter to beyond the orbit of Neptune. Our careful survey design enabled high cadence observations before, during, and after the planet's periastron passage, yielding precise orbital parameter constraints. We searched for stellar or planetary companions that could have excited the planet's eccentricity, but found no candidates, potentially implying that the perturber was ejected from the system. We did identify a bound stellar companion more than 15000 au from the primary, but reasoned that it is currently too widely separated to have an appreciable effect on HR 5183 b. Because HR 5183 b's wide orbit takes it more than 30 au (1") from its star, we also explored the potential of complimentary studies with direct imaging or stellar astrometry. We found that a Gaia detection is very likely, and that imaging at 10 {mu}m is a promising avenue. This discovery highlights the value of long-baseline RV surveys for discovering and characterizing long-period, eccentric Jovian planets. This population may offer important insights into the dynamical evolution of planetary systems containing multiple massive planets.
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- ID:
- ivo://CDS.VizieR/J/AJ/157/192
- Title:
- Radial velocities and transit times for KOI 4
- Short Name:
- J/AJ/157/192
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The discovery of thousands of planetary systems by Kepler has demonstrated that planets are ubiquitous. However, a major challenge has been the confirmation of Kepler planet candidates, many of which still await confirmation. One of the most enigmatic examples is KOI 4.01, Kepler's first discovered planet candidate detection (as KOI 1.01, 2.01, and 3.01 were known prior to launch). Here we present the confirmation and characterization of KOI 4.01 (now Kepler-1658), using a combination of asteroseismology and radial velocities. Kepler-1658 is a massive, evolved subgiant (M_*_=1.45+/-0.06 M_{sun}_, R_*_=2.89+/-0.12 R_{sun}_) hosting a massive (M_p_=5.88+/-0.47 M_J_, R_p_=1.07+/-0.05 R_J_) hot Jupiter that orbits every 3.85 days. Kepler-1658 joins a small population of evolved hosts with short-period (~<100 days) planets and is now the closest known planet in terms of orbital period to an evolved star. Because of its uniqueness and short orbital period, Kepler-1658 is a new benchmark system for testing tidal dissipation and hot Jupiter formation theories. Using all four years of the Kepler data, we constrain the orbital decay rate to be P=<-0.42 s/yr, corresponding to a strong observational limit of Q'_*_>=4.826x10^3^ for the tidal quality factor in evolved stars. With an effective temperature of T_eff_~6200 K, Kepler-1658 sits close to the spin-orbit misalignment boundary at ~6250 K, making it a prime target for follow-up observations to better constrain its obliquity and to provide insight into theories for hot Jupiter formation and migration.
- ID:
- ivo://CDS.VizieR/J/MNRAS/369/783
- Title:
- Radial velocities & distances of carbon stars
- Short Name:
- J/MNRAS/369/783
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Optical radial velocities have been measured for 38 C-type Mira variables (C-Miras). These data together with others in the literature are used to study the differences between optical and CO millimetre (mm) observations for C-Miras and the necessary corrections to the optical velocities are derived in order to obtain the true radial velocities of the variables. The difference between absorption and emission-line velocities is also examined. A particularly large difference (+30km/s) is found in the case of the H{alpha} line. A catalogue is given of 177 C-Miras with estimated distances and radial velocities. The distances are based on bolometric magnitudes derived in Paper I (Whitelock et al., 2006, Cat. <J/MNRAS/369/751>) using South African Astronomical Observatory (SAAO) observations or (for 60 of the stars) using non-SAAO photometry. In the latter case, the necessary transformations to the SAAO system are derived. These data will be used in Paper III (Feast et al., 2006MNRAS.369..791F) to study the kinematics of the C-Miras.
- ID:
- ivo://CDS.VizieR/III/144
- Title:
- Radial Velocities for High Proper Motion Stars
- Short Name:
- III/144
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The machine-readable version of Radial Velocities of High Proper Motion Stars contains UBV photometry, proper motions, and radial (line-of-sight) velocities for 878 high-proper-motion stars that were selected from the subdwarf candidate list of Sandage and Fouts (1986).
- ID:
- ivo://CDS.VizieR/J/ApJ/757/18
- Title:
- Radial velocities for 16 hot Jupiter host stars
- Short Name:
- J/ApJ/757/18
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We provide evidence that the obliquities of stars with close-in giant planets were initially nearly random, and that the low obliquities that are often observed are a consequence of star-planet tidal interactions. The evidence is based on 14 new measurements of the Rossiter-McLaughlin effect (for the systems HAT-P-6, HAT-P-7, HAT-P-16, HAT-P-24, HAT-P-32, HAT-P-34, WASP-12, WASP-16, WASP-18, WASP-19, WASP-26, WASP-31, Gl 436, and Kepler-8), as well as a critical review of previous observations. The low-obliquity (well-aligned) systems are those for which the expected tidal timescale is short, and likewise the high-obliquity (misaligned and retrograde) systems are those for which the expected timescale is long. At face value, this finding indicates that the origin of hot Jupiters involves dynamical interactions like planet-planet interactions or the Kozai effect that tilt their orbits rather than inspiraling due to interaction with a protoplanetary disk. We discuss the status of this hypothesis and the observations that are needed for a more definitive conclusion.
- ID:
- ivo://CDS.VizieR/J/A+A/430/165
- Title:
- Radial velocities for 6691 K and M giants
- Short Name:
- J/A+A/430/165
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The table provides Hipparcos positions, Hipparcos & Tycho-2 proper motions, and CORAVEL radial velocities for 6691 K and M giants in the solar neighbourhood, mostly from the Hipparcos survey. A bayesian maximum-likelihood approach has been used to derive the distances and space velocities. New V-I indices, computed from a color transformation based on Hp-V_T2_, are also provided. Spectroscopic binaries have been identified as well. These data may be used to study the kinematics of giant stars in the solar neighbourhood, and to correlate it with their location in the Hertzsprung-Russell diagram.
- ID:
- ivo://CDS.VizieR/J/ApJS/141/503
- Title:
- Radial Velocities for 889 late-type stars
- Short Name:
- J/ApJS/141/503
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report radial velocities for 844 FGKM-type main sequence and subgiant stars and 45 K giants, most of which had either low-precision velocity measurements or none at all. These velocities differ from the standard stars of Udry et al. (1999IAUCo.170..354U) by 0.035km/s (RMS) for the 26 FGK standard stars in common. The zero-point of our velocities differs from that of Udry et al.: <V_present_-V_Udry_>=+0.053km/s. Thus these new velocities agree with the best known standard stars both in precision and zero-point, to well within 0.1km/s. Nonetheless, both these velocities and the standards suffer from three sources of systematic error, namely, convective blueshift, gravitational redshift, and spectral type mismatch of the reference spectrum. These systematic errors are here forced to be zero for G2V stars by using the Sun as reference, with Vesta and day sky as proxies. But for spectral types departing from solar, the systematic errors reach 0.3km/s in the F and K stars and 0.4km/s in M dwarfs. Multiple spectra were obtained for all 889 stars during four years, with the HIRES echelle spectrometer (Vogt et al., 1994, , Proc. Soc. Photo-Opt. Instr. Eng., 2198, 362) on the 10m Keck I telescope and with the "Hamilton" echelle spectrometer fed by either the 3m Shane or the 0.6m Coude Auxilliary (CAT) Telescopes (Vogt, 1987PASP...99.1214V), and 782 of them exhibit velocity scatter less than 0.1km/s. These stars may serve as radial velocity standards if they remain constant in velocity. We found 11 new spectroscopic binaries and report orbital parameters for them.
- ID:
- ivo://CDS.VizieR/J/A+A/485/303
- Title:
- Radial velocities for 1309 stars and 166 OCl
- Short Name:
- J/A+A/485/303
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the final catalogues of a long term observing program performed with the two Coravel spectrovelocimeters for red giants in open clusters. The main aims were to detect spectroscopic binaries and determine their orbital parameters, determine the membership, and compute mean velocities for the stars and open clusters. We computed weighted mean radial velocities for 1309 stars from 10517 individual observations, including the systemic radial velocities from spectroscopic orbits and for Cepheids. The final results are contained in three catalogues collecting 10517 individual radial velocities, mean radial velocities for 1309 red giants, and mean radial velocities for 166 open clusters, among which 57 are new determinations. We identify 891 members and 418 non-members. We discovered a total of 288 spectroscopic binaries, among which 57 were classified as non-members. In addition 27 stars were judged to be variable in radial velocities, all of them being red supergiants.
- ID:
- ivo://CDS.VizieR/J/AJ/131/1702
- Title:
- Radial velocities for the HD 27638B components
- Short Name:
- J/AJ/131/1702
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report spectroscopic observations of HD 27638B, the secondary in a visual binary in which the physically associated primary (separation ~19") is a B9 V star. The secondary shows strong Li{lambda}6708 absorption, suggesting youth, and has attracted attention in the past as a candidate post-T Tauri star, although this has subsequently been ruled out. It was previously known to be a double-lined spectroscopic binary (F8+G6) with a period of 17.6days and to show velocity residuals indicating a more distant massive third companion with a period of at least 8yr.
- ID:
- ivo://CDS.VizieR/J/AJ/154/122
- Title:
- Radial velocities for the HD 3167 system
- Short Name:
- J/AJ/154/122
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- HD 3167 is a bright (V=8.9), nearby K0 star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02+/-0.38 M_{earth}_ for HD 3167 b, a hot super-Earth with a likely rocky composition ({rho}_b_=5.60_-1.43_^+2.15^ g/cm^3^), and 9.80_-1.24_^+1.30^ M_{earth}_ for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement ({rho}_c_=1.97_-0.59_^+0.94^ g/cm^3^). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509+/-0.045 d (between planets b and c) and a minimum mass of 6.90+/-0.71 M_{earth}_. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.3{deg} because we do not observe transits of planet d. From 1.3{deg} to 40{deg}, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time. From 40{deg} to 60{deg}, Kozai-Lidov oscillations increase the system's instability, but it can remain stable for up to 100 Myr. Above 60{deg}, the system is unstable. HD 3167 promises to be a fruitful system for further study and a preview of the many exciting systems expected from the upcoming NASA TESS mission.
