Sentences with phrase «radial velocity data from»
We simultaneously fit these observations, ground - based photometry from Pepper et al. (2017), radial velocity data from Pepper et al. (2017), and an SED model utilizing catalog magnitudes and the Hipparcos parallax to the system.
https://arxiv.org/
, by Eloy Rodríguez, explains how we are using photometry to complement radial velocity data from HARPS.
Our latest article, by Eloy Rodríguez, explains how we are using photometry to complement radial velocity data from HARPS.
Not exact matches
[1] The team used data from the UVES spectrograph on ESO's Very Large Telescope in Chile (to determine the properties of the star accurately), the Carnegie Planet Finder Spectrograph (PFS) at the 6.5 - metre Magellan II Telescope at the Las Campanas Observatory in Chile, the HIRES spectrograph mounted on the Keck 10 - metre telescope on Mauna Kea, Hawaii as well as extensive previous data from HARPS (the High Accuracy Radial velocity Planet Searcher) at ESO's 3.6 - metre telescope in Chile (gathered through the M dwarf programme led by X. Bonfils and M. Mayor 2003 - 2010.
The data set used by the researchers came from the High Accuracy Radial Velocity Planet Searcher (HARPS) using the ESO's 3.6 m telescope at La Silla Observatory, in Chile.
These new results have been obtained from analysing data from two high - precision planet surveys — the HARPS (High Accuracy Radial Velocity Planet Searcher) and UVES (Ultraviolet and Visual Echelle Spectrograph)-- both operated by the European Southern Observatory in Chile.
«These data recover the well - known solar 5 - minute oscillation at a peak of 3 mHz (5.5 min) from the disk - averaged light with a radial - velocity amplitude of only 47 cm / s, an incredibly small velocity from a stellar point of view», says Prof. Strassmeier, PEPSI principal investigator and director of the Cosmic Magnetic Field branch at the Leibniz Institute for Astrophysics Potsdam (AIP).
The planet mass (derived mostly from the radial velocity data) is comparable, 3.47 ± 0.15 Jupiter masses in the KELT paper, and 3.69 ± 0.18 in ours.
The transit signals were detected in photometric data from the Kepler satellite, and were confirmed to arise from planets using a combination of large transit - timing variations, radial - velocity variations, Warm - Spitzer observations, and statistical analysis of false - positive probabilities.
Here we present results from the analysis of 82 new radial velocity observations of this system obtained with HARPS - N, together with the existing 14 HIRES data points.
We present new mass measurements of three of the planets in the Kepler - 20 system facilitated by 104 radial velocity measurements from the HARPS - N spectrograph and 30 archival Keck / HIRES observations, as well as an updated photometric analysis of the Kepler data and an asteroseismic analysis of the host star (MStar = 0.948 + -0.051 Msun and Rstar = 0.964 + -0.018 Rsun).
Planet «c» or «2» - A residual drift in the radial velocity data over several years suggest the presence of an even larger planet in an outer orbit, at about 3.73 AUs from 47 UMa (between the average orbital distances of Jupiter and the Main Asteroid Belt in the Solar System).
If you are new to this saga make sure you read Tau II Abstract: The successful detection is reported of radial - velocity variations due to orbital motion of the substellar companion of the star tau Boötis, from data obtained with a small aperture (0.4 - m) telescope and a fibre - fed high resolution spectrograph.
«Paul Butler and I have been obtaining precision radial velocity data of Kapteyn's star for over a decade at Keck, and were thus heavily invested in this work,» said Steve Vogt, a professor of astronomy at the University of California, Santa Cruz that contributed the data from Keck Observatory.
The K2 - 18b researchers used data from the prolific planet - finding High Accuracy Radial Velocity Planet Searcher (HARPS) at the La Silla Observatory in Chile.
We find that the asteroseismic parameters allow us to test cluster - membership of the stars, and even with the limited seismic data in hand, we can already identify four possible non-members despite their having a better than 80 % membership probability from radial velocity measurements.
Kepler 10b was detected using the transit method from more than eight months of data collected by the spacecraft between May 2009 and early January 2010 and confirmed by radial velocity measurements, and there evidence for another planet (KOI 72.02) in an outer orbit with a period around 45.3 days (Kepler news release; images, animations, and discovery page; and Batalha et al, 2011).
On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed two super-Earths «b» and «c» with minimum earth - masses of 4.4 (+3.7 / -2.4) and 8.7 (+5.8 / -4.7), respectively, at average orbital distances of 0.080 (+0.014 / -0.004) and 0.176 (+0.009 / -0.030) AU, respectively, from host star Gl 682, with orbital eccentricities of 0.08 (+0.19 / -.08) and 0.010 (+0.19 / -0.10) and periods around 17.5 and 57.3 days, respectively (UH news release; and Tuomi et al, 2014).
On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed two super-Earths «b» and «c.» Planet b has around 4.4 (+3.7 / -2.4) Earth - masses and an average orbital distance of 0.080 (+0.014 / -0.004) AU from host star Gl 682.
The Geneva team used data from HARPS, or the High Accuracy Radial Velocity for Planetary Searcher, a powerful spectrometer on a 3.6 - meter telescope in Chile.
On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed a planet with a minimum of 32 (max 49) Earth - masses at an average orbital distance of 0.97 AU from host star Gl 229, with an orbital period around 471 days (UH news release; and Tuomi et al, 2014).