Sentences with phrase «by radial velocity»

It was discovered by J.B. Irwin in 1956, its membership was confirmed by radial velocity measurements conducted by M.W. Feast of Radcliffs Observatory (the common RV of the cluster members is +4 km / sec).

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).

Subsequent studies failed to resolve a companion star, both by speckle interferometry (Hartkopf and McAlister, 1983) and by radial velocity analysis (Marcy and Benitz, 1989).

HD 211847's substellar companion, previously detected by the radial velocity method, is actually a low - mass star seen face - on.

These imaged companions populate a mass, separation and age domain (mass > 1MJup, orbits > 5AU, age < 1Gyr) quite distinct from the one occupied by exoplanets discovered by the radial velocity or transit methods.

The vast majority of known exoplanets have been indirectly detected by radial velocity, astrometry, transit, etc..

Both 61 Vir b and HD 1461 b were detected by radial velocity, or stellar wobble, measurements alone, meaning that their diameters remain unknown.

Not exact matches

[1] Most of the exoplanets currently known were discovered using indirect techniques — such as radial velocity variations of the host star, or the dip in brightness of the star caused by a transiting exoplanet.

The planet was found with the radial velocity method, a planet - hunting technique that relies upon slight variations in the velocity of a star to determine the gravitational pull exerted by nearby planets that are too faint to observe directly with a telescope.

[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.

HARPS allows for measurements of radial velocities of stars, which can be affected by the presence of nearby planets, to be taken with the highest accuracy currently available.

They analyzed images called spectra taken by the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph, an instrument designed to search for exoplanets.

Researchers employed an instrument called the High Accuracy Radial velocity Planet Searcher (HARPS) attached to a 3.6 - meter telescope operated by the European Southern Observatory (ESO) at La Silla in Chile.

They then calculated the size, position and mass of K2 - 229b by measuring the radial velocity of the star, and finding out how much the starlight «wobbles» during orbit, due to the gravitational tug from the planet, which changes depending on the planet's size.

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.

The other is the regular but minuscule variation in a star's radial velocity — its speed through the galaxy relative to Earth's speed — which indicates that the star is being tugged by an orbiting planet's gravity.

Carotid to radial artery pulse wave velocity and central aortic blood pressures were obtained by applanation tonometry.

The planet was found using the radial velocity method: Telescopes scrutinize a star's light to see if its frequency is periodically stretched and squeezed by the Doppler effect as the star is tugged, first away and then toward us, by an orbiting planet.

Teasing out the subtle signature of small planets in radial - velocity data takes a wealth of observations, especially when the signal is dominated by larger planets in the system, and others are sure to investigate whether the signature of Gliese 581g is real.

The new discoveries were made with the help of the radial velocity method, which looks for the periodic shifts of certain spectral lines in a star's light that are caused by the gravitational tug of invisible planets which orbit the star.

Due to the close binary orbital interactions of the host star with Alpha Centauri A and Star B's own increased stellar activity during recent years, the astronomers were only able to detect the radial - velocity variations of host star B that were caused by the 3.236 - day orbit of the planet (with a semi-major axis of 0.04 AU) only after more than four and a half years of careful observation.

Planet «b» - In 1996, a team of astronomers (including Eric Williams, Heather M. Hauser, and Phil Shirts) led by Geoffrey W. Marcy and R. Paul Butler announced the discovery of a Jupiter - class planet around Upsilon Andromedae (ups And) A using highly sensitive radial - velocity methods (Butler and Marcy, 1997.

The study culminates many years of effort by an international team of scientists who have discovered a large number of the satellite galaxies, developed new techniques to measure their distances, and have used the Keck Observatory with colleagues to measure their radial velocities, or Doppler shifts (the speed of the galaxy relative to the Sun).

One group (including Debra Fisher, Bernie Walp, Howard Isaacson, Greg Laughlin, Javiera Guedes, and Paul Butler) are hoping to find planets as small as the Earth around both Alpha Centauri A and B within three to five years, by assembling 100,000 radial - velocity observations using an unused 1.5 - meter telescope and vintage equipment at the Cerro Tololo Inter-American Observatory (CTIO) in Chile.

Based on 14 years of radial velocity observations from four ground - based observatories as well as astrometric measurements with the Hubble Space Telescope, the astronomers found that planets «c» and «d» are inclined by 30 + / - 1 degrees with respect to each other is expected to affect theories of how multi-planet systems evolve.

Astronomers detected Ross 128 b using the European Southern Observatory's High Accuracy Radial - velocity Planet Searcher (HARPS) at the La Silla Observatory in Chile and measured the slight «wobbles» of the star caused by the orbiting exoplanet.

Due to the close binary orbital interactions of the host star with Alpha Centauri A and Star B's own increased stellar activity during recent years, the astronomers were only able to detect the radial - velocity variations of host star B that were caused by the 3.236 - day orbit of the planet (with a semi-major axis of 0.04 AU) only after more than three years of careful observation.

A companion study led by Dr. Francesco Pepe (University of Geneva, Switzerland) used the same Kepler data but independent radial velocity observations and is being published in the same issue.

No Jupiter - class planets within 3 AUs were detected dusing radial - velocity variations by 2006 (Wittenmyer et al, 2006, page 186, Table 5; (Cumming et al, 1999; Abt and Levy, 1976, page 286, Table 2 for HR 799).

However, later observations by other astronomers using interferometric astrometry and recent radial velocity data found no evidence to support the existence of a companion greater than 0.8 Jupiter mass with an orbital period around Proxima Centauri of between one and about 2.7 years (Benedict et al, 1999).

Prior to 2009, small but significant variations in radial velocity had been detected which may have been caused by a substellar companion of one to nine Jupiter - masses with an orbital period of 50 years of less (Campbell et al, 1988, pages 904, 906, and 919).

Our latest article, by Eloy Rodríguez, explains how we are using photometry to complement radial velocity data from HARPS.

We then measured the planet mass by acquiring twelve radial velocity (RV) measurements of the system using HIRES on the 10 - m Keck I Telescope.

The team analyzed data collected by the European Southern Observatory's High Accuracy Radial velocity Planet Searcher (HARPS) telescope and the Ultraviolet and Visual Echelle Spectrograph (UVES) to search for planet candidates.

In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT - 22A suggesting the presence of another relatively nearby body that is perhaps non-stellar.

, by Eloy Rodríguez, explains how we are using photometry to complement radial velocity data from HARPS.

Abstract: Kepler - 10b was the first rocky planet detected by the Kepler satellite and con - firmed with radial velocity follow - up observations from Keck - HIRES.

As a subgiant star subject to pulsations which affect careful measurements of variations in radial velocity caused by the gravitational pull of substellar companions, astronomers would find it very difficult to detect any Earth - type planet around Beta Hydri using present methods.

To date, there have been thr... ▽ More Proxima Centauri has become the subject of intense study since the radial - velocity discovery by Anglada - Escud \» e et al. 2016 of a planet orbiting this nearby M - dwarf every ~ 11.2 days.

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).

Abstract: Proxima Centauri has become the subject of intense study since the radial - velocity discovery by Anglada - Escud \» e et al. 2016 of a planet orbiting this nearby M - dwarf every ~ 11.2 days.

The planets are amenable to mass measurement by precision radial velocity measurements, and therefore K2 - 138 could represent a new benchmark systems for comparing radial velocity and TTV masses.

Kepler 18 - b, c, and d: A System Of Three Planets Confirmed by Transit Timing Variations, Lightcurve Validation, Spitzer Photometry and Radial Velocity Measurements

Planet «d» or «3» - Planetary candidate d (or 3) was derived by Bayesian analysis of 47 UMa's radial velocity data.

Furthermore, by knowing the mass of a planet from radial velocity measurements and the radius of a planet based on how much starlight it blocked, it is a simple calculation to determine a planet's density, which can tell astronomers whether that planet is rocky or gaseous in nature, or whether it has a small core and a thick atmosphere, or whether it has a large core covered in deep oceans.

Using the radial velocity technique pioneered by Geoffrey Marcy and Paul Butler, the Lick Planet Search for substellar companions has thus far failed to find a brown dwarf or large Jupiter - or Saturn - mass object in a «torch» orbit around Beta Comae Berenices (Cumming et al, 1999).

This is radial velocity work based on data gathered by the HARPS (High Accuracy Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Silla, radial velocity work based on data gathered by the HARPS (High Accuracy Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Sillavelocity work based on data gathered by the HARPS (High Accuracy Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Silla, Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La SillaVelocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Silla, Chile.

Using the radial velocity technique pioneered by Geoffrey Marcy and Paul Butler, the Lick Planet Search for substellar companions has thus far failed to find a brown dwarf or large Jupiter - or Saturn - mass object in a «torch» orbit around Chi1 Orionis A (Cumming et al, 1999).

Finally, there is the exoplanet detection by the method of radial velocity.