Sentences with phrase «in radial velocity»

If not understood, the biases in radial velocity amplitudes will represent an intrinsic limitation for estimating dynamical masses from SB2 + interferometry or SB2 + Gaia.

However, no changes in radial velocity were detected between 1974 and 1984 to confirm possible variations found around 1920 (R. F. Griffin, 1984; and Beardsley et al, 1974).

We also find a slow variation in the radial velocity of Procyon, with good agreement between different telescopes.

In astronomy, the combs are starting to be utilized in the radial velocity, or «wobble» method, the earliest and among the most successful methods for identifying exoplanets.

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).

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.

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.

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).

Planet «c» - A residual drift in the radial velocity data over a decade suggest the presence of even larger planets in outer orbits (Butler et al, 1999).

In 1947, Alfred H. Joy (page 101) reported finding that Groombridge 34 A had an observed range in the radial velocity of 26 km / sec and so may be a spectroscopic binary star.

An attempt to find large planets from December 1986 to February 1987 failed to detect large periodic variations in radial velocities (McMillan and Smith, 1987; more discussion at Hatzes et al, 2004).

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.

Meanwhile, a study to be published in Astrophysical Bulletin that used just the radial velocities of stars found, similar to Moni Bidin's team, that much less dark matter than expected was required to explain the motions of stars in the local universe.

These will include planet - hunting stalwarts such as the HARPS instrument at the European Southern Observatory in La Silla, Chile, and the new Miniature Exoplanet Radial Velocity Array (MINERVA)- Australis, a group of five planned 0.7 - metre telescopes near Toowoomba, Australia.

[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.

A ground - based telescope in Chile discovered 55 of these planets, including HD 85512b, using an instrument called the High Accuracy Radial Velocity Planets Searcher (HARPS).

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.

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.

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.

Using the European Southern Observatory's High Accuracy Radial velocity Planet Searcher instrument in Chile, researchers detected a slight wobble in the position of a star called Ross 128, indicative of an orbiting planet.

And radial velocity searches, which look for Doppler shifts in a star's light as it wobbles under the influence of an orbiting companion, are more attuned to massive planets that induce greater gravitational wobbles in their host stars.

«We designed an experiment to confirm what we suspected was there,» says team leader Guillem Anglada - Escudé of Queen Mary University of London, who used the European Southern Observatory's High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph on a 3.6 - meter telescope in Chile.

Using the High Accuracy Radial Velocity Planet Searcher, or HARPS, at the European Southern Observatory in Chile, his team measured the planet's gravitational influence on its parent star.

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.

As part of a large survey of possible planet - hosting stars, Lovis and his colleagues used the powerful HARPS (for High Accuracy Radial - Velocity Planet Searcher) spectrograph at La Silla Observatory in Chile, 2,400 meters above sea level, which can detect stellar motions with precisions of less than one meter per second, roughly the walking speed of a human being.

Additional simulation work presented in the paper also indicates that long - term telescopic observations may detect wobbles from such planets using the radial velocity method.

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.

Found via radial velocity variations, the planet's true mass could not be known with knowing whether its orbit around Star B is being viewed edge - on, face - on, or somewhere in between.

On October 16, 2012, a team of astronomers announced the discovery of a planet with around 1.13 + / - 0.09 Earth - masses in a very hot and tight, circular orbit around Alpha Centauri B, using the European Southern Observatory's the High Accuracy Radial velocity Planet Searcher (HARPS) instrument on the 3.6 - metre telescope at ESO's La Silla Observatory in Chile.

Therefore, the radial velocity surveys only pick the lowest hanging fruit: Jupiters that have migrated close in to their star, and have orbital periods of literally only a few days.

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 failure, thus far, to find large substellar objects like brown dwarfs or a Jupiter - or Saturn - class planet in a «torch» orbit (closer han the Mercury to Sun distance) around 107 Piscium — with even the highly sensitive radial - velocity technique of Geoffrey W. Marcy and R. Paul Butler — bodes well for the possibility of Earth - type terrestrial planets around this star (Cumming et al, 1999).

The method used to detect carbon monoxide utilized the radial velocity (RV) technique — a technique commonly used in the visible region of the spectrum, to which our eyes are sensitive — for discovering non-transiting exoplanets.

In July 2008, astronomers (Michael Endl and Martin Kürster) analyzed used seven years of differential radial velocity measurements for Proxima Centauri to submit a paper indicating that large planets are unlikely to be orbiting Sol's closest stellar neighbor within its habitable zone — around 0.022 to 0.054 AU with a corresponding orbital period of 3.6 to 13.8 days.

Other instruments, such as HARPS (High Accuracy Radial velocity Planet Searcher) at the La Silla Observatory, could measure a planet's wobbles in order to estimate its mass.

On October 16, 2012, a team of astronomers announced the discovery of a planet with around 1.13 + / - 0.09 Earth - masses in a very hot and tight, circular orbit around Alpha Centauri B, using the European Southern Observatory's High Accuracy Radial velocity Planet Searcher (HARPS) instrument on the 3.6 - metre telescope at ESO's La Silla Observatory in Chile.

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.

Mikayla Mace introduced the most popular methods — radial velocity, transit, and direct imaging — in an earlier post on this blog.

«Results from the three main techniques of planet detection (radial velocity, transit and microlensing techniques) are rapidly converging to a common result: Not only are planets common in the galaxy, but there are more small planets than large ones,» said Stephen Kane, of NASA's Exoplanet Science Institute at the California Institute of Technology, Pasadena, Calif. «This is encouraging news for investigations into habitable planets.»

A subsequent analysis using the most recent kinematic and radial velocity data available in the literature, however, found Proxima «is quitely likely» to be bound to to Stars A and B based on calculations of the binding energy of Proxima relative to the center of mass of the entire triple system, where its orbital semi-major axis exceeds 10,000 AUs and is «on order the same size as Alpha Centauri AB's Hill radius in the galactic potential» (Wertheimer and Laughlin, 2006).

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.

I use the world's best telescopes in order to search and characterize extrasolar planets using a variety of photometric and spectroscopic techniques (radial velocities, transits, microlensing).

Abstract: We report precise radial velocity (RV) measurements of WASP - 47, a G star that hosts three transiting planets in close proximity (a hot Jupiter, a super-Earth and a Neptune - sized planet) and a non-transiting planet at 1.4 AU.

The radial velocity analysis presented in this paper serves as example of the type of analysis that will be necessary to confirm the masses of TESS small planet candidates.

On March 25, 2015, a team of astronomers using the Hubble Space Telescope revealed observations which indicate via the transit method that Alpha Centauri B may have a second planet «c» in a hot inner orbit, just outside planet candidate «b.» After observing Alpha Centauri B in 2013 and 2014 for a total of 40 hours, the team failed to detect any transits involving planet b (previously detected using the radial velocity variations method and recently determined not to be observed edge - on in a transit orbit around Star B).

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.

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.

For the super-Earth WA... ▽ More We report precise radial velocity (RV) measurements of WASP - 47, a G star that hosts three transiting planets in close proximity (a hot Jupiter, a super-Earth and a Neptune - sized planet) and a non-transiting planet at 1.4 AU.