Sentences with phrase «radial velocity planets»

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).

[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.

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.

And a European contingent from the High Accuracy Radial velocity Planet Searcher (HARPS) had an even bigger haul to unveil.

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.

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.

«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.

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.

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.

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.

Radial velocity measurements of Alpha Centauri B with High Accuracy Radial Velocity Planet Searcher spectrograph ruled out planets of more than 4 M ⊕ to the distance of the habitable zone of the star (orbital period P = 200 days).

In 2012, researchers used an instrument called the High Accuracy Radial velocity Planet Searcher to detect a planet around Alpha Centauri B.

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.

On August 29, 2012, the Planetary Habitability Laboratory (PHL) revealed that a team of astronomers working with the High Accuracy Radial velocity Planet Search (HARPS) project had discovered two planets «b» and «c» around the red dwarf star Gliese 163.

That is why the first radial velocity planet (51 Peg), the first transiting planet (OGLE - TR - 056), the first microlensing planet (OGLE 2003 - BLG - 235L), and the first directly imaged planet (GQ Lupi b) were all Jupiter - like or larger.

Not exact matches

ESPRESSO's sensitivity could put Earth - like planets within reach — and rejuvenate the radial velocity technique

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.

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.

[4] Mass estimates for planets observed using the radial velocity method are lower estimates: if the planet's orbit is highly inclined it could have a higher mass and create the same observed effects.

HARPS - North detects planets using the radial velocity method, which allows astronomers to measure a planet's mass.

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 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.

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.

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.

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.

Laughlin is a Co-I on the Lick Carnegie Exoplanet Survey, and along with team members Steve Vogt, Paul Butler, Eugenio Rivera and Stefano Meschiari, is using the Keck, Magellan and AAT telescopes to discover and characterize planets with the Doppler radial velocity technique.

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 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 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.

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.

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.

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,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,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).

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.

Using the ten - meter Keck I telescope fitted with the HIRES instrument, the team employed the radial velocity method to measure how much an orbiting planet causes its star to wobble, to determine the planet's mass.

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).

Still, many of the nearby planets are detectable via three exoplanet hunting methods: planetary transits, high - contrast imaging, and stellar radial velocity measurements.

It appears to be a main sequence red dwarf star of spectral and luminosity type M4.5 V. Because of its small mass and great distance from the primary (Star A), Upsilon Andromedae B appears to have a negligible effect on the radial velocity measurements used to determine that Star A has at least three large planets (Lowrance et al, 2002).

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.

Even though the radial velocity method can only give some rough measurements of an exoplanet's properties, like minimum mass and orbital period, it nevertheless allows astronomers to make some educated guesses regarding the planet's overall structure.

Recent simulations suggest that an Earth - life planet could have formed within the habitable zone around Alpha Centauri B, which can be detected using the radial - velocity «wobble» method (more).

«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.»

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.

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).