Sentences with phrase «s radial velocity»

A relation between distance and radial velocity among extra-galactic nebulae.

[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.

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.

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.

[2] The team looked at radial velocity data of Gliese 667C, a method often used to hunt for exoplanets.

[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.

[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.

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.

Instead of becoming an Earth - shattering revelation, serious doubts were cast on the detection, which also used radial velocity.

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.

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.

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.

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

Initially identified a decade ago through radial velocity measurements, it was later confirmed through transit observations with the MOST and Spitzer space telescopes.

«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.

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.

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.

The results of follow - up observations (see Table 2) are a mixture of results from photometric follow - up (Deeg et al. 2009), which identifies contaminating» diluted EB's that are more than about 2 distant from the third star - which usually coincides with the observing target -, and from spectroscopic (radial velocity) results, which can only identify signals from sources that fall into the spectrograph's entry slit; that is, they have to be very close (less than 1 - 2) to the target.

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.

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.

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.

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.

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).

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.

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

G.D., V.B., S.C.N., M.T.D., T.E., C.G., H.J. - C., D.H.K., A.F., J.G., A.I., J.F.K., M.M., K.M., N.N., T.E.O., P.A.R., G.S., D.C.S., R.R.Y., R.Z., B.J.F. and A.H. all provided photometric or radial velocity data that were important for the interpretation of the system.

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).

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).

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.

Abstract: We report the discovery of a low - mass companion orbiting the metal - rich, main sequence F star TYC 2949 -00557-1 during the MARVELS (Multi-object APO Radial Velocity Exoplanet Large - area Survey) Pilot Project.

For low - mass eclipsing binary stars, the method of eclipse minimum timing allows astronomers to search for smaller masses than those feasible with radial velocity measurements.

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.

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.»