Sentences with phrase «radial velocity exoplanet»

... ▽ More 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.

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.

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.

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.

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

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.

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.

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

«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.»

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.

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

Planets «b, c, and d» - On December 14, 2009, a team of astronomers (Steven S. Vogt; Robert A. Wittenmyer, R. Paul Butler, Simon O'Toole, Gregory W. Henry, Eugenio J. Rivera, Stefano Meschiari, Gregory Laughlin, C. G. Tinney, Hugh R. A. Jones, Jeremy Bailey, Brad D. Carter, and Konstantin Batygin) announced the discovery of one innermost orbiting super-Earth and two outer - orbiting, Neptune - class planets (with at least 5.1, 18.2, and 24.0 Earth - masses, respectively) in moderately circular, inner orbits around 61 Virginis with periods of 4.2, 38.0, and 124.0 days, based on radial - velocity observations over 4.6 years with the Keck Observatory's High Resolution Echelle Spectrometer (HIRES) and the Anglo - Australian Telescope (U.C. Santa Cruz news release; AAO press release; Keck press release; the Lick - Carnegie Exoplanet Survey Team's «Systemic Console;» and Vogt et al, 2009).

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.

Confirming that an exoplanet is real typically relies on measuring the planet's mass, using a technique known as «radial velocity».

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.

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

Our barycentric radial velocities, derived from observations taken at the KPNO 2.1 meter telescope, differ from... ▽ More We demonstrate the ability to measure precise stellar barycentric radial velocities with the dispersed fixed - delay interferometer technique using the Exoplanet Tracker (ET), an instrument primarily designed for precision differential Doppler velocity measurements using this technique.

And the radial velocity method, which helps characterize an exoplanet's mass, will be helped by ESPRESSO, due in 2017

(Many exoplanets have also been discovered using another technique called the radial velocity method, which looks for the gravitational influence of a planet on its star.)

Furthermore, gravitational microlensing can complement other exoplanet detection techniques like radial velocity and the transit method, which are limited in discovering mostly massive planets in relatively close orbits around their host stars.

HARPS has been enormously successful at detecting exoplanets using the radial velocity method, or measuring the gravitational tugs on stars by their planets by watching the stars» spectral lines «wobble» back and forth due to the Doppler effect.

When the first exoplanet was identified via the radial velocity method, the Swiss team was able to detect a wobble in the star 51 Pegasi at a rate of 50 meters per second.