Sentences with phrase «as radial velocity»

The radial velocity sample was supplemented by transiting planets smaller than twice the size of Earth around stars meeting the same criteria as the radial velocity targets.

[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.

As radial velocities will not have been used for the preliminary selection of members, they can be subsequently examined to eliminate further nonmembers.

The various detection techniques such as radial velocities, transit, microlensing, direct imaging, timing or astrometry, provided thousands of planet detections.

Not exact matches

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.

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.

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.

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.

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.

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).

Based on astrometic as well as high - cadence radial velocity measurements, planetary candidate «c» appears to have around 14.0 +2.3 / -5.3 times the mass of Jupiter (McArthur et al, 2010).

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.

It has at least 3.75 times Jupiter's mass, but subsequent astrometic as well as high - cadence radial velocity measurements suggest that planet d may have 10.25 +0.7 / -3.3 times the mass of Jupiter with an inclination of 155.5 ° from Earth's line of sight (McArthur et al, 2010); Han et al, 2000; and Mazeh et al, 1999).

Older calculations indicating that the Wolf 424 system would get as close to the Solar System as 0.95 light - years within around 7,500 years have been determined to be based on a «probably erroneous» radial velocity measurement (Vadim V. Bobylev, 2010; and Mülläri and Orlov, 1996).

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.

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).

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

We also used radial velocity measurements of the host star, spanning a time range of $ \ sim $ 30 yr, to constrain the companion's mass and orbital properties, as well as to probe the host star's spectral age indicators and general spectral energy distribution.

As you might expect, larger radial velocities mean bigger planets.

As TLDR pointed out, maybe Gaia could provide us with some data what with radial velocity measurements being a pain and transit measurements coming up empty (so far).

If the angular distance of a star from the radiant is λ and if the velocity of the cluster as a whole with respect to the Sun is V, then the radial velocity of the star, Vr, is Vr = V cos λ.

Follow - up radial velocity measurements with the Keck HIRES spectrograph on 9 separate nights demonstrate that the planet is more than twice as massive as Jupiter with a mass of 2.114 + / -0.057 and a mean density of 0.894 + / -0.079 g / cm ^ 3.

As CORVAL monitoring failed to detect significant radial velocity variations over period of 3,400 days — or over 9.3 years (Duquennoy and Mayor, 1991, pp. 492 and 506), the detection is now considered to be spurious.

As a subgiant star subject to pulsations which affect careful measurements of radial velocity, astronomers would find it very difficult to detect any Earth - type planet arond this star using present methods.

A spectrograph spreads out the light gathered by a telescope so that it can be analyzed to determine such properties of celestial objects as chemical composition and abundances, temperature, radial velocity, rotational velocity, and magnetic fields.

This result was unexpected because no companion had been reported previously and because the star's previously known characteristics (such as observed radial velocity variations) were incompatible with Arcturus as a binary system (R. F. Griffin, 1998).

Radial velocity data can be combined with transit measurements to yield precise planetary masses as well as densities of transiting planets and thereby limit the possible materials of which the planets are composed.

A spectrograph spreads out the light gathered by a telescope so that it can be analysed to determine properties of celestial objects such as chemical composition or their radial velocity through the Doppler effect.

Radial velocity measurements determine the sizes and shapes of the orbits of extrasolar planets as well as the lower limits of the masses of these planets.

Misalignments in a broader class of systems had been predicted as a consequence of torques from wide - orbiting companions, and indeed radial - velocity measurements revealed a third companion in a wide orbit in the Kepler - 56 system.

Most importantly, as Feng explained via an email exchange shared with Gizmodo, the research pushes the limits of the sorts of planets we can detect with the radial velocity method, boosting our prospects of discovering truly Earth - sized, rocky worlds in the future.

It was found using radial - velocity measurements obtained as part of the the NASA - UC Eta - Earth Survey by the California Planet Search (CPS) group, a systematic search for low - mass planets between three and 30 Earth - masses orbiting the nearest 230 G -, K -.