Sentences with phrase «at radial velocity»

Narrow, stable Ca II and / or Na I absorption features have been detected superimposed to the photospheric lines in 10 out of the 15 observed cold - gas - bearing debris disc.Features are found at the radial velocity of the stars, or slightly blue - or red - shifted, and / or at the velocity of the local interstellar medium (ISM).

Scientists were also able use the infrared spectroscopy to look at radial velocity variations (an analysis of the light spectrum) to determine that water was present.

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

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.

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.

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.

«These data recover the well - known solar 5 - minute oscillation at a peak of 3 mHz (5.5 min) from the disk - averaged light with a radial - velocity amplitude of only 47 cm / s, an incredibly small velocity from a stellar point of view», says Prof. Strassmeier, PEPSI principal investigator and director of the Cosmic Magnetic Field branch at the Leibniz Institute for Astrophysics Potsdam (AIP).

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.

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.

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.

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.

«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.

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.

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).

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.

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).

Five validated planets orbit relatively bright stars (Kp < 12.5) and are expected to yield radial velocity semi-amplitudes of at least 2 m / s.

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).

When we first embarked on this project we were told unequivocally that precision radial velocity measurements were impossible at the amateur level and required the funding and resources of an institution.

This is radial velocity work based on data gathered by the HARPS (High Accuracy Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Silla, radial velocity work based on data gathered by the HARPS (High Accuracy Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Sillavelocity work based on data gathered by the HARPS (High Accuracy Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Silla, Radial Velocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La SillaVelocity Planetary Searcher) spectrometer on the 3.6 - meter telescope at the European Southern Observatory in La Silla, Chile.

The latest radial velocity measurements suggest that 79 Ceti has a companion «b» with at least 77 percent of Saturn's (23 percent of Jupiter's) mass (exoplanets.org).

Our results effectively show that a Michelson interferometer coupled to a spectrograph allows precise measurements of barycentric radial velocities even at a modest spectral resolution of R ~ 5100.

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.

«Paul Butler and I have been obtaining precision radial velocity data of Kapteyn's star for over a decade at Keck, and were thus heavily invested in this work,» said Steve Vogt, a professor of astronomy at the University of California, Santa Cruz that contributed the data from Keck Observatory.

Our barycentric radial velocities, derived from observations taken at the KPNO 2.1 meter telescope, differ from those of Nidever et al. by 0.047 km / s (rms) when simultaneous iodine calibration is used, and by 0.120 km / s (rms) without simultaneous iodine calibration.

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).

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.

Subsequently, Heintz (1996, page 411) suggested that such a companion to Star Ba would have to have a mass of at least half Sol's to reach detectable brightness, and that, among other orbital requirements, Bc's period would have to be less than an Earth year in order to account for the absence of effects on Ba's radial velocities and positions.

On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed two super-Earths «b» and «c» with minimum earth - masses of 4.4 (+3.7 / -2.4) and 8.7 (+5.8 / -4.7), respectively, at average orbital distances of 0.080 (+0.014 / -0.004) and 0.176 (+0.009 / -0.030) AU, respectively, from host star Gl 682, with orbital eccentricities of 0.08 (+0.19 / -.08) and 0.010 (+0.19 / -0.10) and periods around 17.5 and 57.3 days, respectively (UH news release; and Tuomi et al, 2014).

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.

Significantly, the researchers say they have improved the precision of the radial velocity method to arrive at these revised estimates.

On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed a planet with a minimum of 32 (max 49) Earth - masses at an average orbital distance of 0.97 AU from host star Gl 229, with an orbital period around 471 days (UH news release; and Tuomi et al, 2014).

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.

The radial gradient of sap velocity in these trees was quantified in an earlier study (Cohen et al. 2008), indicating a quasi-linear decrease from maximum sap velocity at 5 mm below the cambium down to zero at 40 mm.