Sentences with phrase «velocity measurement»

But a velocity measurement only relates to a specific time.

Here we present a cautionary note outlining how the polarization properties of SMFs can affect the radial velocity measurement precision of high resolution spectrographs.

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).

However, no data on airflow velocity measurement or research on the influence of AC airflow have been available.

The velocity measurement is «a great step forward,» says Douglas Finkbeiner of Harvard University, one of the astronomers who discovered the Fermi bubbles.

If nothing is found wrong with this neutrino - velocity measurement, then of course the modern understanding of physics is thrown entirely «up in the air.»

There must have been something wrong with Jackson's velocity measurements because there is no way he has the weakest arm of that bunch.

Fellow IoA astronomer Floor van Leeuwen agrees, adding that individual velocity measurements of the stars will resolve the question definitively, but probably not before 10 to 15 years from now, when new satellites take to the skies.

These two figures show the internal waves at Dongsha Island on April 23, 2010, as seen by the radar on TerraSAR - X in its conventional mode of operation (left) and in the experimental new mode that permits direct velocity measurements (right), with the measured surface velocities shown in color.

Vogt and Butler's team found the new planet by combining 119 star velocity measurements from HARPS with 122 measurements taken with a similar instrument called HIRES, which is mounted on the 10 - metre Keck 1 telescope in Hawaii.

Rotational velocity measurements made with the European Southern Observatory's Very Large Telescope (VLT) showed that the disk galaxy is spinning more than twice as fast as the Milky Way.

That could be caused by spots on the star, which could confuse velocity measurements, or by the star expanding and contracting (known as stellar pulsations).

Laughlin says it's frustrating that the most interesting planets — small ones like Earth — are so challenging to detect: «You have to get tons and tons and tons of velocity measurements over many years, and then you really, really have to take extreme care — as this Tuomi et al. paper does — to get rid of all the systematic noise.»

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

To locate them, the team relied on velocity measurements based on redshift and blueshift: how an object's light changes colour as it moves away from or towards an observer.

Tracking relative motions within the volume, though, is tough; it requires distance and velocity measurements of high precision.

These velocity measurements led the Dutch astronomer Jan Oort in 1928 to propose that the Milky Way rotates.

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.

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).

The Keck / DEIMOS combination is the only one in the world capable of making these velocity measurements for large numbers of Andromeda stars.»

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.

I. Performances of radial velocity measurements, first analyses of variations.

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).

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).

So velocity measurements help to group objects together but do not determine the distances for those groups.

The host star is bright (V = 11.2, J = 9.1) and so may be a good target for precise radial velocity measurements.

The new radial velocity measurements are now available for download on our website.

The initial transit signal was identified in KELT - North survey data, and the planetary nature of the occulter was established using a combination of follow - up photometry, high - resolution imaging, high - resolution spectroscopy, and precise radial velocity measurements.

The planet has an orbital period of 1.486 days, and radial velocity measurements from the Hobby - Eberly Telescope (HET) show a Doppler signal of 420 + / -15 m.s - 1.

We measure eclipse timing variations (ETVs), which are then combined with the single - lined radial velocity measurements to yield masses in a manner equivalent to double - lined spectroscopic binaries.

Kepler - 19 joins the small number of systems that reconcile transit timing variation and radial velocity measurements.

We identified the initial transit signal in the KELT - North survey data and established the planetary nature of the companion through precise follow - up photometry, high - resolution spectroscopy, precise radial velocity measurements, and high - resolution adaptive optics imaging.

In to - tal, 148 high - quality radial - velocity measurements were obtained over two observing seasons.

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).

The planets are amenable to mass measurement by precision radial velocity measurements, and therefore K2 - 138 could represent a new benchmark systems for comparing radial velocity and TTV masses.

Kepler 18 - b, c, and d: A System Of Three Planets Confirmed by Transit Timing Variations, Lightcurve Validation, Spitzer Photometry and Radial Velocity Measurements

Demonstration of a Near - IR Laser Comb for Precision Radial Velocity Measurements in Astronomy

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.

These observations explore the minimum system requirements for precise radial velocity measurements.

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.

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).

Velocity measurements for the Prestrud and Sulzberger Ice Shelves, West Antarctica.

Furthermore, by knowing the mass of a planet from radial velocity measurements and the radius of a planet based on how much starlight it blocked, it is a simple calculation to determine a planet's density, which can tell astronomers whether that planet is rocky or gaseous in nature, or whether it has a small core and a thick atmosphere, or whether it has a large core covered in deep oceans.

Follow - up radial velocity measurements with th... ▽ More We present 44 days of high duty cycle, ultra precise photometry of the 13th magnitude star Kepler - 5 (KIC 8191672, Teff = 6300 K, logg = 4.1), which exhibits periodic transits with a depth of 0.7 %.

In the EDEN / RV component we are utilizing stellar reflex motion (radial velocity measurements) to search for extrasolar planets around nearby stars.

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 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.

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).

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.