Sentences with word «photometric»

The rotation period distributions show a clear mass - dependent morphology, statistical... ▽ More We report on the results of a time - series photometric survey of M50 (NGC 2323), a ~ 130 Myr open cluster, carried out using the CTIO 4m Blanco telescope and Mosaic - II detector as part of the Monitor project.

Access to the AAVSO database of photometric observations is freely available to anyone online and light curves can be generated using the AAVSO light curve generator.

Ellen Howell (National Astronomy and Ionospheric Centre, NAIC, Arecibo Observatory) and Mikko Kaasalainen (Helsinki University) were provided with photometric data to support radar observations and asteroid shape modeling respectively.

For the basic model parameters Teff, log g and [Fe / H], we interpolate in the grid of GAIA / PHOENIX stellar model atmospheres and compute the corresponding model for the G2 V star alpha Cen A. Comparison with photometric measurements shows excellent agreement between observed photospheric data in the optical and infrared.

Combining our results with those for 86 other L and T dwarfs from the literature show that the detection rate of H$ \ alpha $ emission is very high (94 $ \ % $) for spectral types between L0 and L3.5 and much smaller (20 $ \ % $) for spectral types $ \ ge $ L4, while the detection rate of photometric variability is approximately constant (30 $ \ % - $ 55 $ \ % $) from L0 to T8 dwarfs.

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.

Way, M.J., and A.N. Srivastava, 2006: Novel methods for predicting photometric redshifts from broadband photometry using virtual sensors.

The KELT images have a pixel scale of ~ 23 arsec per pixel (similar to TESS) and a large point spread function, and the KELT reduction pipeline uses a weighted photometric aperture with radius 3 arcmin.

The transit signals were detected in photometric data from the Kepler satellite, and were confirmed to arise from planets using a combination of large transit - timing variations, radial - velocity variations, Warm - Spitzer observations, and statistical analysis of false - positive probabilities.

This includes Doppler spectroscopy, photometric transits, gravitational microlensing, direct imaging and astrometry.

These telescopes are routinely used for high precision photometric monitoring observations including exoplanetary transits.

As an example of the initial photometric results, we present variability measurements that can be used to distinguish dwarf stars from red giants.

The incredibly prolific Sloan Digital Sky Survey has provided photometric observations of around 500 million objects and spectra for more than 3 million objects.

Transiting extrasolar planets are now discovered jointly by photometric surveys and by radial velocimetry, allowing measurements of their radius and mass.

Abstract: The Kepler mission has to date found almost 6,000 planetary transit - like signals, utilizing three years of data for over 170,000 stars at extremely high photometric precision.

As part of the Trans - atlantic Exoplanet Survey (TrES), in 2003/4 we monitored approximately 30,000 stars (9.5 < V < 15.5) in a 5.7 degree x 5.7 degre... ▽ More Driven by the incomplete understanding of the formation of gas giant extrasolar planets and of their mass - radius relationship, several ground - based, wide - field photometric campaigns are searching the skies for new transiting extrasolar gas giants.

Though, the later photometric measurements by MASTER - Amur and spectral measurements by the 6 - metre BTA - 6 telescope showed that the star did not turn red, as, for example, the Sun does before sunset (this happens because it takes longer for the sun rays to pierce the atmosphere).

Abstract: Three transiting exoplanet candidate stars were discovered in a ground - based photometric survey prior to the launch of NASA's -LCB- \ it Kepler -RCB- mission.

The two main techniques were kinematic and photometric distance estimates.

To fully understand the methodology, processes and eventually the results from the mission, we present the underlying rationale that ultimately led to the flight and ground system designs used to achieve the exquisite photometric performance.

Obtaining photometric calibrations for NICMOS data is discussed in Chapter 5 of the NICMOS Data Handbook.

Abstract: Driven by the incomplete understanding of the formation of gas giant extrasolar planets and of their mass - radius relationship, several ground - based, wide - field photometric campaigns are searching the skies for new transiting extrasolar gas giants.

Using an imaging algorithm called photometric stereo, the researchers were able to recover quantitative measurements of brush and tool marks.

By combining these color data, it is possible to make a crude estimate of the distances to the faint background galaxies (called photometric redshift).

Hence, the novel photometric approaches developed by the student will be streamlined, benchmarked and verified in a laboratory environment, and ultimately integrated into Randox Laboratories biomarker analysers to allow pioneering advancements to be made in the treatment of patients around the globe.

Here, we predict the properties of the transiting planets that TESS will detect along with the eclipsing binary stars that produce false - positive photometric signals.

The original WFC laboratory flat fields produce photometric errors of + -5 to + -9 percent from corner - to - corner.

Skilled in photometric testing and operating systems.

The first step in searching out a new dwarf galaxy is to identify an over density of stars in the sky, using photometric data.

Many recently discovered dwarf galaxies, especially those seen in systematic photometric surveys such as the Sloan Digital Sky Survey (SDSS) and the Dark Energy Survey (DES) are very faint with absolute luminosity in the optical waveband below -8 magnitude.

Wu leads a team that has developed a method to effectively select quasars in the distant universe based on optical and near - infrared photometric data, in particular using data from the Sloan Digital Sky Survey and NASA's Wide - Field Infrared Explorer, or WISE, satellite.

Shashank Dholakia and Shishir Dholakia, Adrian C Wilcox High School, Santa Clara, California A Search for Exoplanets in the Open Star Clusters Messier 35 and Koposov 62 Using A Novel Large - Scale Photometric Algorithm for the «Crippled» Kepler Mission

We present 130 ultracool dwarf discoveries with estimated distances $ \ approx9 - 130 $ pc, including 21 that were independently discovered by other authors and 3 that were previously identified as photometric candidates.

Data from the simultaneous photometric campaign is also coming in.

Recent progress has been made to address this: (1) the discovery that gamma Cas is an eccentric binary system (P = 203.59 d) with unknown secondary type, (2) the accumulation of RXTE data at 9 epochs in 1996 - 2000, and (3) the collation of robotic telescope B, V - band photometric observations over 4 seasons.

We successfully modeled our initial photometric observations of GSC 03885 - 00829 as the light from a K dwarf binary system superimposed on the light from a late F dwarf star.

Weak lensing cosmology will be challenging: in addition to highly accurate galaxy shape measurements, statistically robust and accurate photometric redshift (photo - z) estimates for billions of faint galaxies will be needed in order to reconstruct the three - dimensional matter distribution.