Not exact matches
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.
«We built several models of equal quality
from the
photometric data, but we favored a model made of two lobes since some of the best adaptive optics
observations suggest that the Trojan asteroid has a dual structure,» said Josef Durech, co-author and researcher at the Charles University in Prague.
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.
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).
Science Log — We'll be providing regular updates
from Red Dots HARPS
observations, including new releases of data, the progress of the
photometric observations and science articles
from the team and experts around the world.
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.