Mouse anti-Human γ-Catenin monoclonal antibody, clone 26

The Qatar-2 transiting exoplanet system was recently observed in short-cadence mode by Kepler as part of K2 Campaign 6. We identify dozens of starspot-crossing events, when the planet eclipses a relatively dark region of the stellar photosphere. The observed patterns of these events demonstrate that the planet always transits over the same range of stellar latitudes and, therefore, that the stellar obliquity is less than about 10 degrees. We support this conclusion with two different modeling approaches: one based on explicit identification and timing of the events and the other based on fitting the light curves with a spotted-star model. We refine the transit parameters and measure the stellar rotation period (18.5 +/- 1.9 days), which corresponds to a "gyrochronological" age of 1.4 +/-. 0.3 Gyr. Coherent flux variations with the same period as the transits are well modeled as the combined effects of ellipsoidal light variations (15.4 +/- 4.8 ppm) and Doppler boosting (14.6 +/- 5.1 ppm). The magnitudes of these effects correspond to a planetary mass of 2.6 +/- 0.9 M-Jup and 3.9 +/- 1.5 M-Jup, respectively. Both of these independent mass estimates agree with the mass determined by the spectroscopic Doppler technique (2.487 +/- 0.086 M-Jup). No occultations are detected, giving a 2 sigma upper limit of 0.06 on the planet's visual geometric albedo. We find no evidence for orbital decay, although we are only able to place a weak lower bound on the relevant tidal quality factor:. Q(star)(') 1.5 x 10(4) (95% confidence).

The combination of high-resolution and sensitivity offered by ALMA is revolutionizing our understanding of protoplanetary discs, as their bulk gas and dust distributions can be studied independently. In this paper we present resolved ALMA observations of the COnlinnual emission (lambda = 1.3 min) and CO isotopologues ((CO)-C-12, (CO)-C-13, (CO)-O-18, J = 2 - 1) integrated intensity from the disc around the nearby (d = 162 pc), intermediate-mass (M-star = 1.67 M-circle dot) pre-main-sequence star CQ Tau. The data show an inner depression in continuum and in both (CO)-C-13 and (CO)-O-18 emission, We employ a Merino-chemical model of the disc reproducing both continuum and gas radial intensity profiles, together with the disc spectral energy distribution. The models show that a gas inner cavity with size between 15 and 25 au is needed to reproduce the data with a density depletion factor between similar to 10(-1) and similar to 10(-3). The radial profile of the distinct cavity in the dust continuum is described by a Gaussian ring centred at R-dust = 53 au and with a width of sigma = 13 au. Three-dimensional gas and dust numerical simulations of a disc with an embedded planet at a separation from the central star of similar to 20 au and with a mass of similar to 6-9 M-Jup reproduce qualitatively the gas and dust profiles of the CQ Tau disc. 11owever, a one-planet model appears not to be able to reproduce the dust Gaussian density profile predicted using the thermo-chemical modeling.