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Bayesian inference of stellar parameters and interstellar extinction using parallaxes and multiband photometry
Astrometric surveys provide the opportunity to measure the absolutemagnitudes of large numbers of stars, but only if the individualline-of-sight extinctions are known. Unfortunately, extinction is highlydegenerate with stellar effective temperature when estimated frombroad-band optical/infrared photometry. To address this problem, Iintroduce a Bayesian method for estimating the intrinsic parameters of astar and its line-of-sight extinction. It uses both photometry andparallaxes in a self-consistent manner in order to provide anon-parametric posterior probability distribution over the parameters.The method makes explicit use of domain knowledge by employing theHertzsprung-Russell Diagram (HRD) to constrain solutions and to ensurethat they respect stellar physics. I first demonstrate this method byusing it to estimate effective temperature and extinction from BVJHKdata for a set of artificially reddened Hipparcos stars, for whichaccurate effective temperatures have been estimated from high-resolutionspectroscopy. Using just the four colours, we see the expected strongdegeneracy (positive correlation) between the temperature andextinction. Introducing the parallax, apparent magnitude and the HRDreduces this degeneracy and improves both the precision (reduces theerror bars) and the accuracy of the parameter estimates, the latter byabout 35 per cent. The resulting accuracy is about 200 K in temperatureand 0.2 mag in extinction. I then apply the method to estimate theseparameters and absolute magnitudes for some 47 000 F, G, K Hipparcosstars which have been cross-matched with Two-Micron All-Sky Survey(2MASS). The method can easily be extended to incorporate the estimationof other parameters, in particular metallicity and surface gravity,making it particularly suitable for the analysis of the 109stars from Gaia.
| Luminosity-variation Independent Location of the Circum-nuclear, Hot Dust in NGC 4151
After recent sensitivity upgrades at the Keck Interferometer (KI),systematic interferometric 2 ?m studies of the innermost dust innearby Seyfert nuclei are within observational reach. Here, we presentthe analysis of new interferometric data of NGC 4151, discussed incontext of the results from recent dust reverberation,spectro-photometric, and interferometric campaigns. The complete dataset gives a complex picture, in particular the measured visibilitiesfrom now three different nights appear to be rather insensitive to thevariation of the nuclear luminosity. KI data alone indicate twoscenarios: the K-band emission is either dominated to ~90% by sizescales smaller than 30 mpc, which falls short of any dust reverberationmeasurement in NGC 4151 and of theoretical models of circum-nuclear dustdistributions. Or contrary, and more likely, the K-band continuumemission is dominated by hot dust (gsim1300 K) at linear scales of about50 mpc. The linear size estimate varies by a few tens of percentdepending on the exact morphology observed. Our interferometric,deprojected centro-nuclear dust radius estimate of 55 ± 5 mpc isroughly consistent with the earlier published expectations fromcircum-nuclear, dusty radiative transfer models, and spectro-photometricmodeling. However, our data do not support the notion that the dustemission size scale follows the nuclear variability of NGC 4151 as an Rdust vprop L 0.5 nuc scaling relation.Instead variable nuclear activity, lagging, and variable dust responseto illumination changes need to be combined to explain the observations.
| Errata in Magnitudes of Stars in AGK3
Not Available
| The space distribution of late type stars in a North galactic pole region.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1962AJ.....67...37U&db_key=AST
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| Takýmyýldýz: | Buyuk Ayi |
| Sað Açýklýk: | 12h03m51.37s |
| Yükselim: | +42°37'59.8" |
| Görünürdeki Parlaklýk: | 11.143 |
| özdevim Sað Açýklýk: | -11.6 |
| özdevim Yükselim: | -13.1 |
| B-T magnitude: | 12.459 |
| V-T magnitude: | 11.252 |
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