Contents
Images
Upload your image
DSS Images Other Images
Related articles
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.
| 3-5 μm Spectroscopy of Obscured AGNs in ULIRGs
We present the results of infrared L-band (3-4 μm) and M-band (4-5μm) Very Large Telescope (VLT) ISAAC spectroscopy of five brightultraluminous infrared galaxies (ULIRGs) hosting an AGN. From ouranalysis we distinguish two types of sources: ULIRGs in which the AGN isunobscured (with a flat continuum and no absorption features at 3.4 and4.6 μm), and those with highly obscured AGNs (with a steep, reddenedcontinuum and absorption features due to hydrocarbons and CO). Starburstactivity is also present in all of the sources, as inferred from the 3.3μm PAH emission line. A strong correlation is found between continuumslope and CO optical depth, which suggests that deep carbon monoxideabsorption is a common feature of highly obscured ULIRG AGNs. Finally,we show that the AGN dominates the 3-4 μm emission, even if itscontribution to the bolometric luminosity is small.Based on observations collected at the European Southern Observatory,Chile (proposals ESO 73.B-0574, 79.B-0052).
|
Submit a new article
Related links
Submit a new link
Member of following groups:
|
Observation and Astrometry data
| Constellation: | かんむり座 |
| Right ascension: | 15h44m53.94s |
| Declination: | +38°14'26.9" |
| Apparent magnitude: | 10.133 |
| Proper motion RA: | 60.3 |
| Proper motion Dec: | -117.3 |
| B-T magnitude: | 11.252 |
| V-T magnitude: | 10.226 |
Catalogs and designations:
|
INHABITED SKY
