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Millimeter interferometric observations of FU Orionis-type objects in Cygnus
Context. FU Orionis-type objects (FUors) are low-mass young eruptivestars that probably represent an evolutionary phase characterized byepisodic periods of increased accretion rate from the circumstellar diskto the star. Theory predicts that a circumstellar envelope, the sourceof continuous mass infall onto the disk, is necessary for triggeringsuch accretion bursts. Aims: We intend to study the spatial andvelocity structure of circumstellar envelopes around FUors by means ofmolecular line observations at millimeter wavelengths. We target threeprototypical FUors, as well as an object possibly in a pre-outburststate. Methods: We present archival PdBI interferometricobservations of the J = 1-0 line of 13CO at 110.2 GHz. Forthree of our targets, these represent the first millimeterinterferometric observations. The data allow study of the molecularenvironment of the objects with a spatial resolution of a thousand AUand a velocity resolution of 0.2 km s-1. Results:Strong, narrow 13CO(1-0) line emission is detected from allsources. The emission is spatially resolved in all cases, withdeconvolved sizes of a few thousand AUs. For V1057 Cyg and V1331 Cyg,the emitting area is rather compact, suggesting that the origin of theemission is a circumstellar envelope surrounding the central star. ForV1735 Cyg, the 13CO emission is offset from the stellarposition, indicating that the source of this emission may be a smallforeground cloud, also responsible for the high reddening of the centralstar. The 13CO emission towards V1515 Cyg is the mostextended in the sample, and it apparently coincides with the ring-likeoptical reflection nebula associated with V1515 Cyg. Conclusions:We suggest that millimeter interferometric observations areindispensable for a complete understanding of the circumstellarenvironment of FUors. Any theory of the FUor phenomenon that interpretsthe geometry of the circumstellar structure and its evolution usingsingle-beam measurements must be checked and compared to interferometricobservations in the future.
| 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.
| Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample
We are obtaining spectra, spectral types, and basic physical parametersfor the nearly 3600 dwarf and giant stars earlier than M0 in theHipparcos catalog within 40 pc of the Sun. Here we report on resultsfor 1676 stars in the southern hemisphere observed at Cerro TololoInter-American Observatory and Steward Observatory. These resultsinclude new, precise, homogeneous spectral types, basic physicalparameters (including the effective temperature, surface gravity, andmetallicity [M/H]), and measures of the chromospheric activity of ourprogram stars. We include notes on astrophysically interesting stars inthis sample, the metallicity distribution of the solar neighborhood, anda table of solar analogs. We also demonstrate that the bimodal nature ofthe distribution of the chromospheric activity parameterlogR'HK depends strongly on the metallicity, andwe explore the nature of the ``low-metallicity'' chromosphericallyactive K-type dwarfs.
| New light on faint stars. I - The luminosity function in the solar neighbourhood
From photoelectric photometry of red dwarf stars identified in anobjective prism survey, a magnitude-limited complete sample has beendefined. Applying photometric parallaxes, calibrated for theKron-Cousins system by observations of trigonometric parallax stars,this sample is used to determine the space densities of stars withabsolute magnitudes between + 7 and + 12. The resultant luminosityfunction is consistent with the Luyten and Wielen functions for thesolar neighbourhood. An analysis of the stellar kinematics shows littlesignificant evidence of a substantial local population of low spacemotion M-dwarfs.
| Photometry of Southern Hemisphere red dwarf stars
Results are presented for a photometric investigation of aspectroscopically selected sample of red dwarf stars in the SouthernHemisphere. Absolute magnitudes and distances for the stars areestimated from broadband red colors. Three stars which may besubluminous are identified, as are several stars which may be within 25pc. The tangential velocity and velocity dispersion of the sample aresimilar to values found in other studies of nearby late-type stars.
| The space density and kinematics of dwarf M stars
The results of an objective-prism survey for dwarf stars, K7 and later,are presented. One hundred twenty-one red sensitive plates covering 1720sq. degrees of the southern sky were obtained with the Curtis Schmidttelescope at C.T.I.O. The resulting luminosity function rises from log N+ 10 = 7.9 at MV = 8 to about 8.7 at MV = 11 and12. About 75% of the dwarfs in this survey are identified with BPMstars, but inserting the proper motions given into the equations of themethod of mean absolute magnitudes yields values of MB aboutthree magnitudes brighter than the spectral types would indicate. Thatthe method of mean absolute magnitudes appears to be calibrated on starsof higher than average proper motion lends credence to the luminosityfunction result. A galactic mass density is found for the dwarfsconsidered.
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Observation and Astrometry data
| Constellation: | Triangle austral |
| Right ascension: | 16h49m42.59s |
| Declination: | -65°04'33.8" |
| Apparent magnitude: | 10.311 |
| Distance: | 27.1 parsecs |
| Proper motion RA: | 78.4 |
| Proper motion Dec: | -107 |
| B-T magnitude: | 11.986 |
| V-T magnitude: | 10.45 |
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