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Chemically Tagging the HR 1614 Moving Group
We present abundances for a sample of F, G, and K dwarfs of the HR 1614moving group based on high-resolution, high signal-to-noise ratiospectra from the Anglo-Australian Telescope UCLES instrument. Our sampleincludes stars from Feltzing and Holmberg, as well as from Eggen.Abundances were derived for Na, Mg, Al, Si, Ca, Mn, Fe, Ni, Zr, Ba, Ce,Nd, and Eu. The α, Fe, and Fe-peak element abundances show abimodal distribution, with four stars having solar metallicities, whilethe remaining 14 stars are metal-rich, [Fe/H]>=0.25 dex. However, theabundances of these two groups converge for the heavier n-captureelements. Based on their photometry and kinematics, three of the fourdeviating stars are likely nonmembers or binaries. Although one starcannot be excluded on these grounds, we do expect low-levelcontamination from field stars within the HR 1614 moving group's rangeof magnitude, color, and space velocities. Disregarding these fourstars, the abundance scatter across the group members for all elementsis low. We find that there is an 80% probability that the intrinsicscatter does not exceed the following values: Fe, 0.01 dex; Na, 0.08dex; Mg, 0.02 dex; Al, 0.06 dex; Si, 0.02 dex; Ca, 0.02 dex; Mn, 0.01dex; Ni, 0.01 dex; Zr, 0.03 dex; Ba, 0.03 dex; Ce, 0.04 dex; Nd, 0.01dex; and Eu, 0.02 dex. The homogeneity of the HR 1614 group in age andabundance suggests that it is the remnant of a dispersed star-formingevent. Its kinematical coherence shows that such a dispersing systemneed not be significantly perturbed by external dynamical influencessuch as Galactic spiral structure or giant molecular clouds, at leastover a period of 2 Gyr.
| Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
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| Takýmyýldýz: | Karga |
| Sað Açýklýk: | 12h46m13.55s |
| Yükselim: | -14°11'01.9" |
| Görünürdeki Parlaklýk: | 8.56 |
| Uzaklýk: | 146.843 parsek |
| özdevim Sað Açýklýk: | -70 |
| özdevim Yükselim: | 8.3 |
| B-T magnitude: | 8.987 |
| V-T magnitude: | 8.596 |
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