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5 results for “stars: distances”
Spectro-photometric distances and self-calibrated abundances for Apogee DR16 RGB stars within the Milky Way disk
<p>The data file contains 48,853 RGB stars from Apogee DR16 within the Milky Way disk, for which we determine spectro-photometric parallax estimates (as described in Hogg et al. 2019, AJ, 158, 147), as well as self-calibrated stellar element abundances. The data set is described in detail and analyzed in Eilers et al. 2022 (arXiv: 2112.03295).</p>
SI Figure 3: Compositional difference among eukaryotic microinvertebrate external and internal microbiomes, using Bray Curtis distance matrix visualized with a NMDS ordination. Circles indicate each community and stars centroid location of each microbiome type. Communities do not cluster by animal, microbiome type, mat type, or stream. in External and internal microbiomes of Antarctic nematodes are distinct, but more similar to each other than the surrounding environment
SI Figure 3: Compositional difference among eukaryotic microinvertebrate external and internal microbiomes, using Bray Curtis distance matrix visualized with a NMDS ordination. Circles indicate each community and stars centroid location of each microbiome type. Communities do not cluster by animal, microbiome type, mat type, or stream.
SI Figure 2: Compositional differences among bacterial microinvertebrate external and internal microbiomes as well as mats they were isolated from using Bray Curtis distance matrix visualized with a NMDS ordination. Circles indicate each community and stars show centroids of microbiome types for each animal host. All host microbiomes (internal and external) are distinct from mat communities (P<0.05), but external microbiomes are more similar to mats than internal microbiomes are to mats. in External and internal microbiomes of Antarctic nematodes are distinct, but more similar to each other than the surrounding environment
SI Figure 2: Compositional differences among bacterial microinvertebrate external and internal microbiomes as well as mats they were isolated from using Bray Curtis distance matrix visualized with a NMDS ordination. Circles indicate each community and stars show centroids of microbiome types for each animal host. All host microbiomes (internal and external) are distinct from mat communities (P<0.05), but external microbiomes are more similar to mats than internal microbiomes are to mats.
Simple distance estimates for Gaia DR2 stars with radial velocities
<p>Bayesian distance estimates for stars with radial velocities and parallaxes published in <em>Gaia</em> DR2. Our method and prior is designed to apply to this specific subset of stars in <em>Gaia</em> DR2.</p> <p>The method is published in "Simple distance estimates for Gaia DR2 stars with radial velocities", McMillan 2018, arXiv:1806.00426</p> <p>The code used to produce the estimates is here: https://doi.org/10.5281/zenodo.1270548</p>
Precise distances, masses, ages and 3D velocities of ~140000 red clump stars
<p>We present a sample of $\sim$\,140,000 primary red clump (RC) stars of spectral signal-to-noise ratios higher than 20 from the LAMOST Galactic spectroscopic surveys, selected based on their positions in the metallicity-dependent effective temperature--surface gravity and color--metallicity diagrams, supervised by high-quality $Kepler$ asteroseismology data.<br> The stellar masses and ages of those stars are further determined from the LAMOST spectra, using the Kernel Principal Component Analysis method, trained with thousands of RCs in the LAMOST-$Kepler$ fields with accurate asteroseismic mass measurements. <br> The purity and completeness of our primary RC sample are generally higher than 80\,per cent.<br> For the mass and age, a variety of tests show typical uncertainties of 15 and 30\,per cent, respectively.<br> Using over ten thousand primary RCs with accurate distance measurements from the parallaxes of Gaia\,DR2, we re-calibrate the $K_{\rm s}$ absolute magnitudes of primary RCs by, for the first time, considering both the metallicity and age dependencies.<br> With the the new calibration, distances are derived for all the primary RCs, with a typical uncertainty of 5--10\,per cent, even better than the values yielded by the Gaia parallax measurements for stars beyond 3--4\,kpc.<br> The sample covers a significant volume of the Galactic disk of $4\,\leq\,R\,\leq\,16$\,kpc, $|Z|\,\leq\,5$\,kpc, and $-20\,\leq\,\phi\,\leq\,50^{\circ}$.<br> Stellar atmospheric parameters, line-of-sight velocities and elemental abundances derived from the LAMOST spectra and proper motions of Gaia\,DR2 are also provided for the sample stars.<br> Finally, the selection function of the sample is carefully evaluated in the color-magnitude plane for different sky areas.</p> <p>Details about the table:</p> <p> RA: Right ascension (degrees)<br> DEC: Declination (degrees)<br> GLON: Galactic longitude l (degrees)<br> GLAT: Galactic latitude b (degrees)<br> RV: Line-of-sight velocity (km/s)<br> ERR_RV: Uncertainty of line-of-sight velocity (km/s)<br> TEFF: Effective temperature (K)<br> ERR_TEFF: Uncertainty of effective temperature (K)<br> LOGG: Surface gravity<br> ERR_LOGG: Uncertainty of surface gravity<br> FEH: Metallicity<br> ERR_FEH: Uncertainty of metallicity<br> AFE: Alpha-to-iron abundance<br> ERR_AFE: Uncertainty of apha-to-iron abundance<br> AGE: Stellar age (Gyr)<br> ERR_AGE: Uncertainty of stellar age (Gyr)<br> MASS: Stellar mass (solar mass)<br> ERR_MASS: Uncertainty of stellar mass (solar mass)<br> J: 2MASS J band magnitude<br> ERR_J: Uncertainty of 2MASS J band magnitude<br> H: 2MASS H band magnitude<br> ERR_H: Uncertainty of 2MASS H band magnitude<br> KS: 2MASS Ks band magnitude<br> ERR_KS: Uncertainty of 2MASS Ks band magnitude<br> G: Gaia DR2 G band magnitude<br> ERR_G: Uncertainty of Gaia DR2 G band magnitude<br> BP: Gaia DR2 BP band magnitude<br> ERR_BP: Uncertainty of Gaia DR2 BP band magnitude<br> RP: Gaia DR2 RP band magnitude<br> ERR_RP: Uncertainty of Gaia DR2 RP band magnitude<br> EBV: E (B - V) (mag)<br> MKS: Absolute magnitude in Ks band<br> DISTANCE: distance (kpc)<br> ERR_DISTANCE: Uncertainty of distance (kpc)<br> PARALLAX: Gaia DR2 parallax (mas)<br> ERR_PARALLAX: Uncertainty of Gaia DR2 parallax (mas)<br> PMRA: Proper motion in R.A. (mas/yr)<br> ERR_PMRA: Uncertainty of proper motion in R.A. (mas/yr)<br> PMDEC: Proper motion in Dec. (mas/yr)<br> ERR_PMDEC: Uncertainty of proper motion in Dec. (mas/yr)<br> F_CMD: Selection fraction in color-magnitude diagram</p>
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