We combine high-resolution spectroscopic data from APOGEE-2 survey Data Release 16 (DR16) with broad-band photometric data from several sources, as well as parallaxes from Gaia Data Release 2 (DR2). Using the Bayesian isochrone-fitting code StarHorse, we derive distances, extinctions and astrophysical parameters for around 388,815 APOGEE stars, achieving typical distance uncertainties of 6% for APOGEE giants, 2% for APOGEE dwarfs, as well as extinction uncertainties of 0.07mag when all photometric information is available, and 0.17mag if optical photometry is missing. StarHorse uncertainties vary with the input spectroscopic catalogue, with the available photometry, and with the parallax uncertainties. To illustrate the impact of our results, we show that, thanks to Gaia DR2 and the now larger sky coverage of APOGEE-2 (including APOGEE-South), we obtain an extended map of the Galactic plane, providing an unprecedented coverage of the disk close to the Galactic mid-plane (|ZGal|<1kpc) from the Galactic Centre out to RGal 20 kpc. The improvements in statistics as well as distance and extinction uncertainties unveil the presence of the bar in stellar density, as well as the striking chemical duality in the innermost regions of the disk, now clearly extending to the inner bulge. We complement this paper with distances and extinctions for stars in other public released spectroscopic surveys: 324,999 in GALAH DR2, 4,928,715 in LAMOST DR5, 408,894 in RAVE DR6, and 6,095 in GES DR3.
Combining the precise parallaxes and optical photometry delivered by Gaia's second data release with the photometric catalogues of Pan-STARRS1, 2MASS, and AllWISE, we derived Bayesian stellar parameters, distances, and extinctions for 265 million of the 285 million objects brighter than G=18. Because of the wide wavelength range used, our results substantially improve the accuracy and precision of previous extinction and effective temperature estimates. After cleaning our results for both unreliable input and output data, we retain 137 million stars, for which we achieve a median precision of 5% in distance, 0.20mag in V-band extinction, and 245K in effective temperature for G<=14, degrading towards fainter magnitudes (12%, 0.20mag, and 245K at G=16; 16%, 0.23mag, and 260K at G=17, respectively). We find a very good agreement with the asteroseismic surface gravities and distances of 7000 stars in the Kepler, K2-C3, and K2-C6 fields, with stellar parameters from the APOGEE survey, and with distances to star clusters. Our results are available through the ADQL query interface of the Gaia mirror at the Leibniz-Institut fuer Astrophysik Potsdam (gaia.aip.de) and as binary tables at data.aip.de. As a first application, we provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps as a function of distance, and extensive density maps. These demonstrate the potential of our value-added dataset for mapping the three-dimensional structure of our Galaxy. In particular, we see a clear manifestation of the Galactic bar in the stellar density distributions, an observation that can almost be considered direct imaging of the Galactic bar.
We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's Early Data Release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and AllWISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the StarHorse code, allows us to substantially improve the accuracy and precision over previous photo-astrometric stellarparameter estimates. At magnitude G=14 (17), our typical precisions amount to 3% (15%) in distance, 0.13mag (0.15mag) in V-band extinction, and 140K (180K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface (gaia.aip.de) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit render our results useful also beyond the next Gaia release, DR3.
Tables of Stark broadening profiles for the N V 6f, g, h-7f, g, h, i line complex at 4945A have been generated. Modern close-coupling techniques are used for the electron broadening while the important influence of perturbing ions is included within the framework of the model microfield method. Comparison has been made with the results of line formation calculations using approximate formulae for the Stark profiles.
The tables contain the area normalized Stark broadened spectral profiles of the HeI 492.2nm line. Doppler effect has not been included in the profiles. The first column of each table is the wavelength detuning, measured in nanometers, from the unperturbed wavelength. The other columns give the spectral profiles for different cases of perturber mass and electron temperature. Each table contains the data for a fixed electron density, ranging from 10^20^m^-3^ to 10^24^m^-3^ in different tables. Data corresponding to four different reduced masses of the emitter perturber pair, {mu}, are given in each table. The values of {mu} given in the tables are {mu}=0.8, 2.0, 4.0 and 10.0, in units of the proton mass. For each case of {mu} the profiles for different electron temperatures are given in different columns. Each table has a head giving the electron density value, and the values of {mu} and temperature corresponding to each column.
Using a semiclassical perturbation method, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 52 Be III multiplets as a function of temperature and perturber density. Electron temperatures are 10000K; 20000K; 50000K; 100000K; 200000K and 300000K and perturber densities are from 10^11^cm^-3^ up to 10^21^cm^-3^. The obtained results have been used for discussion of regularities and systematic trends along spectral series.
Using the semiclassical perturbation approach, we have calculated electron-, proton-, He II-, Mg II-, Si II- and Fe II-impact line widths and shifts for 189 Ca I multiplets as a function of temperature and perturber density. Perturbers selected here are the main perturbers in solar atmospheres. Obtained results have been compared with the existing theoretical and experimental data.
We have determined matrix elements for all experimental configurations of CaIII, including the 3s^3^p^6^3d configuration. These values have been obtained using intermediate coupling (IC). For these IC calculations, we have used the standard method of least-squares fitting from the experimental energy levels, using the computer code developed by Robert Cowan. In this paper, using these matrix elements, we report the calculated values of the CaIII Stark widths and shifts for 148 spectral lines, of 56 CaIII spectral line transition probabilities and of eight radiative lifetimes of CaIII levels. The Stark widths and shifts, calculated using the Griem semi-empirical approach, correspond to the spectral lines of CaIII and are presented for an electron density of 10^17^cm^-3^ and temperatures T=1.0-10.0(x10^4^K). The theoretical trends of the Stark broadening parameter versus the temperature are presented for transitions that are of astrophysical interest. There is good agreement between our calculations, for transition probabilities and radiative lifetimes, and the experimental values presented in the literature. We have not been able to find any values for the Stark parameters in the references.