adsabs/AstroCLIMB huggingface dataset:
Paper: Chemical Composition of Bright Stars in the Northern Hemisphere: Star–Planet Connection
Authors: G. Tautvaišienė, Š. Mikolaitis, A. Drazdauskas, E. Stonkutė, R. Minkevičiūtė, E. Pakštienė, H. Kjeldsen, K. Brogaard, Y. Chorniy, C. von Essen, F. Grundahl, M. Ambrosch, V. Bagdonas, A. Sharma, and C. Viscasillas Vázquez
Figure caption: Examples of CCFs produced to calculate the radial velocities and detection of double-line binary stars: (a) the double-line spectroscopic binary HD 152274 observed on 2018 September 19, (b) the same HD 152274 star observed on 2019 June 28, (c) HD 160780 showing three profiles, and (d) the fast-rotating system HD 193341.
Paper: Chemical Composition of Bright Stars in the Northern Hemisphere: Star–Planet Connection
Authors: G. Tautvaišienė, Š. Mikolaitis, A. Drazdauskas, E. Stonkutė, R. Minkevičiūtė, E. Pakštienė, H. Kjeldsen, K. Brogaard, Y. Chorniy, C. von Essen, F. Grundahl, M. Ambrosch, V. Bagdonas, A. Sharma, and C. Viscasillas Vázquez
Figure caption: Examples of synthetic spectrum fits to the C2 band heads at 5135 and 5635 Å, to the CN bands at 6478 and 8003 Å, and to the forbidden [O I] line at 6300 Å. The observed spectra are shown as solid black lines with dots. The solid red lines represent the best fits, while the solid blue and green lines represent a change in abundance by ±0.1 dex of the corresponding elements.
Paper: Chemical Composition of Bright Stars in the Northern Hemisphere: Star–Planet Connection
Authors: G. Tautvaišienė, Š. Mikolaitis, A. Drazdauskas, E. Stonkutė, R. Minkevičiūtė, E. Pakštienė, H. Kjeldsen, K. Brogaard, Y. Chorniy, C. von Essen, F. Grundahl, M. Ambrosch, V. Bagdonas, A. Sharma, and C. Viscasillas Vázquez
Figure caption: Comparison of abundances for the 55 stars in common with APOGEE DR16. The average differences and standard deviations are calculated as our results minus the comparison.
Paper: Chemical Composition of Bright Stars in the Northern Hemisphere: Star–Planet Connection
Authors: G. Tautvaišienė, Š. Mikolaitis, A. Drazdauskas, E. Stonkutė, R. Minkevičiūtė, E. Pakštienė, H. Kjeldsen, K. Brogaard, Y. Chorniy, C. von Essen, F. Grundahl, M. Ambrosch, V. Bagdonas, A. Sharma, and C. Viscasillas Vázquez
Figure caption: Distributions of parameters and elemental abundances in planet-hosting stars and planets as a function of planet masses. The green symbols indicate the planet-hosting dwarfs, the pink symbols are for giants, and the gray symbols are for dwarfs investigated by Mishenina et al. (2021). The circles indicate thin-disk stars, and the triangles are for thick-disk stars. See the text for more information.
Paper: Chemical Composition of Bright Stars in the Northern Hemisphere: Star–Planet Connection
Authors: G. Tautvaišienė, Š. Mikolaitis, A. Drazdauskas, E. Stonkutė, R. Minkevičiūtė, E. Pakštienė, H. Kjeldsen, K. Brogaard, Y. Chorniy, C. von Essen, F. Grundahl, M. Ambrosch, V. Bagdonas, A. Sharma, and C. Viscasillas Vázquez
Figure caption: Elemental abundance ratios as a function of metallicity. The blue dots represent the thin-disk stars, and the red dots show the thick-disk. The dashed lines that separate the disks are from Lagarde et al. (2021). The high-mass planet-hosting stars are marked by green symbols (the two belonging to the thick disk are marked by triangles), the stars with low-mass planets are displayed by yellow symbols, and the one with both one high-mass planet and three low-mass planets is shown by the circle filled with both colors.
Paper: Chemical Composition of Bright Stars in the Northern Hemisphere: Star–Planet Connection
Authors: G. Tautvaišienė, Š. Mikolaitis, A. Drazdauskas, E. Stonkutė, R. Minkevičiūtė, E. Pakštienė, H. Kjeldsen, K. Brogaard, Y. Chorniy, C. von Essen, F. Grundahl, M. Ambrosch, V. Bagdonas, A. Sharma, and C. Viscasillas Vázquez
Figure caption: Differences between elemental abundances in the planet-hosting and comparison stars Δ[El/Fe] as a function of the condensation temperatures of chemical elements. The green labels mark stars hosting low-mass planets, the blue labels show stars with high-mass planets, and the red label marks the star with both types of planets. For stars hosting more than one confirmed planet, their number is provided in brackets near the name. The Pearson correlation coefficients and the slopes for the linear regression analysis are displayed in the upper right corners of the plots.
Paper: Chemical Composition of Bright Stars in the Northern Hemisphere: Star–Planet Connection
Authors: G. Tautvaišienė, Š. Mikolaitis, A. Drazdauskas, E. Stonkutė, R. Minkevičiūtė, E. Pakštienė, H. Kjeldsen, K. Brogaard, Y. Chorniy, C. von Essen, F. Grundahl, M. Ambrosch, V. Bagdonas, A. Sharma, and C. Viscasillas Vázquez
Figure caption: Dependences of Δ[El/Fe]–Tc slopes on the stellar parameters and planet masses. The green circles represent the thin-disk dwarfs, the pink dots show the thin-disk giants, and the thick-disk dwarfs are marked by blue triangles. The size of the symbols depends on the number of confirmed planets in the system. The red lines display linear fits to the data points, and their Pearson correlation coefficients are presented as labels in the corners of the panels.
Paper: Measurements and Calculations of Radiative Parameters for Odd-parity Levels in Nb II
Authors: Yidan Geng, Yong Liu, Hongfeng Zheng, Ziqing Yu, Ting Wang, Pascal Quinet, Bing Yan, and Zhenwen Dai
Figure caption: A typical fluorescence decay curve of the 50,497.841 cm−1 level of Nb II from using an excitation pulse and an exponential function.
Paper: Measurements and Calculations of Radiative Parameters for Odd-parity Levels in Nb II
Authors: Yidan Geng, Yong Liu, Hongfeng Zheng, Ziqing Yu, Ting Wang, Pascal Quinet, Bing Yan, and Zhenwen Dai
Figure caption: Comparison of deviation between theoretical (MCDHF and HFR) and experimental lifetimes.
Paper: Measurements and Calculations of Radiative Parameters for Odd-parity Levels in Nb II
Authors: Yidan Geng, Yong Liu, Hongfeng Zheng, Ziqing Yu, Ting Wang, Pascal Quinet, Bing Yan, and Zhenwen Dai
Figure caption: Comparison between the semiempirical and theoretical HFR+CPOL weighted transition probabilities (gA) obtained in the present work for Nb II spectral lines.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Left: spatial distribution of galaxies around the Virgo galaxy cluster, up to ∼12 virial radii from its center, in projection. Points show galaxies coded according to their recession velocities. The red rectangle shows the region of the Virgo cluster, which is examined in more detail in Figure 3. Right: radial velocity distribution of all galaxies in our catalog. The black solid line shows the distribution of galaxies brighter than the absolute magnitude completeness limit of the catalog (Mr = −15.7).
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Comparison between the redshift-independent distances obtained from Steer et al. (2017) and those inferred from vmodel for the galaxies present in the Steer et al. (2017) catalog (black points). The green line is the 1:1 relation. The red line shows the linear fit to the point, while the shaded red region denotes the corresponding ± 1σ scatter.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Left: phase-space diagram for sources in the field of the Virgo cluster. The solid lines show the radial dependence of the escape velocity in the phase-space diagram, according to the prescription by Jaffé et al. (2015). Cluster members defined in the super-Galactic (X, Y, Z) coordinate frame (red points) or within the region (blue points) delimited by the caustics (i.e., the two solid lines) are distinguished from the remaining sources in the field of Virgo cluster (gray points). Right: projected distribution of the cluster members on the sky.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Galaxies in the vicinity of the Virgo III filament. Galaxies within 2 h−1 Mpc are color-coded by the 3D local density, and galaxies with separations greater than 2 h−1 Mpc are shown with the gray points. The filament spine is shown with the black curve. Interactive 3D plots for all filaments are available for download from Zenodo at doi:10.5281/zenodo.6341838.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Spatial distribution of galaxies around the Virgo galaxy cluster. Gray points show all galaxies, colored points show galaxies belonging to the different filaments. This color scheme will be kept in all plots.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Absolute magnitude Mr as a function of velocity Vmodel (black line) and magnitude limit of the survey (horizontal dashed line). Stars represent the magnitude limit proper of each filament separately, and the green square the magnitude limit of the cluster. These limits are obtained as the magnitude including 95% of the data. For display purposes, points of the different filaments are also shown in colors, with an arbitrary vertical shift to avoid the superimposition of the points.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Galaxy density versus distance from the filament spine. Dashed lines show the exponential fit, see text for further details.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Scale length r0 (left) and central density contrast (right), i.e., the ratio of the density enclosed within 1 h−1 Mpc to the best-fit value b at large radii, as a function of filament length.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Euler–Venn diagram summarizing the distribution of galaxies in the different global environments.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Comparison between the local number density estimates for the galaxies in the sample. The x-axis shows the 3D volume number densities. The y-axis displays the 2D surface densities translated into 3D volume densities, obtained dividing by the slice width ΔSGY = 5.6h−1 Mpc.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Left: halo mass distribution for galaxies in the different environments, using the group memberships and halo mass distributions from Kourkchi & Tully (2017). Right: spatial distribution of groups and filaments around the Virgo galaxy cluster. Shaded gray points represent all groups in the velocity range 500 < vr < 3300  km s−1 according to Kourkchi & Tully (2017). Lines represent the filament spines; colored points represent the groups that share galaxies with the corresponding filament, plotted with the same color. The size of the points scales as the halo mass.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Volume 3D number density distribution for galaxies in the filaments (red), in the Virgo cluster (green), and in the field (gray) for galaxies above the absolute magnitude completeness limit. The reported errors are standard deviations, while the error of the means is much smaller, of the order of 0.05 dex at most. The firebrick cross and error bar show the median density for filaments when the W–M Sheet and the Ursa Major Cloud are removed from the filament sample.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Volume number density distribution for galaxies in groups of different halo masses and in filaments (blue histograms). Red histograms show the overall distribution for filament galaxies. The solid vertical lines show the median values of the distributions, while the error bars show the 1σ uncertainties.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Volume number density (n5,3D) distribution for galaxies in each filament separately (red). For each filament, the proper absolute magnitude limit (see Table 5) has been adopted to increase the statistics. For comparison, the distributions of galaxies in the Virgo cluster (green) and in the field (gray) are also reported, above the same completeness limit and limiting the sample to the same velocity. Vertical lines represent median values, horizontal lines the standard deviation, representing the scatter of the distribution.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Fraction of galaxies of different morphological types in the different environments, as described in the legend. A small arbitrary horizontal shift has been applied to the points for the sake of clarity.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Median morphological parameter for filaments (colored stars), pure field (gray point), and the Virgo cluster (green square). Error bars represent 1σ dispersion. The color code for filaments is the same as in Figure 5.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: LT fraction as a function of different environments (left) and local density (center, right). Different environments are considered in the left panel: cluster galaxies (CL), filament galaxies (F), pure field galaxies (PF), galaxies in rich (RG) and poor (PG) groups, as well as a combination of these classes, at intermediate environments. In the central panel, the right border of the green dashed area defines the conservative upper limit to the local density for Virgo cluster galaxies. A small arbitrary horizontal shift has been applied to the points for the sake of clarity.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Bar fraction as a function of the environment (left), local density (center), and morphology (right). Only lenticular galaxies and normal spirals are considered; see text for details. For the left panel, the different environments are reported as in Figure 17 (left). In the central and right panels, filaments (colored stars), pure field (gray point), and the Virgo cluster (green square) are distinguished. The color code for the filaments is the same as in Figure 5.
Paper: Virgo Filaments. II. Catalog and First Results on the Effect of Filaments on Galaxy Properties
Authors: Gianluca Castignani, Benedetta Vulcani, Rose A Finn, Francoise Combes, Pascale Jablonka, Gregory Rudnick, Dennis Zaritsky, Kelly Whalen, Kim Conger, Gabriella De Lucia, Vandana Desai, Rebecca A Koopmann, John Moustakas, Dara J Norman, and Mindy Townsend
Figure caption: Violin plots of the alignments θalignment for ET (top) and LT (bottom) galaxies in filaments. For each filament, medians and the interquartile ranges are also shown with circles and thick bars, respectively. We report in parentheses the number of galaxies in each filament.
Paper: Very Local Interstellar Medium Revealed by a Complete Solar Cycle of Interstellar Neutral Helium Observations with IBEX
Authors: P. Swaczyna, M. A. Kubiak, M. Bzowski, J. Bower, S. A. Fuselier, A. Galli, D. Heirtzler, D. J. McComas, E. Möbius, F. Rahmanifard, and N. A. Schwadron
Figure caption: Linear coefficients of the RV-norm scaling function for each observational season. The red and blue symbols correspond to periods with the nominal and the lowered PAC voltage, respectively, with the coefficient value provided on the left and right axes, respectively.
Paper: Very Local Interstellar Medium Revealed by a Complete Solar Cycle of Interstellar Neutral Helium Observations with IBEX
Authors: P. Swaczyna, M. A. Kubiak, M. Bzowski, J. Bower, S. A. Fuselier, A. Galli, D. Heirtzler, D. J. McComas, E. Möbius, F. Rahmanifard, and N. A. Schwadron
Figure caption: Comparison of the best-fit model using the RV-norm with the IBEX data. Each row shows the result for one observational season. The top part of each panel compares the data with the models, and the bottom part shows the residual signal. Red and blue symbols show results for the global fit and the fit with this observational season, respectively.
Paper: Very Local Interstellar Medium Revealed by a Complete Solar Cycle of Interstellar Neutral Helium Observations with IBEX
Authors: P. Swaczyna, M. A. Kubiak, M. Bzowski, J. Bower, S. A. Fuselier, A. Galli, D. Heirtzler, D. J. McComas, E. Möbius, F. Rahmanifard, and N. A. Schwadron
Figure caption: Top panel: mean survival probability obtained from the WTPM with the nominal ionization model (black line) and a proportionally scaled ionization (gray line; see the text). The colored lines show mean survival probabilities based on the coefficients of the scaling function obtained under three possible scenarios (see the text). Bottom panel: ratio of the ionization rates expected under these scenarios to the ionization rate used in the model. The ratio equal to one indicates consistency with the adopted ionization model. The vertical dashed line indicates the change in the PAC voltage.
Paper: Very Local Interstellar Medium Revealed by a Complete Solar Cycle of Interstellar Neutral Helium Observations with IBEX
Authors: P. Swaczyna, M. A. Kubiak, M. Bzowski, J. Bower, S. A. Fuselier, A. Galli, D. Heirtzler, D. J. McComas, E. Möbius, F. Rahmanifard, and N. A. Schwadron
Figure caption: Fitting results to individual observational seasons (color symbols) and all seasons (black symbols). The best-fit parameters are marked with filled symbols, and ellipses indicate 1σ uncertainty ranges. The following pairs of parameters are presented in panels: longitude-latitude (top left), longitude-temperature (top right), longitude-speed (bottom left), and speed-temperature (bottom right).
Paper: Very Local Interstellar Medium Revealed by a Complete Solar Cycle of Interstellar Neutral Helium Observations with IBEX
Authors: P. Swaczyna, M. A. Kubiak, M. Bzowski, J. Bower, S. A. Fuselier, A. Galli, D. Heirtzler, D. J. McComas, E. Möbius, F. Rahmanifard, and N. A. Schwadron
Figure caption: Temporal changes in the best-fit parameters of the ISN helium flow: longitude (top left), latitude (top right), speed (bottom left), and temperature (bottom right). Blue symbols show the results of independent fits to each observational season. The bars show 2σ uncertainties, and 1σ uncertainties are limited by fences. The red line presents the global time-independent fit (see Section 5) with the 1σ uncertainty band, and the green line shows the fit with linear changes in each parameter also with 1σ uncertainty band. Note that these bands overlap in large portions of the plots.