adsabs/AstroCLIMB huggingface dataset:
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The distribution A(Li) as a function of T eff for the different stellar families indicated in the figure. The program stars are marked by large red diamonds. The best fits for the giants (in blue) and dwarfs (in black) are shown by solid lines along with the 1σ regions for each fit. The slope and σ of the fit for the giants are 0.0012 dex K−1 and 0.19 dex K−1, respectively, while for the dwarfs they are 0.0005 dex K−1 and 0.12 dex K−1, respectively.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The nucleosynthesis pattern for the program stars, compared to the samples from Cayrel et al. (2004) and Cohen et al. (2004). The error bars corresponding to the uncertainties in the abundances for each element are shown as black lines.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The distribution of A(Li) as a function of [Fe/H]. Predictions from the Planck mission and the Spite plateau abundances are shown by black solid lines. The dwarf stars are marked in black, while giant stars are marked in blue. CEMP-no stars are shown as red dots. The program stars with Li detections in this study are shown by filled red diamonds.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: Toomre diagram exhibiting the orbital characteristics of the program stars. The dotted line indicates the split between prograde and retrograde motions. The blue-filled circles represent the program stars, while the red-filled star indicates SDSS J065252.76+410506.0. The blue semicircle shows the expected location of the disk stars in this diagram. The green open circles represent stars in the Spite plateau from the literature.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The distribution of the light elements Al, Mg, Ca, Ti, and Si as a function of [Fe/H]. The blue-filled circles represent the program stars, while the red-filled circle denotes the abundances for SDSS J065252.76+410506.0. The GC escapees are shown as blue-filled diamonds. The abundances of other metal-poor stars in literature compiled from Suda et al. (2008) are shown as black dots. The uncertainties are marked by colored error bars.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The distribution of the Fe-peak elements Sc, Cr, Mn, Co, Ni, and Zn as a function of [Fe/H]. The blue-filled circles represent the program stars, while the red-filled circle denotes the abundances for SDSS J065252.76+410506.0. The abundances of other metal-poor stars in literature compiled from Suda et al. (2008) are shown as black dots. The uncertainties are marked by colored error bars.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: An example of spectral fitting for the molecular CH G-band region. The black-filled circles denote the observed spectra while the colored lines indicate the synthetic spectra. Red shows the best spectral fit, while black and blue lines indicate the spectra for C abundance deviating by ±0.50 dex from the best fit.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The Li abundance for VMP and EMP stars with detections of Li. The black dots mark the dwarf stars, while blue dots represent the giants. The GC escapees from this study are marked with red-filled triangles, and the CEMP-no star is marked with a pink diamond.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: Li abundance as a function of distance from the Galactic plane. The color bar shows the metallicity of the stars. The new stars are marked by filled diamonds.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: Orbital characteristics of the program stars. The black dotted line separates prograde motions from retrograde motions, while the red dotted lines show the regions dominated by stars formed in situ, accreted stars, and the mixed zone. The main-sequence and turnoff VMP and EMP stars with Li measurements compiled from Suda et al. (2008) are shown as green circles. The stars on the Spite plateau are shown as filled green circles, while slightly Li-poor stars are shown with green open circles.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The trajectory of SDSS J0652+4105 in Galactocentric coordinates, which appears in the in situ region of Figure 13. The orbit is shown in the XY, XZ, and YZ planes. The trajectory has been calculated up to 5 Gyr back in time from the present day.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The same as Figure 14 for two representative stars falling in the mixed zone of Figure 13. The names of the individual stars are mentioned on the respective figures.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The distribution of the neutron-capture elements Sr and Ba as a function of [Fe/H]. The blue-filled circles represent the program stars, while the red-filled circle denotes the abundances for SDSS J065252.76+410506.0. The uncertainties are marked by colored error bars.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The same as Figure 14 for SDSS J0646+4116, which appears in the accreted region of Figure 13.
Paper: The Magnetic Field Environment of Active Region 12673 That Produced the Energetic Particle Events of September 2017
Authors: Stephanie L. Yardley, Lucie M. Green, Alexander W. James, David Stansby, Teodora Mihailescu
Figure caption: Panel (a) shows the radial photospheric magnetic field of AR 12673 taken by the Helioseismic Magnetic Imager on board the Solar Dynamics Observatory (SDO/HMI; Scherrer et al. 2012). The radial magnetic field component is from the HMI Spaceweather HMI Active Region Patch (SHARP) data series (Bobra et al. 2014) where positive (negative) field is represented by white (black), respectively, saturated at ±500 G. Panel (b) displays the GOES-13 proton flux (10, 30, 60 MeV channels) with two SEP events detected on 2017 September 4 and 6. The black dashed line represents the 10 MeV warning threshold above which a proton event alert is issued by NOAA/SWPC. The purple dashed lines indicate the start times of the two SEP events, which are 2017 September 4 at 22:30 UT and 2017 September 6 at 12:35 UT, respectively.
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: Discrete and continuous numerical issues with fitting Keplerian orbits to directly observed short-period planets (presumably, the observation cadence would be tailored for a longer-period planet in the habitable zone that is not shown). (a) Three equally spaced observations (diamonds) around the star at (0, 0) can correspond to very different orbits. The orbits marked by dashed red, solid black, and dashed–dotted green lines correspond to planets that complete three, two, and one revolution(s) per year, respectively. Besides this discrete ambiguity in the period, the eccentricity can also take a large range of values from almost 0 (dashed–dotted green line) to over 0.5 (dotted blue line) and still fit the data well (see the discussion on constraining eccentricity by Morgan et al. 2019). Here, each of the orbits fits the data points with an rms error below 0.03 au. (b) rms astrometry errors of best-fit orbits with a given semimajor axis and eccentricity (the other four parameters were optimized over). Many local minima are visible, and some of the corresponding orbits fit the data poorly. Moreover, the narrow curving “valleys” seen in this error map are challenging for gradient-descent algorithms.
Paper: The Magnetic Field Environment of Active Region 12673 That Produced the Energetic Particle Events of September 2017
Authors: Stephanie L. Yardley, Lucie M. Green, Alexander W. James, David Stansby, Teodora Mihailescu
Figure caption: A schematic showing the magnetic field configuration (null point, open magnetic field, Earth-connected field), taken from the PFSS model, at the time of each eruptive event along with the 193 Å  emission and photospheric magnetic field. In the top panels the white (black) features represent the positive and negative magnetic polarities of ARs 12673 and 12674 along with decayed/quiet Sun field. Red lines show the location of closed magnetic field, whereas blue represents the open magnetic field. Purple shows the magnetic field lines that are Earth-connected (EC), taken from the results of the PFSS and ballistic propagation model. In the bottom panels the same labels apply. There is a small coronal hole (CH) visible to the east of AR 12673. The black arrows show the propagation directions of the eruptions. Finally, in panel (c) the green arrow demonstrates the direction of the coronal loops during event 3 that drives reconnection at the null.
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: The confusion problem. (a) Astrometry of directly imaged planets does not reveal which detection corresponds to which planet. Multiple possible combinations of the orbits (b and c) fit the data perfectly and have “reasonable” orbital parameters. The confusion problem might be more severe in realistic observations that will include more epochs in which not all planets are visible or false detections are present.
Paper: The Magnetic Field Environment of Active Region 12673 That Produced the Energetic Particle Events of September 2017
Authors: Stephanie L. Yardley, Lucie M. Green, Alexander W. James, David Stansby, Teodora Mihailescu
Figure caption: The magnetic connectivity of Earth during 2017 September 4–7 (Carrington rotation 2194). The top panel shows the synoptic map of the longitudinal magnetic field taken by GONG on 2017 September 9 at 23:14 UT. The black lines represent the field lines connected to Earth during the time of the four eruptive events moving from right to left, and the location of the heliospheric current sheet. The green line represents the back-projected trajectory of the Earth. The gray dashed lines correspond to the Carrington times labeled above and the red dotted–dashed line indicates the time and longitude that the synoptic map was last updated. In the bottom panel the corresponding SDO/AIA 193 Å synoptic map is shown. The black and green lines correspond to the position of the heliospheric current sheet and backtracked trajectory of as above. The purple, blue, green, and yellow lines show the magnetic field lines connected to Earth on 2017 September 4 at 18:00 UT, 2017 September 4 at 20:05 UT, 2017 September 6 at 11:52 UT, and 2017 September 7 at 14:31 UT, respectively.
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: Deconfusion steps. (a) Unlabeled detections are given in terms of astrometry. (b) Detections are matched with orbits within the given eccentricity and fit-error constraints. (c) Combinations of orbits are ranked based on how well they explain the data (only the first four orbit combinations are shown). Orbits that match more observations are ranked higher, in this case, resulting in combinations with fewer planets. In cases when two detections are matched to a planet (green circles), the orbit is not fully determined. (d) To break ties, orbit scores are refined based on other criteria, such as astrometry errors.
Paper: The Magnetic Field Environment of Active Region 12673 That Produced the Energetic Particle Events of September 2017
Authors: Stephanie L. Yardley, Lucie M. Green, Alexander W. James, David Stansby, Teodora Mihailescu
Figure caption: Potential magnetic field extrapolations on September 4, 6, and 7 at 18:04 UT, 12:04 UT, and 12:04 UT, respectively. The radial magnetic field shows positive (negative) magnetic polarities that are saturated at ±300 G in white (black). The pink lines represent magnetic field that is open, and the blue lines represent magnetic field that belongs to a magnetic null point located between AR 12673 and AR 12674. On September 4 (panel (a)) the field lines associated with the null are closed whereas, on September 6 and 7 (panels (b) and (c)) the magnetic field of the null are partially and completely open on the west side.
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: Analysing confusion rates by random sampling planet astrometry and applying the proposed deconfuser algorithm. The deconfuser finds all possible combinations of orbits that match the observations within a specified tolerance and ranks them based on their explanatory power (see Figure 3 for an example). Cases that yield multiple equally ranked combinations are considered “confusions” in this paper.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Estimates of M TOV and M 99 for different priors on the population a 2 distribution parameters β s and ﹩{a}_{\max }/{a}_{\mathrm{Kep}}﹩, using the “ZS” spin prior: free β s and ﹩{a}_{\max }/{a}_{\mathrm{Kep}};﹩ fixed β s = 0 fixed ﹩{a}_{\max }/{a}_{\mathrm{Kep}};﹩ and ﹩{a}_{\max }/{a}_{\mathrm{Kep}}﹩ (nonspinning); and fixed ﹩{a}_{\min }/{a}_{\mathrm{Kep}}=0.9﹩ (requiring maximally spinning GW190814). All events are fit with a one-component NS mass model and random pairing (β = 0).
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Estimates of M BH for different a 2 priors with pairing function β = 0: uniform and isotropic (“U + I”, black solid), nonspinning BH (default “ZS”, blue dashed), and nonspinning BH + aligned-spin NS (“ZS + AS”, red dotted). Posterior on M BH for the “ZS” spin prior with β = 3 is shown (green dashed–dotted). All events fit with a one-component NS mass model.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Median and 68% credible interval of the nonspinning NS mass distribution p(m 2) as inferred from variations on our fiducial model: All four NSBH events with a one-component NS mass function, the “ZS” spin prior, and β = 0. Each panel shows a different set of variations. The 95% credible interval for m 2 is shown for each NSBH event.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Posterior predictive distributions of NSBH events (conditioned on detection), as inferred under the different models, using the “ZS” spin prior and pairing function β = 0. 68% credible intervals on M TOV and M BH are shown. 90% contours for the LVK NSBH events are overplotted (horizontal and vertical bars). In (a) and (b), the black dotted line shows equal NS and BH mass; we define a mass gap as M TOV < M BH. In (c) and (d), black dotted lines show M crit for a given M TOV and spin a 2/a Kep. (a) and (b) show 2500 draws each; (c) and (d) show events over 2M ⊙ from 10,000 draws.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Constraints on the minimum spin of GW190814's secondary given its mass (using the “ZS” spin model), assuming it is a massive rotation-supported neutron star from population estimates of M TOV. a 2/a Kep = 0 means no spin support is required to make GW190814's mass consistent with the NSBH population inferred from the other events.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Joint posterior (68% and 95% contours) based on data from all NSBH events, the default “ZS” spin prior, and a one-component NS mass model.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Inferred M TOV when ignoring (hashed pattern) versus properly accounting for a spin-dependent maximum mass. Median, 68%, and 95% credibility intervals are shown.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Posteriors on M TOV and the slope A 1 govern the maximum NS mass as a function of NS spin, inferred from 150 mock events at LIGO A+ sensitivity. Contours enclose 68% and 95% of the posterior probability.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Simulated posteriors on M TOV and M BH from 150 NSBH events at LIGO A+ sensitivity. Contours enclose 68% and 95% of the posterior probability.
Paper: Beyond Galaxy Bimodality: The Complex Interplay between Kinematic Morphology and Star Formation in the Local Universe
Authors: A. Fraser-McKelvie, L. Cortese
Figure caption: Histograms of ﹩\mathrm{log}V/\sigma ﹩ for the volume-corrected MaNGA sample in four stellar mass bins. For each panel, the fast rotators are denoted by a purple histogram and the slow rotators by a red histogram. The fast rotators are modeled with a Gaussian mixture model, which is best described by two populations: the dynamically cold disk population, which is shown as a navy line, and 1σ below the mean, shown as a gray dashed line. The gray dashed line denotes the division between dynamically cold disks and intermediate systems for this work.
Paper: H I HOD. I. The Halo Occupation Distribution of H I Galaxies
Authors: Fei Qin, Cullan Howlett, Adam R. H. Stevens, David Parkinson
Figure caption: Parameters of Equations (3a) and (3b) as functions of the H I mass. The blue filled circles are the parameters fitted by comparing the model HOD to the measured HOD in each H I mass bin. The black lines and curve are the best fits to the blue filled circles, resulting in our 15 “hyperparameters”. The orange dashed lines and curve are the best-fit results obtained by comparing model ξ  gg  to the measured ξ  gg . Differences between this figure and Figure 7 for overlapping parameters arise due to the fact that we have forced the remaining two of the parameters of the full HOD model (not plotted here) to follow Equation (18), which was not the case for Figure 7.
Paper: H I HOD. I. The Halo Occupation Distribution of H I Galaxies
Authors: Fei Qin, Cullan Howlett, Adam R. H. Stevens, David Parkinson
Figure caption: Fitted HOD parameters from the galaxy two-point correlation function for the DARK SAGE simulation. In the left-hand panels, the top shows the correlation function measurement (blue filled circles) and the model (red curve) fit to the measurement. This is further decomposed into the corresponding one-halo, ﹩1+{\xi }_{{gg}}^{1h}﹩, and two-halo, ﹩{\xi }_{{gg}}^{2h}﹩, terms (dashed gray and dashed–dotted purple, respectively). The bottom panel shows the measured HOD and that inferred from the fitted correlation function (yellow points and green line, respectively). The fit results of the HOD parameters are shown in the right-hand panels. The histograms show the distribution of the MCMC samples. The shaded areas in the 1D plots indicate the 68% confidence level, while the 2D contours indicate the 1, 1.5, 2, and 2.5σ regions.
Paper: Beyond Galaxy Bimodality: The Complex Interplay between Kinematic Morphology and Star Formation in the Local Universe
Authors: A. Fraser-McKelvie, L. Cortese
Figure caption: Sample selection for this work on the SFR–stellar mass plane. The overall MaNGA sample is shown in gray, galaxies for which kinematics were computed are shown as open mauve circles, and the final sample after quality and stellar mass cuts are shown as filled mauve circles with black outlines. Histograms of all three distributions are shown in stellar mass (top) and SFR (right). There is a strong mass dependence such that low-mass galaxies frequently do not possess kinematic measures. For this reason, coupled with low number statistics at the high-mass end, we restrict our proceeding analysis to ﹩9.75\lt \mathrm{log}{M}_{\star }[{M}_{\odot }]\lt 11.75﹩.
Paper: H I HOD. I. The Halo Occupation Distribution of H I Galaxies
Authors: Fei Qin, Cullan Howlett, Adam R. H. Stevens, David Parkinson
Figure caption: Comparison of the model HOD (green and black curves for central and satellite galaxies, respectively) predicted by our 15 best-fit “hyperparameters” and the measured HOD (pink circles and blue squares for centrals and satellites, respectively) for three example M HI bins. This plot looks functionally very similar to Figure 6, which emphasizes the fact that we are able to recover well the measured HODs for various H I mass bins using our “hyperparameters”, rather than fitting each bin individually.