adsabs/AstroCLIMB huggingface dataset:
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Posterior distribution of hyperparameters for the TWO_COM_R model.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Posterior distribution of hyperparameters for the ONE_COM model.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: The horizontal axis is the velocity in the rest frame of the absorber, where v = 0 km s−1 corresponds to z = 0.39047 (vertical dotted–dashed line). The multicomponent cumulative Voigt profile fits are shown in orange. The different components are shown separately, and their centroids are marked by colored vertical markers. The absorption profile of C III is saturated. The N V λ λ1238, 1242 lines are covered but not detected. The Si III 1206 is contaminated. Hence both these lines are shown in the Appendix, Figure 10. For the Si II, we attempt a three-component model based on the profile structure seen for the 1260−1190 Å lines. Such a simultaneous model does not perfectly fit all lines of the multiplet but recovers the total column density for Si II that we obtain from AOD measurements. The column densities of these three components are added together while modeling the LLS component at v ≈ 0 km s−1. The column densities of the two components of N II are also added together while modeling the LLS. The N III 989 panel is the residual flux after subtracting the absorption feature in the Si II 989 panel from its corresponding Voigt profile model. The vertical dashed lines in that panel define the velocity range over which the apparent optical depth was integrated to get a lower limit on the N III column density.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: Left: corner plot from photoionization modeling of the first component responsible for the Lyman break. It shows the posterior and marginalized distribution of the absorber’s metallicity (Z) and hydrogen number density (n H ). The values denoted by dashed lines are the median and 16th–84th percentile values of the marginalized distribution. Right: observed (blue) column densities of the species C II, Si II, N II, and O VI in the increasing order of their ionization potentials, with 1σ error bars. For Fe II, Fe III, N V, N III, and C III, we have indicated the observed upper and lower limits with arrows. The red curves show the column density predictions for random samples of n H  and Z from posteriors. The thick black line shows the column density predictions for the median values of n H  and Z. It can be seen that Si II is underpredicted by ∼0.4 dex, suggesting a subsolar [C/α] value. For other species, the predictions are in agreement with the observations, except for O VI, which implies that O VI exists in a different phase than the rest of the species detected in this component.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: Column densities of C II, C III, Si II, N III, N V, and O VI predicted by CLOUDY with respect to the number density of hydrogen for the metallicity, ﹩\mathrm{log}(Z/{Z}_{\odot })=-0.90﹩, which is a lower limit. The highlighted portions of the curves show the range of hydrogen number density values that satisfy the observations. The saturated C III absorption is not explained if the metallicity goes below the lower limit. Also, the lower limit on N V column density due to nondetection is explained only if the metallicity of Nitrogen is 0.2 dex lower than the rest of the elements. Thus, we obtain a range for hydrogen number density for which all the observations can be explained.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: Voigt profile fits for the Lyα transition. The top panel shows the two-component Voigt profile fit to the absorption line, with the first and second component fits shown in red and green colors, respectively, and the resultant combined fit shown by the thick profile. The pixels in cyan color are not fit properly by the current Voigt profile. The bottom panel shows a three-component Voigt profile fit (the thick profile), which beautifully fits the entire absorption line. The first, second, and third component fits are shown in red, green, and blue, respectively. The third component is a BLA, as is clear from the broad and shallow profile.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: The top left panel shows a narrow Hα emission image at the location of the absorber, obtained from the continuum and quasar PSF subtracted IFU data cube. The top right panel shows the zoomed-in image of galaxy G0, a GOTOQ. The bottom panels show the emission-line-rich spectra of G1 and G0 extracted by adding the spaxels covered by them, which were used to find their redshifts that resulted in a value almost the same as the absorber redshift ∼0.39. The emission feature labeled “QSO” in the G0 spectrum is residual O II emission, after PSF subtraction, from the quasar itself.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: Ionization fraction models from O. Gnat & A. Sternberg (2007) for ﹩\mathrm{log}(Z/{Z}_{\odot })=-0.50﹩. The blue curve represents the CIE column density of O VI, respectively, with respect to the temperature. The vertical black dashed lines correspond to constant temperature; the gray region shows the 1σ temperature range; and the horizontal dashed line corresponds to the observed O VI column density. This shows that the calculated temperature is in agreement with the CIE models at the observed O VI column density.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: This plot shows the higher-order Lyman series lines, with the flux shown in black; the mean continuum level is shown by the horizontal dotted–dashed line; the magenta curves are the two-component Voigt profile fits to the Lyman lines with the first and second components marked by the red and green markers, respectively. A very high neutral hydrogen “column” density causes a sharp decline in the flux around the location of the redshifted (z ∼ 0.39) Lyman limit break.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Comparison between the measured (red diamonds) and modeled (blue-dashed line) λ MMS. The latter is calculated using Equation (C2) with ﹩{ \mathcal C }=3.4.﹩
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Projected surface density derived from box orbits in model B at t = 4.5 Gyr. Sequential panels display the dependence of box orbit morphologies across bins of the net rotation parameter ﹩\overline{L}{zn}﹩, with the fractional contribution of orbits in each ﹩\overline{L}{zn}﹩ bin to the total structure given as a percentage. Box orbits with higher normalized angular momentum ﹩1\gt \overline{L}{zn}\gt 0.3﹩ predominantly facilitate the OX structure, whereas those within the range of ﹩0.3\gt \overline{L}{zn}\gt -0.2﹩ are forming the CX structure.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: The globally measured bar quantities as a function of time for model A (orange), model B (red), and model C (blue). The panels from top to bottom represent (1) the buckling amplitude (A buck), which is the scaled m = 2 asymmetry about the midplane; (2) the bar amplitude (A  m  = 2), which is the scaled m = 2 Fourier amplitude; (3) the bar length; and (4) the bar pattern speed. For model C, the A  m  values are multiplied by a factor of 0.75, and the pattern speed is multiplied by a factor of 0.3 for better visualization.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Projected surface density from 15,000 selected orbits in model B at t = 4.5 Gyr. The first row displays the x- y plane, while the second row shows the x- z plane. The columns from left to right represent the surface densities of all, OX, CX, box, x 4, LAT, and disk orbits, respectively. Each panel is labeled with the fractional contribution of each orbital structure to the total, given as a percentage.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Unsharp-masked image and projected surface density in face-on and edge-on views for model A (left), model B (middle), and model C (right). The top row shows snapshots taken shortly after the formation of the BP/X structure, while the bottom row represents snapshots taken around the end of the simulation.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: The top row shows the S4G images for NGC 1381 and NGC 4710. The bottom row shows the unsharp-masked version of each image. The BP/X-shaped structure in NGC 1381 is predominantly of the CX shape, while NGC 4710 displays an OX structure.
Paper: Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Oleg Kochukhov, Diogo Souto, C. Allende Prieto, Suvrath Mahadevan, Steven R. Majewski, Philip S. Muirhead, Marc Pinsonneault, Ryan Terrien
Figure caption: Derived mean magnetic fields for the sample of planet-hosting M dwarfs as a function of rotational periods (filled blue circles). Other results for M dwarfs from the literature are also shown (gray xs, S. H. Saar & J. L. Linsky 1985; S. H. Saar 1994, 1996; C. M. Johns-Krull & J. A. Valenti 1996, 2000; O. Kochukhov et al. 2001, 2009; N. Afram et al. 2009; N. Phan-Bao et al. 2009; D. Shulyak et al. 2011, 2014, 2017, 2019; O. Kochukhov & A. Lavail 2017; O. Kochukhov & D. Shulyak 2019; A. Reiners et al. 2022; P. I. Cristofari et al. 2023a, 2023b), along with results for a sample of Pleiades M-dwarf stars from F. Wanderley et al. (2024) (open orange circles). The gray dashed line at P rot = 7 days represents the threshold that separates the saturated from the unsaturated regime. The mean magnetic fields for our sample fall in the unsaturated regime.
Paper: Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Oleg Kochukhov, Diogo Souto, C. Allende Prieto, Suvrath Mahadevan, Steven R. Majewski, Philip S. Muirhead, Marc Pinsonneault, Ryan Terrien
Figure caption: Magnetic field analysis for the star 2M07590587+1523294. The left panels show the four Fe I lines used in the modeling: black dots are the observed APOGEE spectrum, red dashed lines are synthetic profiles computed without a magnetic field, and dark blue lines are our best fits obtained from the Markov Chain Monte Carlo modeling. The right panel is a corner plot that presents the median and uncertainties (from 16th and 84th percentiles) of the derived parameters, which includes filling factors from magnetic fields between 2 and 6 kG in steps of 2 kG. We also show the final magnetic field result and its uncertainties.
Paper: Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Oleg Kochukhov, Diogo Souto, C. Allende Prieto, Suvrath Mahadevan, Steven R. Majewski, Philip S. Muirhead, Marc Pinsonneault, Ryan Terrien
Figure caption: Derived mean magnetic fields for the sample of planet-hosting M dwarfs as a function of Rossby numbers (filled blue circles). Results for M dwarfs from A. Reiners et al. (2022) are shown (gray xs). The gray dashed line at Ro = 0.13 represents the threshold that separates the saturated from the unsaturated regime.
Paper: Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Oleg Kochukhov, Diogo Souto, C. Allende Prieto, Suvrath Mahadevan, Steven R. Majewski, Philip S. Muirhead, Marc Pinsonneault, Ryan Terrien
Figure caption: The distribution of the derived mean magnetic fields for the sample of M dwarfs studied here (blue histogram), and for a sample of M-dwarf stars belonging to the young Pleiades open cluster from F. Wanderley et al. (2024) (orange histogram).
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Top: composite image of the HD 111520 disk from optical HST/STIS data on large scales and GPI H-band data within the HST coronagraph mask. This figure is modified from K. A. Crotts et al. (2022). Middle: synthetic scattered light image of the HD 111520 disk with one planet orbiting outside the warp (a pl = 250 au) Bottom: synthetic scattered light image of the HD 111520 disk with one planet orbiting inside the disk inner edge (a pl = 40 au). For both models, the surface brightness is the same in log scale, and the surface brightness units are arbitrary. Additionally, the disk is inclined by 89°. The white dashed lines trace the fork-like structure and warp induced by the planet, and is the same in all three figures.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Synthetic scattered light image of the HD 111520 disk with one planet orbiting outside the warp (a pl = 250 au). The disk is rotated counterclockwise by 45° intervals starting from ω  d  = 270° all the way to ω  d  = 225°. Left: representation of the disk as observed in the optical with HST/STIS. Right: representation of the disk as observed in the NIR with GPI. The rectangle in the top left figure represents the field of view (FOV) of the NIR models.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Synthetic scattered light image of the HD 111520 disk with one planet orbiting inside the disk inner edge (a pl = 40 au). The disk is rotated counterclockwise by 45° intervals from ω  d  = 270° to ω  d  = 225°. Left: representation of the disk as observed in the optical with HST/STIS. Right: representation of the disk as observed in the NIR with GPI. The rectangle in the top left figure represents the FOV of the NIR models.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Top: density map of the 250pl model face on. Bottom: density map of the 40pl model face on. The red points mark the final position of the planet for both models.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Initial (left) and final (right) orbits (black ellipses) and positions of the planets (black dots) relative to the disk (colored dots) for our two planet model. The two planets start at their pericenters with ω pl = 270° for the outer planet and ω pl = 90° for the inner planet. After 15 Myr, the outer planet is near its apocenter with ω pl ≈ 290°, while the inner planet is slightly past its pericenter with ω pl ≈ 180°.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Initial orbital configurations and positions of the planets and disk for a planet with a = 250 au (left) and a = 40 au (right). The initial setup is viewed both edge on (top) and face on (bottom).
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption:  A  V  distributions for stars in the regions of the Cloud 2-N cluster (left panel) and the Cloud 2-S cluster (right panel). The distributions for stars in the cluster regions are shown as thick lines, while those in the control field are shown as thin lines. The distributions for stars in the control field are normalized by multiplying the ratio of the area of each cluster region to the area of the control field. The distributions obtained by subtracting the normalized distribution for stars in the control field from the distribution for stars in the cluster regions are shown as red lines. The vertical dotted lines show the A  V  ranges of the Cloud 2 clusters set in Section 3.3 for defining the mass-A  V -limited sample.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Pseudocolor images of Cloud 2-S obtained with JWST/NIRCam produced by combining the NIR images, F115W (blue), F150W (green), and F200W (red). The solid white square indicates the 1′ square centered on the Cloud 2-S cluster, shown in Figure 3, while the white dashed square shows the control field. An additional control field is indicated by a dotted square.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: The (m F150W − m F200W) vs. (m F115W − m F150W) color–color diagrams for the Cloud 2-N cluster region (left) and the Cloud 2-S region (right). The blue curve in the lower left portion of each diagram is the locus of points corresponding to unreddened main-sequence stars. The loci of CTTSs are shown with cyan lines. The black arrows show the reddening vectors for A  V  = 5 mag. Typical uncertainties (1σ) of the colors are shown in the upper right corner.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Pseudocolor images of Cloud 2-N obtained with JWST/NIRCam produced by combining the NIR images, F115W (blue), F150W (green), and F200W (red). The solid white square indicates the 1′ square centered on the Cloud 2-N cluster, shown in Figure 3.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Radial density distribution of massless disk particles within 20 au of the disk midplane for our single 1 M jup model left and our single 0.5 M jup model right. The white dashed box highlights the location where the radial distribution of the disk particles differs between the two models. In both frames the density is scaled the same in log space.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Zoomed-in F200W-band images of the Cloud 2-N and 2-S clusters. North is up, and east is to the left. The areas of the images are indicated by the white squares in Figures 1 and 2, with a field of view of about ﹩1^{\prime} \times 1^{\prime} ﹩. The positions of the cluster regions, which are identified in Section 3.1 from the regions where particularly high stellar densities were detected in the MIRI images (N. Izumi et al. 2024), are shown as green ellipses.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Distributions of ﹩{({m}_{{\rm{F}}115{\rm{W}}}-{m}_{{\rm{F}}150{\rm{W}}})}_{0}﹩ for stars in the regions of the Cloud 2-N cluster (left panel) and the Cloud 2-S cluster (right panel). The distributions for stars in the cluster regions are shown as thick lines, while those in the control field are shown as thin lines. The distributions for stars in the control field are normalized by multiplying the ratio of the area of each cluster region to the area of the control field.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: A composite color image of one of the three SpARCS clusters we study, J0224, with HST imaging in the F475W (blue), F625W (green), and F160W (red) filters. Members of this cluster considered for this paper are indicated with white ellipses. On the right is an example of the inner aperture (r < r 50, the orange shaded region) and outer annulus (r 50 < r < r 90, the pink shaded region) determined for this galaxy, used for the analysis presented in this paper. The size and ellipticity of the two apertures is determined based on the total flux in the F160W filter, and then applied to both the F625W and F475W images.