adsabs/AstroCLIMB huggingface dataset:
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: A comparison of stellar mass surface density profiles for massive ghost galaxies (black solid and dashed lines, repeated from Figure 12) and isolated “ordinary” dwarfs that are “quenched” as the result of falling below the virial mass threshold for cooling at z > 0.5. Shaded regions show the 10%−90% range of profiles for quenched dwarfs crossing the cooling threshold at 0.5 < z < 2 (orange) and z > 2 (blue). Half-mass radii for individual dwarfs in the z > 2 sample are shown by blue squares. For the 0.5 < z < 2, we show only the mean (±1 σ half-light radius (dark-blue star). The softening length of the COCO simulation is indicated by the vertical dotted line.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: Left: the cumulative fraction of ghosts merging with the main branch later than a given look-back time. Solid and dashed lines refer to our V cut = 30 and 40 km s−1 models, respectively. We apply weights to the EPS to reflect the true number counts of an N-body simulation and divide each time bin by the total number of ghosts. The red and blue lines correspond to mergers between virialized halos in the EPS and COCO trees, respectively. The green lines correspond to the merger of the subhalo associated with the merger tree branch of the ghost galaxy in the COCO trees, which may be several snapshots after the virialized halos merge. Right: the cumulative fraction of mergers between the ghost branch and the main branch of the merger tree with a progenitor halo mass ratio larger than a given value, measured at the time immediately before those two branches merge. Solid and dashed lines again correspond to V cut = 30 and 40 km s−1.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: The z = 0 stellar mass function of ghostly galaxies predicted using the Behroozi et al. (2019) SMHM relation, as in Figure 9, but here for a model assuming stronger IGM heating due to reionization, V cut = 40 km s−1. Again, solid lines separate the contributions from single (blue) and multiple (orange) ghost trees, and the total is shown by the black dashed line. The typical stellar masses of ghosts are higher than in Figure 9, and the number of trees with multiple ghosts exceeds the number of trees with a single ghost at most masses.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: Same as Figure 5, but showing the effects of varying z cut.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Example of DRW fit performed for the light curve of Sector 33. Panel (a), top: rest-frame TESS light curve for Sector 33 (gray) and best-fit DRW model (orange). Panel (a), bottom: residuals from the DRW fit. As we can see in panel (c), the histogram of the residuals (gray) follows a Gaussian distribution (blue). Panel (b) Distribution of the posteriors from the DRW fit performed with EzTao. Both parameters, i.e., amplitude and τ DRW, are well constrained. See Section 5.2 for details.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: TESS Sector 3 light curve of the non-AGN galaxy 2dFGRS TGS145Z214, extracted with Quaver's full-hybrid method.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Pictor A, Sector 6.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Pictor A, Sector 33.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Pictor A, Sector 4.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Pictor A, Sector 31.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Star 1, Sector 4.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Star 3, Sector 6.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Results of the DRW fit to Sector 5 data as observed.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Results of the DRW fit to Sector 5 data after the five highest-amplitude flares have been masked and removed.
Paper: Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane
Figure caption: Comparison of (q, χ eff) population distributions for the Gaussian copula model (left) and FGM copula model (right). Plots consist of 2 × 104 draws from the population predictive distribution for mass ratio and χ eff, assuming the maximum posterior probability hyper-parameters. These plots use results from analyses excluding GW191109. Note that samples drawn from the non-spinning subpopulation have been randomly offset by χ eff ∼ ±0.005 in order to help with the visualization.
Paper: Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane
Figure caption: Plot of 3 × 104 draws from the population predictive distribution for mass ratio and χ eff, marginalized over the posterior distributions of the population hyper-parameters and excluding GW191109. In red is the purely data-driven                       π                    from Payne & Thrane (2023), consisting of a set of delta functions that attempt to maximize the population likelihood. Darker tones indicate a higher weight, thus higher importance, for the given feature. Our model matches qualitative features present in the                       π                    result. Note that samples drawn from the non-spinning subpopulation have been randomly offset by χ eff ∼ ±0.005 in order to help with the visualization.
Paper: Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane
Figure caption: Comparison between the EXTENDED population model from Tong et al. (2022; blue), and this work (orange). In this demonstration, the hyper-parameters for our model are chosen to resemble the EXTENDED model distributions in blue. The correlation parameter κ is set to zero in this example. Varying κ changes the degree of correlation in the (q, χ eff) plane but leaves every other panel unchanged. The non-spinning subpopulation is also excluded from this demonstration.
Paper: A Dragon Out of Breath? Monitoring High-velocity Outflows from the High-mass Gamma-Ray Binary LS 2883/PSR B1259–63 During the 2017–2021 Binary Cycle
Authors: Jeremy Hare, George G. Pavlov, Gordon P. Garmire, Oleg Kargaltsev
Figure caption: The distance vs. time for the X-ray emitting clump in 2011–2014, 2014–2017, and 2017–2021 binary cycles. The crosses mark the upper limit on the distance. The red lines show the times of periastron passage.
Paper: Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution of the (q, χ eff) correlation κ for analyses excluding (blue) and including (orange) GW191109. Excluding GW191109, we find 90% credible intervals of ﹩\kappa ={28}_{-20}^{+20}﹩. When GW191109 is included, we find 90% credible intervals of ﹩\kappa ={30}_{-21}^{+18}﹩. The prior is indicated with a dashed line, which extends from κ = −50 to κ = 50.
Paper: Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distributions for hyper-parameters governing the marginal distributions relevant to this study. Values listed above the posteriors are the medians, accompanied by 90% credible intervals. These intervals are plotted as dotted lines in the one-dimensional posteriors. From darkest to lightest, the shaded regions in the two-dimensional plots represent 50%, 90%, and 99% credibility regions. This plot uses results excluding GW191109.
Paper: Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane
Figure caption: Population predictive distribution of mass ratio q and effective spin parameters χ eff, χ diff, and ρ 1,2, reconstructed by marginalizing over the hyper-parameter posterior distributions. From darkest to lightest, the shaded regions in the two-dimensional plots encapsulate 50%, 90%, and 99% of the inferred BBH population. This plot uses results excluding GW191109.
Paper: Evidence for a Correlation between Binary Black Hole Mass Ratio and Black Hole Spins
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane
Figure caption: Implied population predictive distribution of mass ratio q and physical spin parameters χ 1,2 and ﹩\cos {t}_{\mathrm{1,2}}﹩, reconstructed by marginalizing over the hyper-parameter posterior distributions. From darkest to lightest, the shaded regions in the two-dimensional plots encapsulate 50%, 90%, and 99% of the inferred BBH population. This plot uses results excluding GW191109.
Paper: Are Switchback Boundaries Observed by Parker Solar Probe Closed?
Authors: Nina Bizien, Thierry Dudok de Wit, Clara Froment, Marco Velli, Anthony W. Case, Stuart D. Bale, Justin Kasper, Phyllis Whittlesey, Robert MacDowall, Davin Larson
Figure caption: Example of a typical switchback. The leading and trailing boundaries are located between the pairs of vertical lines. (a) FIELDS/MAG magnetic field data in the RTN frame; (b) proton velocity from SWEAP/SPC, also in the RTN frame. The average value of the radial velocity has been removed to facilitate visualization; (c) normalized deflection z.
Paper: Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270
Authors: Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal
Figure caption: (a) Intensity-weighted moment-0 map for 13CO (J = 1–0), integrated in the velocity range [−6.0, +1.0] km s−1 toward G083.097+03.270 (G08). Two filaments, Fi-N and Fi-S, are revealed and are found to be intersecting, forming a hub, i.e., with an enhanced gas density at the center. (b) The 13CO moment-1 map shows the filaments to have two different velocity structures. (c) In the 13CO moment-2 map, the large velocity dispersion is traced mostly in and around the junction of filaments. (d) The H2 column density derived from 13CO for the molecular gas with an overplot of square regions each of size ﹩2\buildrel{\,\prime}\over{.} 5﹩ and numbered consequently, selected to study the variation of molecular properties along the filaments axis. Panels (a)–(c) are in linear scaling, whereas (d) is in square-root scaling.
Paper: Are Switchback Boundaries Observed by Parker Solar Probe Closed?
Authors: Nina Bizien, Thierry Dudok de Wit, Clara Froment, Marco Velli, Anthony W. Case, Stuart D. Bale, Justin Kasper, Phyllis Whittlesey, Robert MacDowall, Davin Larson
Figure caption: Schematic view of an arc-polarized switchback boundary. The three vectors are from Equation (3). The blue plane represents the discontinuity plane in which the tips of the field vector rotate, with its normal  n  in green. This is a particular event, for which the plane includes the origin. The orange sphere, of radius ∣ B ∣, represents the constant magnitude during the transition interval. A more general arc-polarized boundary is shown, with the identified plane in red. Both planes have the same normal. It should be noted that the two cases are ideal boundaries. Measured switchback boundaries would not have ( B /∣ B ∣) ·  n  = 0 exactly, mainly because of fluctuations.
Paper: Are Switchback Boundaries Observed by Parker Solar Probe Closed?
Authors: Nina Bizien, Thierry Dudok de Wit, Clara Froment, Marco Velli, Anthony W. Case, Stuart D. Bale, Justin Kasper, Phyllis Whittlesey, Robert MacDowall, Davin Larson
Figure caption: Boundary analysis using the classical classification scheme by Neugebauer et al. (1984). The normalized projection of the magnetic field along the normal ( B /∣ B ∣) ·  n  is plotted against the variation of the magnetic field magnitude across the discontinuity Δ∣ B ∣/∣ B ∣. The dashed lines divide the plane into four quadrants: TDs occur in the upper left quadrant and RDs in the lower right one. The remaining quadrants correspond to unclassified events. The color code represents the normalized magnitude z of the deflection from the Parker spiral (Equation (1)). 186 boundaries are shown, excluding the 64 ambiguous cases.
Paper: Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270
Authors: Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal
Figure caption: Two color integrated intensity CO images, revealing the merging of filaments into a common junction as the hub. In (a) the young stellar objects (Class I: yellow circles; Class II: white triangles; transition-disk: green crosses) from Panja et al. (2022) are overlaid on the 12CO distribution. A scale bar of 5 pc is shown considering a heliocentric distance of 1.52 kpc. In (b) the skeletons of the two filaments (Fi-N and Fi-S) are more clearly depicted by the 13CO distribution. I1 and I2 indicate the subsidiary locations along which Fi-N (western part) and Fi-S are interacting (see Appendix A). At the hub, a massive outflow source MSX G083.0936+03.2724 is marked by a black asterisk symbol.
Paper: Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270
Authors: Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal
Figure caption: Average spectra (blue: 12CO; red: 13CO) fitted with Gaussian (black dashed curves) for the square regions shown in Figure 1(d), each labeled with an ID number. The vertical dashed lines mark velocities of −3.98 km s−1 and −0.83 km s−1, respectively. For ID 7 and 12CO, the T mb (K) is scaled down by a factor of 2.
Paper: Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270
Authors: Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal
Figure caption:  13CO position–velocity diagrams toward G08. (a) Longitude–velocity distribution is integrated for the entire latitude range [2.°82, 3.°72] and (b) latitude–velocity distribution is integrated for the entire longitude range [83.°547, 82.°647]. The white dashed lines mark the velocity of −3.98 and −0.83 km s−1, respectively.
Paper: Are Switchback Boundaries Observed by Parker Solar Probe Closed?
Authors: Nina Bizien, Thierry Dudok de Wit, Clara Froment, Marco Velli, Anthony W. Case, Stuart D. Bale, Justin Kasper, Phyllis Whittlesey, Robert MacDowall, Davin Larson
Figure caption: Boundary thickness as a function of the magnitude of their deflection from the Parker spiral. The thickness is calculated in ion inertial length. The mean ion inertial length over the first encounter of PSP is 16 km.
Paper: Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270
Authors: Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal
Figure caption: (a) Excitation temperature map derived from 12CO. The radio continuum emission from the NVSS 1.4 GHz is depicted in black contours at levels of 0.003, 0.006, 0.012, and 0.020 Jy beam−1. A total of five emission peaks with integrated flux densities above the 3σ  level are detected and are marked as P1–P5. (b) H2 mass distribution derived from 13CO in the velocity range [−6.0, +1.0] km s−1. The C18O intensity map integrated for the same velocity range, as overlaid as white contours at levels of 0.199, 0.398, 0.597, and 0.796 K km s−1. Six massive clumps labeled as C1–C6 are identified from the C18O data.
Paper: Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270
Authors: Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal
Figure caption:  12CO channel maps (background) with overlaid 13CO contours (red) at the levels of 0.5, 1.0, 1.5, 2.0, and 2.5 K km s−1 integrated for the mentioned velocity ranges toward G08. In the first panel, the three black curves (labeled as ne, nw, and s) along the filaments axis and the two black lines (i1 and i2) along the additional interacting zones, each of width ﹩2\buildrel{\,\prime}\over{.} 5﹩ (5 pixels) with arrows, indicate the direction along which position–velocity diagrams are generated.
Paper: Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270
Authors: Alik Panja, Lokesh K. Dewangan, Tapas Baug, Wen Ping Chen, Yan Sun, Tirthendu Sinha, Soumen Mondal
Figure caption:  13CO position–velocity contours (black) are overlaid on the 12CO position–velocity diagrams along (a) ne, (b) nw, (c) s, (d) i1, and (e) i2, as mentioned in Figure 5. The contour levels are at 1, 2, 3, 4, 5, and 6 K, respectively. The white dashed lines mark velocities of −3.98 km s−1 and −0.83 km s−1, respectively.
Paper: Improving Coronal Hole Detections and Open Flux Estimates
Authors: Ronald M. Caplan, Emily I. Mason, Cooper Downs, Jon A. Linker
Figure caption: Schematic of the MIDM method for merging EUV images into a full Sun map on a pixel-by-pixel basis. New data take priority, unless its μ value (a measure of data quality) is lower than the data already present. When two pixels are merged, the minimum intensity of the two is used.
Paper: Improving Coronal Hole Detections and Open Flux Estimates
Authors: Ronald M. Caplan, Emily I. Mason, Cooper Downs, Jon A. Linker
Figure caption: Illustration of CH obscuration. A set of closed loops (blue), with correspondingly high emission, are located adjacent to lower-emission open field (red). The open/closed boundary is obscured for one observer’s LOS (black-dashed line) but is visible from another observer’s LOS (green-dashed line).
Paper: Characterizing the Atmospheric Dynamics of HD 209458b-like Hot Jupiters Using AI-driven Image Recognition/Categorization
Authors: F. Sainsbury-Martinez, P. Tremblin, M. Mancip, S. Donfack, E. Honore, M. Bourenane
Figure caption: AI multi-categorization map(s) for our cool HD 209458b-like atmospheric model. Here we show the categories detected (with the opacity of each detection point representing the strength of the detection) at each pressure level (where an increase in pressure level corresponds to a decrease in actual pressure as we move to higher altitudes) against time (where t = 0 corresponds to solid-body, adiabatic, initialization, and each latter point corresponds to the center of the temporal mean) for two different multi-categorization CNNs, one without thermal inversion detection (left) and one with (right). Note that the CNN that lacked thermal inversion detection also differs from the CNN used throughout the rest of this work in a number of other regards being an earlier iteration of the final model. This includes changes to the color map, resolution, and averaging period of the input data. The categories in question correspond to the detection of a north–south asymmetric thermal structure in blue, a banded (i.e., horizontally homogenized) thermal structure in orange, a radiative-dominated thermal structure (driven by tidal locking) in green, a butterfly thermal structure (i.e., eastward equatorial advection flanked by slight, off-equator, westward advection) in red, a vertical thermal inversion (in the figure on the right-hand side) in purple (increasing T with P) and brown (decreasing T with P), and an equatorial (wind) jet in purple (left-hand side) or pink (RHS).
Paper: Characterizing the Atmospheric Dynamics of HD 209458b-like Hot Jupiters Using AI-driven Image Recognition/Categorization
Authors: F. Sainsbury-Martinez, P. Tremblin, M. Mancip, S. Donfack, E. Honore, M. Bourenane
Figure caption: Temporally averaged zonal wind (arrows) and temperature profile (map) at four different pressure levels (0.0026 bar—left, 0.016 bar—middle left, 0.2 bar—middle right, and 10 bar—right) for both our hot (top) and cool (bottom) HD 209458b-like atmospheric models. Each profile has been labeled with the (class of) tag assigned to it by the CNN.
Paper: Characterizing the Atmospheric Dynamics of HD 209458b-like Hot Jupiters Using AI-driven Image Recognition/Categorization
Authors: F. Sainsbury-Martinez, P. Tremblin, M. Mancip, S. Donfack, E. Honore, M. Bourenane
Figure caption: AI multi-categorization map for our hot HD 209458b-like atmospheric model. Here we show the categories detected (with the opacity of each detection point representing the strength of the detection) at each pressure level (where an increase in pressure level corresponds to a decrease in actual pressure as we move to higher altitudes) against time (where t = 0 corresponds to solid-body, adiabatic, initialization, and each latter point corresponds to the center of the temporal mean). The categories in question correspond to the detection of a north–south asymmetric thermal structure in blue, a banded (i.e., horizontally homogenized) thermal structure in orange, a radiative-dominated thermal structure (driven by tidal-locking) in green, a butterfly thermal structure (i.e., eastward equatorial advection flanked by slight, off-equator, westward advection) in red, a vertical thermal inversion in purple (increasing T with P) and brown (decreasing T with P), and an equatorial (wind) jet in pink.
Paper: Characterizing the Atmospheric Dynamics of HD 209458b-like Hot Jupiters Using AI-driven Image Recognition/Categorization
Authors: F. Sainsbury-Martinez, P. Tremblin, M. Mancip, S. Donfack, E. Honore, M. Bourenane
Figure caption: Latitudinally and temporally averaged (at the equator) T–P profiles for our hot (top) and cool (bottom) HD 209458b-like atmospheric models. Each plot includes profiles from six different longitudes, ranging from the substellar point (whose equilibrium profile is shown in red) eastward to the anti-stellar point (whose equilibrium profile is shown in blue) on the nightside. Note that we have excluded the deep atmospheres (P > 10 bar) from these plots since it has not fully equilibrated.