adsabs/AstroCLIMB huggingface dataset:
Paper: Systematically Measuring Ultradiffuse Galaxies. VII. The H I Survey Overview
Authors: Ananthan Karunakaran, Khadeejah Motiwala, Kristine Spekkens, Dennis Zaritsky, Richard L. Donnerstein, Arjun Dey
Figure caption:  M H I /L  g  (orange stars and blue squares for H I-confirmed UDGs and LSB dwarfs, respectively) and ﹩{M}_{{\rm{HI}}}^{{\rm{lim}}}﹩/L  g  (red circles with downward arrows for nondetections) as a function of the g − r color for our sample. The marginalized distributions are shown along the opposite axes and we show the median of each subset as dotted lines. For comparison in the g − r distribution, we show the median g − r = 0.35 color of the HUDS sample (L. Leisman et al. 2017) as the dashed black line.
Paper: Systematically Measuring Ultradiffuse Galaxies. VII. The H I Survey Overview
Authors: Ananthan Karunakaran, Khadeejah Motiwala, Kristine Spekkens, Dennis Zaritsky, Richard L. Donnerstein, Arjun Dey
Figure caption:                       ﹩\sim 2^{\prime\prime} \times 2^{\prime\prime} ﹩ color grz image cutouts of example galaxies from our sample. We show two randomly selected examples of H I-confirmed UDGs (left column), H I-confirmed LSB dwarfs (middle column), and H I nondetections (right column). In each pair, one was chosen to fall toward the blue end of the g − r color distribution (top row) and the other toward the red end (bottom row). For the UDGs and LSB dwarfs, we list their colors (g − r ), physical effective radii (R eff), and central surface brightness (μ 0, g ). For our nondetections, we show the same values but instead list their angular effective radii (r eff).
Paper: Systematically Measuring Ultradiffuse Galaxies. VII. The H I Survey Overview
Authors: Ananthan Karunakaran, Khadeejah Motiwala, Kristine Spekkens, Dennis Zaritsky, Richard L. Donnerstein, Arjun Dey
Figure caption: (NUV−r) vs. r (left) and NUV SFR as a function of the stellar mass (right) for our sample. Once again, the orange stars and blue squares for H I-confirmed UDGs and LSB dwarfs, respectively. We show the NUV–IR SFRs from A. Durbala et al. (2020) for the α.100 catalog. The SFRs from our sample tend to fall toward the lower end of the α.100 distribution and appear to have specific SFRs (SFR/M *) below the main sequence from the α.100 population.
Paper: Systematically Measuring Ultradiffuse Galaxies. VII. The H I Survey Overview
Authors: Ananthan Karunakaran, Khadeejah Motiwala, Kristine Spekkens, Dennis Zaritsky, Richard L. Donnerstein, Arjun Dey
Figure caption: Comparisons of the difference between the systemic velocities (ΔV sys, top panel), H I fluxes (ΔS H I , middle panel), and velocity widths (ΔW 50, bottom panel) as a function of the logarithm of the signal-to-noise ratio (SNR) in the GBT data between the overlapping galaxies in our sample and literature H I observations. The sources overlapping the ALFALFA α.100 catalog are shown as red inverted triangles, the source from the RESOLVE survey is shown as a blue square, and the source from the MATLAS survey is shown as a black square. In the top panel, we show the RESOLVE and MATLAS sources with downward and upward-facing arrows to indicate their larger offsets from the GBT value. We note that the RESOLVE source does not provide uncertainties on S H I  or quote a W 50 value and the MATLAS source does not have uncertainties on W 50.
Paper: Systematically Measuring Ultradiffuse Galaxies. VII. The H I Survey Overview
Authors: Ananthan Karunakaran, Khadeejah Motiwala, Kristine Spekkens, Dennis Zaritsky, Richard L. Donnerstein, Arjun Dey
Figure caption: Comparison of the best-fit slope and intercept in the ﹩\mathrm{log}[{M}_{{\rm{HI}}}/{M}_{* }]﹩-﹩\mathrm{log}[{R}_{\mathrm{eff}}]﹩ plane. Each row shows the best-fit parameters for each of our fitting procedures: top—LinMix, middle—ODR, and bottom—split-normal. The symbol color represents their stellar mass bin as in Figure 4 and the symbol type represents LSB dwarfs (squares) and UDGs (stars). The left panels include all of our H I detections, whereas the right panels only include dwarf galaxies with R eff > 1.5 kpc.
Paper: Systematically Measuring Ultradiffuse Galaxies. VII. The H I Survey Overview
Authors: Ananthan Karunakaran, Khadeejah Motiwala, Kristine Spekkens, Dennis Zaritsky, Richard L. Donnerstein, Arjun Dey
Figure caption:  g-band surface brightness as a function of the distance for our UDGs (stars) and dwarfs (squares). The filled symbols show UDGs and dwarfs defined using the g-band central surface brightness, μ 0,g , while open symbols show those defined using their g-band effective surface brightness (〈μ eff,g 〉; see text). The marginalized surface brightness distributions are shown along the right-hand axis with the solid lines showing μ 0,g  and dotted lines showing 〈μ eff,g 〉. The vertical solid and dotted lines show the median distances for UDGs and dwarfs for the same surface brightness definitions.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Statistical analysis of the similarities and dissimilarities of the 21 composites using the monthly averaged versions over the common period of 1980 March to 2023 March. (a) The dendrogram clustering of all composites identifies five clear clusters of three to four composites each, labeled here A–E, and two miniclusters of two composites each. (b) The PCA identifies six clear clusters of three to four composites each, labeled here A–F based on the top three principal components (each assigned a separate axis). Clusters A–E are the same for both analyses and cluster F from the PCA comprises the two remaining miniclusters of the dendrogram analysis. In both analyses, each cluster/minicluster is indicated with a different color. For consistency, the colors used here for clusters A–F are the same colors we use in Figures 9–17 for Groups A–F.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Effects of the changes in the Earth–Sun distance over the calendar year on the in situ TSI at Earth's distance. (a) shows the daily Earth–Sun distance (in astronomical units) from 1980 January 1 until 1989 December 31. The dates of the minima and maxima for each year are indicated as are any leap days. (b) shows the corresponding TSI that would be measured in situ in the hypothetical case where there was zero solar variability and TSI at 1 au remained constant at 1362 Wm−2. (c) The annually averaged TSI (over a calendar year) that would be observed in situ at Earth’s distance (solid blue lines) or 1 au (black dashed lines). (d) and (e) Earth–Sun distances relative to that at 1 au on the date of aphelion and perihelion for each year, respectively. (f) and (g) TSI observed at Earth relative to that at 1 au on the date of aphelion and perihelion for each year, respectively.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: All of the 17 new or updated composites with monthly resolution. The data contributing to each part of the composites are indicated using horizontal colored lines in each panel below the composite. The numbering scheme used is somewhat arbitrary, as discussed in the text, but when combined with the four living composites in Figure 2 (Composite Nos. 1, 2, 3, and 8) provides a unique ID number from 1 to 21 for all 21 composites.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Comparison of the six composite group averages to SSN at a monthly resolution after a linear rescaling (using OLS fitting) to match each composite group over the first 12 yr of overlap. (a) SSN; (b) comparison with Group A; (c) comparison with Group B; (d) comparison with Group C; (e) comparison with Group D; (f) comparison with Group E; (g) comparison with Group F. The fitting results and statistics are included in the right-hand panels.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Comparison of the NRL TSI 2.1 proxy-based TSI model (colored lines using the same color scheme of Figure 8) to each of the six composite group averages (solid black line) after a linear offset applied to the model to ensure the averages over the first 12 yr of data—using monthly averaged data. (a)–(f) Composite Groups A–F.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Comparison of the SATIRE-S proxy-based TSI model (colored lines using the same color scheme of Figure 8) to each of the six composite group averages (solid black line) after a linear offset applied to the model to ensure the averages over the first 12 yr of data—using monthly averaged data. (a)–(f) Composite Groups A–F.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Comparison of how each of the six TSI composite group averages (monthly averages at 1 au) suggests that TSI has changed between each of the solar minima and solar maxima over the satellite era (1978 to the present). (a)–(f) Groups A–F.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Comparison of how each of the six TSI composite group averages suggests TSI has changed over the satellite era (1978 to the present)—at (a) daily, (b) monthly, and (c) yearly resolutions.
Paper: Multiple New or Updated Satellite Total Solar Irradiance (TSI) Composites (1978–2023)
Authors: Ronan Connolly, Willie Soon, Michael Connolly, Rodolfo Gustavo Cionco, Ana G. Elias, Gregory W. Henry, Nicola Scafetta, Víctor M. Velasco Herrera
Figure caption: Comparison of the six TSI composite group averages with yearly resolution at 1 au and in situ Earth's distance. (a) annually averaged TSI scaled to 1 au; (b) annually averaged TSI at in situ Earth's distance; (c) the difference between both sets of values.
Paper: New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Surajit Mondal, Devojyoti Kansabanik, Divya Oberoi, Soham Dey
Figure caption: Time series of the amplitude of visibilities averaged over the two polarizations, RR and LL, over the band 244–251 MHz. Each line represents the time series averaged over 50 consecutive baselines (arranged in the order of baseline length) and divided by the mean amplitude of the time series. Vertical bars mark the peaks imaged in this study. Red bars show the peaks for which images are shown in Figure 6.
Paper: New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Surajit Mondal, Devojyoti Kansabanik, Divya Oberoi, Soham Dey
Figure caption: Radio images from different frequency bands at similar times. Left panel: Contours from 244–251 MHz, 236–243 MHz, and 229–235 MHz are shown. The corresponding image times are 04:14:13–04:14:23, 04:14:13–04:14:16, and 04:14:13–04:14:16, respectively. During these times, no type-I burst is detected at the corresponding frequencies. Middle panel: Contours from 244–251 MHz, 236–243 MHz, 229–235 MHz, and 221–228 MHz are shown. The corresponding image times are 04:14:28–04:14:30, 04:14:28–04:14:30, 04:14:28–04:14:30, and 04:14:06–04:14:07, respectively. These times correspond to type-I bursts at their corresponding frequencies. Right panel: Contours from 244–251 MHz, 236–243 MHz, 229–235 MHz, and 221–228 MHz are shown. The corresponding image times are 04:15:52–04:15:57, 04:16:02–04:16:04, 04:16:03–04:16:04, and 04:16:03–04:16:04, respectively. They correspond to the times when a morphology change is seen in the northern source at each of the four frequency bands. The contour levels of the image at 04:14:01–04:14:02 are at −0.3, 0.3, 0.6, and 0.9 times the peak. Contour levels for all other images are −0.5, 0.5, 0.7, and 0.9 times the peak. The green ellipses at the bottom left corner show the resolution of the radio images.
Paper: New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Surajit Mondal, Devojyoti Kansabanik, Divya Oberoi, Soham Dey
Figure caption: Left panel: Stokes I flux density calibrated dynamic spectrum of the MWA is shown at the top, and the time series of the band-averaged flux density is shown at the bottom. Right panel: Stokes I dynamic spectrum of uGMRT normalized using median bandshape is shown at the top, and the time series of the band-averaged relative flux density is shown at the bottom.
Paper: New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Surajit Mondal, Devojyoti Kansabanik, Divya Oberoi, Soham Dey
Figure caption: Left panel: Contours of the uGMRT image are overlaid on the MWA image. Both images correspond to 04:14:14 UTC during a weak type-III radio burst. Right panel: Contours of the uGMRT and MWA images are overlaid on an Atmospheric Imaging Assembly 131 Angstrom image. The contours of the uGMRT and MWA images are cyan and blue respectively.
Paper: New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Surajit Mondal, Devojyoti Kansabanik, Divya Oberoi, Soham Dey
Figure caption: Four example radio images during type-I bursts from the 244–251 MHz band are shown with magenta contours, overlaid over a nearby AIA 131 Å image. The colorscale of the AIA image is inverted grayscale. The title of each panel shows the time of the radio image. The contour levels are at −0.4, 0.4, 0.6, and 0.8 times the peak of the individual radio images. The blue ellipse at the bottom left corner shows the resolution of the radio image.
Paper: New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Surajit Mondal, Devojyoti Kansabanik, Divya Oberoi, Soham Dey
Figure caption: Contours of an example radio image of the Sun for the 244–251 MHz band at 04:14:30 are overlaid on a nearby AIA 131 Å image. The AIA image has an inverted colorscale, where darker shades show brighter regions. The contour levels are at −0.4, 0.4, 0.6, and 0.8 times the peak of the radio image. Solid and dashed lines represent positive and negative contours, respectively.
Paper: New Insights into Type-I Solar Noise Storms from High Angular Resolution Spectroscopic Imaging with the Upgraded Giant Metrewave Radio Telescope
Authors: Surajit Mondal, Devojyoti Kansabanik, Divya Oberoi, Soham Dey
Figure caption: Contours from a radio image made at 244–251 MHz and 04:14:13–04:14:23 have been overlaid on a corresponding nearby AIA 131 Å image. During this time, no type-I burst was detected. The contour levels are at −0.4, 0.4, 0.6, and 0.8 times the peak of the radio image. The blue ellipse at the bottom left corner shows the resolution of the radio image.
Paper: The State of Solar Wind Heavy Ions in Interplanetary Coronal Mass Ejection–Driven Geomagnetic Storms
Authors: Cong Wang, Fei He, Xiaoxin Zhang
Figure caption: Illustration of the variations in physical parameters of ICMEs triggering geomagnetic storms of equal intensity, along with the changes in O ion and Fe ion charge states and abundances. The red solid line represents the occurrence time of shock waves, while the red dashed line represents the start and end times of the ICME.
Paper: Modeling of Long-term Afterglow Counterparts to Gravitational Wave Events: The Full View of GRB 170817A
Authors: Geoffrey Ryan, Hendrik van Eerten, Eleonora Troja, Luigi Piro, Brendan O'Connor, Roberto Ricci
Figure caption: Fiducial optical GRB afterglow light curves of a Gaussian structured jet for a variety of opening angles θ  C  and viewing angle to opening angle ratios θ obs/θ  C  at ν obs = 1014 Hz. Colors denote opening angle (blue: θ  C  = 2°, orange: 4°, green: 8°), line styles the viewing angle ratio (solid: θ obs/θ  C  = 1, dashed: 5, dotted: 10). Parameters for the jet (unless otherwise stated) are chosen to emulate GW170817: θ obs = 19.°4, E 0 = 4.8 × 1053 erg, θ  C  = 3.°2, θ  W  = 4.9θ  C , n 0 = 2.4 × 10−3 cm−3, p = 2.13, ϵ  e  = 1.9 × 10−3, ϵ  B  = 5.75 × 10−4, ξ  N  = 1.0, d  L  = 40 Mpc, and z = 0.0973. Jets with the same ratio θ obs/θ  C  share the same initial power-law slope. At late times (after the jet break), light curves from jets with the same opening angle converge, erasing the effect of the viewing angle. The counter-jet (the jet directed away from the Earth) appears at very late times, ∼104 days.
Paper: Modeling of Long-term Afterglow Counterparts to Gravitational Wave Events: The Full View of GRB 170817A
Authors: Geoffrey Ryan, Hendrik van Eerten, Eleonora Troja, Luigi Piro, Brendan O'Connor, Roberto Ricci
Figure caption: Left panel: Fiducial GRB afterglow centroid offsets of a Gaussian structured jet for a variety of opening angles θ  C  and viewing angles θ obs. Line styles denote opening angle, and colors indicate the viewing angle. Right panel: The apparent velocity of the GRB afterglow centroid measured from the initial burst to the jet break as a function of viewing angle. Line styles denote jet structure profile, and line colors denote jet opening angle. Unless otherwise stated, the jet parameters are identical to those in Figure 1.
Paper: Modeling of Long-term Afterglow Counterparts to Gravitational Wave Events: The Full View of GRB 170817A
Authors: Geoffrey Ryan, Hendrik van Eerten, Eleonora Troja, Luigi Piro, Brendan O'Connor, Roberto Ricci
Figure caption: Afterglow X-ray light curves with (solid lines) and without (pale dashed line) the Deep Newtonian regime at different viewing angles (colors; blue: θ obs = 0°, orange: 22.°5, green: 45°) at ν obs = 5 keV. Unless otherwise stated the jet parameters are identical to those in Figure 1. With these parameters, ϵ  e  = 1.9 × 10−3 and ξ  N  = 1.0, the Deep Newtonian effects begin to alter the light curve when the jet is still trans-relativistic, before the transition to the Sedov phase is complete and the counter-jet appears.
Paper: Modeling of Long-term Afterglow Counterparts to Gravitational Wave Events: The Full View of GRB 170817A
Authors: Geoffrey Ryan, Hendrik van Eerten, Eleonora Troja, Luigi Piro, Brendan O'Connor, Roberto Ricci
Figure caption: GRB afterglow radio images for a GW170817-like jet at different viewing angles θ obs at the time of the jet break. Shown is the specific intensity I  ν  at ν = 5 GHz of the primary jet, scaled so each image has the same maximum intensity. Doppler beaming produces a limb-brightened image, with emission dominated by the high Lorentz factor material near the jet core. Unless otherwise stated, the jet parameters are identical to those in Figure 1.
Paper: Modeling of Long-term Afterglow Counterparts to Gravitational Wave Events: The Full View of GRB 170817A
Authors: Geoffrey Ryan, Hendrik van Eerten, Eleonora Troja, Luigi Piro, Brendan O'Connor, Roberto Ricci
Figure caption: One- and two-dimensional marginalized posterior distributions for the “full model” fit to GW170817 with a power-law structured jet and an additional constant luminous X-ray component L X. Written labels along the diagonal contain 68% uncertainties, and blue lines show the location of the maximum posterior probability density sample.
Paper: Modeling of Long-term Afterglow Counterparts to Gravitational Wave Events: The Full View of GRB 170817A
Authors: Geoffrey Ryan, Hendrik van Eerten, Eleonora Troja, Luigi Piro, Brendan O'Connor, Roberto Ricci
Figure caption: One- and two-dimensional marginalized posterior distributions for the “full model” fit to GW170817 with only a power-law structured jet. Written labels along the diagonal contain 68% uncertainties, and blue lines show the location of the maximum posterior probability density sample.
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Horizontal slices of the R8-4pc model at z = 0 pc and t = 430 Myr, with the same quantities shown in Figure 1. Clockwise from top left the panels represent ISM phase, x  e , T, ﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{LyC}}﹩, ﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{FUV}}﹩, and n H. Source particles are shown in the bottom right panel. The red contour in the x  e  panel represents the boundary between hot and WIM. Additionally, the black contour in each panel represents a classical H II region, which contains a star cluster source of mass 1.3 × 103 M ⊙ (this cluster particle is omitted from the ﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{LyC}}﹩ panel for clarity). The dashed horizontal line shown in the bottom left panel represents the one-dimensional, horizontal ray used in Figure 5.
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Left: Distribution of mass with normalized mean intensity in the FUV band ﹩{\boldsymbol{ \mathcal J }}﹩ and hydrogen number density n H for the midplane gas in model R8-4pc including all snapshots between 250 and 450 Myr. We limit to gas with T < 3.5 × 104 K. Insets show mass-weighted PDFs of log ﹩\,{\boldsymbol{ \mathcal J }}﹩ and log  n H. The red dashed line represents the best fit of Equation (7) to the mode of the distribution. Right: The black points represent the mass-weighted PDF of normalized mean intensity ﹩{\boldsymbol{ \mathcal J }}﹩ (rather than log ﹩\,{\boldsymbol{ \mathcal J }}﹩ as in the left panel). The overplotted lines represent the best fit of the model given in Equation (10) with the log-normal and power-law components represented in blue and orange respectively. The shaded region represents the 16th–84th percentile of the two PDFs of each individual snapshot between 250 and 450 Myr.
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Temporal evolution and statistics of key global simulation quantities, for the R8-4pc model. From top to bottom, the left column shows (a) the LyC (ionizing) photon rate, star formation rate, and FUV energy input rate per unit area averaged over the whole simulation domain, (b) total mass fractions of gas in different thermal phases, (c) scale heights of different phases of gas, as well as n  e  2 (∝emission measure), (d) mean in-plane separations ℓ ⋆ of cluster particle sources (with t age < 20 Myr) as well as their scale heights and maximum and minimum z locations. The right panels show statistical distributions of these same quantities as histograms including all times.