adsabs/AstroCLIMB huggingface dataset:
Paper: Phantom Matter: A Challenging Solution to the Cosmological Tensions
Authors: Adrià Gómez-Valent, Joan Solà Peracaula
Figure caption: Confidence regions in the w  Y -w  X  plane of the wXCDM model, and the corresponding 1D posterior distributions. The dotted lines are set at w  Y  = −1 and w  X  = −1. The intersection of the horizontal and vertical lines in the contour plot corresponds to the Λ s CDM model, which falls ≳3σ away from the preferred region of the wXCDM. See the main text for further comments.
Paper: Phantom Matter: A Challenging Solution to the Cosmological Tensions
Authors: Adrià Gómez-Valent, Joan Solà Peracaula
Figure caption: Full triangle plot for the various models studied in this paper. We show the constraints at 68% and 95% CL in all the relevant planes of the parameter spaces, together with the individual 1D posterior distributions. H 0 is given in km s−1 Mpc−1.
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: Gas richness, ﹩\mathrm{log}({{M}}_{{\rm{HI}}}/{{M}}_{* })﹩, as a function of the physical size, ﹩\mathrm{log}({{R}}_{\mathrm{eff}})﹩, for H I-confirmed UDGs (left) and LSB dwarfs (right). The symbol colors correspond to their stellar mass bins, defined to populate the bins with roughly equal numbers of objects. LSB dwarfs: small (yellow) - ﹩\mathrm{log}({{M}}_{* })=[5.47,7.35)﹩, medium (green) - ﹩\mathrm{log}({{M}}_{* })=[7.35,8.30)﹩, large (pink) - ﹩\mathrm{log}({{M}}_{* })=[8.30,8.59)﹩, X-large (black) - ﹩\mathrm{log}({{M}}_{* })\geqslant 8.59﹩. UDGs: medium (green) - ﹩\mathrm{log}({{M}}_{* })=[7.37,7.99)﹩, large (pink) - ﹩\mathrm{log}({{M}}_{* })=[7.99,8.20)﹩, X-large (black) - ﹩\mathrm{log}({{M}}_{* })\geqslant 8.20﹩. The vertical line in both panels corresponds to the R eff > 1.5 kpc criterion. The dashed colored lines in both panels correspond to the best-fit relations in this plane for each subset obtained using LinMix.
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 derived properties between our H I detections, the HUDS, and the ALFALFA sample. Left: distribution of velocity widths W 50,c,t  for SMUDGes UDGs (orange), SMUDGes LSB dwarfs (blue), the HUDS-B and -R samples (purple and green, respectively), and galaxies from the α.100 catalog with SDSS and GALEX coverage (gray). Right: M H I −M * relation for the same samples as in the left panel. We also show our H I nondetections with distance estimates as red circles with downward arrows, indicating they are upper limits. The open symbols in the right panel indicate sources that would not be included in HUDS due to their low recessional velocities. The dotted black line indicates our target sensitivity limit (i.e., M H I /L  g  = 1M ⊙/L ⊙).
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 apparent properties for our sample: central g-band surface brightness as a function of the g − r color (left panel) and apparent size (r eff;  right panel). Confirmed UDGs and dwarf galaxies are shown as orange stars and blue squares, respectively. H I nondetections are shown as red circles and the grayscale heat map shows the complete SMUDGes sample. The marginalized distributions of each property are shown along the opposite axes.
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: Sky distribution of our UDG candidate H I follow-up sample. In the top panel, we show all of our targets colored by the campaign in which they were observed. In the bottom panel, we show the distribution of our H I detections: orange stars show the confirmed UDGs and the blue squares show the dwarf galaxies. In both panels, we show the complete SMUDGes sample (Z23) as gray circles.
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: Existing living TSI composites currently available and the discontinued composites to be updated in this study, plotted in monthly resolution. The four discontinued composites comprise (a) ACRIM; (b) an alternative ACRIM composite proposed by N. Scafetta (2011); (c) PMOD v1, and (d) SOLID. The four living composites comprise (e) PMOD v2; (f) C3S-RMIB; (g) Kopp’s update to SOLID-c, and (h) an update to the ACRIM composite based on the methodology described by N. Scafetta et al. (2019) and N. Scafetta (2023). The data contributing to each part of the composites are indicated by horizontal colored lines in each panel below the composite. Each panel also indicates when the satellite TSI records used are adjusted from those published by the original satellite mission team. The dotted line and an X symbol indicate when periods of the satellite mission were intentionally deleted before the composite was generated.
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 monthly satellite data from the early satellite era (1978–2003) before and after applying C. Fröhlich’s (2006) F06 adjustments or RMIB’s adjustments as well as before and after the data infilling applied in this study. (a) and (b) plot, respectively, the Nimbus 7/ERB data before and after the F06 adjustments; (c) plots the F06 adjustments; (d) and (e) plot, respectively, the SMM/ACRIM1 data before and after the F06 adjustments; (f) plots the F06 adjustments; (g) and (h) plot, respectively, the ERBS/ERBE data before and after the F06 adjustments; (i) plots the F06 adjustments; (j) plots the denoising and infilling applied by RMIB; (k) plots the denoising adjustments; (l) plots the UARS/ACRIM2 data and indicates the subsetting applied by C. Fröhlich (2006). All data gaps that existed in the original records have been infilled using the GA described in the text, except for the RMIB’s version of ERBS/ERBE, which was infilled using the SATIRE-S proxy model. Infilled data are indicated with black dashed lines where appropriate.
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: Original daily satellite TSI data as provided by the satellite mission teams at 1 au used to generate and update the composites. In this paper, we adopt the common nomenclature for referring to each satellite mission in the format “satellite/instrument.” An additional relevant record not shown here, but often used, is SOHO/VIRGO, which is the average of SOHO/DIARAD and SOHO/PMO6-VA.
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: Ongoing or recent satellite TSI missions with data used in this study for extending composites or comparative purposes—before and after the data infilling applied in this study. (a) SOHO/DIARAD; (b) SOHO/PMO6-VA using the latest adjustments applied to the PMO6 data by the PMOD group (W. Finsterle et al. 2021); (c) SOHO/PMO6(ROB) using the latest adjustments applied to the PMO6 data by the ROB group (S. Dewitte & S. Nevens 2021; S. Dewitte et al. 2022); (d) the SOHO/VIRGO series developed from the average of the DIARAD and PMO6 records after using the latest adjustments applied to the PMO6 data by the PMOD group (W. Finsterle et al. 2021); (e) the two TIM satellite missions with a suitable overlap for compositing purposes, i.e., SORCE/TIM and TSIS-1/TIM; (f) the final ACRIMSat/ACRIM3 mission data (R. C. Willson 2014).
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: Approach taken to composite the infilled versions of the SORCE/TIM and TSIS-1/TIM satellite records into one continuous TIM composite. (a) plots both records before compositing; (b) compares the two records after applying a linear shift to SORCE/TIM to match TSIS-1/TIM over the final 365 days of the overlap; (c) plots the daily difference between both records over the period of overlap; (d) plots the daily ratio between both records over the period of overlap and (e) the final composite.
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: SEA of heavy ion states in ICMEs triggering geomagnetic storms of different intensities. The time interval used in the SEA is 2 hr. The first vertical black line indicates the initiation of ICMEs. The second vertical black line indicates the end of the ICME. The various shades denote the error term. The shaded region in the figure represents the error, which is calculated based on the uncertainties listed in the data set.
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: Relationship between ICME parameters and the intensity of geomagnetic storms triggered by ICMEs. Events with a Kp index of 4 include all events that did not produce geomagnetic storms (Kp < 5); red circles represent events with shock occurrences, while blue circles represent events without shock occurrences; the red line represents the fitted curve of ICME parameters and geomagnetic storm intensity.
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: Depicts the physical parameters of ICMEs triggering geomagnetic storms of varying intensities, as well as the variations in O ion and Fe ion charge states and abundances. The red dashed line represents the start and end times of the ICME.
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-3D 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 three TSI models (EMPIRE, blue dashed line; C. A. Gueymard 2018, pink dashed line; NN-SIM, green dashed line) to each of the six composite group averages (colored lines using the same color scheme of Figure 8) 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: The State of Solar Wind Heavy Ions in Interplanetary Coronal Mass Ejection–Driven Geomagnetic Storms
Authors: Cong Wang, Fei He, Xiaoxin Zhang
Figure caption: Distribution of ICME events generating geomagnetic storms of different intensities. The blue bars represent the number of ICMEs triggering geomagnetic storms of different intensities, the red bars represent the number of ICMEs with interplanetary shocks, and the black line represents the percentage of ICMEs with interplanetary shocks among the ICMEs triggering geomagnetic storms of that intensity.
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 distribution of mean charge state of different heavy ions in ICME events. Points of various colors represent ICMEs triggering geomagnetic storms of varying intensities. The straight lines of different colors correspond to the fitting lines of the points of corresponding colors.
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 T. Chatzistergos et al. (2020)'s two proxy-based TSI models using Ca II K magnetograms with either blue or red continuum (blue or red colored dashed lines) to each of the six composite group averages (colored lines using the same color scheme of Figure 8) 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: 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: The visibility amplitude for the 244–251 MHz band has been plotted as a function of the baseline length, where the baseline length has been measured in units of k λ. All times and frequencies between 244 and 251 MHz have been averaged for this figure.
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: Two solar radio images showing some of the smallest source sizes measured. The time in the title corresponds to that 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: This figure shows the phase variation as a function of frequency for a few chosen baselines. The title shows the median (u, v).
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: The minimum value of ﹩{\tilde{\chi }}^{2}﹩ (black line, computed as −2 × log likelihood) as a function of θ obs (left panel) and E 0 (right panel) for the full model, Gaussian jet with no L X fit. The minimum ﹩{\tilde{\chi }}^{2}﹩ is computed over all MCMC samples with target parameter (θ obs or E 0) within each bin. Also plotted is the marginalized posterior (pale blue line) for both target parameters, the integral of the full posterior over all other parameters. The θ obs panel demonstrates a data (likelihood) driven fit, with the posterior weight sitting in the “bucket” of low ﹩{\tilde{\chi }}^{2}﹩ (high likelihood). The E 0 panel demonstrates the effect of degeneracies in the parameter, where all values of E 0 ≳ 1053.5 have similarly high likelihood (equal-quality fits to the data) but the marginalized posterior remains peaked due to differences in the available parameter volume.
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: The simple geometric constraints assuming a Gaussian jet from measurements of the early light-curve slope and the centroid position. The average apparent velocity of the afterglow centroid β avg from launch to the jet break is shown (solid contours) as a function of θ obs and θ  C . This quantity does not depend on the distance to the burst, the jet energy, nor the environment density. Lines of constant θ obs/θ  C , which can be inferred from the early light-curve slope, are shown by the gray dashed lines. The orange star marks the values for GW170817 under the Gaussian jet assumption, with a β avg ≈ 5 and θ obs/θ  C  ≈ 6.
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: The distance at which the radio flux and primary jet centroid offset at the jet break will take particular values as a function of viewing angle for a GW170817-like jet at ν = 5 GHz. Solid black contours show where the jet break flux F  ν  = 10, 100,... μJy. Brighter jets are nearer and at lower θ obs, the shaded gray region shows where F  ν  ≥ 10 μJy, etc. Dashed blue lines show where the centroid offset ﹩{\tilde{x}}_{{\rm{c}}}=1,3,10,30﹩ mas at the time of the jet break. Larger offsets occur for nearby jets with greater θ obs, the shaded blue regions shows where ﹩{\tilde{x}}_{{\rm{c}}}\geqslant ﹩ 1 mas, etc. The overlapping shaded region shows roughly which GW170817-like jets will have detectable proper motion with VLBI.
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: Projections of the posterior distribution to the full data set of GW170817 for models without (left panel) and with (right panel) an extra L X component. Each plot shows the results under four different assumptions: only fitting the afterglow light-curve data (blue), including the gravitational wave prior on the viewing angle θ obs (orange), including the VLBI centroid measurement (green), and including both VLBI and GW prior (black).
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: The GW170817 light multiband light curve and fits with the full model. Radio, optical, and X-ray data are shown in green, blue, and purple, respectively. Triangles show 3σ upper limits; only data points within 20% of the target frequency are shown. Solid bands show the modeled afterglow emission after MCMC fitting. The solid curve shows the median flux as a function of time, and the pale bands show the 68% and 95% quantiles of the flux at each time. Left panel: fit with a Gaussian jet only. Right panel: fit with a Gaussian jet plus additional late-time constant luminous X-ray component L X.
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: The position of the GW170817 centroid on the sky and fits with the full model. Black data points are radio VLBI measurements (Mooley et al. 2018; Ghirlanda et al. 2019). The gray data point is the HST kilonova position, assumed to be the burst origin (Mooley et al. 2022). Blue regions show the 68% (dark) and 95% (light) posteriors of the fit location at each epoch. Pale blue cloud on the right side of each panel shows the posterior distribution on the burst origin. Top panel: fit with a Gaussian structured jet only. Bottom panel: fit with a Gaussian structured jet plus a constant additional X-ray component.
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 Gaussian 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 Gaussian structured jet. 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: Posterior distributions on the source flux s given observed counts N = 5 and background (Bkg) counts B = 10 under different assumptions of the data distribution. In each case, the posterior p(s) = p(s∣N) is computed from the given likelihood using a uniform prior on s > 0.
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: Vertical slices of the R8-4pc simulation at t = 430 Myr through y = 200 pc. From left to right, the panels show ISM phase (see Table 2 for phase definitions), electron abundance (x  e ), temperature (T), number density of hydrogen (n H), FUV energy density (﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{FUV}}﹩), and LyC energy density (﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{LyC}}﹩). The points in the rightmost panel represent radiation source particles projected onto the y = 200 pc plane. The age of each source is given by its color, and the points are limited to sources with ages less than 20 Myr. In the panel showing x  e , the red contour marks the boundary between the hot and WIM phases.
Paper: Generation of 30 s Waves Observed Upstream of the Martian Bow Shock: A Case Study
Authors: Taifeng Jin, Binbin Ni, Song Fu, Xing Cao, Shuyue Pang, Xiaotong Yun, Minyi Long, Hengle Du
Figure caption: VDF fitting and dispersion relation calculation during 23:03–23:08. (a) H+ VDF fitting from STATIC measurement; (b) electron VDF fitting from SWEA measurement; (c) frequency solution from dispersion relation, blue and magenta lines referring to real and imaginary parts of normalized frequency (ω) using proton gyrofrequency (ω p), respectively. The wavenumber k is normalized by k  n  = ω  pi /c 0, where ω  pi  is the plasma frequency and c 0 the speed of light in the vacuum.
Paper: Generation of 30 s Waves Observed Upstream of the Martian Bow Shock: A Case Study
Authors: Taifeng Jin, Binbin Ni, Song Fu, Xing Cao, Shuyue Pang, Xiaotong Yun, Minyi Long, Hengle Du
Figure caption: Skymap of H+ flux observed by STATIC during 23:00–23:10. (a), (b) Skymap distribution of H+ in 500–4000 eV; (c), (d) H+ in 4–10 keV. The asterisk marks in (a) and (b) refer to the directions of magnetic field in the field of view of STATIC, the red ones indicating starting point of vector series. Similarly, the red segments with asterisk mark tailed in (c) and (d) refer to averaged magnetic field direction during the given time period.