adsabs/AstroCLIMB huggingface dataset:
Paper: Energy Evolution in the Progenitor of Galaxy Shells: A Semi-analytical Model
Authors: Beibei Guo, Xufen Wu, HongSheng Zhao, Lulu Fan
Figure caption: Shows a schematic diagram of a target or host galaxy at the origin being intruded by a rotating dwarf galaxy on a nearly radial prograde orbit at position (r  c , Θ) with velocity  v   c . Also shown are the polar coordinates (﹩{r}_{i}^{{\prime} }﹩,θ  i ) of the ith star in the dwarf. All angles are with respect to the x-axis basis  e  x, pointing to the apocenter before the merger. The solid gray line represents the actual trajectory of the intruding galaxy, with arrows indicating the direction of motion, while the dashed gray line represents the Keplerian orbit.
Paper: Stealth Non-standard-model Confined Flare Eruptions: Sudden Reconnection Events in Ostensibly Inert Magnetic Arches from Sunspots
Authors: Ronald L. Moore, Sanjiv K. Tiwari, Navdeep K. Panesar, V. Aparna, Alphonse C. Sterling
Figure caption: Magnetic setting and progression of the flare ribbons and loops in eruption 2 of Table 1. First column: HMI magnetograms; second column: AIA 1600 Å images; third column: AIA 131 Å images; fourth column: AA 211 Å images; fifth column: AIA 171 Å images. The x, y coordinates of the field of view in arcseconds from the disk center are on the outside of the last magnetogram. The universal time is in the upper right corner of each panel. In the first row, 20 G and 100 G contours (red for positive flux, blue for negative flux) of the magnetogram are plotted on the 1600 Å image. Black arrows and white arrows point to the four feet of the two main flare loops. In panels (r), (w), and (×) the long red arrow points to the longer and dimmer of the two loops, and the short red arrow points to the shorter and brighter of the two loops.
Paper: Stealth Non-standard-model Confined Flare Eruptions: Sudden Reconnection Events in Ostensibly Inert Magnetic Arches from Sunspots
Authors: Ronald L. Moore, Sanjiv K. Tiwari, Navdeep K. Panesar, V. Aparna, Alphonse C. Sterling
Figure caption: Magnetic setting and progression of the flare ribbons and flare loops in eruption 1 of Table 1. The format is the same as in Figure 3. Black arrows point to the four feet of the two main flare loops. Downward red arrows point to the longer and dimmer of the two loops. Upward red arrows point to the shorter and brighter of the two loops. In four of the 171 Å images, white arrows point to an inert dark filament suspended above a ragged PIL seen in the magnetogram.
Paper: Stealth Non-standard-model Confined Flare Eruptions: Sudden Reconnection Events in Ostensibly Inert Magnetic Arches from Sunspots
Authors: Ronald L. Moore, Sanjiv K. Tiwari, Navdeep K. Panesar, V. Aparna, Alphonse C. Sterling
Figure caption: Schematic of the proposed internal structure of the magnetic arch from the big sunspot in AR 11654 before and after the burst of reconnection that makes and heats the two side-by-side main flare loops in eruption 2. Top: the magnetic arch viewed from above (left panel) and from its west side (right panel) before the burst of reconnection. Bottom: the same two views after the burst of reconnection. The minus (plus) signs indicate the negative (positive) polarity of the magnetic arch's end inside (outside) the sunspot. Black curves outline the magnetic arch's outer end and the sunspot's umbra and penumbra. The body of the magnetic arch is outlined by blue curves. In the interior of the magnetic arch before the burst of reconnection, the two blue curves are the two crossed magnetic field strands that are poised to reconnect at their interface. The two side-by-side main flare loops made by the burst of reconnection are red, and outlines of the flare “ribbons” at their feet are red.
Paper: Stealth Non-standard-model Confined Flare Eruptions: Sudden Reconnection Events in Ostensibly Inert Magnetic Arches from Sunspots
Authors: Ronald L. Moore, Sanjiv K. Tiwari, Navdeep K. Panesar, V. Aparna, Alphonse C. Sterling
Figure caption: Schematic of the proposed internal structure of the magnetic arch from the big sunspot in AR 11391 before and after the burst of reconnection that makes and heats the two crossed main flare loops in eruption 1. The format and symbolism are the same as in Figure 6. The two pre-reconnection magnetic field strands cross twice in the top view but only once in the side view. That shows they are poised to reconnect at only their eastern crossing. The burst of reconnection at their interface at their eastern crossing results in the two flare loops, with the longer and dimmer flare loop crossing above the west end of the shorter and brighter flare loop.
Paper: JADES: Spectroscopic Confirmation and Proper Motion for a T-Dwarf at 2 kpc
Authors: Kevin N. Hainline, Francesco D'Eugenio, Fengwu Sun, Jakob M. Helton, Brittany E. Miles, Mark S. Marley, Ben W. P. Lew, Jarron M. Leisenring, Andrew J. Bunker, Phillip A. Cargile, Stefano Carniani, Daniel J. Eisenstein, Ignas Juodžbalis, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer
Figure caption: (Left) 1D NIRSpec/PRISM spectrum compared to the best-fit standard brown dwarf from SPLAT. (Right) Reduced χ 2 compared to spectral type for the L and T standards from SPLAT.
Paper: JADES: Spectroscopic Confirmation and Proper Motion for a T-Dwarf at 2 kpc
Authors: Kevin N. Hainline, Francesco D'Eugenio, Fengwu Sun, Jakob M. Helton, Brittany E. Miles, Mark S. Marley, Ben W. P. Lew, Jarron M. Leisenring, Andrew J. Bunker, Phillip A. Cargile, Stefano Carniani, Daniel J. Eisenstein, Ignas Juodžbalis, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer
Figure caption: (Top) 3 pixel boxcar extracted 1D NIRSpec PRISM spectrum in gray, with the NIRCam fluxes from K. N. Hainline et al. (2024) plotted as red points. We plot the strong molecular absorption bands that shape the observed spectrum, labeled by their species, with purple horizontal lines. In an inset, we show the 2″ × 2″ RGB thumbnail for the brown dwarf, with the NIRSpec MSA slit positions overplotted. (Bottom) 2D NIRSpec PRISM spectrum for JADES-GS-BD-9.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Retrieved atmospheric property biases from neglecting nightside thermal emission. Shown are the posterior distributions from our transmission-only model (blue histograms) and the nightside-emission-included model (red histograms) from retrievals of our simulated WASP-33b JWST data set with three transits per mode. Top row: retrieved molecular abundances. Bottom row: retrieved 10 bar reference radius and atmospheric temperature parameters. The true parameter values used to generate the 2D atmospheric model (dashed crimson lines) are overlaid for comparison with the retrieved median and ±1σ value (error bars). The transmission-only model results in notable biases, most notably in the dayside temperature and the abundances for all molecules with bounded constraints (i.e., H2O, CO, TiOday, and VOday).
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Retrieved transmission spectra for a transmission-only model (purple) versus a model also incorporating nightside thermal emission (orange). Top panel: the retrieved spectra across the full optical-to-mid-infrared wavelength range. Middle panels: zoomed-in highlights of two specific regions in the near-infrared (4–6 μm) and mid-infrared (10–12 μm). All model spectra are shown at a resolution of R = 100 for clarity. Even though the magnitude of nightside contamination mathematically increases with wavelength (Equation (3)), the transmission-only model can both underpredict (middle left panel) and overpredict (middle right panel) the transit depth compared to the correct model including nightside emission. The bottom two panels represent the residuals between the simulated data and the value of the retrieved spectrum not including nightside contamination in units of uncertainty of the data.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Retrieved posterior distributions for various atmospheric properties of WASP-33b for a simulated three-transit observation. Top: retrieved posterior probability distribution for a model of WASP-33b with a 1D distribution of H2O. This is equivalent to the distributions seen in Figure 7. Bottom: retrieved posterior distributions for a model of WASP-33b with a difference in the abundance of H2O between the dayside and nightside. The blue distributions indicate the results for a retrieval that does not account for nightside thermal emission, while the red shows the results for the retrieval models that do. The dashed crimson lines indicate the true value of each parameter that was used to generate the simulated spectrum.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: 2D retrieval validation for a transmission spectrum including nightside thermal emission. Upper right: simulated JWST data for WASP-33b (error bars) compared to the median retrieved spectrum (purple line) and confidence intervals (1σ and 2σ contours). The model and data are shown at R = 100. Lower left: corresponding posterior probability distribution from the retrieval. The purple contours represent the 1σ, 2σ, and 3σ confidence intervals (in order of increasing opacity). The true parameter values used to generate the simulated JWST data (green lines) compare well with the median retrieved value (solid blue line), and all parameters are correctly retrieved within the 1σ confidence interval (dashed blue lines in the histograms).
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Instrument mode dependence of retrieved atmospheric properties from simulated WASP-33b JWST data. Posterior distributions are shown for one transit with a single instrument mode, assuming a transmission-only model, for NIRISS SOSS (purple), NIRSpec G395H (blue), and MIRI LRS (green). The abundances of H2O, TiO, and VO are best constrained by NIRISS SOSS, while NIRSpec G395H provides the tightest constraints on CO. Retrieval biases are not seen for single-instrument modes, unlike Figure 7, indicating that a broad wavelength range provides sensitivity to nightside emission contamination.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Transit dependence of retrieval biases from neglecting nightside thermal emission from simulated WASP-33b JWST data. The posterior probability distributions for each atmospheric property are shown for one transit (red), two transits (yellow), and three transits (green) per instrument mode (i.e., NIRISS SOSS + NIRSpec G395H + MIRI LRS) compared to the true value of each parameter (crimson dashed line). The median retrieved parameter has almost the same bias regardless of the number of transits, but the biases are more noticeable with additional transits due to the smaller 1σ confidence intervals.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Impact of neglecting nightside emission on retrieved pressure–temperature profiles. The retrieved nightside (blue) and dayside (red) P-T profiles for the transmission-only retrieval model. The true profiles (dashed lines) are compared to the median retrieved profiles (solid lines) and the 1σ confidence intervals (blue and red shading). These day and night profiles correspond to the blue posterior distributions in Figure 7. The dayside P-T profile is significantly biased, with a much smaller vertical temperature gradient than the true dayside profile.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Simulated JWST data for a 2D model transmission spectrum of WASP-33b. Shown are the predicted precisions from PandExo (N. E. Batalha et al. 2017) for a single transit per instrument mode for NIRISS SOSS (green), NIRSpec G395H (light blue and orange for the NRS1 and NRS2 detectors, respectively), and MIRI LRS (red). The model transmission spectrum corresponds to Figure 3 (dark blue line). All data are binned to R = 100 and shown without Gaussian scatter.
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: The solid lines show the distribution of time delays between detectable strongly lensed image pairs as obtained from our simulation (scale relative to the “O3, 109 M ⊙” case). The assumed observing run and the mass of the lensing CO are shown in the legend. The dashed line shows the distribution of time delays between pairs of events observed in O3 (scaled to peak at 1). The numbers of simulated samples are 5446, 1694, and 5085 for the “O3, 109 M ⊙”, “O2, 109 M ⊙,” and “O3, 107 M ⊙” cases, respectively, while 3081 pairs were observed in O3. Even if all of the dark matter was made of 109 M ⊙ COs, the lensing time delay would not exceed ∼105 s (gray shaded region). We have used a GW source redshift distribution from P. Madau & M. Dickinson (2014) for this simulation.
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Upper panel: the intrinsic distribution of the redshifts of BBHs, as well as the distribution of detected BBHs (both unlensed and lensed; these are scaled to reflect their abundance relative to the intrinsic population). Please refer to Appendix B for details of our simulations. Lower panel: strong lensing optical depth for the smooth (filled cone) and inhomogenous (empty cone) cosmologies.
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Posterior distribution of the fraction of dark matter f DM in the form of COs of mass M  ℓ . Solid (dotted) lines and filled squares (circles) respectively show the posteriors and 90% upper bounds on f DM assuming a flat (Jeffreys) prior in Equation (3). We have assumed that the BBH mergers have component masses which are distributed according to the “power law + peak” model from R. Abbott et al. (2023b), and are distributed in redshift following P. Madau & M. Dickinson (2014, thick lines) or K. Belczynski et al. (2016, thin lines).
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Current and expected 90% upper bounds on the fraction of dark matter f DM in the form of COs of mass M  ℓ  = 107 M ⊙, as a function of the number of BBH observed mergers with no detected lensed events. The black and gray lines correspond to flat and Jeffreys priors, respectively. We have used a GW source redshift distribution from P. Madau & M. Dickinson (2014) for this simulation.
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Probability distribution of the strongest lens’s impact parameter; see Equation (A2). The dotted lines show the linear approximation P(y 1) ∝ y 1. Note that for large τ, the distribution deviates from the linear approximation even at small values of y 1.
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Ninety percent upper bounds on the fraction of dark matter f DM in the form of COs of mass M  ℓ . Results are shown for two different source redshift distributions (shaded regions vs. hatches) and two different priors in Equation (3), flat (blue shades) and Jeffreys (red shades).
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: (Reversed) cumulative distributions of magnifications and time delays of the loudest two images from one (lighter solid lines) and two (darker dashed lines) lenses. While the distributions of μ 2 and ΔT remain more or less unchanged, the distribution of μ 1 is altered slightly due to the presence of a second lens.
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Magnification of images due to a point-mass lens as a function of the impact parameter y; see Equation (A1).
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Expected fraction u of detectable strongly lensed events if a fraction f DM of dark matter is made up of COs of mass M  ℓ .
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: Shown here is the power-law photon index plotted against each spectrum’s power-law cutoff energy, color coded by the blackbody temperature. While many observations demonstrate the expected behavior of a soft spectrum with a high blackbody temperature, some of the highest-temperature blackbodies are coincident with steep illuminating powerlaws with very low energy cutoffs. These observations are at the edge of the limits of XILLVERCO, which assumes illumination by a power law, even if the disk is being physically illuminated by the thermal NS boundary layer. In these cases, the model attempts to force the illuminating power law into a shape resembling that of a blackbody.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: Shown is the emissivity index q plotted against the total unabsorbed flux of the system. Flatter emissivity profiles are generally consistent with the system in a low–hard state, while steeper values of q correspond with the high/soft state. This is potentially explained by a corona which is extending spatially during low-flux states.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: The distribution of edge energies for the model containing both edges. We see that the higher energy edge near 0.87 keV (consistent with an Ne K or Fe L edge) is very well constrained, while the lower energy edge around 0.4 keV (consistent with an N detector edge) has a significant amount of spread. This is to be expected for a feature that sits at or below the given NICER band but should be addressed more carefully in future studies with higher resolutions and improved collecting areas at the softest energies.
Paper: Phantom Matter: A Challenging Solution to the Cosmological Tensions
Authors: Adrià Gómez-Valent, Joan Solà Peracaula
Figure caption: EOS diagram for the energy conditions of the cosmic fluids. The quintessence (Q) region (−1 < w < −1/3 with ρ > 0, p < 0) is marked cross-hatched, and the conventional phantom region (w ≤ −1 with ρ > 0, p < 0) is the blue sector indicated as P. The gray dotted area corresponds to the peculiar PM region: w < − 1 with ρ < 0 and p > 0. Notice that PM satisfies the strong energy condition, ρ + p ≥ 0, ρ + 3p ≥ 0 (all of the gray area), but not the weak energy condition, ρ ≥ 0, ρ + p ≥ 0 (shaded area, except the P and PM sectors). The DE component X in our analysis behaves as PM, whereas the Y component behaves as quintessence. The EOS line w = −1 marks off the classical vacuum. The RVM fulfills this EOS only approximately near our time owing to quantum effects (C. Moreno-Pulido & J. Solà Peracaula 2022b). See also J. Grande et al. (2006) and N. E. Mavromatos & J. Solà Peracaula (2021a) for the modern developments on PM.
Paper: Is Gamma-Ray Burst 221009A Really a Once-in-10,000 yr Event?
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: A plot of N(>S 1) vs. S 1 (i.e., the “log(N)–log(S)” distribution). The blue squares and black circles are the observed GBM and total GRBs, taken from E. Burns et al. (2023). The curves are the δ function models (from Section 2.1) with E  γ  = 1051 erg and two GRB populations with different θ  j , as indicated in the legend. The θ  j  = 6° population uses ﹩{z}_{\max ,* }=10﹩ while the θ  j  = 0.°8 population uses ﹩{z}_{\max ,* }=0.36﹩.
Paper: Phantom Matter: A Challenging Solution to the Cosmological Tensions
Authors: Adrià Gómez-Valent, Joan Solà Peracaula
Figure caption: Contour plots at 68% and 95% CL and the corresponding 1D posterior distributions for some of the parameters that are relevant in the discussion of the cosmological tensions, for all the models under study. H 0 is given in km s−1 Mpc−1. The complete triangle plot is presented in Figure 4.
Paper: Is Gamma-Ray Burst 221009A Really a Once-in-10,000 yr Event?
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: The peak afterglow flux density as a function of θ/θ  j  for E  γ  = 1051 erg, d  L  = 1028 cm, taken from H. van Eerten et al. (2010). The blue circles indicate the results taken from their light-curve calculation. The green lines indicate our interpolation. Left: optical (1014 Hz). Right: radio (109 Hz).
Paper: Is Gamma-Ray Burst 221009A Really a Once-in-10,000 yr Event?
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: A plot of N(>F) vs. flux density F for the afterglows of the GRB populations with log-normal distributions for θ  j  and E  γ . Left: the calculation for optical (1014 Hz) afterglows, as would be seen by Rubin. The solid curves include dust extinction, while the dashed curves do not. The vertical dashed line indicates the flux sensitivity limit of Rubin for its standard 30 s exposure. Right: the calculation for radio (109 Hz) afterglows, as would be seen by SKA. The vertical line is approximately the sensitivity limit for SKA Phase 1 used by G. Ghirlanda et al. (2014).
Paper: Is Gamma-Ray Burst 221009A Really a Once-in-10,000 yr Event?
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: A plot of rates per comoving volume for CCSNe and the two GRB populations in all directions (not just those pointed at the Earth).
Paper: Is Gamma-Ray Burst 221009A Really a Once-in-10,000 yr Event?
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: Same as Figure 1 but using log-normal distributions for θ  j  and E  γ .
Paper: Is Gamma-Ray Burst 221009A Really a Once-in-10,000 yr Event?
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: Left: the distributions for ﹩{\theta }_{j}={\cos }^{-1}{\mu }_{j}﹩ used in our calculations. Right: the distributions of E  γ  used in our calculations.