adsabs/AstroCLIMB huggingface dataset:
Paper: Walk on the Low Side: LOFAR Explores the Low-frequency Radio Emission of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Benedetta Vulcani, Bianca M. Poggianti, Alessia Moretti, Timothy Shimwell, Andrea Botteon, Reinout J. van Weeren, Ian D. Roberts, Jacopo Fritz, Neven Tomičić, Giorgia Peluso, Rosita Paladino, Myriam Gitti, Ancla Müller, Sean McGee, Marco Gullieuszik
Figure caption: Integrated radio luminosity at 144 MHz vs. SFR. For each galaxy, the SFR H α  from Vulcani et al. (2018) (red points) and SFRrecent (gold points; see Section 3.3), with the corresponding errors, are connected by the dashed lines. We show also the best-fit L Rad−SFR relations from Gürkan et al. (2018) (blue line) and Roberts et al. (2021b) (red line). The shaded regions show the dispersion at 1σ around the corresponding best-fit relations.
Paper: Walk on the Low Side: LOFAR Explores the Low-frequency Radio Emission of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Benedetta Vulcani, Bianca M. Poggianti, Alessia Moretti, Timothy Shimwell, Andrea Botteon, Reinout J. van Weeren, Ian D. Roberts, Jacopo Fritz, Neven Tomičić, Giorgia Peluso, Rosita Paladino, Myriam Gitti, Ancla Müller, Sean McGee, Marco Gullieuszik
Figure caption: Results of MCptp with 100 iterations for each galaxy of the GASP-LOFAR sample. For each galaxy, the mean and the standard deviation of the distribution is reported in the respective label.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Evolution of mass (top) and mass accretion rate (bottom) of the sink particle for the collision of unequal-mass cores. The blue lines correspond to the contributions from gas initially labeled C 1 = 1.0. The green lines correspond to those from gas labeled C 2 = 1.0. The cyan lines indicate the total amounts. In the top row, the black dashed–dotted lines indicate the mass fraction of gas initially labeled C 1 = 1.0 for the sink particle.
Paper: Sigmoid Formation through Slippage of a Single J-shaped Coronal Loop
Authors: Hanya Pan, Tingyu Gou, Rui Liu
Figure caption: Temporal evolution during the preflare phase. Panel (a) shows the evolution of magnetic flux from the rectangular region marked in Figure 9(a) over 3 days prior to the flare of interest. Panels (b)–(d) zoom in on a 2 hr interval before and at the flare onset to show GOES 1–8 Å flux, normalized brightness of six AIA EUV passbands averaged over the elliptical region marked in Figure 7, and the evolution of coronal structures seen through the slit S1 marked in Figure 1(f). In panel (c), the ratio R  S  of the dimming slope during the slipping phase, over that during the preslipping phase is annotated for each passband (Section 2.5). The shaded bar indicates the time range during which counterstreaming flows were observed (Section 2.6). Panel (e) shows the evolution of the slipping speed with estimated error bars (Section 2.3). Panel (f) shows the average temperature of the eastern and western segments of the S-shaped loop and of the blob. The segments are indicated by yellow curves in Figure 6(a).
Paper: Sigmoid Formation through Slippage of a Single J-shaped Coronal Loop
Authors: Hanya Pan, Tingyu Gou, Rui Liu
Figure caption: Current density distribution in the corona in relation to the loop slippage. Panel (a) shows the vertical component J  z  of current densities derived from HMI vector magnetograms (hmi.sharp_cea_720s data products) during the loop slippage. Vector magnetograms are smoothed by a 4 × 4 pixel2 running box before J  z  is calculated. Panel (b) shows the integration of the absolute value of column current density over the height range from 2.9 to 47.4 Mm. The orange and blue contours in (a) and (b) indicate the B  z  component of photospheric magnetic fields at ±400 G, respectively. The color coded curves show the loop position obtained from the composite of 131 and 94 Å running difference images at different time instants. Panel (c) gives the variation of electric current density with increasing height in a representative region of strong current density (black box in (b)) and in a reference region of weak current density (white box in (b)). The green shaded range indicates the standard deviation of current densities in the selected box regions. The gray shaded bar indicates the height range within which the column current density in (b) is obtained.
Paper: Catastrophic Cooling in Superwinds. III. Nonequilibrium Photoionization
Authors: A. Danehkar, M. S. Oey, W. J. Gray
Figure caption: UV diagnostic diagrams plotting O VI λ λ 1032,1038/He II λ1640 vs. C IV λ λ 1548,1551/He II λ1640 for the radiation-bounded NPI models. Symbols and line types are as in Figure 4. The CPI results are shown by lightly shaded colors.
Paper: Catastrophic Cooling in Superwinds. III. Nonequilibrium Photoionization
Authors: A. Danehkar, M. S. Oey, W. J. Gray
Figure caption: The same as Figure 6, but for the partially density-bounded models.
Paper: Sigmoid Formation through Slippage of a Single J-shaped Coronal Loop
Authors: Hanya Pan, Tingyu Gou, Rui Liu
Figure caption: Filament in different periods. Panels (a) and (b) were observed before the loop slippage. Panel (c) was observed after the loop slippage but right at the flare onset. Panel (d) was observed during the flare gradual phase.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Cumulative multi-messenger detection rates as a function of redshift (luminosity distance) for our NSNS population. The left-hand panel assumes the counterpart search detection limits, representative of a search for an EM counterpart over the GW localization volume (see Table 1). The light gray line (All NSNS) represents the intrinsic merger rate in a cumulative form, with the gray band showing its assumed uncertainty (Abbott et al. 2021d), which propagates as a constant relative error contribution to all the other rates shown in the figure. The black (HLVK O4) and gray (HLV O3) lines are the cumulative GW detection rates (events per year with network S/N ≥12, accounting for the single-detector duty cycles) in O4 and O3. The blue (KN+O4), red (GRB Afterglow+O4), and orange (GRB Prompt+O4) lines are the cumulative detection rates for the joint detection of GW and a KN, GRB afterglow or GRB prompt in O4 (in at least one of the considered bands, all-sky except for the dashed line, which accounts for the Fermi/GBM duty cycle and field of view). The right-hand panel assumes deeper detection limits (see Table 1) representative of the monitoring of a well-localized candidate (and a subthreshold search for the GRB prompt). For the GRB afterglow we show separately the radio, optical, and X-ray band detection rates (solid, dashed, and dotted, respectively).
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Distribution of O4 KN optical and near-infrared magnitude as a function of time. The left-hand panel shows the apparent AB magnitude vs. post-merger time for our simulated KN light curves, restricting to O4 GW-detectable sources. The shaded regions contain 50%, 90%, and 99% of the KN light curves. Blue and red colors refer, respectively, to the g (484 nm) and z (900 nm) bands. Colored circles show extinction-corrected AT2017gfo data rescaled to the median distance of our population (∼181 Mpc). The right-hand panel shows the cumulative distributions of apparent magnitude at peak, at 3 days and 5 days after the merger (solid, dashed, and dotted lines, respectively).
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption:  F  ν , AB magnitude, and ν L  ν  vs. time for the GRB afterglow light curves associated with O4-detectable sources in our population. Solid and dashed contours contain 50% and 90% of the peaks, respectively. Red, green, and blue colors indicate the radio (1.4 × 109Hz), optical (4.8 × 1014Hz), and X-ray (2.4 × 1017Hz) bands, respectively. The colored circles are the observed data of GRB 170817A (Makhathini et al. 2021) at the median distance of our population. The gray lines in the background are 500 randomly sampled optical light curves.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Rest-frame SED peak photon energy E peak vs. the isotropic-equivalent energy E iso for our NSNS population. The filled green colored regions contain 50%, 90%, and 99% of the binaries both GRB Prompt- and O4-detectable. The magenta lines contain 50%, 90%, and 99% (solid, dashed, and dotted, respectively) of the GRB Prompt-detectable binaries. The black dashed line contains 90% of the O4-detectable binaries. The black dots with error bars represent an SGRB sample for comparison (Salafia et al. 2019). The orange dot is GRB 170817A.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Posterior probability density on our chirp mass probability distribution parameters ﹩{{ \mathcal M }}_{c,\min }﹩ and α. Filled contours show the two-dimensional posterior probability density, with lighter colors corresponding to larger values, as defined in the color bar.
Paper: Multi-messenger Observations of Binary Neutron Star Mergers in the O4 Run
Authors: Alberto Colombo, Om Sharan Salafia, Francesco Gabrielli, Giancarlo Ghirlanda, Bruno Giacomazzo, Albino Perego, Monica Colpi
Figure caption: Posterior probability density on the β parameter of our assumed mass ratio probability distribution parameterization. The red solid curve shows the result of Equation (A5) using the mass information on 10 Galactic NSNS binaries that merge within a Hubble time from Farrow et al. (2019). The pink shaded area shows the 90% credible interval, while the vertical dashed line marks the maximum a posteriori.
Paper: Search for Coincident Gravitational-wave and Fast Radio Burst Events from 4-OGC and the First CHIME/FRB Catalog
Authors: Yi-Fan Wang, 一帆 王, Alexander H. Nitz
Figure caption: The posterior distribution of sky location for 190701_223118 from Bayesian inference given hypothesis ﹩{{ \mathcal H }}_{2}﹩, which assumes the R.A. and decl. are free parameters to be inferred by gravitational-wave strain data. The 90% and 50% credible regions are shown. The marker represents the sky location of FRB 20190701E measured by the CHIME/FRB Collaboration (2018).
Paper: Search for Coincident Gravitational-wave and Fast Radio Burst Events from 4-OGC and the First CHIME/FRB Catalog
Authors: Yi-Fan Wang, 一帆 王, Alexander H. Nitz
Figure caption: Histogram of the detection statistic values for our search candidates and background noise. The y-axis represents the number of events per observation time of 2.4 months, and the bin width is 0.3. The most significant trigger has a λ gw+frb = 8.92 with a false alarm rate 0.29 per observation time.
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption: BH mass spectra for the resolutions in Table 1. All panels share a similar x-axis, the initial He core mass M He in M ⊙, and y-axis, the BH mass in M ⊙. Resolutions that are only shown at their respective peak BH masses are labeled with asterisks on either side. The horizontal dashed and solid lines indicate the location of the peak BH mass for each resolution.
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption: The difference in convection and nuclear burning between the three stellar models, as discussed in Section 3.1. The figures in the left column are shown vs. the model number from the He burning to CC. The figures in the right column are shown vs. the logarithm of the time to CC, beginning at the onset of the shell C burning. The different fuels that are burned are labeled. Each figure shows the signed logarithm of the net specific power, ﹩\mathrm{sign}\left({\epsilon }_{\mathrm{nuc}}-{\epsilon }_{\nu }\right){\mathrm{log}}_{10}\left(\max \left(1.0,| {\epsilon }_{\mathrm{nuc}}-{\epsilon }_{\nu }| \right)\right)﹩, where ϵ nuc is the specific energy generation rate and ϵ  ν  is the specific energy loss from neutrinos. The purple regions denote strong neutrino cooling and the red regions denote regions of strong nuclear burning. The light blue regions indicate standard-mixing-length convection, the gray regions indicate convection with reduced mixing, because of the shorter convective timescales, and, for model 2, the beige–orange regions (e.g., near the surface) indicate where the diffusive mixing coefficient is set to D = 10−2 cm2 s−1.
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption: The BH mass spectra for different values of the 12C(α,γ)16O rate—top (σ = −3); bottom (σ = +3); and middle (σ = 0)—for five of the resolutions listed in Table 1. All panels share a similar x-axis, the initial He core mass M He in M ⊙, and y-axis, the BH mass in M ⊙. Resolutions that are only shown at their respective peak BH masses are labeled with asterisks on either side. The horizontal dashed and solid lines indicate the location of the peak BH mass for each resolution.
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption: Both panels share the same x-axis, the logarithmic time to CC, in seconds. The top panel shows the neutrino luminosity and the Kelvin–Helmholtz timescale, normalized to account for the energy lost to neutrinos, which dominates over photon cooling in the evolutionary phases shown. The integrated 〈Γ1 − 4/3〉 is shown in the bottom panel, to illustrate when the models are evolving dynamically. The hatched regions indicate where the C shell, O core, and Si core burning take place.
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption:  12C(α, γ) reaction rate ratios, σ  i /σ 0, as a function of temperature. σ  i  spans −3.0 to 3.0 in 0.5 step increments, with σ 0 being the current nominal rate. Negative σ  i  are shown with the gray curves and positive σ  i  are shown with the green curves. The ±1, 2, and 3 σ  i  curves are labeled. The blue band shows the range of temperatures encountered during the core and shell He burning.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Sensitivity test showing the atmospheric mixing ratios of N2O as a function of surface flux for an Earthlike atmosphere with pO2 = 100% PAL and an eddy diffusion (k  zz ) profile matching the Earth average (solid) and increased by a factor of 10 uniformly through the upper atmosphere (dashed).
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption: The same as Figure 1, but with an example of a calculated BH mass spectrum (the teal line and diamonds). The magenta line marks M BH = M He. The peak BH mass is labeled. The smaller masses, just to the left of the peak, show weak pulses. The larger masses, just to the right, show strong pulses.
Paper: Resolving the Peak of the Black Hole Mass Spectrum
Authors: Ebraheem Farag, Mathieu Renzo, Robert Farmer, Morgan T. Chidester, F. X. Timmes
Figure caption: Illustration of a single-star BH mass spectrum.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Balance of energy fluxes in the quiet Sun corona. Panel (a): conservation of magnetic energy. The black solid line is the mean vertical Poynting flux (S  z ) on the left-hand side of Equation (9). The red dotted line shows the sum of specific energy fluxes for the Lorentz force work (﹩{{ \mathcal F }}_{\mathrm{wlr}}﹩) and resistive heating (﹩{{ \mathcal F }}_{\mathrm{res}}﹩) on the right-hand side of Equation (9). The individual contributions of ﹩{{ \mathcal F }}_{\mathrm{wlr}}﹩ and ﹩{{ \mathcal F }}_{\mathrm{res}}﹩ are shown by the orange dashed and dotted lines, respectively. All of these energy fluxes are averaged over 11.5 hr. Panel (b): balance of temporally averaged energy fluxes on the right-hand side of Equation (10). Lines are noted by the names with corresponding colors. Positive and negative values are shown as solid and dashed lines, respectively. Panel (c): balance of energy fluxes (also as functions of time) at the base of the quiet Sun corona (z = 5.28 Mm) as given by Equation (10). Lines are noted by the names with corresponding colors. See Section 3.5 for details.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Distribution of the free magnetic energy with height (z > 0 Mm). Panel (a): time–height diagram showing the evolution of the horizontally averaged free magnetic energy density (e free). The contour lines of f cum indicate the percentage of the free energy contained in the volume below a certain height, as given by Equation (14). The dashed lines mark three evolution stages, over which temporal averages of e free are calculated. Panel (b): horizontally and temporally averaged magnetic energy density in the quiet Sun (QS). The solid black line plots the total magnetic energy density (e tot), and the solid red line is e free. The dotted black line is the ratio between the red and black lines, i.e., the percentage of the free energy among the total magnetic energy. Panel (c): the same analysis as in panel (b) for the early stage of active region evolution (AR early). The notations of the lines are identical to those in panel (b). Panel (d): the same analysis as in panel (b) for the late stage of active region evolution (AR late). The notations of the lines are identical to those in panel (b).
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Temporal evolution of magnetic flux that emerged in the photosphere and the magnetic energy contained in the domain above the photosphere. (a): The solid line shows the total unsigned vertical magnetic flux. The dotted line is the flux emergence rate given by the time derivative of the magnetic flux. (b): The black and red lines plot the total magnetic energy (E tot) and free magnetic energy (E free), respectively. In particular, the solid red line is for E free in the domain above the photosphere, and the dotted red line only accounts for E free in the domain above z = 2 Mm, which corresponds to the low β corona. A zoomed view of a time period of 2 hr showing the evolution of the free magnetic energy during an eruption event is presented in the insert. (c): Rate of change of the total and free magnetic energy from panel (b).
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Time–distance diagrams of the disturbances in (a) AIA 193 intensity, (b) plasma pressure, (c) v  x , and (d) B  x . The diagrams are constructed along the slit shown in Figure 6(b) and for a time period of 70 minutes. The blue lines in each panel illustrate the travel paths of sound waves (starting from five different time instances) according to Equation (4). Similarly, green lines show the paths of Alfvénic disturbances as given by Equation (5).
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Transition from the strongly non-force-free magnetic field and high β plasma in the interior to the (close to) force-free magnetic field and low β plasma in the corona. Panel (a): the PDF of r  f  defined by Equation (15). Panel (b): a zoomed view of the same quantity as in panel (a) in the domain between z = −5 and 5 Mm. Panel (c): the PDF of plasma β. Panel (d): a zoomed view of the same quantity in panel (c) in the domain between z = −5 and 5 Mm. The white line in each panel indicates the most probable value of the quantity shown in that panel.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Evolution of the magnetic field in the photosphere and low corona as active regions emerge. Grayscale images in the square panels present B  z  at the τ = 1 surface at six time instances. The color-scale panel below each grayscale image shows the magnetic field strength in the first 45 Mm of the vertical domain (from 10 Mm beneath to 35 Mm above the photosphere), overlaid by two contour lines that illustrate the asymmetry of coronal magnetic field strength. The magnetic field strength is averaged in the y-direction between the two dotted lines in the B  z  maps.
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Evolution of a magnetic flux rope spontaneously formed in the quiet Sun. The blue lines are magnetic field lines that outline the flux rope. The grayscale images in the 3D views show B  z  in the photosphere (+/− 100 G). Red-frame panels present B  z  (grayscale image, +/− 100 G) and the horizontal velocity field (arrows) at the (positive polarity) leg of the flux rope. The location of the red-frame panels (about 1 Mm above the photosphere and fixed in time) is marked by the small red frame in panel (d). The red, green, and blue arrows indicate the x-, y-, and z-directions, respectively. The 3D visualization is produced with VAPOR (Li et al. 2019).
Paper: A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
Authors: Feng Chen, Matthias Rempel, Yuhong Fan
Figure caption: Mean (unlimited) Alfvén velocity in the first 45 Mm of the vertical domain (from 10 Mm beneath to 35 Mm above the photosphere). The Alfvén velocity is averaged in the y-direction between the two dotted lines in Figure 9. Time instances are identical to those in Figure 9. The actual maximum Alfvén velocity allowed by the Boris correction is marked above each panel and plotted as a contour line on the map of the mean Alfvén velocity.
Paper: The Longest Delay: A 14.5 yr Campaign to Determine the Third Time Delay in the Lensing Cluster SDSS J1004+4112
Authors: J. A. Muñoz, C. S. Kochanek, J. Fohlmeister, J. Wambsganss, E. Falco, R. Forés-Toribio
Figure caption: The light curves of the four bright quasar images in SDSS J1004+4112. The B, C, and D images are offset by 2, 4, and 6 magnitudes, respectively, for display purposes. The data span 14.5 yr, from 2003 December 20, until 2018 June 21.