adsabs/AstroCLIMB huggingface dataset:
Paper: Observation of Anomalous Electron Fluxes Induced by GRB221009A on CSES-01 Low-energy Charged Particle Detector
Authors: R. Battiston, C. Neubüser, F. M. Follega, R. Iuppa, V. Vitale, R. Ammendola, D. Badoni, S. Bartocci, A. Bazzano, S. Beolè, I. Bertello, W. J. Burger, D. Campana, A. Cicone, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, F. De Angelis, C. De Donato, C. De Santis, P. Diego, A. Di Luca, E. Fiorenza, G. Gebbia, A. Lega, M. Lolli, B. Martino, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, A. Morbidini, F. Nuccilli, F. Nozzoli, A. Oliva, G. Osteria, E. Papini, F. Palma, F. Palmonari, A. Parmentier, B. Panico, S. Perciballi, F. Perfetto, A. Perinelli, P. Picozza, M. Piersanti, M. Pozzato, G. Rebustini, D. Recchiuti, E. Ricci, M. Ricci, J. Rodi, A. Russi, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, X. Shen, A. Sotgiu, R. Sparvoli, S. Tofani, P. Ubertini, N. Vertolli, V. Vilona, U. Zannoni, Z. Zeren, S. Zoffoli, P. Zuccon
Figure caption: Fraction of GRBs with the highest-energy photon detected by Fermi above selected threshold energies (Ajello et al. 2019). The energy distribution corrected for the source redshift is indicated by the dashed green line. The dashed black line shows a linear fit to the values corresponding to the center of each bin.
Paper: Observation of Anomalous Electron Fluxes Induced by GRB221009A on CSES-01 Low-energy Charged Particle Detector
Authors: R. Battiston, C. Neubüser, F. M. Follega, R. Iuppa, V. Vitale, R. Ammendola, D. Badoni, S. Bartocci, A. Bazzano, S. Beolè, I. Bertello, W. J. Burger, D. Campana, A. Cicone, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, F. De Angelis, C. De Donato, C. De Santis, P. Diego, A. Di Luca, E. Fiorenza, G. Gebbia, A. Lega, M. Lolli, B. Martino, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, A. Morbidini, F. Nuccilli, F. Nozzoli, A. Oliva, G. Osteria, E. Papini, F. Palma, F. Palmonari, A. Parmentier, B. Panico, S. Perciballi, F. Perfetto, A. Perinelli, P. Picozza, M. Piersanti, M. Pozzato, G. Rebustini, D. Recchiuti, E. Ricci, M. Ricci, J. Rodi, A. Russi, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, X. Shen, A. Sotgiu, R. Sparvoli, S. Tofani, P. Ubertini, N. Vertolli, V. Vilona, U. Zannoni, Z. Zeren, S. Zoffoli, P. Zuccon
Figure caption: A map of the Earth with the CSES-01 orbit 259770 on 2022 October 9 shown in gray. The data-taking of HEPP-L started at 13:17:29 and ended at 13:54:34 UTC. The colored part along the orbit marks the seconds from 13:20:00 UTC for 6 minutes. The red shaded area shows the approximate illumination area of GRB221009A, estimated for the central impact point (red dot) at 19.°8 and 71° in latitude and longitude, respectively.
Paper: Observation of Anomalous Electron Fluxes Induced by GRB221009A on CSES-01 Low-energy Charged Particle Detector
Authors: R. Battiston, C. Neubüser, F. M. Follega, R. Iuppa, V. Vitale, R. Ammendola, D. Badoni, S. Bartocci, A. Bazzano, S. Beolè, I. Bertello, W. J. Burger, D. Campana, A. Cicone, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, F. De Angelis, C. De Donato, C. De Santis, P. Diego, A. Di Luca, E. Fiorenza, G. Gebbia, A. Lega, M. Lolli, B. Martino, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, A. Morbidini, F. Nuccilli, F. Nozzoli, A. Oliva, G. Osteria, E. Papini, F. Palma, F. Palmonari, A. Parmentier, B. Panico, S. Perciballi, F. Perfetto, A. Perinelli, P. Picozza, M. Piersanti, M. Pozzato, G. Rebustini, D. Recchiuti, E. Ricci, M. Ricci, J. Rodi, A. Russi, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, X. Shen, A. Sotgiu, R. Sparvoli, S. Tofani, P. Ubertini, N. Vertolli, V. Vilona, U. Zannoni, Z. Zeren, S. Zoffoli, P. Zuccon
Figure caption: A Computer-Aided Design (CAD) rendering and a schematic top view of HEPP-L are show in (a) and (b), respectively. The collimator system, the anticoincidence detector (plastic scintillator), used to shield from out-of-acceptance particles, and the silicon detector (SD) are displayed in (b) (Li et al. 2019).
Paper: The Neon Gap: Probing Ionization with Dwarf Galaxies at z ∼ 1
Authors: John Pharo, Yicheng Guo, David C. Koo, John C. Forbes, Puragra Guhathakurta
Figure caption: Left: example spectrum of a HALO7D dwarf emission-line galaxy. The blue solid line gives the observed spectrum. The orange solid line shows the continuum estimate, and the green solid line shows the continuum-subtracted spectrum. Prominent emission lines are labeled and indicated by vertical dashed lines. Black and gray dashed lines indicate strong and/or Balmer series emission lines. Green dashed lines indicate typically fainter ionized metal lines, and the blue dashed line shows the location of a blend of the faint He I λ3889 and Hζ emission lines. The two magenta dashed lines show the locations of the Ca H and K stellar absorption lines though these features are not prominent in this spectrum, which has little stellar continuum due to its low stellar mass as well as a likely young stellar population. Right: a zoom-in on the spectrum showing the [OII]λλ3727,3729 doublet, as well as the [NeIII]λ3869 emission line and He I–Hζ blend.
Paper: The Neon Gap: Probing Ionization with Dwarf Galaxies at z ∼ 1
Authors: John Pharo, Yicheng Guo, David C. Koo, John C. Forbes, Puragra Guhathakurta
Figure caption: Left: Ne3O2 vs. O32 for individual HALO7D galaxies (green circles) and composite HALO7D spectra (blue circles) compared with 2 < z < 3 composite spectra from J20 (red diamonds) and individual measurements from S17 (maroon line). We also include median values for local H II regions (blue triangles) assembled in J20 from Pilyugin & Grebel (2016), Croxall et al. (2016), and Toribio San Cipriano et al. (2016). The gray shaded region indicates the 90% boundary for local SDSS galaxies measured in S17. The dashed black line shows a linear fit of the HALO7D points. Individual [NeIII]λ3869 detections in HALO7D exhibit comparable ionization properties to (typically more massive) 2 < z < 3 galaxies but with high scatter that may be related to metallicity variations. The red, purple, and yellow curves give the BPASS models from S17. Right: the Ne3O2 offset from the linear Ne3O2-O32 fit as a function of the R23 metallicity.
Paper: The Neon Gap: Probing Ionization with Dwarf Galaxies at z ∼ 1
Authors: John Pharo, Yicheng Guo, David C. Koo, John C. Forbes, Puragra Guhathakurta
Figure caption: Ne3O2 vs. stellar mass for individual HALO7D galaxies (green circles) and composite HALO7D spectra (blue circles) compared with z ∼ 2 individual and composite measurements from J20 (red diamonds), local SDSS composite measurements from AM13 (purple triangles), and local low-mass individual detections (light blue triangles) and composite measures (blue triangles) from LVL. Measurements of three z > 7 galaxies are shown as crimson stars (Schaerer et al. 2022). Composite HALO7D spectra have lower Ne3O2 compared to the median individual detection at fixed stellar mass, suggesting the individual detections have higher excitation than the average for their mass and redshift. This relation holds in the z ∼ 2 and z ∼ 0 samples as well. Composite HALO7D spectra have similar Ne3O2 to z ∼ 0 stacks at low mass, indicating that the Ne3O2 behavior does not evolve substantially from z ∼ 1 to z ∼ 0. The median error of individual HALO7D galaxies is given in black in the lower left.
Paper: The Neon Gap: Probing Ionization with Dwarf Galaxies at z ∼ 1
Authors: John Pharo, Yicheng Guo, David C. Koo, John C. Forbes, Puragra Guhathakurta
Figure caption: The stellar mass vs. redshift distribution of the HALO7D galaxy sample. The vertical dashed line separates the dwarf and massive galaxy populations, defined at ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })=9.5﹩. The gray points and histograms indicate the overall sample of galaxies for which a good redshift fit was obtained from spectral features, as described in Pharo et al. (2022). The green points and histograms denote the subsample of galaxies with significant (S/N > 3) detections of the [NeIII]3869 and [OII]3727,3729 emission lines. This yields a sample of 167 galaxies (out of 1432 in the HALO7D catalog), including 112 dwarf galaxies (out of 646), with a redshift range of 0.3 < z < 1.4. The dark blue points and histograms indicate the emission-line galaxy sample used for composite galaxy stacking, described in Section 2.4.
Paper: On the Origin of Dust Structures in Protoplanetary Disks: Constraints from the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin, Leonardo Krapp
Figure caption: The effect of bump heating on the existence of stable dust traps, where the bump amplitude on the y-axis is A  T  in the right panel and A Σ in the left and middle panels. Left: the red shaded region denotes stable dust traps in the fiducial case of isothermal bumps. This red region is repeated more transparently in the other panels for comparison, with arrows roughly showing the directions that the boundaries change. Middle: the purple shaded region shows stable dust traps for bumps in both surface density and temperature, related adiabatically. The parameter space for stable dust traps is reduced. Right: the case of a temperature bump with no surface density variation. There is no blue shaded region as stable dust traps do not exist in this case due to the relative locations of the pressure-trapping boundary (solid) and the RWI boundary (dashed).
Paper: On the Origin of Dust Structures in Protoplanetary Disks: Constraints from the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin, Leonardo Krapp
Figure caption: The ability of ringlike surface density bumps—with amplitude, A Σ, and width relative to local gas scale height, W/H 0—to trap dust and/or trigger hydrodynamic instability is shown for our fiducial disk model. Left: the shaded region, above and to the left of the purple solid curve denotes bumps that reverse the sign of the background pressure gradient and thus can trap dust. Middle: the shaded region, below and to the right of the red dashed curve, denotes bumps that are stable to the RWI or with a low growth rate. Right: the yellow shaded region shows where the previous shaded regions overlap, giving a region where the bumps can both trap dust and not trigger significant RWI. Gas rings with these properties could produce observed dust rings. Bumps with amplitude and width outside the shaded region will fail to trap dust and/or be modified by the RWI.
Paper: On the Origin of Dust Structures in Protoplanetary Disks: Constraints from the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin, Leonardo Krapp
Figure caption: The effect of the background disk on the properties of stable dust-trapping rings (indicated by the shaded regions) is shown, generalizing the fiducial case shown in Figure 2. The effects of slopes in the background surface density (n, left) and temperature (q, middle) and of the aspect ratio (h 0, right) are shown. The most significant effect is that colder disks with smaller h 0 can host stable dust-trapping rings with smaller amplitudes and over a greater range of widths.
Paper: On the Origin of Dust Structures in Protoplanetary Disks: Constraints from the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin, Leonardo Krapp
Figure caption: The behavior of three different bumps in our fiducial disk model: “Strong” (which is also narrow), “Weak,” and “Wide,” with A Σ = (1, 0.4, 1), W/H 0 = (1.5, 1.5, 3), respectively. Top two panels: surface density, Σ, and midplane pressure, P, in the vicinity of the bump. Third panel: the pressure gradient, which only becomes positive in the “Strong” case, indicating a dust-trapping pressure maximum. Bottom panel: the disk’s squared radial oscillation frequency, relative to the squared Keplerian frequency. These radial frequencies are related to disk stability.
Paper: On the Origin of Dust Structures in Protoplanetary Disks: Constraints from the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin, Leonardo Krapp
Figure caption: Our approximate stability criterion (dotted) is compared to our numerical results (dashed) for the same models as Figure 4. The approximate condition for marginal stability is ﹩\min (({\kappa }^{2}+{N}_{R}^{2})/{{\rm{\Omega }}}_{{\rm{K}}}^{2})=0.6﹩. The Lovelace criterion (dotted–dashed), a necessary but not sufficient criterion for the RWI, is shown for comparison. Our approximate criterion can be used to estimate conditions for the RWI to occur.
Paper: Dissipative Capture of Planets into First-order Mean-motion Resonances
Authors: Konstantin Batygin, Antoine C. Petit
Figure caption: Numerical simulations of a k = 3 resonant encounter within the context of the circular restricted three-body problem. The top and bottom panels depict phase-space evolution and the time series of the orbital frequency ratio, respectively. Differently colored curves correspond to distinct migration timescales, as labeled in the inset between the two panels. The simulation setup is as follows: an exterior test particle, initialized on a circular, planar ﹩a^{\prime} =0.15\,﹩ au orbit around a M ⋆ = 1M ⊙ star, migrates convergently toward a m = 1 × 10−5 M ⊙ ≈ 3 M ⊕ planet residing at a = 0.1 au, eventually encountering the 3:2 mean-motion commensurability. Eccentricity damping is applied with a characteristic timescale that is a factor of ﹩{ \mathcal K }=1000﹩ shorter than the migration time, ﹩{\tau }_{m}^{{\prime} }﹩. Simultaneous migration and circularization of the outer orbit is indicated with shaded arrows on the diagram. As ﹩{\tau }_{m}^{{\prime} }﹩ is reduced from 80  kyr toward the analytically predicted critical value of 5 kyr (Equation (10)), the equilibrium value of the resonant angle, ϕ, tends from π to 3π/2. The equilibrium value of the eccentricity, on the other hand, stabilizes at ﹩e^{\prime} =1/\sqrt{4\,{ \mathcal K }}\approx 0.016﹩ in all cases. The behavior of this heavily damped system is fully consistent with expectations provided by analytic theory.
Paper: Dissipative Capture of Planets into First-order Mean-motion Resonances
Authors: Konstantin Batygin, Antoine C. Petit
Figure caption: A dimensionless mass vs. migration time map of k = 3 resonance capture for an equal-mass (﹩m=m^{\prime} ﹩) planetary system. The filled circles indicate parameter combinations where numerical simulations yield successful resonant capture, whereas empty circles indicate passage through the 3:2 resonance. The left and right panels correspond to the heavily (﹩{ \mathcal K }=1000﹩) and moderately (﹩{ \mathcal K }=100﹩) damped regimes, respectively. Both panels additionally show analytic stability and adiabaticity capture criteria as dashed and solid lines. While the stability criterion regulates capture in the heavily dissipated case, adiabaticity controls the outcome of resonant encounters in the moderately damped regime.
Paper: Dissipative Capture of Planets into First-order Mean-motion Resonances
Authors: Konstantin Batygin, Antoine C. Petit
Figure caption: Comparison between analytic and numeric determination of resonance capture. Using the nebular surface density as a proxy for the critical migration rate, the results of the Kajtazi et al. (2023) simulation suite (﹩{ \mathcal K }\approx 570﹩) are shown with blue points for a range of resonant indexes, k. Analytic stability and adiabaticity criteria are overplotted with gray and black points, respectively. Although not exact, the critical value of the surface density given by the stability criterion (Equation (16)) matches the numerical data to within 20%.
Paper: Dissipative Capture of Planets into First-order Mean-motion Resonances
Authors: Konstantin Batygin, Antoine C. Petit
Figure caption: Same as Figure 1 but with a reduced eccentricity-damping factor of ﹩{ \mathcal K }=100﹩. While resonant capture ensues for long migration timescales, the analytically predicted critical value of ﹩{\tau }_{m}^{{\prime} }=1.5\,﹩ kyr leads to passage through the 3:2 commensurability and capture into the 5:4 resonance instead. Failure of the stability criterion given by Equation (10) in this example indicates that the orbital circularization is sufficiently slow that a different mechanism—namely, adiabaticity—regulates resonance capture.
Paper: Sporadic Spin-orbit Variations in Compact Multiplanet Systems and Their Influence on Exoplanet Climate
Authors: Howard Chen, Gongjie Li, Adiv Paradise, Ravi K. Kopparapu
Figure caption: Time series of N-rigid-body simulation outcomes (a)–(b) that are used as inputs to the climate model results for TRAPPIST-1 e and f (c)-(f). The top panels show the substellar point longitude, and the bottom panels show global-mean surface temperatures and sea-ice thickness. The inclusion of sporadic planet interactions does not affect the mean climate of planet e, while increased pace of global glaciation is found for planet f with the inclusion of planet interactions. In the latter planet scenarios, as the location of maximum stellar heating moves away from the open ocean areas, the high surface albedo of the newly formed sea-ice makes deglaciation extremely difficult, and the planet rapidly transitions into a snowball state over ∼200 yr. 180° is the substellar longitude for the 1 : 1 resonant state.
Paper: Sporadic Spin-orbit Variations in Compact Multiplanet Systems and Their Influence on Exoplanet Climate
Authors: Howard Chen, Gongjie Li, Adiv Paradise, Ravi K. Kopparapu
Figure caption: Cartoon schematic illustrating the relationship between ψ, the long-axis misalignment and ϕ, the substellar longitude (a), and example time-series plot showing the variability of substellar longitude and planetary rotation period due to spin-axis dynamics calculated by an N-rigid-body integrator on a 100 yr time step (b). This study explores the effects of variations in ψ and ϕ on exoplanet climate using an intermediately complex Earth system model.
Paper: Sporadic Spin-orbit Variations in Compact Multiplanet Systems and Their Influence on Exoplanet Climate
Authors: Howard Chen, Gongjie Li, Adiv Paradise, Ravi K. Kopparapu
Figure caption: Hemispheric-mean mass streamfunctions at three snapshots in time for TRAPPIST-1 e with Earthlike atmospheres, averaged between longitudes 90° and 270°. We show that the patterns of the overturning circulation can be modified dramatically depending on the exact longitudinal location of stellar heating: (a) 185°, the original position, (b) 20°, near the antistellar point, and (c) 277°, at the terminator. The first scenario represents the 1:1 state, the second indicates downwelling at the ITCZ, and the third is an example of a “transitional” circulation pattern.
Paper: Sporadic Spin-orbit Variations in Compact Multiplanet Systems and Their Influence on Exoplanet Climate
Authors: Howard Chen, Gongjie Li, Adiv Paradise, Ravi K. Kopparapu
Figure caption: Time series of N-rigid-body simulation outcomes (a), (b) that are used as inputs to the climate model results for TRAPPIST-1 f (c), (d), exploring different levels of system excitation. The top panels show the substellar point longitude, and the bottom panels show global-mean surface temperatures and sea-ice thickness.
Paper: Cosmological-model-independent Determination of Hubble Constant from Fast Radio Bursts and Hubble Parameter Measurements
Authors: Yang Liu, Hongwei Yu, Puxun Wu
Figure caption: The 〈DMIGM〉 − z relation for the n = 1 piecewise linear function (blue line). The shadow region denotes the 1σ uncertainty. The gray points are eighteen 〈DMIGM〉 data samples. The dashed line is the theoretical value of 〈DMIGM〉 based on the ΛCDM model.
Paper: Cosmological-model-independent Determination of Hubble Constant from Fast Radio Bursts and Hubble Parameter Measurements
Authors: Yang Liu, Hongwei Yu, Puxun Wu
Figure caption: The constraints on H 0. The gray and orange lines represent the results from the Planck CMB observations and the nearby SNe Ia data, respectively. The blue line shows our result.
Paper: Nuclear Activity in the Low-metallicity Dwarf Galaxy SDSS J0944-0038 : A Glimpse into the Primordial Universe
Authors: Michael Reefe, Shobita Satyapal, Remington O. Sexton, Nathan J. Secrest, William Matzko, Emma Schwartzman, Kristina Nyland, Gabriela Canalizo, Barry Rothberg, Ryan W. Pfeifle, Jenna M. Cann, Archana Aravindan, Camilo Vazquez, Tracy Clarke
Figure caption: Left: A BPT ratio plot of the CLASS sample with the values obtained from the 1″ aperture centered on Nuclei 1 and 2 being displayed by the red diamonds. The color of each point corresponds to the stellar mass of the galaxy obtained from the Max Planck Institute for Astrophysics/Johns Hopkins University (MPA/JHU) catalog. The star-forming, “composite,” and AGN regions are marked with text and separated by the curves defined in Kauffmann et al. (2003) and Kewley et al. (2001). The gray shading displays the BPT values for the entire MPA/JHU catalog Right: A WISE color–color plot of the class sample with the value for J0944−0038 being displayed by the red diamond. The coloring of the points and contours is defined the same way as in the BPT plot. The AGN demarcation box from Jarrett et al. (2011) is shown by the black line, the demarcation box from Satyapal et al. (2018) is shown by the red line, and the demarcation box from Blecha et al. (2018) is shown in green.
Paper: Nuclear Activity in the Low-metallicity Dwarf Galaxy SDSS J0944-0038 : A Glimpse into the Primordial Universe
Authors: Michael Reefe, Shobita Satyapal, Remington O. Sexton, Nathan J. Secrest, William Matzko, Emma Schwartzman, Kristina Nyland, Gabriela Canalizo, Barry Rothberg, Ryan W. Pfeifle, Jenna M. Cann, Archana Aravindan, Camilo Vazquez, Tracy Clarke
Figure caption: Top Left: [Fe X] λ6374 emission line flux map from VLT/MUSE. Top Right: [O III] λ5007 flux map. Bottom Left: Hα flux map. Bottom Right: continuum at λ5100 flux map. The white circles in each image correspond to the positions of the peak continuum for the two brightest central clumps, which we refer to as Nucleus 1 (northern source), which is coincident with the SDSS fiber location, and Nucleus 2 (southern source). Scale bars in kpc are given at the top left of each plot. The color scales for [O III], Hα, and the continuum are logarithmic, while the color scale for [Fe X] is linear. Additionally, the fluxes have been convolved with a 5 × 5 median filter, and [Fe X], [O III], and Hα have been masked so that only spaxels with an S/N > 3 are shown.
Paper: Nuclear Activity in the Low-metallicity Dwarf Galaxy SDSS J0944-0038 : A Glimpse into the Primordial Universe
Authors: Michael Reefe, Shobita Satyapal, Remington O. Sexton, Nathan J. Secrest, William Matzko, Emma Schwartzman, Kristina Nyland, Gabriela Canalizo, Barry Rothberg, Ryan W. Pfeifle, Jenna M. Cann, Archana Aravindan, Camilo Vazquez, Tracy Clarke
Figure caption: Top panel: Hubble Space Telescope (HST) image of J0944−0038, constructed from UV (F336W, blue channel), Hα (F657N, green channel), and visual/near-IR (F814W, red channel) archival data. Bottom panel: stellar mass distribution of the subset of dwarf galaxies in the CLASS sample compared to the samples of AGNs identified by Reines et al. (2013) and Molina et al. (2021). The stellar mass of J0944−0038, and other coronal line emitters, is significantly lower than the mass regime probed by traditional optical narrow line ratios.