adsabs/AstroCLIMB huggingface dataset:
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: Comparison of the SFR enhancement as a function of the projected separation of interactions and mergers (0.5 < z < 3.0) to the pair sample in the local universe (0.02 < z < 0.20) from Patton et al. (2013). SFR enhancement is defined as the ratio of the average SFR of the pair sample to that of the control sample (Equation (1)). The dotted line corresponds to a value of one, which represents no interaction-induced SFR enhancement. The blue filled circles show the SFR enhancement for our complete galaxy pair sample (﹩\mathrm{log}({M}_{\mathrm{pair}}/{M}_{\odot })\gt 10.3﹩ and 0.5 < z < 3.0). The filled green diamond, filled purple square, and filled orange triangle correspond to the SFR enhancements for our visually identified merger sample, blended interaction sample, and non-blended interaction sample, respectively. The gray region corresponds to the merger (or post-merger) stage. The filled black stars correspond to the Patton et al. (2013) SFR enhancement results for a pair sample in the local (0.02 < z < 0.20) universe selected from SDSS observations. While we see significant enhancement for galaxy mergers in our high-redshift sample, the overall level of enhancement is less than that seen in the local pair sample, indicative of a change in the role of interactions and mergers in inducing star formation over cosmic time.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: SFR enhancement for our visually identified mergers (filled green diamonds), blended interactions (filled purple squares), and non-blended interactions (filled orange triangles) at z < 1.6 (left) and z < 1.6 (right) compared to their star-forming control samples. The dotted line corresponds to a value of one, which represents no interaction-induced SFR enhancement. While we see evidence of increasing enhancement with decreasing projected separation in both redshift bins, we see a decreased level of enhancement for the z > 1.6 bin.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: SFR enhancement as a function of projected separation for the pair sample with ΔV < 1000 km s−1. The left- and right-hand-side plots correspond to the results for star-forming blended pairs (and non-blended paired galaxies) and non-star-forming blended pairs (and non-blended paired galaxies). The dotted line corresponds to a value of one, which represents no interaction-induced SFR enhancement.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: SFR enhancement for our visually identified mergers (filled green diamonds), blended interactions (filled purple squares), and non-blended interactions (filled orange triangles) as a function of their median projected separations. The merged/coalesced systems are plotted at a separation of zero, since they are no longer in a pair but are in a single coalesced galaxy. The dotted line corresponds to a value of one, which represents no interaction-induced SFR enhancement. Note that for this sample, we see a clear trend of increasing SFR enhancement with decreasing projected separation, with the largest level of enhancement seen in the coalesced systems.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Reduced and telluric-corrected spectra of seven program stars in the HPF spectral order that contains He I 10830.3 Å. The left-hand panel shows the entire HPF order that contains the λ10830 line. The right-hand panel zooms in to a 10 Å interval centered on the λ10830 feature. The wavelength of the strongest two components of the He I triplet is shown with a dotted line.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Example of telluric-absorption-line cancellation near the λ10830 transition. For this figure a program star with very high SNR but weak He I absorption depth was chosen. The top panel contains the stellar+telluric spectrum, and the middle panel has the spectrum of a warm (essentially featureless) star. The division of these two spectra produces the purely stellar program star spectrum in the bottom panel.
Paper: Investigating the Effect of Galaxy Interactions on Star Formation at 0.5 < z < 3.0
Authors: Ekta A. Shah, Jeyhan S. Kartaltepe, Christina T. Magagnoli, Isabella G. Cox, Caleb T. Wetherell, Brittany N. Vanderhoof, Kevin C. Cooke, Antonello Calabro, Nima Chartab, Christopher J. Conselice, Darren J. Croton, Alexander de la Vega, Nimish P. Hathi, Olivier Ilbert, Hanae Inami, Dale D. Kocevski, Anton M. Koekemoer, Brian C. Lemaux, Lori Lubin, Kameswara Bharadwaj Mantha, Stefano Marchesi, Marie Martig, Jorge Moreno, Belen Alcalde Pampliega, David R. Patton, Mara Salvato, Ezequiel Treister
Figure caption: SFR enhancement for only star-forming visually identified mergers (filled green diamonds), blended interactions (filled purple squares), and non-blended interactions (filled orange triangles) at z < 1.6 (left) and z < 1.6 (right) compared to their star-forming control samples.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Top panel: He I 10830 Å spectra of three red horizontal-branch stars (Sneden et al. 2021). Bottom panel: +Li I 6707 Å resonance feature in these stars (Afśar et al. 2018; Z. Bozkurt et al. 2022, in preparation).
Paper: Common Envelope Mass Ejection in Evolved Stars: Modeling the Dust Emission from Post-RGB Stars in the LMC
Authors: Geetanjali Sarkar, Raghvendra Sahai
Figure caption: Illustration showing post-RGB dust geometry with an inner disk and an outer shell. R in and R out are the inner and outer radius of the disk (shell). A disk with an opening angle θ  d  intercepts Sin(θ  d /2) (referred to as disk fraction in this paper) of starlight.
Paper: Oblique Electromagnetic Instabilities Driven by Pickup Ion Ring-beam Distributions in the Outer Heliosheath. I. Linear Instability Analysis
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The wavenumber (a), propagation angle (b), growth rate (c), and real frequency (d) of the most unstable mirror wave as a function of α.
Paper: The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism
Authors: Tanausú del Pino Alemán, Ernest Alsina Ballester, Javier Trujillo Bueno
Figure caption: Fractional circular polarization V/I profiles for a LOS at the solar disk center, computed in the FAL–P model with a vertical magnetic field of 500 G following the procedure described in Section 2. The different columns show the lines of the Mn I UV multiplet ordered by their wavelength from left to right. The black solid curves show the calculation accounting for the incomplete Paschen-Back effect for fine structure (top panels) and for both fine structure and HFS (bottom panels). The red curves in the bottom panels show the result of the calculation assuming the linear Zeeman approximation (LZA; i.e., assuming that the energies of the various magnetic sublevels depend linearly on the magnetic field strength). The black dotted lines show the WFA profile for the same longitudinal magnetic field and the effective Landé factor calculated by assuming LS coupling and neglecting HFS (﹩\bar{g}﹩, indicated in the top panels for each line).
Paper: The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism
Authors: Tanausú del Pino Alemán, Ernest Alsina Ballester, Javier Trujillo Bueno
Figure caption: Intensity contribution function (top row) and circular polarization response function (middle row) for the three lines of the Mn I UV multiplet (ordered from left to right for increasing wavelength) in the FAL–P semiempirical model with a constant vertical 100 G magnetic field, neglecting HFS. The panel in the bottom row shows the circular polarization response function for the wavelength range including the Mn I UV multiplet and the Mg II h and k lines and subordinate lines at 279.88 nm. We show the logarithm of the contribution and response functions normalized to the maximum for each wavelength range. For the circular polarization, the red (blue) color indicates that the response to the circular polarization is negative (positive).
Paper: The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism
Authors: Tanausú del Pino Alemán, Ernest Alsina Ballester, Javier Trujillo Bueno
Figure caption: Intensity (top panels) and fractional circular polarization V/I (bottom panels) profiles for a LOS at the solar disk center, computed in the FAL–P model with a vertical magnetic field of 500 G following the procedure described in Section 2. The different columns show the lines of the Mn I UV multiplet ordered by their wavelength from left to right. The black (red) solid curve shows the calculation neglecting (accounting for) HFS. The red dotted curve shows the circular polarization profile in the linear Zeeman approximation (i.e., assuming that the energies of the various magnetic sublevels depend linearly on the magnetic field strength), which significantly underestimates the circular polarization amplitude in two of the Mn I resonance lines.
Paper: The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism
Authors: Tanausú del Pino Alemán, Ernest Alsina Ballester, Javier Trujillo Bueno
Figure caption: Grotrian diagram of the atomic models for the Mn I (bottom panel) and the Mn II (top panel) atoms used to calculate the population balance. The solid lines show the considered radiative transitions. Every atomic level is connected to every other level via inelastic collisions with electrons and every Mn I level is connected with the ground term of Mn II via photoionization and recombination (these transitions are not shown in the diagrams for a better visualization). The green line shows the transition corresponding to the Mn I UV multiplet. The horizontal dashed lines show the ionization energy for each corresponding atomic species, with the atomic configuration of the ground term of the next ionization stage.
Paper: The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism
Authors: Tanausú del Pino Alemán, Ernest Alsina Ballester, Javier Trujillo Bueno
Figure caption: Grotrian diagram for the Mn I UV multiplet neglecting (left panel) and accounting for (right panel) HFS. The four J-levels radiatively coupled by three transitions become 22 F-levels connected by 42 transitions.
Paper: The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism
Authors: Tanausú del Pino Alemán, Ernest Alsina Ballester, Javier Trujillo Bueno
Figure caption: The energy of the HFS levels corresponding to each of the atomic levels, indicated above each panel, of the Mn I resonance lines, for different magnetic fields (black solid curves). The gray dashed lines show the same, but with the linear Zeeman approximation.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Left: hard X-ray (14–195 keV) flux vs. redshift for our clean sample of 118 blazars (see Section 2.2). The data points represent all identified blazars at ∣b∣ > 10° detected above 5σ with F 14–195 keV > 5.4 × 10−12 erg cm−2 s−1 (dashed line) from the BAT 105 catalog: (red filled circles) BZQs, (blue filled circles) BZBs, including three BZGs and one BZU. Right: K-corrected hard X-ray (14–195 keV) luminosity as function of redshift for our clean sample.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: The Swift-BAT sky coverage for ∣b∣ > 10° and 5σ detection threshold, derived from Oh et al. (2018; see Section 2.2), rises from 300 deg2 at the minimum sky coverage flux (blue dashed line) to 34,089 deg2 above F 14–195 keV > 10−11 erg cm−2 s−1.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Distribution of θ (P(θ), normalized to 1), Γ (P(Γ), normalized to 1), and δ (P(δ)) for the beaming fit to the BAT FSRQ population for p = 5 (top) and p = 7 (bottom). The average for the θ and Γ distribution are shown by the yellow solid line. For the latter, the associated errors are represented by the yellow dashed lines. We note how a lower value of p predicts a lower average Γ, as well as a narrower range of predicted Γ values, with respect to a higher value of p. On the other hand, the viewing angle distribution is broader for a lower value of p, though they remain distributed between 1° and 10° and have an average θ ∼ 2°–3°, quite independently of p.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Comparison between average BAT-blazar and LAT-blazar SEDs. BAT blazar SEDs are shown by the magenta solid lines and are the ones derived from this work in the X-ray luminosity bins (﹩\mathrm{log}{L}_{\mathrm{BAT}}=[46.6,47.3],[47.3,48.3],[48.3,48.8]\,\mathrm{erg}\,{{\rm{s}}}^{-1}﹩; see also Figure 7). The LAT SEDs are the ones reported in A12 for the bolometric luminosity (derived in their work from the γ-ray luminosity) bins ﹩\mathrm{log}{L}_{\mathrm{bol}}=[47.6,47.9],[47.9,48.5],[48.5,49.3]\,\mathrm{erg}\,{{\rm{s}}}^{-1}﹩ and are shown by the blue dashed lines. This Figure highlights that BAT blazars have their high-energy peak located at lower energies than the LAT sources. Moreover, neither class of objects shows strong evolution of the SED shape and/or peak depending on the chosen luminosity bin.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Left: predicted logN-logS from our best-fit XLF and SED models in different MeV bands. It can be seen that an instrument with a uniform sensitivity of S = 10−12 erg cm−2 s−1 would be able to detect between 103 and 105 sources (depending on the energy range). Right: histogram of fraction of sources as a function of redshift expected to be detected by proposed MeV mission (see Section 8.5).
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Median Doppler factors (﹩\widetilde{\delta }﹩, left) and median viewing angles (﹩\widetilde{\theta }﹩, right) as a function of 14–195 keV luminosity derived from the beaming fit to the BAT FSRQ population for p = 5 (red stars) and p = 7 (blue dots). As the luminosity of the sources decreases, the δ factors become smaller and viewing angles get larger (corresponding to lower Γ factors).
Paper: On the Characterization of GJ 504: A Magnetically Active Planet-host Star Observed by the Transiting Exoplanet Survey Satellite (TESS)
Authors: Maria Pia Di Mauro, Raffaele Reda, Savita Mathur, Rafael A. García, Derek L. Buzasi, Enrico Corsaro, Othman Benomar, Lucía González Cuesta, Keivan G. Stassun, Serena Benatti, Valentina D'Orazi, Luca Giovannelli, Dino Mesa, Nicolas Nardetto
Figure caption: Evolutionary tracks plotted in two plans of the H-R diagram calculated for different values of the mass and the metallicity, while all the other parameters are fixed. The initial hydrogen abundance is X  i , and the mixing-length coefficient is α = 1.8. The rectangle defines the 1σ error box for the observed gravity and effective temperature. Colored dots indicate the position of the four structure models (see Table 3), which best reproduce the observations of GJ 504.
Paper: On the Characterization of GJ 504: A Magnetically Active Planet-host Star Observed by the Transiting Exoplanet Survey Satellite (TESS)
Authors: Maria Pia Di Mauro, Raffaele Reda, Savita Mathur, Rafael A. García, Derek L. Buzasi, Enrico Corsaro, Othman Benomar, Lucía González Cuesta, Keivan G. Stassun, Serena Benatti, Valentina D'Orazi, Luca Giovannelli, Dino Mesa, Nicolas Nardetto
Figure caption: Spectral energy distribution. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black).
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Differential BAT-blazars logN-logS , i.e., number of sources per flux bin corrected for the survey sky coverage, dN/dS, as a function of flux. The observed differential logN-logS is represented by the red data points, while the blue solid and green dashed lines show the prediction from the best-fit mPLE and mPDE models, respectively. The error bars are calculated using Poisson statistics.
Paper: A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Patrick M. Koch, Ya-Wen Tang, Paul T. P. Ho, Pei-Ying Hsieh, Jia-Wei Wang, Hsi-Wei Yen, Ana Duarte-Cabral, Nicolas Peretto, Yu-Nung Su
Figure caption: Dust continuum emission in color scale with a resolution of 0.″1 (∼2.6 mpc or ∼540 au) around 230 GHz (∼1.3 mm) in Band 6 with ALMA for W51 e2, except the upper left panel, which shows the earlier still more roundish detection with a 0.″26 resolution (Koch et al. 2018). White segments display the magnetic field in the right panels at half of the synthesized beam resolution (white ellipses in the lower left corners). Outflows are overplotted in the bottom middle and right panel. The cyan and faint-red contours denote the blue- and redshifted 12CO 2−1 outflow component, and the blue and red contours mark the blue- and redshifted SiO 5−4 outflow emission. Dust lanes and streamers are labeled in the bottom left panel, where continuum contours are identical to the ones described in the right panels in Figure 8. The bottom right panel marks the sectors of nearly straight field lines (yellow rectangles) and the possible small disk (black ellipse) as discussed in Section 3.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: Maps for cloud fraction of low clouds at low resolution with convective parameterization (left column) and at high resolution with explicit treatment of cloud microphysics (NSW6; right column). Right panels beside maps show zonally averaged cloud fraction.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: Vertical cross sections of zonal mean zonal wind (color; m/s) and the mass stream function (contours; kg/s) for (a) ϕ = 0°, (b) ϕ  = 23.5°, (c) ϕ = 45°, and (d) ϕ = 60°, averaged in boreal summer (June–July–August). All cases were run with a low resolution and parameterization for clouds. The contour intervals were set to 5 × 1010 kg/s.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: Zonally averaged cloud radiative forcing at low resolution with convective parameterization (left column) and at high resolution with explicit treatment of cloud microphysics (NSW6; right column). The net cloud radiative forcing, the cloud shortwave radiative forcing, and the cloud longwave radiative forcing are represented in the solid, dotted, and dashed lines, respectively.