adsabs/AstroCLIMB huggingface dataset:
Paper: Two Intermittent Eruptions of a Minifilament Triggered by a Two-step Magnetic Reconnection Within a Fan-spine Configuration
Authors: Liping Yang, Zhike Xue, Jincheng Wang, Liheng Yang, Qiaoling Li, Yian Zhou, Yang Peng, Xinsheng Zhang
Figure caption: Panels (a1) and (b1) are vertical components of the vector magnetic fields before the first and the second minifilament eruptions, respectively, in which the white (black) area is the positive (negative) polarity. The cyan rectangles R8 and R9 are the horizontal cross sections (z = 0) used to obtain the squashing factor (Q) maps of panels (a2) and (b2), respectively. The Q maps are correspondingly superposed over panels (a1) and (b1) in the form of yellow contours. The red line AB (CD) represents the vertical cross section that is used to obtain the Q maps shown in panels (c) and (d). Panels (a3) and (b3) are the AIA 1600 Å images showing the two circular ribbon flares associated with the minifilament eruptions, in which the dotted green circles C1 and C2 represent the main negative polarity region of the fan-spine configuration at 23:24 UT (on April 7) and at 01:36 UT (on April 8), respectively. The green (white, cyan, and yellow) arrows point to the QSL region (fan-spine structure). In panel (e), the green and yellow lines are the results of the NLFFF extrapolation and represent the inner spine and the outer spine, respectively. The cyan lines are the results of local PFSS extrapolation and represent the minifilament. The blue, red, and black arrows point to the fan-spine structure, null point, and closed outer spine, respectively. The white (cyan) arrow points to the footpoints of the dome field lines (minifilament, labeled “MF”). Besides, the positive (negative) polarity of the vertical component of the vector magnetic fields is indicated by the crimson (dark blue) area.
Paper: Two Intermittent Eruptions of a Minifilament Triggered by a Two-step Magnetic Reconnection Within a Fan-spine Configuration
Authors: Liping Yang, Zhike Xue, Jincheng Wang, Liheng Yang, Qiaoling Li, Yian Zhou, Yang Peng, Xinsheng Zhang
Figure caption: Panels (a) and (b) show the profile of GOES SXR flux in 1.0–8.0 Å (red curve), 304 Å (magenta curve), 171 Å (orange curve), and 335 Å (cyan curve) from 22:00 UT on April 7 to 04:00 UT on April 8. Panels (c1)–(c2) are the total EM maps showing the thermal evolution of plasmas at the reconnection site (at 23:28:56 UT on April 7 and 01:39:32 UT on April 8). The DEM was obtained by integrating over the temperature range of 5.7–7.3 (log T). The black arrows point to the brightening site. The areas enclosed by black rectangles are used to calculate the average EM and average temperature at the brightening sites, as well as the DEM results shown in panels (d1) and (d2). The red and black curves in panels (d1) and (d2) are the curves of the best-fit DEM and 100 Monte Carlo simulations, respectively.
Paper: Two Intermittent Eruptions of a Minifilament Triggered by a Two-step Magnetic Reconnection Within a Fan-spine Configuration
Authors: Liping Yang, Zhike Xue, Jincheng Wang, Liheng Yang, Qiaoling Li, Yian Zhou, Yang Peng, Xinsheng Zhang
Figure caption: Panels (a2) and (b2) are the time–distance diagrams obtained along the cyan slit “EF” in panel (a1) and green slit “GH” in panel (b1), respectively. Panel (a2) shows the plasma flows during the null point reconnection associated with the second eruption of the minifilament, and panel (b2) shows the trajectory of the second eruption of the minifilament. Besides, the white vertical lines in panels (a2) and (b2) mark the onset time of the second eruption of the minifilament.
Paper: Equilibrium States of Galactic Atmospheres. II. Interpretation and Implications
Authors: G. Mark Voit, Christopher Carr, Drummond B. Fielding, Viraj Pandya, Greg L. Bryan, Megan Donahue, Benjamin D. Oppenheimer, Rachel S. Somerville
Figure caption: Dependence of a halo’s asymptotic stellar baryon fraction f *,asy on the ratio ﹩{\varepsilon }_{\mathrm{fb}}/{v}_{{\rm{c}}}^{2}﹩ relating the specific energy of outflowing gas (﹩{\varepsilon }_{\mathrm{fb}}={\eta }_{E}{\varepsilon }_{\mathrm{SN}}/{\eta }_{M})﹩ to the halo’s circular velocity. Left panel: equilibrium states of Paper I’s generic atmosphere model for coupled outflows, in which supernova feedback is primarily preventative. Right panel: equilibrium states of Paper I’s ballistic circulation scenario for uncoupled outflows, in which supernova feedback is primarily ejective. Numerical labels give values of ﹩{\eta }_{E}{\varepsilon }_{\mathrm{SN}}/{v}_{{\rm{c}}}^{2}﹩ for each set of lines. Feedback models in the red region to the right of the solid vertical line marking ε fb = ε acc expand a galaxy’s atmosphere. Models in the blue region to the left of that vertical line allow a galaxy’s atmosphere to contract. Models in the gray region to the left of the dotted line marking ﹩{\varepsilon }_{\mathrm{fb}}={v}_{{\rm{c}}}^{2}﹩ fail to propel gas very far out of a galaxy, resulting in a low-altitude fountain that quickly recycles ejected gas and does little to limit star formation.
Paper: Equilibrium States of Galactic Atmospheres. I. The Flip Side of Mass Loading
Authors: G. Mark Voit, Viraj Pandya, Drummond B. Fielding, Greg L. Bryan, Christopher Carr, Megan Donahue, Benjamin D. Oppenheimer, Rachel S. Somerville
Figure caption: Trajectories of generic atmosphere models in the M CGM–E CGM plane. Both panels show models with ﹩{\varepsilon }_{\mathrm{acc}}/{v}_{{\rm{c}}}^{2}=4﹩ and ﹩{\eta }_{E}{\varepsilon }_{\mathrm{SN}}/{v}_{{\rm{c}}}^{2}=10﹩. Trajectories in the left panel (solid orange lines) have η  M  = 0, and trajectories in the right panel have η  M  = 5. They all start at M CGM = M CGM,init with various values of E CGM and converge toward the dashed green lines along which E CGM/M CGM = ε eq. Gray lines indicate ε CGM = ε acc. Models with less mass loading end up in the red (expanded) region with ε CGM > ε acc. Models with more mass loading end up in the blue (contracted) region with ε CGM < ε acc.
Paper: Equilibrium States of Galactic Atmospheres. II. Interpretation and Implications
Authors: G. Mark Voit, Christopher Carr, Drummond B. Fielding, Viraj Pandya, Greg L. Bryan, Megan Donahue, Benjamin D. Oppenheimer, Rachel S. Somerville
Figure caption: Comparisons of predicted f *–M halo relations with observations. A gray band shows the low-redshift relation from P. Behroozi et al. (2019). Purple lines show predicted relations from C. Carr et al. (2023) for η  E  = 0.3 and various values of η  M  given in the legend. A dashed red line shows the asymptotic stellar baryon fraction predicted by the minimalist regulator model for η  E  = 0.3, ξ = 0.7, and negligible radiative losses. A solid blue line shows the minimalist regulator model’s prediction for ﹩{\eta }_{E}=0.3{\left({M}_{\mathrm{halo}}/{10}^{11}\,{M}_{\odot }\right)}^{-1/3}﹩ and ξ = 0.7.
Paper: Equilibrium States of Galactic Atmospheres. I. The Flip Side of Mass Loading
Authors: G. Mark Voit, Viraj Pandya, Drummond B. Fielding, Greg L. Bryan, Christopher Carr, Megan Donahue, Benjamin D. Oppenheimer, Rachel S. Somerville
Figure caption: Dependence of equilibrium specific energy ε eq (solid lines) and asymptotic stellar baryon fraction f *,asy (dashed lines) on the mass-loading parameter η  M  in the generic atmosphere model of Section 4.4.1. Colors represent supernova feedback strength ﹩{\eta }_{E}{\varepsilon }_{\mathrm{SN}}/{v}_{{\rm{c}}}^{2}﹩ as labeled. A horizontal solid line marks ε eq = ε acc. A horizontal dotted line marks ﹩{\varepsilon }_{\mathrm{eq}}={v}_{{\rm{c}}}^{2}﹩. All examples have ﹩{\varepsilon }_{\mathrm{acc}}=4{v}_{{\rm{c}}}^{2}﹩. Atmospheres with ε eq in the red shaded area have expanded. Atmospheres with ε eq in the blue shaded area have contracted. Each line is truncated as ε eq drops into the gray region because the generic atmosphere model breaks at small values of ε CGM.
Paper: Equilibrium States of Galactic Atmospheres. I. The Flip Side of Mass Loading
Authors: G. Mark Voit, Viraj Pandya, Drummond B. Fielding, Greg L. Bryan, Christopher Carr, Megan Donahue, Benjamin D. Oppenheimer, Rachel S. Somerville
Figure caption: Trajectories of generic atmosphere models in the f CGM–ε CGM phase plane. All examples have ﹩{\varepsilon }_{\mathrm{acc}}/{v}_{{\rm{c}}}^{2}=4﹩ and ﹩{\eta }_{E}{\varepsilon }_{\mathrm{SN}}/{v}_{{\rm{c}}}^{2}=10﹩. The panels show trajectories for η  M  = 0, 1, 2, 3, 5, and 10, as labeled. Those trajectories (orange lines) converge toward the green dots marking each atmosphere’s equilibrium configuration. Excess heating leads to equilibria in the red (expanded) region (ε CGM > ε acc). Excess cooling leads to equilibria in the blue (contracted) region (ε CGM < ε acc).
Paper: Accurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars
Authors: David M. Nataf, Kevin C. Schlaufman, Henrique Reggiani, Isabel Hahn
Figure caption: Left: MIST isochrones of solar metallicity and of ages τ = 3 and 8 Gyr, with indicative EEPs shown as red points. Middle: the uncertainty in the derived ages as a function of EEP, color coded by the uncertainty in the apparent distance modulus. Right: Normalized distribution of the age precisions for stars with 450 ≤ EEP ≤ 475 (subgiants, orange) and other stars (blue). We see that the derived ages are more precise at all phases of stellar evolution when the assumed apparent distance moduli are more precise, and the best precision is achieved on the subgiant branch.
Paper: Equilibrium States of Galactic Atmospheres. I. The Flip Side of Mass Loading
Authors: G. Mark Voit, Viraj Pandya, Drummond B. Fielding, Greg L. Bryan, Christopher Carr, Megan Donahue, Benjamin D. Oppenheimer, Rachel S. Somerville
Figure caption: Schematic summary of the paper’s foundational concepts and key results.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: EAZY fit to JADES-GS-z11-0 (left) and JADES-GS-z13-0 (right). In each panel, the NIRSpec PRISM spectrum and uncertainty are plotted in blue, and synthetic photometry estimated from the spectrum through the JADES NIRCam bands are given with blue circles. In black we plot the EAZY SED corresponding to the minimum χ 2 of the fit (the redshift of each fit is given in the legend), and with black squares are the EAZY photometry derived from that SED. In the inset in each panel, we show the EAZY P(z) in orange, and plot with a black vertical line the photometric redshift z  a  and a blue dashed vertical line the fiducial spectroscopic redshift. For each source, the photometric redshift is biased high compared to our fiducial photometric redshifts due to the shallower Lyα break in the observed spectrum, which is not simulated based on the IGM model in the EAZY fit.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: The combined emission-line detection p-value X  T  as a function of redshift for JADES-GS-z11-0. The prominent peak at z = 11.122 is evident.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Photometry and EAZY fit (top panel), and NIRCam 2″ × 2″ thumbnails for JADES-GS+53.16474-27.77471. This distinct source, which can be most easily seen south of JADES-GS-z11-0 in the F277W thumbnail, has a best-fit photometric redshift z  a  = 12.41 when fitting to the 0.″2 circular aperture photometry (black points), as represented by the blue fit in the top panel. In the inset, we show the P(z) surface from EAZY, where we indicate our spectroscopic redshift for JADES-GS-z11-0 with a green vertical line. The NIRCam data for F182M, F210M, F430M, F460M, and F480M are taken from the JEMS data and are shallower than the other filters, and nondetections are not surprising in these filters given the flux levels of this source.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Corner plot (top) and SED fit (bottom) for JADES-GS-z13-0 where we allow the redshift and DLA H I column density to vary while fitting the observed spectrum. We begin with the fiducial BEAGLE fit, shown with the green line in the bottom panel, and then explore the relationship between redshift, IGM absorption, and DLA absorption. The χ 2 does not change when we include a DLA as a free parameter for this source, demonstrating that it is not statistically preferred by the data.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: The potential line flux signal-to-noise ratio vs. wavelength for JADES-GS-z11-0. The overlay shows the locations of the emission lines searched for at the peak redshift of z = 11.122.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: The line flux signal-to-noise ratio vs. wavelength for JADES-GS-z13-0. The overlay shows the locations of the emission lines searched for at the peak redshift of z = 12.922.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Radial profile fits to the F200W images for JADES-GS-z11-0 (top row) and JADES-GS-z13-0 (bottom row). In the left column, we show the F200W image centered on each source, with circular apertures used in calculating the radial profile. In the right column, we plot the normalized radial profile for each source with black points and error bars as compared to the F200W mosaic PSF, which we plot with a red line. For JADES-GS-z11-0, we mask a nearby source and show this mask with a gray box.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: Posterior on ﹩\mathrm{log}({N}_{\mathrm{HI}}/{\mathrm{cm}}^{-2})﹩ (top) and SED fit (bottom) for JADES-GS-z11-0, where we fix the source at z spec = 11.122 while allowing the DLA H I column density to vary. For this fit, we fix the IGM H I fraction ﹩{\hat{x}}_{\mathrm{HI}}=1﹩. Here, because of the spectroscopic redshift of this source, we find a DLA is required with ﹩\mathrm{log}({N}_{\mathrm{HI}}/{\mathrm{cm}}^{-2})={22.43}_{-0.12}^{+0.10}﹩ to account for the shape of the Lyα break.
Paper: Searching for Emission Lines at z > 11: The Role of Damped Lyα and Hints About the Escape of Ionizing Photons
Authors: Kevin N. Hainline, Francesco D'Eugenio, Peter Jakobsen, Jacopo Chevallard, Stefano Carniani, Joris Witstok, Zhiyuan Ji, Emma Curtis-Lake, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Mirko Curti, Stephane Charlot, Jakob M. Helton, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Alex J. Cameron, Eiichi Egami, Daniel J. Eisenstein, Ryan Hausen, Nimisha Kumari, Roberto Maiolino, Pablo G. Pérez-González, Marcia Rieke, Aayush Saxena, Jan Scholtz, Renske Smit, Fengwu Sun, Christina C. Williams, Christopher N. A. Willmer, Chris Willott
Figure caption: The combined emission-line detection p-value X  T  as a function of redshift for JADES-GS-z13-0. The peak seen at z = 12.922 is likely a chance occurrence.
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Left: temperature map of Kepler-7b’s dayside hemisphere at 1 mbar. Middle: averaged temperature profiles of Kepler-7b for the western limb (blue) and hot dayside (red) regions, with the condensation curves (gray dashed) of the clouds (MgSiO3, Mg2SiO4, Al2O3, and TiO2) modeled in this study. Right: globally averaged K  zz  profile of the atmosphere. Low/negative K  zz  values at pressures >0.1 bar are set to the K  zz  minimum (105 cm2 s−1) before calculating Virga clouds. The SPARC/MITgcm data and condensation curves are from D. J. Adams et al. (2022).
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Left: full-resolution optical depth map of the dayside hemisphere at 1 mbar and a wavelength of 604 nm. Right: eight corresponding 20 × 20 grid phase maps used to compute reflected-light spectra. The optical depth maps here are generated with Virga considering Mg2SiO4, Al2O3, and TiO2 as cloud condensates with f sed = 0.03. The substellar point is located at the center of each map (0° latitude, 0° longitude).
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Temperature maps of the dayside hemisphere at 1 mbar illustrating how PICASO regrids and rotates the GCM for eight discrete planetary phases with 20 × 20 spatial grid resolution. The substellar point is located at the center of each map (0° latitude, 0° longitude), meaning these maps show the dayside hemisphere of Kepler-7b. Only colored regions contribute to reflected-light intensity. A phase angle of 0° corresponds to the secondary eclipse where the entire dayside hemisphere is visible. A phase angle of 180° (not shown) corresponds to the primary eclipse (transit). The planetary phase diagrams, which are included for reference, show the hemisphere seen by the observer as the planet orbits and both the dayside (white) and nightside (black) regions.
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Cloud optical depth per layer for all cloudy scenarios as a function of longitude and pressure for the dayside hemisphere, at a latitude of 1.°4N and a wavelength of 604 nm. The columns represent the three cloud scenarios: MgSiO3 only, Mg2SiO4 only, and Mg2SiO4, Al2O3, and TiO2. The rows represent the four sedimentation efficiencies considered in this study (0.03, 0.1, 0.3, and 1.0). White regions indicate regions with no clouds.
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: The planet-to-star flux ratio in parts per million (ppm) at phase 0° (secondary eclipse) for Kepler-7b for the cloudless case (black solid), and the MgSiO3-only (green dashed–dotted lines), Mg2SiO4-only (orange dashed lines), and Mg2SiO4, TiO2, and Al2O3 (blue solid lines) cloudy cases as calculated by Virga. The decreasing opacity of the curves corresponds to increasing values of f sed (0.03, 0.1, 0.3, and 1.0). The Kepler response function is plotted in light gray.