adsabs/AstroCLIMB huggingface dataset:
Paper: Late Jets, Early Sparks: Illuminating the Premaximum Bumps in Superluminous Supernovae
Authors: Ore Gottlieb, Brian D. Metzger
Figure caption: (a) Bolometric luminosity peaks soon after breakout (t  b ) and then declines. The dashed magenta lines illustrate the rise of the main Type I SLSN peak. (b) Color temperature of the radiating gas. (c) Absolute (left vertical axis) and apparent (right vertical axis) magnitude at various bands (f NUV = 1.2 × 1015 Hz, f  u  = 8.6 × 1014 Hz, f  g  = 6.3 × 1014 Hz, f  r  = 4.8 × 1014 Hz, f  y  = 3.0 × 1014 Hz) demonstrate that the peak magnitude aligns with observations of SLSN early bumps. (d) Luminosity-weighted average dimensionless velocity of the radiating gas at the trapping radius demonstrates that the emitting gas is always subrelativistic. The dimensionless front ejecta velocity is shown in red for comparison.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Mass–radius diagram showing the small planets in the sample of JWST Cycle 2 Program GO 4098 (triangle markers) and how they compare to the larger K2-18 b. We also display planets from the NASA Exoplanet Archive with 3σ or better mass measurements, colored by their equilibrium temperatures for an Earth-like albedo of 0.3. The planets span both sides of the radius valley (gray). We highlight the compositional degeneracy in mass–radius space with constant composition lines calculated using smint for planets with H2/He envelopes or H2O in the supercritical+vapor state (mass–radius relationships from E. D. Lopez & J. J. Fortney 2014; A. Aguichine et al. 2021). We display mass–radius curves for water-rich compositions of 10% and 50% water in the supercritical+vapor state assuming an irradiation temperature of 670 K (representative of GJ 9827 d; blue solid lines) and isocomposition curves for 0.2% and 1% by mass solar composition H2-dominated gas for a 1 Gyr planet receiving like GJ 9827 d approximately 35 times the Earth’s insolation (navy dashed lines), both atop Earth-like cores. The positions of Venus and the Earth are indicated with black letters, and the light gray shaded area in the bottom right corner highlights planets smaller than expected from collisional stripping of planetary mantles (R. A. Marcus et al. 2010). With a mass of 3.02 M ⊕ and a radius of 1.98 R ⊕, GJ 9827 d hugs the upper size end of the radius valley, in line with its high predicted hydrogen escape rates.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Top panels: results from the white light-curve fit of the supreme-SPOON reduction for visits 1 (left) and 2 (right) and fitted systematics models. The order 1 systematics-corrected light curves are shown (teal points), binned for visual purposes, along with the best-fit transit model (black) and the systematics model including the GP component (red, with the GP scaled for visualization purposes). The vertical blue shaded regions indicate the three candidate flares with the highest-S/N spectra and following typical flare evolution profiles (see Appendix B). Bottom panels: spectroscopic light-curve fits to the two NIRISS/SOSS transits of GJ 9827 d from the supreme-SPOON reduction. The left panel corresponds to the first visit and the right panel to the second visit. We show the detrended broadband light curve for order 2 and seven spectroscopic light curves from order 1 from top to bottom. The best-fit astrophysical model is shown for each light curve (black), and the light curves are offset relative to each other for clarity.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Results from the free retrieval performed on the JWST/NIRISS/SOSS + HST/WFC3 spectrum of GJ 9827 d. Left panels: the semitransparent lines are sample spectra from the posterior distributions of the SCARLET free retrievals when only the atmosphere (top panel) or both the atmosphere and stellar contamination component (bottom two panels) are accounted for. The black line is the best-fit model, and the black (gray) points are the measured NIRISS/SOSS (HST/WFC3) transit depths. The retrievals were performed using the R = 100 version of the JWST/NIRISS/SOSS spectrum, and a binned version is shown for visual comparison purposes. Even when stellar contamination is accounted for, the planetary atmosphere component of the model captures the H2O absorption features, and the constraints on the H2O abundance are not affected. The model including the contribution from spots only introduces an additional slope and does not affect the retrieval results. Right panels: posterior distributions obtained on H2O in both retrieval setups and on the spot covering fraction and temperature in the joint retrieval. For the POSEIDON retrievals (CLR prior), we only show in this figure the samples where the spot is at most 800 K cooler than the photosphere, for clarity (see full posteriors in Figure A8). Our inference of a water-rich steam atmosphere is robust to the marginalization over stellar contamination contributions and to the choice of priors (H2/He as the background gas in blue, CLR prior in pink).
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Constraints on the atmospheric composition from the POSEIDON retrieval with the agnostic (CLR) prior on the background gas (pink), the SCARLET retrieval with H2/He assumed to be the background gas (blue), and SCARLET chemically consistent retrieval (orange). Left panel: contours representing the 0.5σ, 1σ, 1.5σ, and 2σ levels in the joint posterior probability distribution on the atmospheric metallicity and the gray cloud-top pressure for all three retrievals. Right panel: kernel density estimations of the atmospheric metal mass fraction Z atm obtained from all posterior samples for each retrieval setup.
Paper: Late Jets, Early Sparks: Illuminating the Premaximum Bumps in Superluminous Supernovae
Authors: Ore Gottlieb, Brian D. Metzger
Figure caption: Top-hat jet afterglow light curves at ν = 6 GHz for observers at θ obs = 0.5 rad (solid lines) and on-axis observers (dashed lines) at z = 0.25, assuming jet Lorentz factor Γ = 100, opening angle θ  j  = 0.1 rad, and the following microphysics parameters: electron equipartition parameter ϵ  e  = 0.1, magnetic equipartition parameter ϵ  B  = 10−4, electron energy power-law index p = 2.2, and wind velocity v  w  = 1000 km s−1. The black circles denote the most constraining upper limits measured for Type I SLSN Gaia2016apd (D. L. Coppejans et al. 2018), placing the source at z = 0.25.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Qualitative description of the major oxygen-, carbon-, nitrogen-, and sulfur-bearing species expected in metal-rich atmospheres as a function of atmospheric origin and mantle composition (white labels inside of each mantle composition case). Water-dominated atmospheres can result from magma ocean–atmosphere interactions under oxidized mantle conditions (E. S. Kite et al. 2020; H. E. Schlichting & E. D. Young 2022) or from the planet-forming or accreted solids that coagulated beyond the water-ice line. Depending on the redox state of the mantle and the H/C ratio of the mantle (P. Liggins et al. 2022), CH4 or CO/CO2 can be the dominant carbon-bearing species, and NH3 or N2 can be the dominant nitrogen-bearing species. Further O2 buildup can occur over time as H is gradually lost to space (J. Krissansen-Totton et al. 2021; C. E. Harman et al. 2022).
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Search for metastable He absorption around 10833 Å in both NIRISS/SOSS transits of GJ 9827 d. The top and bottom panels respectively show the spectrum fitted after extraction at pixel resolution and 2 pixel resolution for each of the two visits (supreme-SPOON reduction). We do not detect significant absorption from the He I metastable triplet, in line with more sensitive ground-based high-resolution observations.
Paper: Nearby Supernova and Cloud Crossing Effects on the Orbits of Small Bodies in the Solar System
Authors: Leeanne Smith, Jesse A. Miller, Brian D. Fields
Figure caption: One possible trajectory of a 1 μm dust grain in the Kuiper Belt subject to a constant wind from a dense interstellar cloud, corresponding to the “LxCC” case in Table 1. (a) shows the full 3D path, and (b) and (c) show projections in the x–y and x–z planes, respectively. Note that (c) is not an equal aspect ratio.
Paper: Nearby Supernova and Cloud Crossing Effects on the Orbits of Small Bodies in the Solar System
Authors: Leeanne Smith, Jesse A. Miller, Brian D. Fields
Figure caption: Integrated time evolution of a 1 μm Kuiper Belt dust grain subject to a wind from a 20 pc SN (top), a 50 pc SN (middle), and the LxCC (bottom). Plotted quantities are the semimajor axis (blue solid), eccentricity (orange dashed), and inclination (green dotted). Note that in the bottom panel, the semimajor axis and time are on different scales than the top and middle.
Paper: Nearby Supernova and Cloud Crossing Effects on the Orbits of Small Bodies in the Solar System
Authors: Leeanne Smith, Jesse A. Miller, Brian D. Fields
Figure caption: Histograms of orbital parameters of Oort Cloud comets in their initial distribution (blue) and after being hit by a remarkably close SN 10 pc away (orange). The parameters shown are (left to right, top to bottom) semimajor axis, eccentricity, angle of inclination, R.A. of the ascending node, argument of periapsis, and the true anomaly.
Paper: Nearby Supernova and Cloud Crossing Effects on the Orbits of Small Bodies in the Solar System
Authors: Leeanne Smith, Jesse A. Miller, Brian D. Fields
Figure caption: Fraction of comets of a given size that become unbound from an SN blast, evaluated for SN distances of 10, 20, 50, and 100 pc from the solar system. The dashed line comes from a simplified calculation by S. A. Stern (1990) for an SN 40 pc away for particles orbiting 20,000 au from the Sun.
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: Archival PS-DR1 images centered on the location of AT2023vto. There are two distinct sources within a few arcseconds of the location of the transient; the fainter extended source directly underlies the position of AT2023vto and is its host galaxy (the brighter point source is a likely foreground star). Right: a zoomed-in image with the point source subtracted. We find that AT2023vto coincides with the center of its host galaxy, supporting its TDE origin.
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: Optical/UV light curves of AT2023vto. The magnitudes are corrected for Galactic extinction. Photometry has been obtained from ZTF (circles), ATLAS (squares), LCO (diamonds), and Swift (crosses). AT2023vto peaks in the g band about 50 days postdiscovery with a peak absolute magnitude of m  g  ≈ −23.2. The g − r color is blue (≈ −0.4 mag) and does not evolve significantly during the rise and decline phase of the light curve for about 155 days, typical of TDEs.
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: Spectral energy distribution of the host galaxy of At2023vto (green points) along with the best-fit model from Prospector (red points and gray curve). The host photometry has been measured from PS-DR1 images with the nearby point source subtracted (see Figure 1).
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: Transmission spectrum of GJ 1214 b with two data reductions and illustrative models. The top panel shows the results of data reduction by the tshirt and Eureka! pipelines, demonstrating that two independent pipelines yield consistent results within 1σ error bars. The solid black, solid gray, and dashed–dotted gray lines show the median spectrum from the chemically consistent model, chemically agnostic free model, and a flat line (with stellar inhomogeneities), respectively, fit to the HST, JWST NIRSpec (tshirt), and JWST MIRI panchromatic spectrum. The lower panels show the illustrative transmission spectra to exhibit the transit depth shape of relevant molecules; we create clear isothermal (T = 500 K) N2 atmospheres with only one gas at a time with a volume mixing ratio = 10−4 and repeat for all molecules.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: Left: wavelength selections for CO2 and out-of-feature coadding. We use the chemically consistent model (purple curve) and a threshold (dashed black line) to select wavelengths that are dominated by CO2 opacity (brown circles) and wavelengths that are outside of features (pink circles). Individual spectra are shown for the NRS1 and NRS2 detectors and per observation (Obs 18 NRS1, blue; Obs 18 NRS2, orange; Obs 19 NRS1, green; and Obs 19 NRS2, red). Right: differential light curve inside and outside of significant CO2 features. Each detector and observation’s fluxes are summed for wavelengths inside a feature and divided by the fluxes summed outside this feature. The same blue, orange, green, and red colors are used on the left and right to code each detector and observation. Finally, an average in-feature vs. out-of-feature light curve across both observations is shown in purple and brown on the bottom for NRS1 and NRS2, respectively. The same wavelengths’ best-fit models are shown as black curves, which use a limb-darkened starry model. Linear trends have been removed from all time series, and vertical offsets were applied for clarity.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: 2D light curves binned to a resolution of R = 100 and 40 time bins for NRS2 (top row) and NRS1 (bottom row), with both transits averaged. The normalized flux in percentage (after linearly detrending at each wavelength) is shown in panel (A). The differential time series after dividing by the broadband for a given detector is shown in ppm in panel (B). The differential light-curve model is shown in panel (C), and the residuals of the light curve subtracted by the model are shown in panel (D). The start of ingress and end of egress times are marked as vertical dashed lines. Increased and decreased transit depths relative to the broadband light curve are visible as dark and bright bands between ingress and egress. The most noticeable features are increased transit depths near 4.3 and 2.8 μm and decreased transit depths near 3.6 and 4.6 μm.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: Top: NGTS and AIT photometry of the GJ 1214 system. A binned version of the NGTS photometry is shown at a cadence of one point per night. The epochs of the two JWST NIRSpec observations are highlighted as dark red dashed vertical lines. Middle: the integrated stellar spectra between our two observations overplotted to check for differences in stellar spot coverage. Bottom: the difference between the two observations, with a median difference of 0.04% in NRS1 and 0.02% in NRS2.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: Broadband light curves from the tshirt pipeline separated by detector and observation number. The top panels show the light curves at full time resolution and the maximum a posteriori light-curve models (R. Luger et al. 2019). The residuals of the data subtracted by the model are shown in the bottom panels, and binned residuals are shown for clarity. The first point in the time series (red) is discarded from the fits.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: The calculated limb-darkening coefficients are very close to the Phoenix stellar model. We fit for a scale factor for this model and then fix the q 1 and q 2 coefficients for a second iteration of spectroscopic light-curve fitting. Stellar parameters are T eff = 3300 K, [M/H] = 0.5, log(g) = 5.0.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: Median CO2+CH4 atmospheric models for the spectrum taken at each individual observational epoch. The upper and lower rows show the modal-data comparison for tshirt and the Eureka! data reduction pipeline, respectively.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: A posterior distribution of the temperature difference in the stellar spot from the mean effective temperature. The left panel shows the spot contrast temperature (in K). The middle and right panels show the retrieved spot contamination spectrum.
Paper: Lyman Continuum Leakers at z > 3 in the GOODS-S Field: Starburst or Not?
Authors: Shuairu Zhu, 帅儒 朱, Fang-Ting Yuan, Chunyan Jiang, Zhen-Ya Zheng, Ruqiu Lin
Figure caption: Observed SEDs (dots) of the LyC leakers. The red dots are measurements from the JADES catalog, and the blue and green dots are measurements from the 3D-HST catalog. The triangles indicate the 3σ upper limits for nondetections. We exclude photometric points (in green) affected by the IGM. We show the best SED fit with orange solid lines (IGM attenuated) and gray dashed lines (IGM unattenuated). The integrated fluxes based on the best SED fit are shown in black circles.