adsabs/AstroCLIMB huggingface dataset:
Paper: Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity
Authors: Wladimir Lyra, Chao-Chin Yang, 朝欽 楊, Jacob B. Simon, Orkan M. Umurhan, Andrew N. Youdin
Figure caption: Density-diffusion relation for the 2563 resolution runs shown in Figure 5. The x-axis shows a pebble density threshold, and the y-axis the diffusion computed as an average of all mesh cells with pebble density above the threshold, in space and time (see the main text). The dotted lines show the steady-state solution of Lyra & Lin (2013) for pebbles trapped in a vortex considering stellar vertical gravity, drag force, and diffusion. The runs that achieve collapse (Hill density ρ  p  = 90) have diffusion under the steady-state prediction. The runs that do not achieve collapse (green line and magenta line) have maximum density consistent with the analytical solution.
Paper: Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity
Authors: Wladimir Lyra, Chao-Chin Yang, 朝欽 楊, Jacob B. Simon, Orkan M. Umurhan, Andrew N. Youdin
Figure caption: Distribution of protoplanets formed in the higher resolution model (5123 mesh resolution, 7.5 × 106 superparticles). The left panels show the vertically averaged vertical vorticity; the right panels show the vertically integrated (column) density of pebbles. The upper panels correspond to 2 orbits after the insertion of particles, the middle panel after 5, and the lower panel after 12 orbits. The protoplanets are overlaid as white circles in the left panels, and black circles in the right panels. The radius of the circle marks the Hill radius of the protoplanet. Protoplanets are formed inside the vortex, which continuously spawns planetary mass objects.
Paper: Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity
Authors: Wladimir Lyra, Chao-Chin Yang, 朝欽 楊, Jacob B. Simon, Orkan M. Umurhan, Andrew N. Youdin
Figure caption: Time evolution of the maximum pebble density as a function of resolution (left), Stokes number (middle), and dust-to-gas ratio (right). The Hill density for this simulation is ρ  d  = 90 in code units. When a clump of pebbles achieves this density, a sink particle replaces it.
Paper: Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity
Authors: Wladimir Lyra, Chao-Chin Yang, 朝欽 楊, Jacob B. Simon, Orkan M. Umurhan, Andrew N. Youdin
Figure caption: Left: differential mass function, 50 orbits after particle insertion, as a function of resolution. The simulations converge at high mass, but as we increase the resolution, more small mass objects are formed, with no convergence in sight. The horizontal stripes seen from our highest 5123 resolution is due to the mass discretization of the superparticles; see Equation (7). Right: cumulative mass function, 50 orbits after particle insertion, as a function of resolution.
Paper: Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity
Authors: Wladimir Lyra, Chao-Chin Yang, 朝欽 楊, Jacob B. Simon, Orkan M. Umurhan, Andrew N. Youdin
Figure caption: Efficiency of conversion of pebbles into protoplanets. The y-axis in the inset is shown in linear scale. Seen from the 1283 at different particle resolution, that quantity has converged. Convergence is not seen with mesh resolution, although 2563 to 5123 has not changed the rate as much as from 1283 to 2563. At 2563 resolution the available dust density drops 1 order of magnitude in 100 orbits.
Paper: Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity
Authors: Wladimir Lyra, Chao-Chin Yang, 朝欽 楊, Jacob B. Simon, Orkan M. Umurhan, Andrew N. Youdin
Figure caption: Evolution of the cummulative mass distribution, as a function of resolution. Notice the different final times. The mass distribution did not converge in time or resolution.
Paper: Analyses of Johannes Kepler’s Sunspot Drawings in 1607: A Revised Scenario for the Solar Cycles in the Early 17th Century
Authors: Hisashi Hayakawa, Koji Murata, E. Thomas H. Teague, Sabrina Bechet, Mitsuru Sôma
Figure caption: Kepler’s solar drawings upon his observation on 1607 May 28 at (a) Kepler’s house and (b) Burgi’s workshop, as well as (c) his schematic presentation, as reproduced from Kepler (1609).
Paper: Analyses of Johannes Kepler’s Sunspot Drawings in 1607: A Revised Scenario for the Solar Cycles in the Early 17th Century
Authors: Hisashi Hayakawa, Koji Murata, E. Thomas H. Teague, Sabrina Bechet, Mitsuru Sôma
Figure caption: Our calculations of the heliographic coordinates of the solar disk as seen in the sky upon Kepler’s first and second observations, overlaid with Kepler’s sunspot drawings in corrected orientations. The first and second images show those at Kepler’s house (N50°05′, E014°25′) at 15:29 ± 0:30 UT (Figure 1(a)) and Justus Burgi’s workshop in the citadel (N50°05′, E014°24′) at 17:37 ± 01:20 UT (Figure 1(b)).
Paper: Analyses of Johannes Kepler’s Sunspot Drawings in 1607: A Revised Scenario for the Solar Cycles in the Early 17th Century
Authors: Hisashi Hayakawa, Koji Murata, E. Thomas H. Teague, Sabrina Bechet, Mitsuru Sôma
Figure caption: Fractions of the reported sunspot group in each heliographic-latitude range against the population of the entire sunspot group, according to the USET data set in 1940–2023.
Paper: Analyses of Johannes Kepler’s Sunspot Drawings in 1607: A Revised Scenario for the Solar Cycles in the Early 17th Century
Authors: Hisashi Hayakawa, Koji Murata, E. Thomas H. Teague, Sabrina Bechet, Mitsuru Sôma
Figure caption: Our solar-cycle minimum constraint between Solar Cycles −14 and −13, shown with red lines as their boundaries. These constraints are compared with reconstructed sunspot number based on 14C data in the black curve (Usoskin et al. 2021) and the green curve (Miyahara et al. 2021), as well as sunspot group number of Svalgaard & Schatten (2016), multiplied by a factor of 20, according to Muñoz-Jaramillo & Vaquero (2019), shown in the blue curve.
Paper: Analyses of Johannes Kepler’s Sunspot Drawings in 1607: A Revised Scenario for the Solar Cycles in the Early 17th Century
Authors: Hisashi Hayakawa, Koji Murata, E. Thomas H. Teague, Sabrina Bechet, Mitsuru Sôma
Figure caption: Distributions of the reported sunspot latitudes in 1607–1629, contrasting our three scenarios for Kepler (Figures 1(a) and (b)), in comparison with V+21 (Vokhmyanin et al. 2021), V+20 (Vokhmyanin et al. 2020), A+16 (Arlt et al. 2016), C+19 (Carrasco et al. 2019), H+21 (Hayakawa et al. 2021a), C+21 (Carrasco et al. 2021), and VZ18 (Vokhmyanin & Zolotova 2018).
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Positions of significant atomic lines and molecular bands in the NIRISS spectrum (0.6–2.8 μm).
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: A corner plot of the inferred parameters of the 1-comp model. Here “t1,” “rstar,” “dist,” “scale,” and “logf” represent the temperature of the quiescent component, the star’s radius, the star’s distance, the scaling parameter, and additional noise present in the data, respectively. The model was constructed using the PHOENIX spectral grid and NIRSpec data.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: A corner plot of the inferred parameters of the 1-comp model. Here “t1,” “rstar,” “dist,” “scale,” and “logf” represent the temperature of the quiescent component, the star’s radius, the star’s distance, the scaling parameter, and additional noise present in the data, respectively. The model was constructed using the SPHINX spectral grid and NIRISS data.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: A corner plot of the inferred parameters of the 1-comp model. Here “t1,” “rstar,” “dist,” “scale,” and “logf” represent the temperature of the quiescent component, the star’s radius, the star’s distance, the scaling parameter, and additional noise present in the data, respectively. The model was constructed using the PHOENIX spectral grid and NIRISS data.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Near-IR and IR SED of TRAPPIST-1. Red symbols represent the observed photometric measurements. Blue symbols are the model fluxes from the best-fit SPHNIX atmosphere model (gray). Overlaid on the model are the absolute flux-calibrated spectrophotometric observations from NIRISS (yellow) and NIRSpec (black).
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Activity indicators of TRAPPIST-1 in the SpeX+MagE and UVES spectra.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Photospheric modeling of TRAPPIST-1 using the NIRISS and NIRSpec out-of-transit stellar spectra. The modeling was conducted based on the SPHINX spectral grid.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Photospheric modeling of TRAPPIST-1 using the NIRISS and NIRSpec out-of-transit stellar spectra. The modeling was conducted based on the PHOENIX spectral grid.
Paper: Unveiling the Interplanetary Solar Radio Bursts of the 2024 Mother’s Day Solar Storm
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, David Lario, Teresa Nieves-Chinchilla, Juan Carlos Martinez Oliveros
Figure caption: Detailed analysis of three type III bursts from STEREO-A/WAVES (events #6, #7, and #9). (a)–(c) Radio spectra from STEREO-A/WAVES, with the magenta curve representing the GOES 1–8 Å X-ray flux. The black rectangles denote the time–frequency intervals used for propagation analyses. White dashed curves are fitted beam speeds assuming a fundamental emission with a constant velocity. Event #7 includes a fitted CME with the same assumption, shown as an orange dashed curve. (d)–(f) Peak radio fluxes as a function of frequency within the selected time–frequency interval (magenta squares) and corresponding wavevector azimuths for peak fluxes (gray circles). Corrected azimuths between 350 kHz and 1 MHz are denoted as colored circles. (g)–(i) Location of STEREO-A in the HEEQ coordinate system (red square) and corrected wavevector directions (colored arrows). The Sun is represented by a yellow circle and the Earth by a green circle. The Parker spiral rooted at the GOES solar flare location is shown as a black dashed curve, assuming a solar wind speed of 400 km s−1. Fitting results from corrected azimuths for the Parker spiral using the density model, showing the derived solar flare location (red dashed curve). The gray and red shaded areas indicate regions with Parker spirals corresponding to solar wind speeds between 300 and 600 km s−1.
Paper: Unveiling the Interplanetary Solar Radio Bursts of the 2024 Mother’s Day Solar Storm
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, David Lario, Teresa Nieves-Chinchilla, Juan Carlos Martinez Oliveros
Figure caption: (a) Time series of 1–8 Å X-ray flux from GOES (orange curve) from 2024 May 8 to May 15. The radio flux at 1 MHz from Wind/WAVES and STEREO-A/WAVES is shown by green and red lines, respectively. X-class solar flares are marked with vertical dotted lines, with those associated with type III bursts in magenta and those without type III bursts in gray. (b) Radio spectra from Wind/WAVES, displaying type II, III, and IV bursts. (c) Radio spectra from STEREO-A/WAVES, showing similar features. (d) Proton intensities observed by GOES in several integral energy channels (blue, green, yellow, and orange curves) alongside the Dst index reported in https://wdc.kugi.kyoto-u.ac.jp (magenta curve), highlighting the geomagnetic storm peak with a minimum of −412 nT on May 11.
Paper: Unveiling the Interplanetary Solar Radio Bursts of the 2024 Mother’s Day Solar Storm
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, David Lario, Teresa Nieves-Chinchilla, Juan Carlos Martinez Oliveros
Figure caption: Statistical analysis of the type III bursts associated with X-class solar flares from NOAA region 13664. (a) Fitted longitudes of the radio bursts as a function of the GOES solar flare longitudes. The red dashed line represents the average eastward drift of −13.°42 ± 11.°63 from the y = x line (black dashed line). (b) Correlation between the GOES X-ray flux and the GOES solar flare longitudes, showing a high Kendall’s tau correlation coefficient of 0.535. (c) Correlation between the radio flux at 1 MHz and the soft X-ray flux from GOES, showing a high Kendall’s tau correlation coefficient of 0.648. (d) Histogram of the timing difference between the GOES maximum soft X-ray flux and the electron beam onset time, indicating an average delay of 3.24 ± 4.42 minutes.
Paper: Unveiling the Interplanetary Solar Radio Bursts of the 2024 Mother’s Day Solar Storm
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, David Lario, Teresa Nieves-Chinchilla, Juan Carlos Martinez Oliveros
Figure caption: Radio spectra from STEREO-A/WAVES for all nine type III burst events observed between 2024 May 8 and May 14. Each panel shows radio spectra from STEREO-A/WAVES, with the magenta curve representing the GOES 1–8 Å X-ray flux. The black rectangles denote the time–frequency intervals selected for propagation analysis. White dashed curves represent fitted beam speeds, assuming a fundamental emission with a constant velocity.
Paper: Understanding the Variability of Helium Abundance in the Solar Corona Using Three-fluid Modeling and Ultraviolet Observations
Authors: Leon Ofman, Yogesh, Silvio Giordano
Figure caption: Representation of global magnetic field topology from PFSS model (Wang & Sheeley 1992) for the Carrington rotation centered on the HERSCHEL observation date (model available at NISP NSO Integrated Synoptic Program). The closed field lines are plotted in blue, and regions of open positive and negative flux are represented by green and red, respectively. The neutral line is drawn in black.
Paper: Understanding the Variability of Helium Abundance in the Solar Corona Using Three-fluid Modeling and Ultraviolet Observations
Authors: Leon Ofman, Yogesh, Silvio Giordano
Figure caption: The results of the 3D three-fluid model of the tilted streamer belt shown in the r−θ plane at longitude ϕ = 0.76 rad. The distance is in solar radii, and angles are in radians. The densities are normalized in terms of n  e0 = 5 × 108 cm−3. The white lines mark several field lines of the modeled magnetic field. (a) The normalized density of the He++ ions. (b) The normalized proton density (blue). (c) The He++ radial velocity in km s−1. (d) The proton radial velocity in kilometers per second.
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: A comparison of the results from the 1D-RCPE and the free-retrieval atmospheric modeling, demonstrating their agreement. The free retrieval’s posterior distributions (gray) are shown against the abundance profiles (colored lines) from the 1D-RCPE grid modeling. The dotted lines show the expected composition of a solar metallicity and solar C/O atmosphere. The dashed–dotted lines show the expected abundance profiles for a 125× solar metallicity atmosphere with a C/O of 0.35, as estimated for GJ 3470 b, under chemical equilibrium. The solid colored lines and shaded regions show the median 1σ and 2σ profiles for GJ 3470 b under the disequilibrium conditions in the 1D-RCPE modeling. Note that for all molecules except for CH4 and SO2, the abundances estimated from the 1D and free-retrieval modeling match the equilibrium abundances of the 125× solar metallicity atmosphere with a C/O of 0.35. This indicates that CH4 is likely being depleted and SO2 enhanced via disequilibrium processes.
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: Three independent reductions of the NIRCam F322W2 and F444W data agree within their uncertainties The top panel shows the F322W2 and F444W transmission spectra, as reduced using the Pegasus, Eureka, and tshirt pipelines, plotted with their associated 1σ uncertainties using constant 0.015 μm wide spectral bins. All of the F322W2 spectra have been offset down by 163 ppm to correct for a bias offset in the F322W2 transit depths compared to the F444W and Spitzer data (see Appendix B.3). All three reductions agree on the shape of the transmission spectrum and show features due to H2O (2.5–3.2 μm), CH4 (3.2–3.5 μm), SO2 (3.9–4.1 μm), and CO2 (2.6–2.9 μm and 4.2–4.5 μm). The absorption cross sections of the prominent species in this wavelength range are shown in the bottom panel.
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: The combined NIRCam and HST/WFC3 transmission spectrum of GJ 3470 b showing major absorption features. The measured transit depths are plotted with their associated 1σ uncertainties. The NIRCam data have been binned into 0.06 μm wide spectral channels (black points) for visual clarity. The background gray points show the NIRCam data binned in 0.015 μm wide channels, which is the direct result of our analysis and was used in our atmospheric modeling. The solid dark gray line shows the best-fit model transmission spectrum from the atmospheric free-retrieval analysis. The colored regions illustrate the contributions of various molecules and clouds to the best-fit model. Note that the new NIRCam data and the refined HST transit depths strongly disfavor the previously suggested Mie scattering feature near 3 μm (dashed gray line; Benneke et al. 2019a).
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: The broadband lightcurve data and best-fit transit models used in this analysis. To refine the orbital parameters of GJ 3470 b, we simultaneously fit archival broadband HST/WFC3 and Spitzer/IRAC data (top panels) together with the new JWST photometric (F210M) and spectroscopic (F322W2 and F444W) data (bottom panels). This provides significantly more precise measurements of the orbital ephemerides and the orbital separation. We use these results to fix the orbital properties of GJ 3470 b in our spectroscopic fitting. The full results of the joint broadband fit are given in Table 2. Note that the F210M panel shows both F210M lightcurves overplotted on top of each other, one from each of the F322W2 and F444W observations.
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: Our fit to the SED of GJ 3470. Using catalog 2MASS and AllWISE measurements of GJ 3470's brightness along with the Gaia DR3 parallax to the system, we modeled the SED from the star GJ 3470. We measure the stellar radius to be R * = 0.50 ± 0.01 R ⊙ and its mass to be M * = 0.44 ± 0.04 M ⊙. Using the results from our lightcurve fitting, this allows us to refine the radius and mass of the planet GJ 3470 b to be R  p  = 4.22 ± 0.09 R ⊕ and M  p  = 11.1 ± 0.9 M ⊕.
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: The impact of composition and temperature on the SO2 abundance in cool (<800 K) sub-Neptune atmospheres. The left panel illustrates the column-averaged (1 μbar–0.1 mbar) volume mixing ratio of SO2 (contours) as a function of the atmospheric metallicity (relative to solar) and the carbon-to-oxygen ratio for the nominal temperature of GJ 3470 b. There is a steep falloff in SO2 with increasing C/O and increasing carbon-to-oxygen ratio. The right panel shows the dependency of the column-averaged SO2 abundances with planetary irradiation temperature for representative metal enrichment. The presence of SO2 at these temperatures substantially restricts the possible atmospheric composition. The retrieved SO2 abundance (navy contour on the left and the shaded box on the right) strongly indicates an atmosphere with ∼100× stellar metallicity and a substellar carbon-to-oxygen ratio.
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: A comparison of the three different NIRCam data reductions. The NIRCam F322W2 and F444W transmission spectra from all three of the data reduction pipelines, smoothed using a three-point wide boxcar filter for clarity. The F322W2 spectra have all been offset down by 163 ppm (see discussion in the text). All three spectra show spectra features with similar shapes and amplitudes. Compared to our nominal Pegaus spectra, the Eureka! and tshirt results differ by χ 2/dof = 0.13 for Pegasus vs. Eureka! and χ 2/dof = 0.21 for Pegasus vs. tshirt.