adsabs/AstroCLIMB huggingface dataset:
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: Key X-ray XMM-Newton time lag results: Left: lag–frequency spectrum with bias-subtracted coherences computed between a reflection-dominated band (0.3–1 keV) and a continuum-dominated band (1–4 keV). A positive lag indicates the hard band lagging the soft band. Right: the lag–energy spectrum when isolating low frequencies (upper) reveals lags increasing with energy, commonly attributed to the inward propagation of mass-accretion rate fluctuations. The lag–energy spectrum at high frequencies (lower) instead exhibits features consistent with reverberation (albeit at low significance, due to larger uncertainties above 3 keV), including peaks in the lags below 1 keV where we expect the soft excess, and in the 6–10 keV bin where we expect the Fe K.
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: Lags as a function of frequency in the UVOIR bands (with respect to the UVW2 reference band), with corresponding bias-corrected coherence values below. The accessible frequencies (∼10−2–100 day−1, i.e., ∼10−8–10−6 Hz), are over two orders of magnitude lower than those studied using the XMM-Newton observation. The lags predicted by the disk reprocessing model (orange) given the mass and accretion rate of Mrk 817 poorly describe the measured lags at low frequencies. The fit improves significantly when we include a simple model component to account for additional contribution to the lags from a distant reprocessor (final model in blue). The radius of this reprocessor is constrained at ∼23 days, consistent with previous measurements of the Hβ lag indicative of the BLR size scale.
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: Top: light curves in three energy bands for the XMM-Newton observation used in our analysis. The lower-energy bands spanning 0.3–4 keV exhibit clear variability, from which we compute frequency-resolved time lags probing the innermost accretion flow. Bottom: the XMM-Newton spectrum from the same observation divided by a power-law model with a photon index of 2. Purple horizontal lines visualize the 0.3–1 keV and 1–4 keV energy ranges used in the timing analysis to isolate reflection and the direct coronal continuum, respectively.
Paper: AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags
Authors: Collin Lewin, Erin Kara, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Gerard A. Kriss, Hermine Landt, Jonathan Gelbord, John Montano, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Michael S. Brotherton, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Michael R. Goad, Juan V. Hernández Santisteban, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Kirk T. Korista, Peter Kosec, Andjelka Kovačević, Missagh Mehdipour, Jake A. Miller, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Luka Č. Popović, David Sanmartim, Marianne Vestergaard, Martin J. Ward, Fatima Zaidouni
Figure caption: Left: lags and bias-subtracted coherence values as a function of frequency computed between the Swift X-ray bands (SX: 0.3–1.5 keV, HX: 1.5–10 keV) and the UVW2 band. A positive lag indicates that the X-ray variability lags the UV, opposite to the negative lag predicted by the disk model (orange). These lags can be reproduced by including a model component corresponding to reprocessing at a radius consistent with the BLR (blue). Right: (a) Swift 0.3–10 keV and (b) UVW2 light curves. Dotted lines visualize the 3.5 day lag (the average of the SX and HX vs. UVW2 lags) between these two bands. Both bands exhibit a similar decrease in flux over time, which may be producing these measured lags on long timescales.
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Impact of clumpy medium properties on the Σ–D curve (except for panel (a), which shows different uniform densities). The plot legend shows the variables of interest (n 0 is in cm−3). The values of all other variables that are not explicitly written on the graph are n 0 = 0.1 cm−3, ﹩{\bar{\rho }}_{j}=10﹩, f  c  = 0.2, and R  d  = 5 pc. The black dashed line represents the uniform case for n 0 = 0.1 for panels (a)–(e) and n 0 = 0.03 for panel (f). The clump radius r  c  = 1 pc is the same for all graphs.
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Panels show the Galactic SNR sample from B. Vukotić et al. (2019) and its comparison to Models A, B, and C. The contours represent the normalized PDDs at levels 0.025, 0.1, 0.2, 0.5, and 0.8. The PDD is made using the method from P. W. Duin (1976; same as in B. Vukotić et al. 2019). The thick line represents the bin-averaged value of Σ depending on D (the line connects the average Σ in 50 bins; the width of a bin is 0.26). Black refers to the MW sample, and red refers to a modeled sample. The model parameters are listed on graphs: PL—power-law density distribution; CL—clumpy medium; n 0 is in cm−3; R  p  and R  d  are in pc. The three outliers that are present in the MW sample are removed from the three graphs comparing models to the MW sample.
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Left: slopes β of uniform medium Σ–D relations in different concentrations (in cm−3), depending on SNR diameter. Right: slopes β for n 0 = 0.1 cm−3 in clumpy medium of different mean density jump (R  d  = 10 pc, f  c  = 0.2). At first interaction with clumps, the emission rise causes a negative slope. After the peak in Σ, a further decrease is significantly steeper than in uniform medium, while the steepness depends on the mean density jump (i.e., the density contrast).
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Results for C10F10, C30F10, and C100F10. The points and lines represent the simulation results and the semianalytical model, respectively. Blue and red stand for ICM and CL average values, respectively. Green lines show the uniform evolution in ρ icm and ﹩\bar{\rho }﹩ ambient densities. Top: black represents the mean energy (higher curves) and pressure (lower curves) of the forward shock. Middle: velocity graphs. Black represents the total average. Bottom: Σ–D graphs. Black represents the total value.
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Simulation results and semianalytical model for the LDB2, LDB5, and LDB10 setup. The black points and red line represent the simulation results and semianalytical model, respectively. Green lines show the uniform evolutions in ρ  l  and ρ  h  ambient densities. From top to bottom row: evolutions of the energy (higher curves) and pressure (lower curves), velocity behind the shock, and the Σ–D relation.
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Comparison of theoretical (line) and uncalibrated simulation results (points) for model U1. The graphs show the surface area of the shock S (left) and the mean velocity behind the shock v 2 (middle) as a function of SNR diameter, as well as the Σ–D relation (right). Apart from the left panel, where the systematic error of ≈5% is present, it is clearly seen that, as the SNR covers more cells, the values converge to theoretical ones.
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Top: comparison of SNR surface area ratio (Equation (41)) obtained from simulations and the analytical model. Bottom: comparison of CL shock fraction from simulations and the analytic model. The points and lines represent the simulation results and the analytic model, respectively. The simulation setups are denoted in the legend.
Paper: Supernova Remnants in Clumpy Medium: A Model of Hydrodynamic and Radio Synchrotron Evolution
Authors: Petar Kostić, Bojan Arbutina, Branislav Vukotić, Dejan Urošević
Figure caption: Results for C10F25, C30F25, and C100F25. The graph properties are the same as in Figure 11.
Paper: Next-generation Accretion Disk Reflection Model: High-density Plasma Effects
Authors: Yuanze Ding, Javier A. Garcıa, Timothy R. Kallman, Claudio Mendoza, Manuel Bautista, Fiona A. Harrison, John A. Tomsick, Jameson Dong
Figure caption: Broadband reflection spectra for different densities and ionizations. Spectra at different densities are normalized by a factor of 1, 102, 105, and 108 for clarity. See also Figure 7 for a clearer view of the narrow atomic features. In the low-density regime, Model 2 is in good agreement with Model 1 except for the narrow-line features at low energies. These two versions show larger differences at higher density. The dips present at low energies for models with ﹩\mathrm{log}(\xi /﹩ erg cm s −1) = 1 or 2 are due to the extremely large opacity at those energies, which prevents the radiative transfer solution from fully converging. Model 1 for n = 1021 cm−3 is not shown because that code cannot properly iterate, due to the incorrect calcium cross sections.
Paper: Next-generation Accretion Disk Reflection Model: High-density Plasma Effects
Authors: Yuanze Ding, Javier A. Garcıa, Timothy R. Kallman, Claudio Mendoza, Manuel Bautista, Fiona A. Harrison, John A. Tomsick, Jameson Dong
Figure caption: Simulated observations (blue data points), best-fit model (green, power-law + reflection components), injected reflection spectra (cyan, reflection only) and fitted reflection spectra (red, reflection only). Data points are generated by convolving injected spectra (composed of the cyan reflection curve and an unshown power law, assuming photon index Γ = 1.5) with instrumental response from XMM-Newton and NuSTAR. Injected spectra refer to the model spectra we assumed when generating the simulated data points. The simulated spectra are fitted with publicly available XILLVER in RELXILL version 2.3. ξ is the same for each row, while densities are the same for each column. Key parameters assumed for each simulation group are shown in the first column and above the first row. This figure illustrates how differently the models describe the same data. In reality, we never know the true reflection curve in astrophysical sources. Here we can consider the cyan curve as the true value for the reflection component.
Paper: Next-generation Accretion Disk Reflection Model: High-density Plasma Effects
Authors: Yuanze Ding, Javier A. Garcıa, Timothy R. Kallman, Claudio Mendoza, Manuel Bautista, Fiona A. Harrison, John A. Tomsick, Jameson Dong
Figure caption: Comparison of various modifications made to the XSTAR routines when including their updated version in the XILLVER code (i.e., Model 2). In Model 2, REX is turned off (which was on in Model 1), while implementing stimulated recombination. The impact of REX is tested through the comparison between Models 2 and 3. Though REX has a relatively large effect on the spectra, we find that in a high-density setting none of these modifications alone can account for the largest deviations from Model 1 (see Table 1 for differences between models).
Paper: Next-generation Accretion Disk Reflection Model: High-density Plasma Effects
Authors: Yuanze Ding, Javier A. Garcıa, Timothy R. Kallman, Claudio Mendoza, Manuel Bautista, Fiona A. Harrison, John A. Tomsick, Jameson Dong
Figure caption: Temperature profiles of the illuminated slab as a function of the Thomson optical depth (τ T). Model 2 (using XILLVER 3.5) in the high-density regime generally produces a lower-temperature solution. Model 1 (using XILLVER 3.4b) cannot iterate correctly when n > 1020 cm−3, which is due to the erroneous calcium cross sections.
Paper: Next-generation Accretion Disk Reflection Model: High-density Plasma Effects
Authors: Yuanze Ding, Javier A. Garcıa, Timothy R. Kallman, Claudio Mendoza, Manuel Bautista, Fiona A. Harrison, John A. Tomsick, Jameson Dong
Figure caption: Differences between Models 1, 2, and 5. In Models 1 and 5, the calcium photoionization cross sections are not corrected. The deviation in 10–20 keV almost disappears after correcting the cross-section issue. The Fe K line complex shown in the zoom-in panel is similar between Models 2 and 5 (notably the line ratio and flux), indicating that the calcium cross-section issue did not significantly affect the ionization solution.
Paper: Toward Accelerated Nuclear-physics Parameter Estimation from Binary Neutron Star Mergers: Emulators for the Tolman–Oppenheimer–Volkoff Equations
Authors: Brendan T. Reed, Rahul Somasundaram, Soumi De, Cassandra L. Armstrong, Pablo Giuliani, Collin Capano, Duncan A. Brown, Ingo Tews
Figure caption: PDFs on two EOS model parameters, computed using the five-parameter model, for a fictitious high-precision measurement of the tidal deformability of a 1.4 M ⊙ NS described in the text. The PDFs for all emulators match well with that obtained using the full TOV solver (black circles).
Paper: Toward Accelerated Nuclear-physics Parameter Estimation from Binary Neutron Star Mergers: Emulators for the Tolman–Oppenheimer–Volkoff Equations
Authors: Brendan T. Reed, Rahul Somasundaram, Soumi De, Cassandra L. Armstrong, Pablo Giuliani, Collin Capano, Duncan A. Brown, Ingo Tews
Figure caption: Same as Figure 6 but for the ten-parameter model.
Paper: Toward Accelerated Nuclear-physics Parameter Estimation from Binary Neutron Star Mergers: Emulators for the Tolman–Oppenheimer–Volkoff Equations
Authors: Brendan T. Reed, Rahul Somasundaram, Soumi De, Cassandra L. Armstrong, Pablo Giuliani, Collin Capano, Duncan A. Brown, Ingo Tews
Figure caption: Same as Figure 6 but for the five-parameter model.
Paper: Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses
Authors: Stephanie LaMassa, Alessandro Peca, C. Megan Urry, Eilat Glikman, Tonima Tasnim Ananna, Connor Auge, Francesca Civano, Aritra Ghosh, Allison Kirkpatrick, Michael J. Koss, Meredith Powell, Mara Salvato, Benny Trakhtenbrot
Figure caption: Rest-frame, nonabsorption-corrected 2–10 keV X-ray luminosity as a function of redshift for all spectroscopically identified AGN from Stripe 82 XMM-AO10 and XMM-AO13 at r < 22. At these X-ray and optical flux limits, the Stripe 82X survey is 90% spectroscopically complete. (Left) Since Stripe 82X is a shallow, wide-area survey, it largely samples the high X-ray luminosity AGN parameter space. The obscured AGN (Type 2 AGN, reddened AGN, and X-ray obscured AGN; red stars) are predominantly at lower X-ray luminosities and redshifts and make up the majority of low X-ray luminosity (L X < 1043 erg s−1) Stripe 82X AGN (see also Table 3). (Right) Of the obscured AGN population, the Type 2 AGN (green circles) are at the lowest X-ray luminosities and redshifts. The X-ray obscured AGN (where N H > 1022 cm−2; purple squares) extend to high X-ray luminosities (L X > 1044.5 erg s−1) and high redshifts (z > 1). The reddened AGN (red crosses) are found at moderate-to-high X-ray luminosities, overlapping the tail of the Type 2 AGN L − z distribution. There is some overlap in these subpopulations of obscured AGN (see Figure 2) (Bottom) X-ray luminosity–redshift distribution for AGN that are classified as obscured based on multiple metrics (as indicated in the legend). The Type 2 + X-ray obscured AGN span a range of redshifts and X-ray luminosities, while the AGN that are reddened and also Type 2 and/or X-ray obscured are at higher X-ray luminosities (L X = 1043 erg s−1) and mostly above z > 0.5, but they do not extend to as high redshift or X-ray luminosity as the AGN that are only X-ray obscured.
Paper: Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses
Authors: Stephanie LaMassa, Alessandro Peca, C. Megan Urry, Eilat Glikman, Tonima Tasnim Ananna, Connor Auge, Francesca Civano, Aritra Ghosh, Allison Kirkpatrick, Michael J. Koss, Meredith Powell, Mara Salvato, Benny Trakhtenbrot
Figure caption: (Left) Distribution of the Eddington ratio (λ Edd) for Stripe 82X AGN that have intrinsic X-ray luminosities calculated via spectral fitting (A. Peca et al. 2023). Due to the wide dispersion in black hole mass measurements from the single-epoch broad emission-line formulas, we consider separately Type 1 AGN with reference black hole mass measurements derived from the Mg II line (λ Edd, Mg II ) and those derived from the Hβ line (λ Edd,Hβ ). Most Stripe 82X Type 1 AGN are accreting at rates below 30% Eddington. (Right) Eddington ratio plotted as a function of the intrinsic X-ray luminosity (L 2−10 keV,intrinsic) demonstrating that X-ray luminous AGN (>1045 erg s−1) are associated with higher accretion rates. (Bottom) Eddington ratio as a function of redshift, showing no strong trends with cosmic time, though the sample presented here is incomplete due to multiple selection effects.
Paper: Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses
Authors: Stephanie LaMassa, Alessandro Peca, C. Megan Urry, Eilat Glikman, Tonima Tasnim Ananna, Connor Auge, Francesca Civano, Aritra Ghosh, Allison Kirkpatrick, Michael J. Koss, Meredith Powell, Mara Salvato, Benny Trakhtenbrot
Figure caption: (Left) Distribution of black hole masses for Type 1 AGN where the individual single-epoch emission-line calculations that are chosen as the reference M BH are plotted separately. The higher mass black holes are found from the Mg II- and C IV-derived black hole mass measurements. (Right) Distribution of the AGN bolometric luminosity for the various black hole mass formulations, showing that the AGN with Mg II- and C IV-derived black hole masses are associated with more luminous AGN, which are also at higher redshift (see Table 5).
Paper: Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses
Authors: Stephanie LaMassa, Alessandro Peca, C. Megan Urry, Eilat Glikman, Tonima Tasnim Ananna, Connor Auge, Francesca Civano, Aritra Ghosh, Allison Kirkpatrick, Michael J. Koss, Meredith Powell, Mara Salvato, Benny Trakhtenbrot
Figure caption: Example of spectra from our follow-up campaign with (top) Palomar DoubleSpec, (middle) Keck LRIS, and (bottom) Keck DEIMOS, illustrating both (left) Type 2 AGN and (right) Type 1 AGN. Identifying information is given in the legend of each plot, including estimated 2–10 keV luminosity and observing run in which spectrum was taken. Emission lines used to determine spectroscopic redshift are marked. Spectra from the red (blue) arm are Gaussian smoothed with a σ = 1.0 (σ = 1.5) kernel. The spectra are not telluric corrected nor do they have an absolute flux calibration applied.
Paper: Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses
Authors: Stephanie LaMassa, Alessandro Peca, C. Megan Urry, Eilat Glikman, Tonima Tasnim Ananna, Connor Auge, Francesca Civano, Aritra Ghosh, Allison Kirkpatrick, Michael J. Koss, Meredith Powell, Mara Salvato, Benny Trakhtenbrot
Figure caption: Intercomparison of black hole masses calculated from the various single-epoch emission-line formulas. We find good agreement between the Balmer-derived and Mg II-derived black hole masses, albeit with a spread of a factor of 2–3, but a significant systematic offset when comparing the Mg II-derived black hole masses with those calculated from the C IV line. See Table 6 for details.
Paper: Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses
Authors: Stephanie LaMassa, Alessandro Peca, C. Megan Urry, Eilat Glikman, Tonima Tasnim Ananna, Connor Auge, Francesca Civano, Aritra Ghosh, Allison Kirkpatrick, Michael J. Koss, Meredith Powell, Mara Salvato, Benny Trakhtenbrot
Figure caption: Redshift distribution of all Type 1 AGN in Stripe 82X with those that have black hole masses measured shown in the hatched region. The distributions are similar, indicating that our black hole mass subsample is not biased in redshift space relative to broad-line AGN in Stripe 82X.
Paper: Afterglow Linear Polarization Signatures from Shallow GRB Jets: Implications for Energetic GRBs
Authors: Gal Birenbaum, Ramandeep Gill, Omer Bromberg, Paz Beniamini, Jonathan Granot
Figure caption: An illustration of our adopted local magnetic field structure for five different values of ξ.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: The JWST MIRI/LRS data set, showing the observed phase curve (black points), the fitted ﹩{{\ell }}_{\max }=2﹩ eclipse map model (red line) shown in Figure 3, and the systematics model (blue line) fitted alongside the eclipse map.