adsabs/AstroCLIMB huggingface dataset:
Paper: High-energy Neutrino Emission Associated with GWs from Binary Black Hole Mergers in AGN Accretion Disks
Authors: Zi-Hang Zhou, Kai Wang
Figure caption: Neutrino fluences from diverse shocks at a distance of 100 Mpc. The different colors represent different shock types. Each line type represents different accretion rates, i.e., ﹩0.1{\dot{m}}_{\mathrm{BHL}}﹩ (solid), ﹩1{\dot{m}}_{\mathrm{BHL}}﹩ (dashed), to ﹩10{\dot{m}}_{\mathrm{BHL}}﹩ (dotted).
Paper: High-energy Neutrino Emission Associated with GWs from Binary Black Hole Mergers in AGN Accretion Disks
Authors: Zi-Hang Zhou, Kai Wang
Figure caption: Expected all-flavor diffuse neutrino fluence contributed from BBH mergers in AGN disks. Diverse local event rates and accretion rates are considered. Red points and upper limits are the observed diffuse neutrino fluence by IceCube (Aartsen et al. 2015, 2021a). The gray lines are 90% upper limit of the cosmogenic neutrino for diverse instruments.
Paper: A Self-interacting Dark Matter Solution to the Extreme Diversity of Low-mass Halo Properties
Authors: Ethan O. Nadler, Daneng Yang, Hai-Bo Yu
Figure caption: Left panel: projected logarithmic density profile slope, averaged from 0.75 to 1.25 kpc, vs. enclosed projected mass within 1 kpc for all subhalos of the group-mass host with ﹩{V}_{\max }\gt 30\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩ in our CDM (black) and SIDM (blue) simulations; isolated halos are shown by small unfilled points. The corresponding properties and 1σ uncertainties for the SDSSJ0946+1006 perturber derived in M21 are shown for a truncated NFW profile (tNFW; magenta) and when including higher-order multipoles in the lens model (tNFWmult; cyan). Right panel: density profiles of subhalos with ﹩{V}_{\max }\gt 30\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩ in CDM (black) and SIDM (blue). Lines become dotted when fewer than 1000 particles are enclosed; the vertical dashed line shows a resolution limit of 2.8ϵ = 680 pc. Dashed magenta (cyan) lines show best-fit tNFW (tNFWmult) profiles from M21 for the observed perturber. The SIDM halo closest to the tNFW (tNFWmult) perturber is circled in magenta (cyan) in the left panel and shown by the solid magenta (cyan) line in the right panel; Appendix B shows that the magenta density profile is measured smoothly.
Paper: A Self-interacting Dark Matter Solution to the Extreme Diversity of Low-mass Halo Properties
Authors: Ethan O. Nadler, Daneng Yang, Hai-Bo Yu
Figure caption: Left panel: circular velocity evaluated at 2 kpc vs. maximum circular velocity for seven isolated UDGs studied in K22, with means and 1σ uncertainties shown for AGC 114905 (red), 122966 (green), 219523 (blue), 248945 (orange), 334315 (magenta), 749290 (brown), and 242019 (black). Black (blue) points show the same quantities for isolated halos throughout the 6 Mpc high-resolution region of our CDM (SIDM) simulation. Only halos resolved with more than 2000 particles at z = 0 are shown; the dashed line shows the one-to-one relation. Right panel: density profiles of isolated halos with ﹩30\,\mathrm{km}\,{{\rm{s}}}^{-1}\lt {V}_{\max }\lt 50\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩ and M 200 > 5.5 × 109 M ⊙ in our CDM (black) and SIDM (blue) simulations. Lines become dotted when fewer than 1000 particles are enclosed. Dashed lines show best-fit Read et al. (2016) density profiles from K22 for each observed UDG.
Paper: A Self-interacting Dark Matter Solution to the Extreme Diversity of Low-mass Halo Properties
Authors: Ethan O. Nadler, Daneng Yang, Hai-Bo Yu
Figure caption: The effective DM self-interaction cross section (main panel) and viscosity cross section (inset) for our Group SIDM model (red), and for the SIDM models from Yang et al. (2023a, purple) and Kaplinghat et al. (2016, black). Vertical dotted lines show the approximate velocity scales of the UDGs and strong-lens perturber.
Paper: A Self-interacting Dark Matter Solution to the Extreme Diversity of Low-mass Halo Properties
Authors: Ethan O. Nadler, Daneng Yang, Hai-Bo Yu
Figure caption: The 3D density profile (left), surface density (middle), and project density slope profile for the tNFW strong-lensing perturber analog from our SIDM simulation, corresponding to the magenta halo in Figure 2.
Paper: A Self-interacting Dark Matter Solution to the Extreme Diversity of Low-mass Halo Properties
Authors: Ethan O. Nadler, Daneng Yang, Hai-Bo Yu
Figure caption: Top panel: the exact viscosity cross section for our Group SIDM model Equation (A1) (red line) and the fitting function implemented in our simulation Equation (A2) (unfilled red circles). Bottom panel: ratio of the fitting function to the exact viscosity cross section, illustrating that they agree at the percent level.
Paper: The Importance of the Upper Atmosphere to CO/O2 Runaway on Habitable Planets Orbiting Low-mass Stars
Authors: Sukrit Ranjan, Edward W. Schwieterman, Michaela Leung, Chester E. Harman, Renyu Hu
Figure caption: Non-resolution of the CO2 photolysis peak drives CO/O2 runaway. Concentrations of key atmospheric species (left column) and CO2 and H2O photolysis rates (right column) as a function of altitude, for pCO2 = 0.01, 0.03, and 0.1 bar, CHO chemistry only (S, N excluded). The key photochemical products CO and O2 are highlighted with thicker lines in the left column. “Dry pressure” refers to the atmospheric pressure due to CO2 and N2, excluding the contribution from water vapor. Solid lines correspond to calculations with the model top at 0.34 μbar, while dashed lines correspond to calculations with a higher 100 km model top. At 0.01 bar, the photolysis peak is resolved by both models, and they report identical results. As pCO2 increases, the CO2 photodissociation peak moves upward and is not resolved by the calculations with the 0.34 μbar model top, resulting in large increases in pCO and especially pO2.
Paper: The Importance of the Upper Atmosphere to CO/O2 Runaway on Habitable Planets Orbiting Low-mass Stars
Authors: Sukrit Ranjan, Edward W. Schwieterman, Michaela Leung, Chester E. Harman, Renyu Hu
Figure caption: Vertically resolved reaction rates of key OH-producing (left column) and radical-radical (right column) reactions, for both truncated (solid lines) and extended (dashed lines) model atmospheres. The top row shows pCO2 = 0.01 bar, for which both model tops return the same results, while the bottom shows pCO2 = 0.1 bar, for which CO/O2 runaway has begun in the truncated model top (but for which an NUV-attenuating ozone layer has not yet formed). CHO chemistry only (S, N excluded). The key reaction O + O + M→O2+M in the right column is highlighted with a thicker line. The concentration of O production in a single model bin in the truncated atmosphere leads to more intense O–O reactions, which are chain termination reactions that remove radicals from the atmosphere and impede the radical-driven recombination of CO and O2.
Paper: The Importance of the Upper Atmosphere to CO/O2 Runaway on Habitable Planets Orbiting Low-mass Stars
Authors: Sukrit Ranjan, Edward W. Schwieterman, Michaela Leung, Chester E. Harman, Renyu Hu
Figure caption: A closer look at the mechanics of CO/O2 runaway. Change in column-integrated mixing ratio of key species (top) and column-integrated reaction rates for main radical species (middle) and main OH-producing reactions (bottom) as a function of pCO2, relative to pCO2 = 0.01 for which both truncated (solid lines) and extended (dashed lines) model calculations produce the same result. Suppression in OH concentrations, likely due to suppression of OH production pathways, underlies CO/O2 runaway.
Paper: The Importance of the Upper Atmosphere to CO/O2 Runaway on Habitable Planets Orbiting Low-mass Stars
Authors: Sukrit Ranjan, Edward W. Schwieterman, Michaela Leung, Chester E. Harman, Renyu Hu
Figure caption: Simulated transmission spectra of an Earth-sized planet orbiting a late M dwarf star with a CO2-dominated atmosphere in and out of CO/O2 runaway, corresponding to Runs 4 and 5 of Table 1. Key molecular absorption features that differ between the runaway/non-runaway cases are highlighted. Runaway spectral features are as strong as 50 ppm and the runaway/non-runaway spectra differ by 10 s of ppm, which is potentially detectable with JWST.
Paper: The Importance of the Upper Atmosphere to CO/O2 Runaway on Habitable Planets Orbiting Low-mass Stars
Authors: Sukrit Ranjan, Edward W. Schwieterman, Michaela Leung, Chester E. Harman, Renyu Hu
Figure caption: Top: top-of-atmosphere (TOA) number flux from the Sun and TRAPPIST-1 (left y-axis). Also co-plotted are the photolysis cross sections of CO2 (right abscissa). Bottom: CO2 cross sections weighted by the stellar emission of TRAPPIST-1 and the Sun. The bluer spectrum of TRAPPIST-1 increases the weight of shortwave ﹩{\sigma }_{{{\rm{CO}}}_{2}}﹩, which is larger, driving an increase in ﹩\overline{{\sigma }_{\mathrm{UV},{\rm{g}}}}﹩.
Paper: The Importance of the Upper Atmosphere to CO/O2 Runaway on Habitable Planets Orbiting Low-mass Stars
Authors: Sukrit Ranjan, Edward W. Schwieterman, Michaela Leung, Chester E. Harman, Renyu Hu
Figure caption: TRAPPIST-1 spectra employed by MEAC and Atmos in this study.
Paper: The Gas Accretion Rate of Galaxies over z ≈ 0–1.3
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The two panels show the redshift-averaged SFR (R SF, in blue), molecular gas formation rate (R Mol, in orange), and net gas accretion rate (R Acc, in green) of main-sequence galaxies, as a function of the final stellar mass, over (A) z = 1.3 to z = 1.0 and (B) z = 1.0 to z = 0. The shaded regions around each curve show the 68% confidence intervals. The top x-axis of panel (A) shows the initial stellar mass of the galaxies at z = 1.3, while the bottom x-axis shows the final stellar mass at z = 1.0. This final stellar mass at z = 1.0 is plotted as the top x-axis of panel (B), with the bottom axis of the panel showing the final stellar mass of the galaxies at z = 0. The evolution of the stellar masses was obtained using Equation (1). Panel (A) shows that the redshift-averaged molecular gas formation rate, and SFR are similar for all but the most massive galaxies over the interval z = 1.3 to z = 1.0, but the average net gas accretion rate over the same period is much lower than the other two rates. Panel (B) shows that both the average molecular gas formation rate and the average net gas accretion rate are lower than the average SFR for the lower-redshift interval, z = 1.0 to z = 0, for galaxies of all stellar masses. See main text for discussion.
Paper: The Gas Accretion Rate of Galaxies over z ≈ 0–1.3
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The panels show (in blue), as a function of stellar mass, (A) the SFR (Section 2.2), (B) the molecular gas mass (Section 2.3), and (C) the atomic gas mass (Section 2.4) for main-sequence galaxies at z ≈ 0, z ≈ 1.0 and z ≈ 1.3. The red curve in panel (A) shows the evolutionary track of a galaxy with M * = 1010 M ⊙ at z ≈ 1.3 obtained using Equation (1). The corresponding evolution of the molecular gas mass of the galaxy, obtained using Equations (1) and (9), is shown in panel (B). Finally, the red points in panel (C) show the atomic gas mass of the galaxy at the three redshifts, obtained using Equation (14). Note that the M Atom–M * relation of Equation (14) is not a continuous function of redshift; the dashed line in the panel is hence only for visual aid, showing a linear interpolation between the points. See main text for discussion.
Paper: The Gas Accretion Rate of Galaxies over z ≈ 0–1.3
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The ratio of the baryonic mass of main-sequence galaxies at z ≈ 1.3 to that at z = 0, as a function of their final stellar mass at z ≈ 0 (the initial stellar mass of the galaxies, at z ≈ 1.3, is shown on the top axis). The black dot indicates the position on the relation of a galaxy with the stellar mass of the Milky Way today. The dashed horizontal line is at a ratio of 1, indicating no change in the baryonic mass between z = 1.3 and z = 0. It is clear that the highest-mass (M * ≳ 1010.5 M ⊙ at z ≈ 1.3) galaxies had the bulk of their baryonic mass in place by z ≈ 1.3; the baryonic mass of these galaxies has declined over the past ≈9 Gyr. Conversely, the baryonic mass of galaxies with stellar mass M * ≲ 1010 M ⊙ at z ≈ 1.3 has increased since z ≈ 1.3 by approximately 30% for galaxies with M * ≈ 109 M ⊙ at z ≈ 1.3.
Paper: Influence of Intermittency on the Energy Transfer Rate of Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: Dependence on θ RB of the averaged energy transfer rate for the original (black, 〈ϵ 〉 ) and conditioned (red, 〈ϵ  c  〉 ) fluctuations and the ratio (blue, 〈ϵ  c  〉 / 〈 ϵ 〉 ).
Paper: Influence of Intermittency on the Energy Transfer Rate of Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: Energy transfer rate of the original (left) and conditioned (right) fluctuations for the magnetic field as a function of τ measured in different ranges of θ RB with the color shown in the color bar.
Paper: RNO 54: A Previously Unappreciated FU Ori Star
Authors: Lynne A. Hillenbrand, Adolfo Carvalho, Jan van Roestel, Kishalay De
Figure caption: Portions of the optical spectrum of RNO 54 (magenta) compared to the recent FU Ori outburst sources Gaia 18dvy (blue) and Gaia 17bpi (orange), as well as to a non-outbursting but heavily accreting classical T Tauri star, BP Tau (green). Spectra have been normalized and offset, for clarity. The lower three objects are similar in terms of their line presence, depth, and width, exhibiting absorption from a mix of low-excitation and higher-excitation neutral and ionized species. The top spectrum, by contrast, is less complicated and while similar to the FU Ori objects over small spectral ranges, has fewer high-excitation lines, somewhat deeper lines, and much narrower lines.
Paper: Influence of Intermittency on the Energy Transfer Rate of Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: Left: scaling exponents ξ of the original (colors in viridis map denote θ RB) and conditioned (red) structure functions for the magnetic field as a function of the order p measured in different ranges of θ RB. The green (blue) dashed lines denote the predictions of the log-Poisson intermittency model with C = 1 (C = 2) but different g. Right: dependence of g on θ RB for the original (viridis colors) and conditioned (red) scaling exponents. The error bar shows the standard errors. The blue dashed line corresponds to g = 2.44. The black dashed line corresponds to g = 3 and g = 4.
Paper: RNO 54: A Previously Unappreciated FU Ori Star
Authors: Lynne A. Hillenbrand, Adolfo Carvalho, Jan van Roestel, Kishalay De
Figure caption: Infrared spectrum of RNO 54 compared to that of V960 Mon. The two sources do not have similar continuum shapes, with V960 Mon artificially adjusted to attempt to match the reddening of RNO 54. However, both sources have absorption features from a mix of molecules (TiO, VO, H2O, CO; red), low-excitation (Mg I, Ca I, Al I), and higher-excitation (Si I, S I, C I, Ca II) neutral and ionized species (black), as well as the Sr II, CN, and Si I indicators of low surface gravity (orange). In addition, both sources show broad blueshifted absorption in the He I 10830 line (see inset for RNO 54), indicating a strong wind.
Paper: RNO 54: A Previously Unappreciated FU Ori Star
Authors: Lynne A. Hillenbrand, Adolfo Carvalho, Jan van Roestel, Kishalay De
Figure caption: Optical spectrum of RNO 54 (magenta) compared to the FU Ori objects HBC 722 (PTF 10qpf), V1057 Cyg, and V1515 Cyg, and to the continuum-plus-emission objects V1331 Cyg and V2492 Cyg (PTF 10nvg). RNO 54 has an absorption spectrum similar to the broad-line FU Ori stars V1057 Cyg and HBC 722 (PTF 10qpf); V1515 Cyg has narrower and deeper lines than the others, due to its nearly face-on inclination. RNO 54 thus appears to be an extreme accretor, and does not have the emission line spectrum of mere atypically high accretion rate sources.
Paper: Influence of Intermittency on the Energy Transfer Rate of Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: Top: magnetic-trace structure functions vs. timescale τ measured in the direction parallel to the local magnetic field. (a) Original S  p ; (b) conditioned S  c   p  with the intermittency removed. The blue, orange, green, red, and purple represent the S  p  with order p = 1, 2, 3, 4, 5, respectively. The blue shadow denotes the range within which the scaling exponents are obtained by fitting. Bottom: magnetic-trace structure functions vs. timescale τ measured in the direction perpendicular to the local magnetic field, with the same formats as the top panels.
Paper: RNO 54: A Previously Unappreciated FU Ori Star
Authors: Lynne A. Hillenbrand, Adolfo Carvalho, Jan van Roestel, Kishalay De
Figure caption: Left: assembled photometric SED (blue points), spectrophotometry from SpeX (black line), and accretion disk model fit (red line). Right: “corner plot” showing the physical parameters in the model; red lines mark median values while blue lines are modal values. The gas disk model is appropriate over the optical and near-infrared wavelength range, where accretion dominates the emission. Beginning in the mid-infrared, dust contributions from an inactive or passive disk become important, while in the far-infrared dust emission from an envelope dominates; these cooler contributions to the SED are not part of our modeling effort.
Paper: RNO 54: A Previously Unappreciated FU Ori Star
Authors: Lynne A. Hillenbrand, Adolfo Carvalho, Jan van Roestel, Kishalay De
Figure caption: Segments of the optical spectrum of RNO 54 emphasizing lines showing wind signatures, including the K I 7669,7699 Å doublet, the O I 7773 Å triplet, the deep Na I D doublet, the Mg Ib doublet, Hα, and the Ca II triplet. The Li I 6707 Å signature of stellar youth is also highlighted, showing line splitting consistent with a disk profile, similar to Ca I 6717 Å.
Paper: Elusive Iron: Detection of the FeC Radical (X 3Δ i ) in the Envelope of IRC+10216
Authors: L. A. Koelemay, L. M. Ziurys
Figure caption: Rotational transitions of FeC (X 3Δ i ) observed toward IRC+10216 using the ARO 12 m and SMT at 2 and 1 mm, respectively. Each spectrum has a spectral resolution of 3 km s−1, smoothed from 1.2 km s−1 (0.625 MHz) at 160 GHz, and 1.2–1.5 km s−1 (1 MHz) at 201–241 GHz. The temperature scale is ﹩{T}_{A}^{* }﹩(mK). The figure shows the J = 4 → 3 transition near 160 GHz (upper panel), J = 5 → 4 line near 201 GHz (middle panel), and the J = 6 → 5 transition near 241 GHz (lower panel), each marked by red (or gray scale) arrows. The inset in each panel shows enlarged versions of each line, with the ESCAPADE-derived fits superimposed (red or gray scale). Integration times are 52, 72, and 91 hr at 160, 201, and 241 GHz, respectively.
Paper: Elusive Iron: Detection of the FeC Radical (X 3Δ i ) in the Envelope of IRC+10216
Authors: L. A. Koelemay, L. M. Ziurys
Figure caption: Qualitative energy level diagram of the FeC radical in its ground electronic state (X 3Δ i ). This electronic state consists of three spin ladders, denoted by the quantum number Ω, where J ≥ Ω, and J defines the total angular momentum excluding nuclear spin. The rotational transitions J + 1 → J in the lowest spin ladder of FeC, Ω = 3, observed in this work toward the circumstellar envelope of IRC+10216, are highlighted by red (or gray scale) arrows. The other spin–orbit ladders Ω = 2 and 1 lie higher in energy by ∼360 and ∼720 K.
Paper: Constraining the AGN Luminosity Function from JWST with the X-Ray Background
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: Unresolved X-ray background constraints (EI XRB) as a function of rest energy E from fitting to the Swift XRT and Chandra observations by Moretti et al. (2012, red dashed line), with the red shaded region showing the unresolved XRB measurement uncertainty. Overplotted is the expected X-ray background from the measured JWST UV LFs (black solid line and associated gray region), and that from enhancing the UV emissivities in Shen et al. (2020) by factors of 2×, 5×, and 10× (blue dashed, blue dashed-dotted, and blue dotted lines) over the z ∼ 4–7 interval.
Paper: Elusive Iron: Detection of the FeC Radical (X 3Δ i ) in the Envelope of IRC+10216
Authors: L. A. Koelemay, L. M. Ziurys
Figure caption: Radial abundance profiles for FeC (blue, dashed) and FeCN (red, dots) within the envelope of IRC+10216, derived from the model fitting, plotted as a function of distance from the star (in cm or R *). The abundances are shown in log scale. The black solid line marks a radius of 1000 R *. The FeC distribution is closer to the star than that of FeCN, with some overlap, suggesting the cyanide forms from the carbide through photochemistry.
Paper: Constraining the AGN Luminosity Function from JWST with the X-Ray Background
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: The UV emissivity at 912 Å (black jagged line) from the results of JWST (Harikane et al. 2023) compared to the fitting form of Shen et al. (2020, blue solid line). The dashed, dashed-dotted, and dotted blue lines show the results of hiking the Shen et al. (2020) emissivity by factors of 2×, 5×, and 10× respectively. The red dashed horizontal line denotes the constant value of comoving emissivity required (Haardt & Salvaterra 2015) to saturate the unresolved X-ray background measured by Moretti et al. (2012).
Paper: Constraining the AGN Luminosity Function from JWST with the X-Ray Background
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: Top panel: value of the Cressie–Read χ 2 statistic for the cases of multiplication of the emissivity at 912 Å constrained by Shen et al. (2020) by factors of 2×, 5×, and 10× respectively, compared to that measured by the JWST results (Harikane et al. 2023). Lower panel: the two-dimensional KS statistic (d-value), a measure of the deviation between the X-ray background data (Moretti et al. 2012) and that predicted by the Shen et al. (2020) model multiplied by the same factors (higher value indicates larger deviation). As the multiplicative factor increases, the fit to the JWST ϵ 912 becomes progressively better, with that to the XRB data becoming simultaneously worse.
Paper: Constraining the AGN Luminosity Function from JWST with the X-Ray Background
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: The UV LF at 1450 Å at z ∼ 5 from the results of JWST spectroscopic surveys (Harikane et al. 2023) and the UNCOVER survey (Greene et al. 2023), as compared to the fitting form of Shen et al. (2020) matched to previous AGN data.
Paper: The Importance of the Upper Atmosphere to CO/O2 Runaway on Habitable Planets Orbiting Low-mass Stars
Authors: Sukrit Ranjan, Edward W. Schwieterman, Michaela Leung, Chester E. Harman, Renyu Hu
Figure caption:  T–P and Eddy diffusion profiles employed by MEAC and Atmos in this study.
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: MWL light curve of 5BZB J0630−2406 from γ-rays 						and X-rays to the optical band. The top panel shows the γ-ray light curve with 1 yr binning, available from the 						4FGL-DR4 catalog. The second panel displays the measurements from Swift-XRT, 						XMM-Newton, and NuSTAR used for the modeling. The third panel shows the 						values taken by Swift-UVOT in the three optical filters V, B, and U. The fourth panel shows the V-band and g-band data collected by 						ASAS-SN, and the bottom panel shows the KAIT Clear-band measurement, the SMARTS R band, and the ZTF r band and 							g band. The X-ray and optical light curves 						are corrected for galactic extinction. The orange line highlights the time 						of the quasi-simultaneous data used in the SED analysis. GROND data also 						used for modeling but not included in this panel are discussed in Section 							3.2.