adsabs/AstroCLIMB huggingface dataset:
Paper: AT2025ulz and S250818k: Deep X-Ray and Radio Limits on Off-axis Afterglow Emission and Prospects for Future Discovery
Authors: Brendan O'Connor, Roberto Ricci, Eleonora Troja, Antonella Palmese, Yu-Han Yang, Geoffrey Ryan, Hendrik van Eerten, Muskan Yadav, Xander J. Hall, Ariel Amsellem, R. L. Becerra, Malte Busmann, Tomás Cabrera, Simone Dichiara, Lei Hu, Ravjit Kaur, Keerthi Kunnumkai, Ignacio Magaña Hernandez
Figure caption: The maximum detectable distance of a GW170817-like afterglow (G. Ryan et al. 2024) versus the viewing angle θv/θc using our deep X-ray and radio limits. The distance of GW170817 (40 Mpc) and AT2025ulz (400 Mpc) are shown for reference as dashed horizontal lines. A dashed vertical line marks the viewing angle of GW170817 (G. Ryan et al. 2024). The afterglow parameters used to generate the lightcurves are the same as those shown in the caption of Figure 2.
Paper: AT2025ulz and S250818k: Deep X-Ray and Radio Limits on Off-axis Afterglow Emission and Prospects for Future Discovery
Authors: Brendan O'Connor, Roberto Ricci, Eleonora Troja, Antonella Palmese, Yu-Han Yang, Geoffrey Ryan, Hendrik van Eerten, Muskan Yadav, Xander J. Hall, Ariel Amsellem, R. L. Becerra, Malte Busmann, Tomás Cabrera, Simone Dichiara, Lei Hu, Ravjit Kaur, Keerthi Kunnumkai, Ignacio Magaña Hernandez
Figure caption: Optical lightcurve (g band) of AT2025ulz out to 25 days from discovery compared to an off-axis afterglow model. Optical data from FTW 3KK and Gemini GMOS are reproduced from X. J. Hall et al. (2025c). X-ray (black) and radio (gray) upper limits from this work are shown (Tables 1 and 2 in Appendix A) and rule out that the optical rebrightening is due to an off-axis afterglow.
Paper: AT2025ulz and S250818k: Deep X-Ray and Radio Limits on Off-axis Afterglow Emission and Prospects for Future Discovery
Authors: Brendan O'Connor, Roberto Ricci, Eleonora Troja, Antonella Palmese, Yu-Han Yang, Geoffrey Ryan, Hendrik van Eerten, Muskan Yadav, Xander J. Hall, Ariel Amsellem, R. L. Becerra, Malte Busmann, Tomás Cabrera, Simone Dichiara, Lei Hu, Ravjit Kaur, Keerthi Kunnumkai, Ignacio Magaña Hernandez
Figure caption: Same as Figure 4 but for a wider jet θc = 0.1 rad. For wider jets, we are less constraining on the other jet parameters.
Paper: AT2025ulz and S250818k: Deep X-Ray and Radio Limits on Off-axis Afterglow Emission and Prospects for Future Discovery
Authors: Brendan O'Connor, Roberto Ricci, Eleonora Troja, Antonella Palmese, Yu-Han Yang, Geoffrey Ryan, Hendrik van Eerten, Muskan Yadav, Xander J. Hall, Ariel Amsellem, R. L. Becerra, Malte Busmann, Tomás Cabrera, Simone Dichiara, Lei Hu, Ravjit Kaur, Keerthi Kunnumkai, Ignacio Magaña Hernandez
Figure caption: Same as Figure 4 but for p = 2.6.
Paper: The JWST Rocky Worlds DDT Program Reveals GJ 3929b to Likely Be a Bare Rock
Authors: Qiao Xue, Michael Zhang, Brandon Park Coy, Madison Brady, Xuan Ji, Jacob L. Bean, Michael Radica, Andreas Seifahrt, Julian Stürmer, Rafael Luque, Ritvik Basant, Nina Brown, Tanya Das, David Kasper, Caroline Piaulet-Ghorayeb, Eliza M.-R. Kempton, Edwin Kite
Figure caption: (a) Phase-folded RV measurements from MAROON-X, CARMENES, HPF, and NEID used in our joint fit, overplotted with the best-fit eccentric orbit model with rotation GP. (b) GJ 3929b in the mass–radius diagram with Rp and Mp from the joint fit (see Section 2). With the new MAROON-X data, we are able to improve the mass precision by a factor of 3.5. We compare the planet’s mass and radius to various interior composition models from L. Zeng et al. (2019) as well as steam atmosphere models with 1% and 5% water from M. Turbet et al. (2020). GJ 3929b is most consistent with a purely rocky or Earth-like composition (32.5% Fe + 67.5% MgSiO3). The gray points are all the other rocky planets with emission measurements from JWST. (c) and (d) Median and ±1σ uncertainty of the measured secondary eclipse time for each individual visit compared to the predicted T﹩{}_{{\rm{\sec }}}﹩ from our joint RV and transit fit. The prediction is T = T﹩{}_{0}+\tfrac{P}{2}(1+\tfrac{4}{\pi }e\cos \omega )+NP+\tfrac{2a}{c}﹩, where T0, P, e, and ω are drawn from the joint-fit chains, N is the number of epochs between the reference epoch T0 and the JWST observation, and ﹩\frac{2a}{c}﹩ accounts for the light travel time. The circular orbit predictions are obtained by fixing e to 0. The covariance between T0 and P is fully propagated by sampling directly from the joint-fit MCMC chains. The x-axis shows the full observation window, with the shaded region indicating the part excluded from the fitting.
Paper: The JWST Rocky Worlds DDT Program Reveals GJ 3929b to Likely Be a Bare Rock
Authors: Qiao Xue, Michael Zhang, Brandon Park Coy, Madison Brady, Xuan Ji, Jacob L. Bean, Michael Radica, Andreas Seifahrt, Julian Stürmer, Rafael Luque, Ritvik Basant, Nina Brown, Tanya Das, David Kasper, Caroline Piaulet-Ghorayeb, Eliza M.-R. Kempton, Edwin Kite
Figure caption: Planetary dayside temperature of GJ 3929b as a function of effective albedo at 15 μm and heat redistribution efficiency compared to estimated values for solar system bodies. For airless Mercury and Moon, we adopted the Bond albedo from A. Mallama (2017) and G. Matthews (2008), as their Aeff,15 μm. For Mars, Earth, and Venus, since their atmospheres contain CO2, we compute Aeff,15 μm from the modeled brightness temperature spectra of Venus and Earth (E. Miller-Ricci et al. 2009, their Figure 1) and from the observed Mars spectrum (G. Tinetti et al. 2013, their Figure 23), averaging over the MIRI/F1500W bandpass using the filter throughput. Aeff,15 μm is then solved using ﹩{T}_{p,15\,\mu {\rm{m}}}=\tfrac{{T}_{\mathrm{eff}}}{\sqrt{a/{R}_{\star }}}{(1-{A}_{\mathrm{eff},15\,\mu {\rm{m}}})}^{1/4}{\left(\tfrac{2}{3}-\tfrac{5}{12}\epsilon \right)}^{1/4}﹩, where the heat redistribution efficiency ϵ is estimated from the equator–pole temperature contrast, following Q. Xue et al. (2024, their Figure 4), since these planets are not tidally locked. We plot the lower 1σ to 4σ values of the inferred planet dayside temperature (Tp) of GJ 3929b for better visualization. The median Tp lies (slightly) above ﹩{T}_{{\rm{day}},{\rm{\max }}}﹩ and therefore falls outside the plotted range, but its value is indicated on the color bar.
Paper: The JWST Rocky Worlds DDT Program Reveals GJ 3929b to Likely Be a Bare Rock
Authors: Qiao Xue, Michael Zhang, Brandon Park Coy, Madison Brady, Xuan Ji, Jacob L. Bean, Michael Radica, Andreas Seifahrt, Julian Stürmer, Rafael Luque, Ritvik Basant, Nina Brown, Tanya Das, David Kasper, Caroline Piaulet-Ghorayeb, Eliza M.-R. Kempton, Edwin Kite
Figure caption: Left: select HELIOS emission spectra for different atmospheric scenarios. The shaded regions indicate 1σ uncertainties due to the planet-to-star-radius ratio Rp/R⋆. The black point represents our joint-fit eclipse depth, whereas the red error bars show the individual visits (Table 1). The triangles represent the F1500W bandpass-integrated model eclipse depths. Right: HELIOS-derived temperature–pressure profile for each atmospheric scenario, with individual atmospheric layers indicated by the horizontal lines. The disk-averaged surface temperatures for bare-rock surfaces are indicated by triangles. SO2 acts as extreme greenhouse gases, efficiently warming the lower atmosphere to high temperatures. Our results rule out a variety of CO2-rich atmospheres thicker than 100 mbar.
Paper: The JWST Rocky Worlds DDT Program Reveals GJ 3929b to Likely Be a Bare Rock
Authors: Qiao Xue, Michael Zhang, Brandon Park Coy, Madison Brady, Xuan Ji, Jacob L. Bean, Michael Radica, Andreas Seifahrt, Julian Stürmer, Rafael Luque, Ritvik Basant, Nina Brown, Tanya Das, David Kasper, Caroline Piaulet-Ghorayeb, Eliza M.-R. Kempton, Edwin Kite
Figure caption: GJ 3929b in the context of the cosmic shoreline. The blue line represents the original XUV-driven shoreline proposed by K. J. Zahnle & D. C. Catling (2017), with the cumulative XUV flux converted to bolometric, following their Equation (27), with a stellar mass of 0.3 M⊙. The green line is based on Equation (10) of E. K. Pass et al. (2025), using a refined cumulative XUV history and pre-main-sequence phase/flare corrections. The yellow line represents a 90% retention probability shoreline from X. Ji et al. (2025), estimated from the hydrodynamic escape of the CO2 atmosphere, assuming an initial carbon inventory of 0.1 wt% planetary mass. The planets in the comparison are the ones with JWST measurements in emission with host star masses from 0.2 to 0.4 M⊙
Paper: The JWST Rocky Worlds DDT Program Reveals GJ 3929b to Likely Be a Bare Rock
Authors: Qiao Xue, Michael Zhang, Brandon Park Coy, Madison Brady, Xuan Ji, Jacob L. Bean, Michael Radica, Andreas Seifahrt, Julian Stürmer, Rafael Luque, Ritvik Basant, Nina Brown, Tanya Das, David Kasper, Caroline Piaulet-Ghorayeb, Eliza M.-R. Kempton, Edwin Kite
Figure caption: (a) and (b) JWST light curves overplotted with the best-fit models using the parameters listed in Table 2. Data excluded from the fit are in a paler shade. To make the eclipse more easily visible, we have binned the individual integrations (pink points) with a bin width of 80 integrations (green points). (c) and (d) Phase-folded light curves with systematics divided out, overplotted with the best-fit eclipse model. Panel (d) shows the residuals relative to the best-fit model. The vertical dashed lines indicate the observed start, midpoint, and end of the eclipse.
Paper: The JWST Rocky Worlds DDT Program Reveals GJ 3929b to Likely Be a Bare Rock
Authors: Qiao Xue, Michael Zhang, Brandon Park Coy, Madison Brady, Xuan Ji, Jacob L. Bean, Michael Radica, Andreas Seifahrt, Julian Stürmer, Rafael Luque, Ritvik Basant, Nina Brown, Tanya Das, David Kasper, Caroline Piaulet-Ghorayeb, Eliza M.-R. Kempton, Edwin Kite
Figure caption: An example of ap_extract.py’s diagnostic plot, showing the MAD of light curves as a function of aperture and annulus sizes.
Paper: The Brown-dwarf Desert Persists as a Mass-ratio Desert around Low-mass Stars
Authors: Keming Zhang, 可名 张
Figure caption: Mass-ratio distribution of microlensing companions from the KMTNet (2016–2019) and MOA-II (2007–2012) survey samples, extended out to q = 0.047. The black points (left axis) show occurrence rate densities in bins of the mass ratio, shown as the posterior median and 16–84 percentile interval under a Jeffreys prior. The solid orange line represents the best power-law fit over –3.4 ﹩\lt \mathrm{log}(q)\lt ﹩ –1.75, with the shaded region indicating the 1σ confidence interval. The light shading shows extrapolation to the mass-ratio desert. The histogram (right axis) shows the number of detections in each bin.
Paper: The Brown-dwarf Desert Persists as a Mass-ratio Desert around Low-mass Stars
Authors: Keming Zhang, 可名 张
Figure caption: Cumulative number of detected microlensing companions with mass ratios smaller than each value on the horizontal axis, shown on a logarithmic scale. Events with severe degeneracies in the mass ratio are excluded from this plot. The gray shading indicates a dearth of detections between mass ratios of 0.017 < q < 0.047.
Paper: A Remote Brightening from Interactions between an Extreme-ultraviolet Jet and a Magnetic Null
Authors: Chao Zhang, Zhenghua Huang, Hengyuan Wei, Yuandeng Shen, Mijie Shi, Bo Li, Maria S. Madjarska, Xiuhui Zuo, Lidong Xia
Figure caption: (a) Time–distance plot along the blue solid line in Figure 7(a). (b) Time–distance plot along the orange solid line in Figure 7(a). The solid lines trace the bidirectional flows.
Paper: A JWST Transmission Spectrum of the Temperate Sub-Neptune TOI-732 c
Authors: Frances E. Rigby, Nikku Madhusudhan, Subhajit Sarkar, Lorenzo Pica-Ciamarra, Måns Holmberg, Julianne I. Moses
Figure caption: The posterior probability distributions retrieved for the mixing ratios of key molecules for the retrieval cases described in Section 3.3. Horizontal error bars denote the median and corresponding 1σ interval for the molecules with significant evidence, while the arrows denote the 2σ upper limits. “6+4X” is the model described in Section 3.3, consisting of the six key CNO molecules (CH4, CO2, CO, H2O, NH3, and HCN) and the four chemical species X that exhibit moderate preference across the retrieval cases in this work (1-pentene, isobutylene, diisobutylene, and diethyl sulfide). “4+4X” is the baseline model (CH4, CO2, CO, H2O) used in Section 3.2, along with the four moderate-preference chemical species. The remaining models (“4+X”) show the baseline model with one of isobutylene and 1-pentene. All models consider one offset between the NIRISS and NIRSpec data. Evidence for CH4 is found at a significance of ﹩\mathrm{ln}B\sim 3.1﹩ (∼3σ). Furthermore, evidence for excess absorption beyond the six expected CNO species is also present in the NIR. As discussed in Section 3.2, this may be due to a number of degenerate species. These include isobutylene and 1-pentene, which we include here. As shown, while each of these species presents a distinct peak in the respective “4+X” model, only one (isobutylene, in this case) does when multiple complex species are considered at once. The abundance estimates and detection significances are shown in Table 3.
Paper: A JWST Transmission Spectrum of the Temperate Sub-Neptune TOI-732 c
Authors: Frances E. Rigby, Nikku Madhusudhan, Subhajit Sarkar, Lorenzo Pica-Ciamarra, Måns Holmberg, Julianne I. Moses
Figure caption: The transmission spectrum of TOI-732 c in the NIR. We show the spectrum and retrieved model fits for the one-offset retrieval, as discussed in Section 3.3. This model includes the six key CNO molecules (CH4, CO2, CO, H2O, NH3, and HCN) and the two species found to exhibit moderate preference across our retrieval cases, referred to as X, as discussed in Section 3.2. The data in orange and red show the NIRISS and NIRSpec spectra, respectively, covering 0.9–2.8 μm and 2.8–5.2 μm. The retrievals were carried out using the native resolution data. For visual clarity, these are shown binned to resolutions of R ≈ 25 and R ≈ 55 for the NIRISS and NIRSpec data, respectively. The NIRSpec spectrum has been vertically offset by the median retrieved value for the one-offset retrieval, by ≈112 ppm. In blue we show the median retrieved spectrum, with the lighter-blue contours indicating the 1σ and 2σ intervals. The points in yellow show this median spectrum binned to the resolution of the observations.
Paper: A JWST Transmission Spectrum of the Temperate Sub-Neptune TOI-732 c
Authors: Frances E. Rigby, Nikku Madhusudhan, Subhajit Sarkar, Lorenzo Pica-Ciamarra, Måns Holmberg, Julianne I. Moses
Figure caption: White light curves for the primary transit of TOI-732 c obtained with the three different instruments: NIRISS SOSS (top), NIRSpec G395H (middle), and MIRI LRS (bottom). In each case, the white light curve obtained using the JExoRES pipeline is shown along with the residuals from subtracting a median model fit. For NIRSpec, the combined white light curve from the two detectors NRS1 and NRS2 is shown, while for NIRISS we show the white light curve for Order 1. The standard deviations of the residuals for NIRISS, NIRSpec, and MIRI are 138, 119, and 547 ppm, respectively. These are ∼2.2, ∼1.2, and ∼1.3 times the expected level, respectively. The white light curves for NIRISS and NIRSpec show planet crossing of stellar heterogeneities during transit, as discussed in Section 2.
Paper: A JWST Transmission Spectrum of the Temperate Sub-Neptune TOI-732 c
Authors: Frances E. Rigby, Nikku Madhusudhan, Subhajit Sarkar, Lorenzo Pica-Ciamarra, Måns Holmberg, Julianne I. Moses
Figure caption: Contributions of several molecular species to the transmission spectrum in the 0.9–5.2 μm range (top) and 5–12 μm range (bottom). The individual contributions from each molecule are shown. This nominal model assumes an isothermal P–T profile at 350 K and mixing ratios consistent with our retrievals: 10−2 for CH4, 10−4 for all the other species. The contributions for each molecule show the transmission spectrum from this molecule, in addition to collision-induced absorption of H2–H2 and H2–He. The molecular species shown are those which exhibit moderate evidence across at least three of our four retrieval cases, as shown in Table 2.
Paper: A JWST Transmission Spectrum of the Temperate Sub-Neptune TOI-732 c
Authors: Frances E. Rigby, Nikku Madhusudhan, Subhajit Sarkar, Lorenzo Pica-Ciamarra, Måns Holmberg, Julianne I. Moses
Figure caption: The MIRI JexoPipe and JExoRES data with retrieved spectral fits to the JexoPipe data. The spectral fits, represented by the solid curves, show the median retrieved spectra, obtained with POSEIDON retrievals on the MIRI JexoPipe data. In this setup, the model includes the four baseline molecules (CH4, CO2, CO, H2O) in addition to, in turn, either of the two molecules showing moderate evidence across all retrieval cases, 1-pentene and isobutylene.
Paper: Reconnection-driven Flares in M87*: Proton–Synchrotron-powered GeV Emission
Authors: Hayk Hakobyan, Amir Levinson, Lorenzo Sironi, Alexander Philippov, Bart Ripperda
Figure caption: Time evolutions of space-averaged quantities for two simulations with marginal (red; ﹩{\gamma }_{{\rm{syn}}}^{\pm }/{\sigma }_{\circ }=0.5﹩) and strong (blue; ﹩{\gamma }_{{\rm{syn}}}^{\pm }/{\sigma }_{\circ }=0.15﹩) synchrotron cooling of pairs. (a) Width of the layer along z measured as the FWHM of the energy density (averaged in x and y) of pairs (dashed) and protons (solid); the shaded region corresponds to about 25% variation in the FWHM value, indicating how steep the gradient of w(z) is. (b) Mean Lorentz factor of pairs (dashed) and protons (solid) that have participated in reconnection. (c) Space-averaged dimensionless reconnection rate measured as (E × B)z/B2 in the region 0.1 < z < 0.2. Note that in the case with stronger cooling (blue), the pressure inside the plasmoids is partially provided by the out-of-plane magnetic field. Thus, the width of the pair-dominated region in (a) at later times is similar for both strong and weak cooling.
Paper: Reconnection-driven Flares in M87*: Proton–Synchrotron-powered GeV Emission
Authors: Hayk Hakobyan, Amir Levinson, Lorenzo Sironi, Alexander Philippov, Bart Ripperda
Figure caption: Schematic illustration of the simulation box (the black rectangle) near the exposed equatorial current layer around the black hole. Toroidal magnetic field lines of different polarities are sketched with the red and blue arrows. The colored x-, y-, and z-axes correspond to the actual orientations of the axes in our simulation. Note that the geometry of the layer implies the absence of a guide magnetic field (in this case, a component along the y-axis).
Paper: Reconnection-driven Flares in M87*: Proton–Synchrotron-powered GeV Emission
Authors: Hayk Hakobyan, Amir Levinson, Lorenzo Sironi, Alexander Philippov, Bart Ripperda
Figure caption: Snapshots from two different simulations, with the columns corresponding to different values for the synchrotron cooling strengths of pairs, as indicated in the headings. Each panel is split into two: on the left, we show all the quantities related to pairs, while on the right, we show the quantities related to protons. The first row shows the number densities of pairs and protons (the number density of protons is compensated by their upstream ratio). In the second row, we show the cold (left half) and the hot (right half) magnetization parameters, where the role of ions is clearly emphasized. The final row shows the mean Lorentz factors. These plots demonstrate a clear separation between the cooled pairs confined within the plasmoids and the hot uncooled protons that supply most of the pressure farther upstream.
Paper: Reconnection-driven Flares in M87*: Proton–Synchrotron-powered GeV Emission
Authors: Hayk Hakobyan, Amir Levinson, Lorenzo Sironi, Alexander Philippov, Bart Ripperda
Figure caption: Time-averaged energy distributions for ions (solid) and pairs (dashed) for two runs with different pair-cooling strengths. The averaging is done in a steady state, over a period of 6 ≲ ct/L ≲ 8. The black arrows indicate σ∘ and σi (the same for both runs), while the colored arrows indicate the average Lorentz factors of ions (solid arrows) and pairs (dashed arrows).
Paper: Reconnection-driven Flares in M87*: Proton–Synchrotron-powered GeV Emission
Authors: Hayk Hakobyan, Amir Levinson, Lorenzo Sironi, Alexander Philippov, Bart Ripperda
Figure caption: Time- and x–y-averaged forces plotted against the z-coordinate (perpendicular to the layer) for the ﹩{\gamma }_{{\rm{syn}}}^{\pm }/{\sigma }_{\circ }=0.15﹩ simulation. The green line shows the magnetic tension force acting toward z = 0 attempting to compress the sheet. The blue and red lines show the pressure gradients of pairs and protons, respectively, acting in opposition to the j × B force. Outside ∣z∣ ≳ 0.02, the magnetic tension is balanced primarily by the pressure of ions.
Paper: Star Formation under a Cosmic Microscope: Highly Magnified z = 11 Galaxy behind the Bullet Cluster
Authors: Maruša Bradač, Jon Judež, Chris Willott, Gregor Rihtaršic, Nicholas S. Martis, Anishya Harshan, Giordano Felicioni, Yoshihisa Asada, Guillaume Desprez, Douglas Clowe, Anthony H. Gonzalez, Christine Jones, Brian C. Lemaux, Maxim Markevitch, Vladan Markov, Lamiya Mowla, Gaël Noirot, Annika H. G. Peter, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki, Tim Schrabback, Roberta Tripodi
Figure caption: Top: image of BulletArc-z11. Shown are different filters and an red-green-blue (RGB) image (B = F090W+F115W+F150W, G = F200W+F277W+F356W, and R = F356W+F410M+F444W). The white ticks mark the central position of the source (given by R.A., decl. in Table 2). The galaxy consists of two unresolved (1 and 3) and one barely resolved clump (2) and an underlying smooth component (labeled G). The sizes of cutouts are ﹩1\mathop{.}\limits^{^{\prime\prime} }6\times 1\mathop{.}\limits^{^{\prime\prime} }6﹩. The point source near the center in the F115W filter is the contaminant GC in the Bullet Cluster. Bottom: NIRSpec prism spectrum of BulletArc-z11. In the top panel, we show the 2D spectrum, while the bottom panel shows the 1D optimal extraction, as well as a cutout showing placement within the MSA shutters. The wavelengths of commonly observed emission lines are marked; however, none are detected with S/N > 3. The model spectrum (red line) includes a fully neutral IGM, a neutral hydrogen damping wing column, and a foreground contaminant source modeled as a GC at the Bullet cluster redshift (blue dashed line).
Paper: Reconnection-driven Flares in M87*: Proton–Synchrotron-powered GeV Emission
Authors: Hayk Hakobyan, Amir Levinson, Lorenzo Sironi, Alexander Philippov, Bart Ripperda
Figure caption: Reconstructed multiwavelength emission of the M87* black hole during the reconnection-driven flaring event. The red line ≲100 MeV corresponds to the synchrotron emission of strongly cooled pairs, and its luminosity is fixed at around Lrec, which corresponds to the total power dissipated during the reconnection event. The synchrotron emission of protons is shown with a red band between 100 MeV and ≲100 GeV, and its luminosity corresponds to our estimate from Section 2. The IC emission of pairs upscattering soft photons from the disk is shown with a blue strip beyond ≳100 GeV; the luminosity of this component corresponds to the estimates by H. Hakobyan et al. (2023). The points with error bars correspond to the observations performed at different times by the Fermi satellite (≲100 GeV) and the HESS, MAGIC, and VERITAS detectors (≳100 GeV; J. Ballet et al. 2023; J. C. Algaba et al. 2024). Note that our reconstructed spectrum is only valid during the strong flaring event that lasts for ∼10 rg c–1 (∼ a few days), while the observed GeV spectrum in this plot is integrated over a span of at least a few months, which thus includes quiescence where likely no significant flares occur.