adsabs/AstroCLIMB huggingface dataset:
Paper: XRISM Resolves Relativistic Effects from the Innermost Accretion Disk in Serpens X-1
Authors: R. M. Ludlam, J. M. Miller, E. M. Cackett, J. A. García
Figure caption: The XRISM/Resolve (a) light curve and (b) color–color diagram for Serpens X-1. The average count rate during the observation was 73.1 counts s−1 with variability of 22% from the average. We designate the high-flux state as count rates in excess of 78.2 counts s−1 (upper 15% of the source intensity) and the low-flux state as count rates below 67.9 counts s−1. The vertical dotted lines indicate the times of the bursts that were removed from the data analyzed herein. The color–color diagram shows that the source remains in the soft banana state throughout the observation. The designated low- and high-flux states correspond to the lower banana (LB) and upper banana (UB) states, respectively. The XRISM data were binned to 500 s.
Paper: XRISM Resolves Relativistic Effects from the Innermost Accretion Disk in Serpens X-1
Authors: R. M. Ludlam, J. M. Miller, E. M. Cackett, J. A. García
Figure caption: The ratio of the XRISM/Resolve data to the continuum model for the time-averaged (tavg), lower banana (LB), and upper banana (UB) state, respectively. Data were rebinned for clarity.
Paper: Threading the Magellanic Needle: Hypervelocity Stars Trace the Past Location of the LMC
Authors: Scott Lucchini, Jiwon Jesse Han
Figure caption: Orbital trajectory of the LMC with expanded proper motion errors. The left panel shows the combined available orbital space as in Figure 1; however, the proper motion uncertainties have been artificially inflated so as to encompass the N. Kallivayalil et al. (2013) values. The gray region now shows the total 1σ orbital space using the expanded R.A., decl., distance, and proper motion uncertainties, and the red region shows the region for those orbits with combined HVS posterior values above the 1σ level. The right panel shows the proper motions from N. Kallivayalil et al. (2013) and Z. Wan et al. (2020) in comparison to the expanded uncertainties used (gray oval) and the proper motions of the 1σ HVS orbits (red dot and oval).
Paper: Threading the Magellanic Needle: Hypervelocity Stars Trace the Past Location of the LMC
Authors: Scott Lucchini, Jiwon Jesse Han
Figure caption: The changes in on-sky posterior and mean orbital trajectory for HVS 7 with different MW (left) and LMC (right) masses. The top panels show 1σ ellipses for different masses, while the bottom panels show the mean of the orbits with posteriors greater than the 1σ level. While the posterior distributions do not change significantly, there is strong variation in orbital path when changing the MW mass, and the LMC mass has a weaker effect. The bottom panels have the same extent as Figure 1.
Paper: Threading the Magellanic Needle: Hypervelocity Stars Trace the Past Location of the LMC
Authors: Scott Lucchini, Jiwon Jesse Han
Figure caption: Same as Figures 1 and 3, except with a top-hat prior extending across the face of the LMC. On the right, the trajectories of the 1σ orbits calculated with the top-hat prior are shown as the red shaded regions, while the limits of the orbital space calculated with the Gaussian prior (see Figure 1) are shown as the red lines.
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: Snapshot from an EGRMHD, MAD, and a* = 15/16 simulation. (a) Poloidal (r, θ) slices of fluid rest-mass density (left) and dimensionless temperature (right). (b) Poloidal slices of heat flux normalized by the free-streaming value (left) and pressure anisotropy normalized by magnetic energy density (right). The black contour marks σ = 1, which separates the accretion disk from the magnetically dominated jet. (c) Mass-weighted distribution of pressure anisotropy as a function of β within r ≤ 20rg for the snapshot shown in panels (a) and (b). The black dotted (dashed) lines indicate the mirror (firehose) instability threshold.
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: Comparison of time-averaged fluid quantities between extended and ideal simulations (MAD, a* = 15/16). (a) The top row shows the time- and azimuthally averaged rest-mass density, ρ, and the bottom row displays plasma magnetization, σ. The left column shows the extended simulation, and the right column shows the ideal simulation. (b) Angular momentum transport in the disk: components of the density-weighted average ﹩\langle {T}_{\phi }^{r}\rangle ﹩ normalized by gas pressure 〈P〉 are plotted as a function of radius. (c) Radial profiles of β for extended and ideal simulations.
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: Electromagnetic observables for MAD a* = 15/16 simulation with Rhigh = 160 at a viewing angle of 30°. (a) and (b) Time-averaged 230 GHz total intensity images for the EGRMHD and IGRMHD simulations, respectively. (c) Comparison of time-averaged spectra for the simulations shown in (a) and (b). (d) Light curves at 230 GHz over a duration of Δt = 15,000 tg (∼84 hr for Sgr A*).
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: The 3 hr modulation index for all models considered in this work. The marker color represents the magnetization state (MAD versus SANE), while the marker shape indicates the black hole spin. Points below the dashed line represent models where the EGRMHD simulation produces 230 GHz light curves with lower variability than their ideal counterparts.
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: GRMHD quantities from the SANE a* = 15/16 simulation. (a) Poloidal slices of the dissipative variables: heat flux normalized by the free-streaming value (left) and pressure anisotropy normalized by magnetic energy density (right). The black contour marks σ = 1. (b) Mass-weighted distribution of pressure anisotropy as a function of β within r ≤ 20rg. (c) Time-averaged radial profile of angular momentum transport in the disk.
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: Time-averaged, mass-weighted distribution functions of q/qmax, ΔP/ΔPmax, and ΔP/P for (a) a* = 0 and (b) a* = 15/16 simulations. ΔPmax = ΔPmirror if ΔP > 0, and ΔPmax = ΔPfirehose if ΔP < 0.
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: A schematic flowchart illustrating the sequence of operations during a half-step (tn → tn+1/2) in the EGRMHD evolution. The gray box marks the Implicit kernel, which iteratively determines the next fluid state.
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: Electromagnetic observables for SANE a* = 15/16 simulation with Rhigh = 10 at a viewing angle of 10°. (a) and (b) Time-averaged 230 GHz total intensity images for the EGRMHD and IGRMHD simulations, respectively. (c) Comparison of time-averaged spectra for the simulations shown in (a) and (b).
Paper: Electromagnetic Observables of Weakly Collisional Black Hole Accretion
Authors: Vedant Dhruv, Ben Prather, Mani Chandra, Abhishek V. Joshi, Charles F. Gammie
Figure caption: Convergence tests for EGRMHD test problems. (a) Damped linear waves in flat space. (b) Hydrostatic equilibrium in Schwarzschild geometry with a radial temperature gradient. (c) Spherical accretion with anisotropic viscosity, neglecting the backreaction of viscosity on the steady-state inflow.
Paper: ELPIS: Accelerated Metal and Dust Enrichment in a Protocluster Core at z ≈ 8
Authors: Hideki Umehata, Yoichi Tamura, Yoshinobu Fudamoto, Yurina Nakazato, Daniel Ceverino, Naoki Yoshida, Akio K. Inoue, Ryota Ikeda, Yuma Sugahara, Shutaro Inui, Santiago Arribas, Tom Bakx, Masato Hagimoto, Takuya Hashimoto, Luis Colina, Yi W. Ren, Wataru Osone, Alejandro Crespo Gómez, Ken Mawatari, Javier Álvarez-Márquez
Figure caption: The middle panel shows a Hubble Space Telescope+JWST color composite image (F814W/F115W/F444W) of a portion of the A2744-z7p9OD protocluster, with F814W assigned to blue, F115W to green, and F444W to red, at z ≈ 7.88. Yellow contours indicate the stellar-mass-weighted density map constructed from spectroscopically confirmed member galaxies, corresponding to 55%, 75%, and 95% of the peak mass density (C. Witten et al. 2025a). The left and right panels show enlarged views of the Chain and Quintet groups, respectively, with overlaid 1.26 mm dust continuum (top) and [C II] line (bottom) white contours starting at ±2σ and increasing in steps of 1σ. Naturally weighted maps are used for the Quintet, while tapered images are shown for the Chain. [C II] emission is detected from five galaxies across both regions, while dust continuum is detected only in the Quintet.
Paper: Not All Sub-Neptune Exoplanets Have Magma Oceans
Authors: Bodie Breza, Matthew C. Nixon, Eliza M.-R. Kempton
Figure caption: Location of the envelope–mantle boundary in pressure–temperature space as a function of parameters within the model grid. Each curve represents the locus of boundary locations across a different parameter range, with an upward-facing triangle representing the maximum value and a downward triangle representing the minimum. In some cases, the model radius exceeds 4R⊕ before the maximum (or minimum) is reached when μ = 2.35 g mol−1, meaning the following models are not shown at that MMW: T0 > 500 K, Prc < 31.6 bar, and xenv > 3.5%. Additionally, we do not include the model with μ = 18 g mol−1 and T0 = 300 K as this is impacted by water condensation. The phase diagram of MgSiO3 is shown to indicate the phase at the envelope–mantle boundary for each model in the grid, including the solid–liquid and bridgmanite–postperovskite (Brg–PPv) boundaries. Different line colors represent the MMW of the model. Fiducial values for parameters that are not varied in a given plot are shown below the panels.
Paper: Not All Sub-Neptune Exoplanets Have Magma Oceans
Authors: Bodie Breza, Matthew C. Nixon, Eliza M.-R. Kempton
Figure caption: Boundaries for the presence or absence of a magma ocean in xenv–MMW space. Each line represents the boundary with a particular Mp (represented by color) and T0 (represented by line style). Different panels show different values of Prc. Models that lie above and to the right of the colored lines lack magma oceans, whereas those that lie to the left and below the lines do possess magma oceans. Blue shading represents regions of the parameter space for which all models feature a solid silicate surface, and red shading represents regions where all models feature a magma ocean (liquid silicate surface). Gray shaded regions represent models whose radius exceeds 4R⊕. We do not include models with T0 = 500 K and Prc = 100 bar since they are impacted by water condensation.
Paper: ELPIS: Accelerated Metal and Dust Enrichment in a Protocluster Core at z ≈ 8
Authors: Hideki Umehata, Yoichi Tamura, Yoshinobu Fudamoto, Yurina Nakazato, Daniel Ceverino, Naoki Yoshida, Akio K. Inoue, Ryota Ikeda, Yuma Sugahara, Shutaro Inui, Santiago Arribas, Tom Bakx, Masato Hagimoto, Takuya Hashimoto, Luis Colina, Yi W. Ren, Wataru Osone, Alejandro Crespo Gómez, Ken Mawatari, Javier Álvarez-Márquez
Figure caption: DGR, ﹩\mathrm{log}({M}_{{\rm{dust}}}/{M}_{{\rm{gas}}})﹩, as a function of gas-phase metallicity for galaxies in our sample and comparison samples (A. Harshan et al. 2024; Z. Ma et al. 2024; H. Algera et al. 2025). The solid curve indicates the predicted relation from (semi)analytical calculations of G. Popping et al. (2017) at z = 7. YD1 and YD4+YD6 in the Quintet exhibit relatively high metallicities, comparable to those of the REBELS sample, suggesting that they may be undergoing rapid dust mass buildup driven by grain growth in the ISM.
Paper: ELPIS: Accelerated Metal and Dust Enrichment in a Protocluster Core at z ≈ 8
Authors: Hideki Umehata, Yoichi Tamura, Yoshinobu Fudamoto, Yurina Nakazato, Daniel Ceverino, Naoki Yoshida, Akio K. Inoue, Ryota Ikeda, Yuma Sugahara, Shutaro Inui, Santiago Arribas, Tom Bakx, Masato Hagimoto, Takuya Hashimoto, Luis Colina, Yi W. Ren, Wataru Osone, Alejandro Crespo Gómez, Ken Mawatari, Javier Álvarez-Márquez
Figure caption: Comparison of dust mass (Mdust) versus stellar mass (M⋆) for our sample and other z ∼ 7–8 galaxies (D. Watson et al. 2015; T. J. L. C. Bakx et al. 2020, 2021; Z. Ma et al. 2024; H. Algera et al. 2025), along with model predictions at z = 7 (G. Popping et al. 2017) and at z = 6–12 (D. Narayanan et al. 2025). The A2744-z7p9OD protocluster galaxies occupy the lower stellar mass regime and show relatively low dust-to-stellar mass ratios, ﹩\mathrm{log}({M}_{{\rm{dust}}}/{M}_{\star })﹩, compared to the REBELS sample at z ∼ 7. Simulations predict that a rapid rise in this ratio occurs around ﹩\mathrm{log}({M}_{\star }/{M}_{{\odot }})\sim 9﹩ at z ∼ 8, driven by efficient dust growth via metal accretion in the ISM. The galaxies in the Quintet and Chain may represent this transitional phase.
Paper: ELPIS: Accelerated Metal and Dust Enrichment in a Protocluster Core at z ≈ 8
Authors: Hideki Umehata, Yoichi Tamura, Yoshinobu Fudamoto, Yurina Nakazato, Daniel Ceverino, Naoki Yoshida, Akio K. Inoue, Ryota Ikeda, Yuma Sugahara, Shutaro Inui, Santiago Arribas, Tom Bakx, Masato Hagimoto, Takuya Hashimoto, Luis Colina, Yi W. Ren, Wataru Osone, Alejandro Crespo Gómez, Ken Mawatari, Javier Álvarez-Márquez
Figure caption: Distribution of galaxies in the A2744-z7p9OD protocluster and other z ∼ 7–8 samples (S. Arribas et al. 2024; A. Harshan et al. 2024; Z. Ma et al. 2024; H. Algera et al. 2025; L. E. Rowland et al. 2025) in the stellar mass–metallicity plane. All metallicities are derived using strong-line calibrations. The mass–metallicity relation from T. Morishita et al. (2024) and M. Curti et al. 2024 is shown for comparison as a blue (green) shaded region. YD1 and YD4+YD6 in the Quintet exhibit elevated gas-phase metallicities relative to the relation, while ZD3+ZD6 and ZD12 in the Chain lie on or below the relation.
Paper: ELPIS: Accelerated Metal and Dust Enrichment in a Protocluster Core at z ≈ 8
Authors: Hideki Umehata, Yoichi Tamura, Yoshinobu Fudamoto, Yurina Nakazato, Daniel Ceverino, Naoki Yoshida, Akio K. Inoue, Ryota Ikeda, Yuma Sugahara, Shutaro Inui, Santiago Arribas, Tom Bakx, Masato Hagimoto, Takuya Hashimoto, Luis Colina, Yi W. Ren, Wataru Osone, Alejandro Crespo Gómez, Ken Mawatari, Javier Álvarez-Márquez
Figure caption: Results of the multicomponent Gaussian fit to the Quintet map. The left, middle, and right panels show the observed image, the best-fit model, and the residual (data−model), respectively. Three components (YD1, YD4+YD6, and YD7W) are modeled. Cyan, magenta, and yellow contours are drawn for observed, modeled, and residual images, respectively, at ±2σ, ±3σ, … .
Paper: Threading the Magellanic Needle: Hypervelocity Stars Trace the Past Location of the LMC
Authors: Scott Lucchini, Jiwon Jesse Han
Figure caption: Orbital history of the LMC, using Z. Wan et al. (2020) measurements of the systemic proper motions. The gray shaded region shows the 1σ extent of the extrapolated orbit based on the present-day dynamical center measured by Z. Wan et al. (2020), while the red shaded region shows the constraints derived from hypervelocity stars (HVSs). The HVS-based constraints are ∼2× tighter than those from simple extrapolation, despite allowing the LMC’s dynamical center to vary freely; the prior on the center spans a much larger region than the Z. Wan et al. (2020) measurement. All HVSs shown were ejected less than 500 Myr ago. The main panel displays the combined constraints from multiple HVSs, while the side panels show individual constraints from HVS 3, HVS 7, and HVS 15.
Paper: Threading the Magellanic Needle: Hypervelocity Stars Trace the Past Location of the LMC
Authors: Scott Lucchini, Jiwon Jesse Han
Figure caption: Comparison of the LMC’s past orbit as constrained in this study with previously published models. The red shaded region shows the 1σ range of trajectories allowed by HVSs. Each curve represents a different orbital model, with model types indicated in superscript: nbody for N-body simulations (N. Garavito-Camargo et al. 2021; S. Lilleengen et al. 2023; E. Vasiliev 2024), hydro for hydrodynamical simulations (G. Besla et al. 2012; S. Lucchini et al. 2021), and int for analytic integrations (E. Patel et al. 2020). The gray inset box corresponds to the spatial region shown in Figure 1, or roughly ∼800 Myr into the past. Beyond this range, the timescales significantly predate the ejection of the HVSs and enter a regime where their trajectories no longer provide meaningful constraints. Among the models shown, the second passage N-body model of E. Vasiliev (2024) and the first passage hydrodynamical model of S. Lucchini et al. (2021) are most consistent with the HVS-based constraints.
Paper: Threading the Magellanic Needle: Hypervelocity Stars Trace the Past Location of the LMC
Authors: Scott Lucchini, Jiwon Jesse Han
Figure caption: The on-sky distributions of the present-day positions of the LMC dynamical center that are consistent with the ejection of the hypervelocity stars. The right panels show the 1 (solid) and 2 (dashed) sigma curves for HVS 3, 7, and 15, compared against the dynamical centers determined using the H I (cross), carbon stars (plus), red giant branch stars (circle), and main-sequence stars (star) (S. Kim et al. 1998; Z. Wan et al. 2020). The left panel shows the 1σ contours for each star as well as the combined posterior in white.
Paper: Monitoring of the Spectral and Timing Properties of the Ultraluminous X-Ray Pulsar NGC 7793 P13
Authors: Marina Yoshimoto, Tomokage Yoneyama, Shogo B. Kobayashi, Hirokazu Odaka, Taiki Kawamuro, Hironori Matsumoto
Figure caption: Long-term evolution of the unabsorbed flux or luminosity (upper panel) and the spin period (lower panel) for NGC 7793 P13. The data sets after 2020 are published for the first time in this work. The error is 90% and 1σ confidence level for the unabsorbed flux and the spin period, respectively. In the upper panel, the solid line (gray) shows the Eddington luminosity of a 1.4M⊙ NS assuming the distance of 3.4 Mpc. In the lower panel, the dashed–dotted line (sky blue) and dotted line (sky blue) show the long-term derivative of the spin period of ﹩{\dot{P}}_{{\rm{long}}}^{({\rm{pre}})}=-3.87\times 1{0}^{-11}\,{\rm{s}}\,{{\rm{s}}}^{-1}﹩ and ﹩{\dot{P}}_{{\rm{long}}}^{({\rm{post}})}=-6.79\times 1{0}^{-11}\,{\rm{s}}\,{{\rm{s}}}^{-1}﹩, respectively.
Paper: Monitoring of the Spectral and Timing Properties of the Ultraluminous X-Ray Pulsar NGC 7793 P13
Authors: Marina Yoshimoto, Tomokage Yoneyama, Shogo B. Kobayashi, Hirokazu Odaka, Taiki Kawamuro, Hironori Matsumoto
Figure caption: Results for count rate, hardness ratio (HR), photon index Γ, and intrinsic absorption NH of phase-resolved spectra from XMM-Newton (left panel) and NuSTAR (right panel) data. Only on- and off-pulse results are shown, except for count rates. The absorption value is fixed at 4 × 1020 cm−2 for the NuSTAR data. The colors are the same as in Figure 3.
Paper: Monitoring of the Spectral and Timing Properties of the Ultraluminous X-Ray Pulsar NGC 7793 P13
Authors: Marina Yoshimoto, Tomokage Yoneyama, Shogo B. Kobayashi, Hirokazu Odaka, Taiki Kawamuro, Hironori Matsumoto
Figure caption: Left panel: the background-subtracted folded light curve for two cycles in the energy range of 3–10 keV extracted from the 2019 May XMM-Newton observation (obsID: 0840990101). The fitting model is shown with a solid line. The curve is divided into four phases: “on-pulse” (red), “falling” (orange), “off-pulse” (blue), and “rising” (green) to extract the phase-resolved spectra. Right panel: the phase-resolved spectra in 0.35–7.5 keV based on the folded light curve from the same observation. The off-pulse spectrum is clearly softer than the on-pulse spectrum.
Paper: Monitoring of the Spectral and Timing Properties of the Ultraluminous X-Ray Pulsar NGC 7793 P13
Authors: Marina Yoshimoto, Tomokage Yoneyama, Shogo B. Kobayashi, Hirokazu Odaka, Taiki Kawamuro, Hironori Matsumoto
Figure caption: Relation between the unabsorbed flux or luminosity and the pulsed fraction (PF) in the energy range of 3−10 keV from 2012 to 2024. We use a distance of 3.4 Mpc to convert flux into luminosity. The red plots represent the data sets after 2020, which are published for the first time in this work.
Paper: Monitoring of the Spectral and Timing Properties of the Ultraluminous X-Ray Pulsar NGC 7793 P13
Authors: Marina Yoshimoto, Tomokage Yoneyama, Shogo B. Kobayashi, Hirokazu Odaka, Taiki Kawamuro, Hironori Matsumoto
Figure caption: Schematic of an accretion column viewed from a side. If the hot/high-energy emission originates from the root of the accretion column, the apparent fraction of the hard spectral component to the soft component in the off-pulse phase could be highly dependent on the height of the accretion column.
Paper: Monitoring of the Spectral and Timing Properties of the Ultraluminous X-Ray Pulsar NGC 7793 P13
Authors: Marina Yoshimoto, Tomokage Yoneyama, Shogo B. Kobayashi, Hirokazu Odaka, Taiki Kawamuro, Hironori Matsumoto
Figure caption: Light curve of Swift/XRT monitoring observations in 2010–2025.
Paper: Outflow–Cloud Interaction as the Possible Origin of the Peculiar Radio Emission in the Tidal Disruption Event AT2018cqh
Authors: Lei Yang, Xinwen Shu, Guobin Mou, Yongquan Xue, Luming Sun, Fabao Zhang, Zhumao Zhang, Yibo Wang, Tao Wu, Ning Jiang, Hucheng Ding, Tinggui Wang
Figure caption: The radio light curves of AT2018cqh, including the data from the ASKAP observations at 0.89 GHz, 1.36 GHz, and 1.66 GHz, the e-MERLIN observations at 1.51 GHz, the VLASS observations at 3 GHz, the VLBA observations at 1.56 GHz, and the VLA observations at 3.0 GHz (Section 3.2). The radio emission appears later relative to the time of optical discovery (MJD = 58285) and shows a continuous rising in flux that can vary on timescales down to ∼2 months. For the nondetections, the corresponding 3σ upper limits on flux density are shown. The vertical dashed lines represent the three epochs for which the radio SED can be constrained (Figure 3), corresponding to 1246, 1730, and 2243 days after the optical discovery, respectively.
Paper: Outflow–Cloud Interaction as the Possible Origin of the Peculiar Radio Emission in the Tidal Disruption Event AT2018cqh
Authors: Lei Yang, Xinwen Shu, Guobin Mou, Yongquan Xue, Luming Sun, Fabao Zhang, Zhumao Zhang, Yibo Wang, Tao Wu, Ning Jiang, Hucheng Ding, Tinggui Wang
Figure caption: The radio SEDs for the three epochs that have quasi-simultaneous observations at different frequencies. For the nondetections, the corresponding 3σ upper limits on the flux density are shown. The green, orange, and blue lines represent the best fits to each SED from our MCMC modeling (Section 3.3), which are the model realizations on a basis of 500 random samples from the MCMC chains. There is a steady rise in both the peak flux density and frequency between the three epochs.