adsabs/AstroCLIMB huggingface dataset:
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: The white lightcurves from NIRISS (Order 1), and NIRSpec/G395H NRS1 and NRS2, shown from top to bottom, respectively, along with the best-fit secondary eclipse models including polynomial detrending. The corresponding residuals are displayed beneath each lightcurve.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: Emission spectra obtained from both Eureka! and exoTEDRF are overplotted for comparison, along with their relative difference. The mean absolute difference between the two spectra is ∼0.5σ, indicating excellent statistical agreement.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: Posterior distribution of the model parameters from the equilibrium chemistry retrieval of the Eureka! spectra.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: Posterior distribution of the model parameters from the free chemistry retrieval of the Eureka! spectra.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: A zoomed-in version of Figure 2 at shorter wavelengths.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Structure and evolution of the simulation d0.3hiE (RCBM = 0.3 × 1015 cm, Tej,in = 5 × 105 K) at four representative epochs. Each quadrant of each panel shows a different quantity: density ρ (upper left), gas temperature T (upper right), tangential velocity vθ (lower left), and ionization structure (lower right). Explanation of the color scale is given in the legend at the bottom. Tangential velocity is positive for motions toward the plane of symmetry. Ionization structure is based on the evaluation of Saha-like equations for each species with more detailed explanation shown in Figure A1. Hatched circles show regions where arT4/3 exceeds the gas pressure, but the dynamical effect of radiation depends on the local value of the flux limiter (Equation (A2)). White lines show the location of the τ = 2/3 surface measured along radial rays, with solid and dashed lines showing results based on Rosseland and Planck mean opacities, respectively.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Bolometric light curves (upper row) and photospheric temperatures (lower row) of our simulations for the two different initial ejecta temperatures (left and right columns). In the upper row, colored solid lines are for different values of RCBM, while solid black lines show simulations without CBM. Colored dotted lines indicate shock power for the appropriate ejecta and CBM combination calculated using semianalytic models for the same ejecta and CBM properties (B. D. Metzger et al. 2014; B. D. Metzger & O. Pejcha 2017; O. Pejcha et al. 2022). In the lower row, solid lines indicate gas temperatures at the Rosseland photosphere, and dashed lines are at the Planck photosphere. Photospheric temperatures are shown only for times when the entire photosphere is located on the computational grid. Gray shaded areas indicate regions where the results are significantly affected by the choice of initial conditions.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Evolution of radiative flux for simulation d0.3hiE with Tej,in = 5 × 105 K and RCBM = 2.0 × 1015 cm. The background color shows the absolute value of the radiative flux, while the arrows show its direction. The solid white line shows the position of the τ = 2/3 surface measured along radial rays using Rosseland mean opacity.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Ray tracing of our simulation runs d0.1hiE (left column) and d2.0hiE (right column). The upper row shows the evolution of luminosities calculated using ray tracing for nine orientation angles θ (thin lines with colors transitioning from black to orange), the angular average of the ray tracing (thick red line), and the angular average of the radiative flux in the simulations (thick blue line; same as in Figure 3). The lower part shows ray-traced images for four selected orientation angles and at five different epochs indicated by thin gray vertical lines in the top row.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Effect of irradiation from the central source. The left panel shows the luminosities (blue) and photospheric temperatures (red) for the fiducial (dashed; s0.1loE) and irradiated (solid; s0.1loEirr) models. The middle and right panels show the density and gas temperature structure of the irradiated model at one selected epoch indicated by the vertical gray dotted line in the left panel.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Comparison of our simulated luminosities (upper panel) and photospheric temperatures (lower panel) to observed LRNe. Our models are shown with thick solid lines with the explanation for the colors given in the upper panel legend. Observed LRNe are AT 2017jfs (gray stars; A. Pastorello et al. 2019b), AT 2021biy (gray triangles; Y. Z. Cai et al. 2022), AT 2021blu (pink hatches), AT 2018bwo (green hatches), AT 2021afy (orange circle hatches; A. Pastorello et al. 2023), and AT 2018hso (blue star hatches; Y. Z. Cai et al. 2019).
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: Posterior distribution of the model parameters from the free chemistry retrieval of the exoTEDRF spectra.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: Posterior distribution of the model parameters from the equilibrium chemistry retrieval of the exoTEDRF spectra.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Effect of applying opacity floor and ceiling on the luminosity and photospheric temperature. The upper two rows show results for simulations with Tej,in = 5 × 105 K (hiE series of models), while the lower two rows show results for Tej,in = 1 × 105 K (loE series of models). Each column shows results for different RCBM. Model series s was calculated with analytic EOSs and opacities. All other model series used tabulated EOSs and opacities, where series d presents the default results for runs with CBM. Model series e, g, h, and n have the same ﹩{\dot{M}}_{\,\rm{wind}\,}﹩, which is a factor of 10 higher than for series d, but this is inconsequential for the light curves. Series e, g, and h differ by a value of κR,floor = 10−3, 10−4, and 10−5 cm2 g−1, respectively. Model series n does not apply any opacity floor. We also show models that had to be terminated before reaching the postplateau phase due to numerical problems (Table 1).
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Comparison of a theoretical nickel-free Type IIP supernova calculated with SNEC (solid black line) with our simulated runs with Mej = 10 M⊙, Eej,kin = 9.8 × 1050 erg, and three initial ejecta temperatures (blue, pink, and orange solid lines). The upper panel shows luminosities as functions of time. The dashed–dotted lines indicate models with the same initial conditions but using a Γ-law EOS. The lower panel shows the time evolution of the Rosseland photospheric temperatures. The dashed pink line shows the time evolution of the Planck photospheric temperature for the model where Rosseland and Planck opacities differ.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Adiabatic index Γ of our tabulated EOS (K. Tomida et al. 2013, 2015) as a function of ρ and T. Black solid lines show empirical Saha-like functions that we used to determine the ionization state of gas, and black circles indicate the region where arT4/3 exceeds the gas pressure (see Figures 1 and B1–B6).
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Comparison of the effect of different EOSs and ﹩{\dot{M}}_{\,\rm{wind}\,}﹩ on luminosity (upper row) and photospheric temperature (lower row) for two different initial ejecta thermal energies (left and right column). Simulation parameters are given in Table 1.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Comparison of opacity prescriptions used in this work. Each panel shows a temperature dependence of the opacity for a different density. Solid lines denote Rosseland means, and dotted lines denote Planck means. Black lines show original tables from K. Tomida et al. (2013), blue lines apply smoothing, orange lines further apply the Rosseland mean floor of 10−3 cm2 g−1, and green lines show the analytic prescription from Equation (A20).
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Same as the top panel of Figure 4 but for the spherically symmetric model without CBM: enocbmhiE.
Paper: Two-dimensional Radiation-hydrodynamic Simulations of Luminous Red Novae
Authors: Anthony Kirilov, Diego Calderón, Ondřej Pejcha, Paul C. Duffell
Figure caption: Resolution study for CBM runs with RCBM = 2.0 × 1015 cm and Tej,in = 1 × 105 K for different combinations of Nr × Nθ given in the legend.
Paper: Dust Budget Crisis in Little Red Dots
Authors: Kejian Chen, 可鉴 陈, Zhengrong Li, Kohei Inayoshi, Luis C. Ho
Figure caption: Parameter survey showing the upper limit on AV as a function of the density distribution parameters (γ, n0), assuming the SMC (left) and Orion Nebula (right) extinction curves for LRD A2744–45924. Black solid curves divide the regions where the maximum allowed AV value is constrained by MIRI F1000W, F2100W, or ALMA data (from top to bottom). White dashed contours label the total dust mass Mdust, computed using Equation (4) based on the corresponding AV upper limit. Orange stars mark the density configurations shown in the right panel of Figure 2. The bottom right region (i.e., steeper profiles with lower density normalization) requires extended dust distribution with rout ≥ 10 kpc to achieve sufficient column density and is therefore ruled out as unphysical configurations.
Paper: Dust Budget Crisis in Little Red Dots
Authors: Kejian Chen, 可鉴 陈, Zhengrong Li, Kohei Inayoshi, Luis C. Ho
Figure caption: Extinction curves as a function of wavelength used in this work, covering from UV to infrared wavelengths: the SMC, the interstellar dust in the MW with RV = 3.1 (J. C. Weingartner & B. T. Draine 2001), and the Orion Nebula (J. A. Baldwin et al. 1991). We also show the modified Calzetti’s attenuation law proposed in S. Noll et al. (2009) with δ = −1.8 (see main text). The extinction Aλ is normalized at the V-band 5500 Å (dotted vertical line). The UV-to-optical part is used to compute dust attenuation of the incident radiation flux (blue shaded region), and the IR part is used to calculate the reemission from heated dust (red shaded region).
Paper: Dust Budget Crisis in Little Red Dots
Authors: Kejian Chen, 可鉴 陈, Zhengrong Li, Kohei Inayoshi, Luis C. Ho
Figure caption: Multiwavelength SED of the brightest LRD, A2744–45924 (orange curve), with JWST NIRCam/MIRI detection (circles) and nondetection in Herschel and ALMA bands (triangles). Left: incident (corrected for extinction) and reprocessed IR reemission spectra for fixed dust distribution parameters γ = 0.5 and n0 = 103 cm−3 with varying visual extinction AV. Right: reemission SEDs for four different dust density configurations: (γ, n0) = (0.5, 103 cm−3), (0.5, 10 cm−3), (0, 10 cm−3), and (2.0, 104 cm−3). For each case, the maximum allowed AV is applied such that the resulting IR flux does not violate the observational constraints.
Paper: Dust Budget Crisis in Little Red Dots
Authors: Kejian Chen, 可鉴 陈, Zhengrong Li, Kohei Inayoshi, Luis C. Ho
Figure caption: Summary of the upper limits on AV derived for the four different SEDs analyzed in this work: the two individual bright LRDs (A2744–45924 and RUBIES-BLAGN-1) and the two stacked LRD samples from H. B. Akins et al. (2025a) and I. Delvecchio et al. (2025). The bar chart compares the results across the four dust opacity laws (from left to right: a modified Calzetti law with δ = −1.8, SMC, MW, and Orion Nebula). Each solid rectangle shows the least restrictive AV upper limit (﹩{A}_{V}^{{\rm{lim}}}﹩) found from the entire (γ, n0) parameter space with an error bar representing ﹩{A}_{V}^{{\rm{lim}}}﹩ under different dust mass limits: Mdust ≤ 104, 105, and 106 M⊙ from bottom to top. The dashed lines indicate the more stringent limit obtained when restricting the analysis to physically motivated, concentrated density profiles (γ ≥ 1). The gray shaded region indicates the extinction range typically assumed in obscured AGN scenarios (AV ≃ 3.48 ± 0.70 mag; H. B. Akins et al. 2025a).
Paper: Dust Budget Crisis in Little Red Dots
Authors: Kejian Chen, 可鉴 陈, Zhengrong Li, Kohei Inayoshi, Luis C. Ho
Figure caption: Left: infrared reemission SEDs with the maximum allowed AV for different dust density configurations, constrained with the stacked LRD SED from I. Delvecchio et al. (2025; filled circles and triangles). The stacked SED from H. B. Akins et al. (2025a) is also shown for comparison (open circles and triangles). The parameter combinations are chosen as (γ, n0) = (0.5, 103 cm−3), (0.25, 10 cm−3), (0, 10 cm−3), and (0, 105 cm−3). Right: parameter survey showing the upper limit on AV as a function of the density distribution parameters (γ, n0), assuming the stacked LRD SED and the SMC opacity curve. Black solid curves divide the regions where the maximum allowed AV value is constrained by MIRI F1280W, F1500W, F2100W, or ALMA data (from top to bottom).
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: Top: The best-fit light curve after including different ranges of data. The color of the line represents the maximum δt days since discovery that was used when selecting data to fit. Bottom: The change in total score (red), photometry score (blue), distance score (black), and two-dimensional score (orange) over time as we include additional information/measurements of SN 2025ulz. The distance score drops after a spectroscopic redshift is measured at δt ≈ 2.6 days. After the light curve turns over, the photometry score drops, since this turnover is inconsistent with KN models and the AT 2017gfo light curve.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: The evolution of the SN 2025ulz score (blue) as compared to the evolution of the scores of the rest of our candidates (gray). The red line shows the number of candidates with a better score than SN 2025ulz over time (right y-axis). The labels near the red line are the number of candidates with a score greater than SN 2025ulz at that time.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: Light curves of the publicly available data from ATLAS and TNS on AT 2025uxu (blue) and AT 2025uow (red) as compared to AT 2017gfo (black; V. A. Villar et al. 2017). We scale the observed magnitudes of AT 2025uxu and AT 2025uow to the mean distance in the corresponding HEALPix tile in the localization map of S250818k. The merger date associated with S250818k is shown as a gray dashed vertical line. Different markers indicate different telescope filters.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: Flow diagram outlining our current candidate scoring algorithm. In general, it takes in IGWN alerts, TNS transients, various static catalogs, and forced photometry and derives multiple “subscores” from the data, eventually multiplying them together to obtain a total overall score for a candidate.
Paper: Dust Budget Crisis in Little Red Dots
Authors: Kejian Chen, 可鉴 陈, Zhengrong Li, Kohei Inayoshi, Luis C. Ho
Figure caption: Observed flux densities (fν) of the brightest LRD (A2744–45924) at zspec = 4.4655, comparing modeled dust reemission with current observational data and future detection capabilities with PRIMA. Observed photometric data points for A2744–45924 are shown in circles and triangles, together with the JWST spectrum (black line). The colored curves represent the maximum predicted IR reemission flux densities from various dust distribution models, each calculated to be consistent with existing observational constraints from JWST MIRI and ALMA, with the colors indicating the derived upper limit on visual extinction (AV) for each model. All models presented correspond to a fixed dust mass of Mdust = 105 M⊙. The black dashed curve presents the expected intrinsic spectrum with dust correction assuming AV = 0.6 mag, which does not agree with the shape of the low-z AGN composite spectral template (cyan; D. E. Vanden Berk et al. 2001). The orange lines indicate the anticipated 5σ sensitivity for a 20 hr PRIMA exposure for ﹩10\,{{\rm{arcmin}}}^{2}﹩ areas. Colored boxes at the bottom illustrate the wavelength coverage of relevant telescopes and instruments.
Paper: Dust Budget Crisis in Little Red Dots
Authors: Kejian Chen, 可鉴 陈, Zhengrong Li, Kohei Inayoshi, Luis C. Ho
Figure caption: Similar to the left panel of Figure 3 but examining two alternative treatments of the intrinsic UV flux that is reprocessed to IR. Left: assuming a scattering fraction of fscat = 0.01, where a small fraction of the intrinsic AGN UV light is observed without dust attenuation. Right: excluding all incident UV radiation at λ < 3645 Å when computing the dust-reprocessed IR emission (dust-free galaxy component).