adsabs/AstroCLIMB huggingface dataset:
Paper: Continued Photometric Monitoring Supports Long-term Dynamical Evolution in the Young Binary Star–Disk System KH 15D
Authors: Luke Lamitina, Lynne Hillenbrand, Michael Poon
Figure caption: Phased lightcurves with M. Poon et al. (2021) model (black) of KH 15D split into seven seasons (∼208 days/season) between 2018 and 2024, as defined in Figure 3. The model has been translated by +1.8 mag.
Paper: Continued Photometric Monitoring Supports Long-term Dynamical Evolution in the Young Binary Star–Disk System KH 15D
Authors: Luke Lamitina, Lynne Hillenbrand, Michael Poon
Figure caption: Color in g − r as a function of phase (top) and brightness (bottom). There is some amount of color variation that occurs mainly during eclipse ingress and egress, consistent with light from the stellar components of KH 15D interacting with the circumbinary material. It is noted that at dimmer magnitudes this interaction is more apparent, supporting the notion of clumping within the trailing edge of the disk or ring.
Paper: Continued Photometric Monitoring Supports Long-term Dynamical Evolution in the Young Binary Star–Disk System KH 15D
Authors: Luke Lamitina, Lynne Hillenbrand, Michael Poon
Figure caption: Phased ZTF lightcurve of KH 15D using the derived period of 48.36 days. Colors highlight the points used for fits of the central inflection (red) and points used for the fit of the broad eclipse (blue).
Paper: Continued Photometric Monitoring Supports Long-term Dynamical Evolution in the Young Binary Star–Disk System KH 15D
Authors: Luke Lamitina, Lynne Hillenbrand, Michael Poon
Figure caption: Combined r-band and g-band ZTF photometry of the KH 15D binary-star system over the seven seasons (highlighted gray) spanning 2018–2024. An offset of +1.01 was applied to the r-band data in order to combine it with the g-band data for the following analysis.
Paper: Continued Photometric Monitoring Supports Long-term Dynamical Evolution in the Young Binary Star–Disk System KH 15D
Authors: Luke Lamitina, Lynne Hillenbrand, Michael Poon
Figure caption: Two-sided hyperbolic tangent fits for the KH 15D data intended to quantify the ingress and egress portions of the overall lightcurve.
Paper: Continued Photometric Monitoring Supports Long-term Dynamical Evolution in the Young Binary Star–Disk System KH 15D
Authors: Luke Lamitina, Lynne Hillenbrand, Michael Poon
Figure caption: Central rebrightening event fit across seasons 2–7. Gray shaded region represents one standard deviation error.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Predicted and measured spectral energy distribution (SED) of the Didymos–Dimorphos system. The black (solid) and red (dashed) lines illustrate the predicted SED (i.e., with no impact or dust) for 2022 September 27 and 2022 October 6, respectively. The blue and red diamonds represent the measured SED at 8.7, 10.5, and 11.7 μm for September 27 and October 6, respectively. The dashed–dotted blue line shows the best-fit SED for the Didymos–Dimorphos system 11 hr after the DART impact.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Predicted N-band fluxes for 1989 ML for a range of albedos (red line) and diameters (black line). The horizontal dashed line corresponds to the 5σ flux we would have detected in ∼47 minutes of integration time. The red line flux solutions were computed for a sphere with radius obtained from the  E. F. Tedesco et al. (1992) relationship and assuming the JPL-Horizons HV solution. The black line flux solutions were computed for various sphere sizes with a fixed pV of 50%. We conclude that this object must have an albedo higher than 0.25 and a diameter smaller than 400 meters.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Simultaneous optical and thermal lightcurves of NEO 7482 as a function of time (hours) after the beginning of the observation on 2022 January 18. The left y-axis illustrates the R-band magnitudes (black circles). The right y-axis shows the flux variability at the 8.7 μm (blue diamonds) and 11.7 μm (red diamonds) filters.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: MIRSI transmission filter curves obtained at room temperature at the IRTF as a function of wavelengths in microns. Gray continuous curves correspond to the 1.6 mm atmospheric transmission from Maunakea.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Visible (V-band) and absolute magnitudes (HV) of the MIRSI+MOC NEO survey. In black circles are those magnitude's solutions derived in this work, while red circles correspond to the JPL-Horizons systems. The top and right subpanels are the histogram distribution of the absolute and visible magnitudes, respectively.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Visible albedo as a function of diameter for the 31 NEOs observed with MIRSI. The dark diamonds show the results using the MOC–HV, while the red ones show the solutions with JPL–HV.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Average visible albedo of NEOs by taxonomic type. Black and red diamonds illustrate the average pV using HV from MOC and JPL, respectively. In blue diamonds, we show the comparable average albedos for complex taxonomies from previous ExploreNEOs work by C. A. Thomas et al. (2011). In green, we show the average and the range of albedos for X-complex based on our estimates from weakly detected objects.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Two-dimensional histogram of the posterior probability function for albedos and diameters solutions for the NEO 7482. Darker shades indicate more probable values. The top and right subpanels are the one-dimensional marginal distributions of the likelihood probability function for the diameter and albedo, respectively.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Retrieved transmission spectra, P-T profile along with the rcf, C/O ratio, and metallicity posteriors with grid retrieval. The top panel consists of median transmission spectra and P-T profile of HD 209458 b for the three grid retrievals, with just JWST (NIRCam), WFC3 + NIRCam, and STIS + WFC3 + NIRCam observations. All the spectra shown here are generated with 5000 random equal-weighted samples from PyMultiNest and binned at a resolution of R ∼ 200. The shaded region indicates the 1σ uncertainty in the median fit. JWST observations are represented in green, while combined STIS and WFC3 observations are shown in brown. A retrieved median offset of 90 ppm is applied to the STIS + WFC3 observations, whereas the offset for WFC3 in the case of the WFC3 + JWST combination is not shown here. For all the retrievals, the corresponding P-T profiles are shown beside the median spectra. The bottom panel shows the posteriors of the recirculation factor, C/O ratio, and ﹩{\mathrm{log}}\,(Z)﹩.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Retrieved transmission spectra, P-T profile, C/O, and metallicity posteriors of HD 209458 b with equilibrium chemistry. The top panel consists of median transmission spectra and P-T profile of HD 209458 b for the three retrievals, JWST (NIRCam), WFC3 + NIRCam, and STIS + WFC3 + NIRCam. All the spectra shown here are generated with 5000 random equal-weighted samples from PyMultiNest and binned at a resolution of R ∼ 200. The shaded region indicates the 1σ uncertainty in the median fit. JWST observations are represented in green, while combined STIS and WFC3 observations are shown in brown. A retrieved median offset of 39 ppm is applied to the STIS + WFC3 observations, whereas the offset for WFC3 in the case of the WFC3 + JWST combination is not shown here. For all the retrievals, the corresponding P-T profiles are shown beside the median spectra. The bottom panel shows the posteriors of C/O and ﹩{\mathrm{log}}\,(Z)﹩ by varying C and varying O for the C/O ratio. The posterior values shown in this panel correspond to the results shown in Table 5.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Left: median P-T profile of HD 209458 b for the three retrievals, free chemistry (orange), equilibrium chemistry (violet), and grid retrieval (pink), performed using STIS+WFC3+NIRCam observations. The shaded region shows 1σ uncertainty on the P-T profile. Right: corresponding mixing ratios of CO2 (solid) and H2O (dashed) obtained from the median values of all three retrievals are shown.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Comparison of grid-based interpolation and otf interpolation when generating the forward model. This comparison was performed for a WASP-96 b–type planet with an isothermal temperature of 1205 K, with abundances provided by J. Taylor et al. (2023).
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Best-fit transmission spectrum (orange) from equilibrium chemistry retrieval for STIS+WFC3+NIRCam observations is compared to the spectrum where the best-fit metallicity value is changed to match the retrieved H2O abundance from the free-chemistry retrieval shown in blue.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Comparison of forward models from SANSAR and POSEIDON. Here, we have used the opacity files of POSEIDON in SANSAR. The bottom panel shows the difference between SANSAR and POSEIDON forward model binned at R ∼ 100.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Retrieved posterior of different parameters with free-chemistry retrieval of HD 209458b obtained with STIS+WFC3+NIRCam observations. Here, retrieval was performed with the correlated-k method.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: This figure shows the accuracy of bicubic convolution interpolation. The red curve represents the true k-coefficient at ∼ 1 mbar and 1360 K, pressure and temperature, respectively, whereas the green curve is the interpolated. The bottom plot shows the percentage error of interpolated values with respect to the true value.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Side view schematic of a planet in transit being observed by a telescope (JWST).
Paper: A Short History of (Orbital) Decay: Roman’s Prospects for Detecting Dying Planets
Authors: Kylee Carden, B. Scott Gaudi, Robert F. Wilson
Figure caption: The distributions of dP/dt and σdP/dt for each simulated planet detection. These quantities are highly correlated due to the strong dependence of each on the planet’s orbital period, as shown by the color bar. WASP-12 b has dP/dt ∼ 30 ms yr–1.
Paper: A Short History of (Orbital) Decay: Roman’s Prospects for Detecting Dying Planets
Authors: Kylee Carden, B. Scott Gaudi, Robert F. Wilson
Figure caption: The histogram of orbital decay SNRs > 10−3 using three distinct values of ﹩{Q}_{* }^{{\prime} }﹩.
Paper: A Short History of (Orbital) Decay: Roman’s Prospects for Detecting Dying Planets
Authors: Kylee Carden, B. Scott Gaudi, Robert F. Wilson
Figure caption: The distribution of the planets from the R. F. Wilson et al. (2023) simulated planet catalog in period and radius. The color bar indicates the apparent magnitude of each planet’s host star.
Paper: A Short History of (Orbital) Decay: Roman’s Prospects for Detecting Dying Planets
Authors: Kylee Carden, B. Scott Gaudi, Robert F. Wilson
Figure caption: The reduction in uncertainty, relative to the GBTDS uncertainty σdP/dt,0, that can be achieved with an additional season of observing carried out some number of months after the conclusion of the GBTDS.
Paper: A Short History of (Orbital) Decay: Roman’s Prospects for Detecting Dying Planets
Authors: Kylee Carden, B. Scott Gaudi, Robert F. Wilson
Figure caption: Example transit timing for planet #1923 in Table 1 from the GBTDS using the M. T. Penny et al. (2019) notional survey. This planet has the most robust detection of orbital decay in the simulated catalog.
Paper: A Short History of (Orbital) Decay: Roman’s Prospects for Detecting Dying Planets
Authors: Kylee Carden, B. Scott Gaudi, Robert F. Wilson
Figure caption: Comparison of the analytic estimate of uncertainty with the numerical results as a function of period, showing good agreement for all three parameters in the short-period regime.
Paper: A Short History of (Orbital) Decay: Roman’s Prospects for Detecting Dying Planets
Authors: Kylee Carden, B. Scott Gaudi, Robert F. Wilson
Figure caption: The histogram of orbital decay SNRs > 10−3 using the ﹩{Q}_{* }^{{\prime} }﹩ parameterization from S. C. Millholland et al. (2025).
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: KDEs of posterior stellar mass (left), young fraction by mass (middle), and medium-aged fraction by mass (right) for the set of mock galaxies simulated at distances from 5 to 19 Mpc (see Figure 3); the colors of these curves match the points in that figure. Priors are shown in light gray, and the true values are shown as vertical dashed lines. We note that the apparent leaking of the posterior distributions beyond the prior bounds is a visual artifact from the KDE smoothing. We find that, in addition to the distances being recovered for these mocks, the stellar population parameters are also reasonably well-fit. We do not show the KDEs for metallicity, as the mass–metallicity relation prior influences the derived metallicity (but they are consistent with the model values as well). The fraction of the mass in young (50–250 Myr old) stars has a prior that preferences an Fy of 0, so the ability for the inference to constrain it to 0.02 (the value for this model) with no weight at 0.0 implies the value is not prior dominated. In contrast, the intermediate-age population (a single-age burst of 1.5 Gyr in age) is relatively unconstrained from its uniform prior between 0 and 0.2, though there is a recovered increased likelihood toward the correct value for this model.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Schematic overview of the Silkscreen architecture. The external inputs to Silkscreen are shown at the top, colored by where in the code they are used; in our bespoke fitting paradigm, easily measurable parameters of input galaxies, including the Sérsic parameters, are fixed, along with the parameters describing the cutout image (i.e., which survey bands the imaging was obtained in, the exposure times therein, and the empirical PSF in the vicinity of the target). These inputs are passed to ArtPop, and all generated simulations will share the values set by these inputs. Additionally, we pass a large “injection patch” of sky from the survey being used in the vicinity of the galaxy cutout to ArtPop. During training, generated model galaxies are placed in randomly chosen locations in this large patch. The final input to Silkscreen is the multiband image cutout of the real galaxy, which is utilized in the learning stage. In four rounds, ArtPop generates 25,000 simulations, drawn (at first) from highly uninformative priors. These simulations and labels are then passed to the ResNet for summary statistic extraction; then, SBI is used to infer via neural flows the posterior on the fit parameters given the span of generated models and the true input image. The posterior inferred in each round is then adopted as the prior for the subsequent round, and the process is repeated. As illustrated in the bottom row of the schematic, each sequential round (tends to) tighten the posterior, as progressively smaller regions of parameter space (at progressively higher likelihoods) are sampled. The final round’s posterior is adopted as the output posterior distribution on the parameters.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Inferred vs. actual distance for a simulated model galaxy of log M* = 7.4 M⊙, with a metallicity of −1.4, with Fy set to 0.02 (2% by mass) and Fm set to 0.17. We inject this galaxy at different distances and fit it with Silkscreen. We keep a fixed Sérsic index of 1.1 for this test, and fix the effective radius to 15″. This means that the more distant galaxies are intrinsically larger, and so it allows for the demonstration that Silkscreen is not using the apparent size as a marker for distance. We find that Silkscreen is able to recover the distances to the injected systems well, with all galaxies falling within 1σ of the true values and with no systematic bias in the recovered distances.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: HSC three-color image of ESO 294-010 (∼2 Mpc) compared with an ArtPop model output. The images generated by ArtPop achieve remarkable fidelity in the regime of semi-resolved galaxies, combining both the intrinsic properties of the stellar systems with the observational properties of a given input telescope and survey to produce images that are in many cases indistinguishable from the data. This ability to produce realistic “simulations” unlocks the use of simulation-based inference as a technique for comparing ArtPop models to real images in a likelihood-free manner. In this example, the galaxy parameters for the ArtPop model shown were inferred using the framework presented in this paper.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Simulation-based calibration (SBC) tests applied to the initial round of training for the galaxy ESO 410-005 using 500 prior samples. The distribution of ranks for an unbiased posterior is uniformly distributed; for our network, we find no statistical departure from uniformity across the posterior ranks. The gray band shows the expected range of values calculated using the 0.5%–99.5% percentile of the binomial distribution for a given number of bins (S. Talts et al. 2018).
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Showcasing Silkscreen inference performed on the galaxy ESO 410-005 at a known distance of 1.9 Mpc (G. S. Da Costa et al. 2010; R. B. Tully et al. 2013). This corner plot displays the prior distribution along with the posterior produced from each successive round of training. The constraints from the posterior become more precise after the initial round of training, where targeted simulations are used and appear to converge between the third and fourth rounds. The distance is very well-determined. The posteriors of the stellar population parameters Fm and [Fe/H] follow the prior, but the stellar mass and Fy are also reasonably well-constrained.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Comparing the observed colors of ESO 410-05 to those measured from the posterior predictive images produced by Silkscreen. The red and blue histograms show the spread of g − r and r − z colors measured directly for 25 posterior predictive images. The lines show the observed color. We find the observed g − r color matches that of the posterior predictive images while the observed r − z color is slightly bluer by 0.075 mag.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Distance recoveries for a set of injections all at 10 Mpc, varying the model intrinsic size between 0.5, 0.75, and 1 kpc with a fixed n = 1, and the Sérsic index between 0.7, 1.0, and 1.5 with a fixed re = 0.75 kpc. We find that Silkscreen recovers the correct distance within 1σ in all cases, with no apparent systematic biases in recovered distance based on these parameters (albeit with a small test sample). The scatter in the distance estimates is ∼0.5 Mpc, corresponding to 5% at a distance of 10 Mpc.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: The observed image DECaLS image (top left) for the galaxy ESO 410-005 alongside posterior predictive images produced by Silkscreen. The simulated images match the overall characteristics of the observed image well “by eye,” reinforcing the idea that ArtPop, and the parameterization chosen here, can produce realistic images of dwarf galaxies.