adsabs/AstroCLIMB huggingface dataset:
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Scale height H as a function of mean molecular weight μ using the best-fit properties for KELT-24 b derived in by each of our analyses Section 4. The shaded region is the 1σ deviation in H created by drawing from posteriors in T eq, R p, and M p. The mean molecular weights and scale heights of Jupiter and Saturn are shown for reference.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Top panel: Lomb–Scargle (Lomb 1976; Scargle 1982) periodogram in the RV data presented in this analysis. The ≈5.55 day period of KELT-24 b is strongly evident. Bottom panel: Lomb–Scargle periodogram of the residual RVs. We find weak evidence for periodicity at 149.2 days.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Allowed periods for a bound companion as the source of the single transit observed in TESS photometry are shaded in green, while possible periods that have been forbidden are hatched and shaded in red.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Mass–radius diagram of all known exoplanets with reported values for both parameters. The mass and radius of KELT-24 b determined by each of our individual global analyses are drawn in for reference. Density lines are also included. While there is good agreement between our three results here regarding the general nature of KELT-24 b as a large, dense planet, their internal discrepancies are apparent.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Phase-folded diagram of all 291 RVs used in our analysis. T1–T4 are the four MINERVA telescopes.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Full RV time series including all 291 RVs used in our analysis.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Simulated NIRISS SOSS (orange) and NIRSpec G395H (red) transmission spectra of KELT-24 b using four transit observations with each of the instruments generated using Pandexo (Batalha et al. 2017). The underlying model assumes a cloud-free, solar-metallicity atmosphere, which should be broadly representative given KELT-24 b’s mass and equilibrium temperature, and was created using Exo-Transmit (Kempton et al. 2017). These observations would be able to strongly constrain the overall metallicity in the atmosphere, as well as the specific atmospheric abundances of water, methane, carbon dioxide, and carbon monoxide. In principle, these constraints would also measure KELT-24 b’s atmospheric C/O ratio, which could place interesting constraints on the planet’s formation pathway.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Top panel: distribution of exoplanets with known projected obliquities, divided at a stellar temperature of T eff = 6100 K per the Kraft break (Kraft 1967). We note that all three of our stellar models derived here estimate an effective stellar temperature for KELT-24 well above 6100 K. Bottom panel: the same, but narrowed in on projected obliquities for well-aligned ﹩\left(| \lambda | \lt 10^\circ ,\,| {\sigma }_{\lambda }| \lt 10^\circ \right)﹩ planets. KELT-24 b is observed to be among the most massive planet with an orbit that is well-aligned to its host star.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Grid of all exoplanets with published masses, radii, and insolation fluxes. The relative point size corresponds to planet radius. Top: surface gravity g vs. insolation flux S. Bottom: planet density ρ vs. insolation flux S. The three planetary models for KELT-24 b are shown here, and it is, regardless of choice, among the most dense, high-gravity, highly irradiated exoplanets. All data are sourced from the NASA exoplanet archive.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Expected flux through the atmosphere of all known transiting exoplanets. Each of our three derived solutions for KELT-24 b are included here, and in any case it is estimated to be in the top 13% of all known transiting planets in terms of stellar flux passing through its atmosphere. We note that this derived flux is nearly identical for Sections 4.1 and 4.3, and so they appear to overlap here.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Collection of all transiting planets with measured masses, where the point size corresponds to the host star’s brightness. KELT-24 is in all cases among the brightest stars with a massive, transiting hot Jupiter.
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: (Left) Measured polarized light SPF for the disk, split between the eastern and western halves of the disk as defined by the approximate minor axis. We observe an asymmetry between the eastern and western halves, consistent with recent findings in Crotts et al. (2024) suggesting this disk may be slightly eccentric. (Right) The measured east/west SPFs divided by a Rayleigh polarization curve, along with HG functions fit to each SPF. There is a lesser but still distinct asymmetry between the two halves of the disk, and the HG function is a poor fit for the eastern half.
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: Maximum-likelihood SED model from MCFOST (as a dashed black line, with synthetic photometric points marked) compared to available photometry (colored according to its source). The best-fit model requires sub-blowout size grains and a close-in inner radius around ∼3 au. Five hundred additional SED models randomly drawn from the post-burn-in MCMC are plotted in gray.
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: Single-component blackbody models using best-fit values to available photometry for HD 156623, with fractional residuals shown below. The dust’s blackbody contribution to the SED is plotted in red. (Left) For a simple single-component blackbody SED, the photometry is best fit with temperature T = 184 ± 23 K. (Right) For a modified-emissivity single-component blackbody SED, the photometry is best fit with T = 140 ± 23 K and λ 0 = 219 μm. Neither model is able to capture the 9 μm AKARI point, and a modified emissivity is necessary to reproduce the flux observed by ALMA.
Paper: Gemini Planet Imager Observations of a Resolved Low-inclination Debris Disk around HD 156623
Authors: Briley L. Lewis, Michael P. Fitzgerald, Thomas M. Esposito, Pauline Arriaga, Ronald López, Katie A. Crotts, Gaspard Duchêne, Katherine B. Follette, Justin Hom, Paul Kalas, Brenda C. Matthews, Maxwell Millar-Blanchaer, David J. Wilner, Johan Mazoyer, Bruce Macintosh
Figure caption: Corner plot for MCMC fit with photometry and MCFOST SED models. The reported value for r in is an upper bound (<13.43 au at 99.7% confidence), as seen in the posterior distribution. Additionally, the value for log﹩{a}_{\min }﹩ is also only an upper limit of −0.685 (0.21 μm); this suggests that different assumptions for the grain composition and/or size distribution may be needed to fully understand the minimum grain size of this system.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: The figure shows simulated images with different levels of 							complex-background noise. The second and third parts show the results of 							the same original simulated image using different levels of 							complex-background noise. The first column image represents the original 							simulated image, while the second to fourth columns images represent 							images with different complex-background noise. Images of columns 5 to 7 							are results obtained by our method with different mask sizes and 							combinations of original image and the contour of ground-truth 							complex-background noise distribution.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: This figure shows MAE of new sets of simulated images obtained by our 							methods (from FWHM = 0.5 to FWHM = 2.0). The black straight line stands 							for mean values of all images and the red dotted line stands for MAEs of 							the same image with different blur levels.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: The figure shows the photometric error comparison between the masked 							region and other areas for each image under different MAE results.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: The figures presented here depict simulated images generated based on the 							previously defined parameters. As illustrated, these images encompass a 							variety of celestial objects, including stars and galaxies.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: The figure shows the masking results by our method in continuous 							observations, along with the corresponding variations in photometric 							errors in different regions.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: This figure shows MAE and complex-background noise. As this diagram 							shows, the MAE could be used to assess complex-background noise levels. 							However, when the complex-background noise level is high, our algorithm 							is not sensitive to changes.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: The figure shows the relationship between the MAE and the photometric 							errors. The black straight line stands for mean values and the red 							dotted line stands for the median values of all images.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: Two frames of GWAC images affected by shutter malfunctions and their 							corresponding masks.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: This figure shows the data selected by our algorithm with different mask 							ratios.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: Sample diagnostic plots for 19,916 asteroids detected in the J band. Left: absolute magnitude in J vs. predicted absolute magnitude in V. The color indicates the varying search radius sizes (blue: 5.″0 radius, orange: 1.″0 radius, green: 0.″25 radius). A larger match threshold creates more scatter away from the line, which are probably incorrect (false) matches. A smaller match threshold increases fidelity but decreases the overall size of our catalog. We choose a compromise value of 1″. Right: predicted J values (calculated from average V–J color of 1.54) vs. observed J values in the WSA catalog. The vertical lines show the limiting magnitudes for signal-to-noise ratio SNR = 5, 10.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: The positions of asteroid matches plotted over the footprint of the publicly released UHS survey. White spaces designate sky coverage elsewhere in the UKIDSS series (Large Area Survey, Galactic Plane Survey, and/or Galactic Cluster Survey), which was excluded from the UHS public release. The matches are densely clustered around the ecliptic, as is expected for asteroid populations.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: Histograms of the distribution of asteroid magnitudes in the V (left), J (center), and K (right) filters. There are 19,916 asteroid recoveries in J and 6,222 total asteroid recoveries in K. The V magnitudes are for all 26,138 recoveries and are predicted by the MPC as queried by asteroid number. The approximate limiting magnitudes of our detections are J ∼ 20, K ∼ 18, and V ∼ 20. A few objects have V–J  > 4 and are likely false positives. This is discussed at length in Section 5.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: Dependence of J–K color on absolute (left) and apparent (right) V magnitude. The vertical line on the right panel shows the approximate limiting magnitude of Sykes (2000). The majority of our objects lie to the left of this line, indicating that our data represent a novel magnitude range that generally corresponds to smaller objects.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: The number of observations, in either filter, of the recovered asteroids. Most asteroids were found only once. The maximum number of observations for a single asteroid is six. Only asteroids with two or more observations can possibly have J–K colors derived.
Paper: Infrared Colors of Small Serendipitously Found Asteroids in the UKIRT Hemisphere Survey
Authors: Samantha G. Morrison, Ryder H. Strauss, David E. Trilling, Andy J. López-Oquendo, Justice Bruursema, Frederick J. Vrba
Figure caption: Prevalence of internal processing flags in preliminary asteroid match attempts. The flag meanings are detailed in Table 1. The majority of image/asteroid pair rejections are due to flag −3: asteroid found outside the image’s panels. This is likely due to the particularities of the WFCAM focal plane layout. The next most common flag is −4 due to blank source catalogs in the WFCAM Science Archive.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: JWST NIRSpec IFU G395H/F290LP R ∼ 2900 spectrum of HD 19467 B spanning 2.9–5.3 μm, obtained for a companion at a contrast of ∼10−4 and separation of 1.″6 relative to the host star. The custom data analysis developed to process and extract this spectrum is summarized in Section 2 and a more detailed procedure can be found in Ruffio et al. (2024). A cursory molecular inventory in this NIRSpec spectrum indicates the presence of H2O, CH4, CO, and CO2, which are labeled in gray above their corresponding wavelength ranges. The spectrum is in dark blue, the error is in light blue, and NIRCam photometry from our re-reduction of the Greenbaum et al. (2023) observations is shown in pink. The top panel shows the entirety of JWST data for HD 19467 B. The middle panel focuses in on the first detector wavelength range of NIRSpec (2.9–4.1 μm), and the third panel shows the second detector wavelength range of NIRSpec (4.2–5.3 μm).
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: The NIRSpec spectrum of HD 19467 B in black plotted against the best-fit models; BT-Settl08 in magenta in the top panel, Sonora Bobcat in blue in the second panel, DRIFT-PHOENIX in orange in the third panel, and NEWERA-PHOENIX, in green in the fourth panel. The residuals are plotted in the final panel in the corresponding colors to their models. A black line was drawn at zero, and the smallest residuals were from the NEWERA-PHOENIX model grid with the NIRSpec continuum errors plotted in gray. This illustrates the need for updated models that include disequilibrium effects to properly fit the 3–5 μm wavelength regime.