adsabs/AstroCLIMB huggingface dataset:
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Histograms of the distributions of all fit parameters from the three-planet transit model fit. The parameters fitted for TOI-6276.01 (HD 101581 c), TOI-6276.02 (HD 101581 b), and TOI-6276.03 are shown in green, orange, and red, respectively.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: 18.5 μm image of NGC 7027 (gray scale) created from a 3 × 3 mosaic of MRS Channel 4A observations from PID 1523. The blue, green, yellow, and red rectangles represent the single-tile MRS fields of view for Channels 1, 2, 3, and 4 respectively.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Photometric calibration vectors for Channel 1B derived from observations of O9 V star 10 Lac and G3 V star 16 Cyg B. Gray and blue lines show the ratio of the model to observed stellar spectrum for 10 Lac and 16 Cyg B, respectively, while the black and orange lines show the basis-spline fits. The dashed vertical lines indicate the wavelength limits used by the standard pipeline to build spectral cubes for this band; outside these limits partial spatial coverage of the field makes the spectra unreliable. The vertical offset between calibration vectors derived from 10 Lac vs. 16 Cyg B is real. The emission feature in the 10 Lac spectrum at 5.908 μm is the H I 9–6 (Humphreys γ) transition.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Relative photometric calibration vectors of individual stars (colored lines) compared to that found for 10 Lac. Larger values correspond to stars that are fainter than the model and thus need larger correction factors to bring into agreement; note that discontinuities can occur between spectral bands. The dashed black line shows a low-order polynomial fit to the average of all 10 stars at λ < 18 μm; we adjust the calibration vector derived from 10 Lac by this model average.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Pixel flat field for MIRI MRS Channel 2A (7.51–8.77 μm) derived from observations of the planetary nebula NGC 7027. Note the narrow artifacts in the “dirty” flat (left panel) due to bright emission lines within the nebula that are patched to create the final “clean” flat (right panel). Prominent spectral artifacts are labeled; dark artifacts near the top of the detector are due to extremely bright [Mg V] emission in Channel 1A on the other half of the detector. Large-scale variations in flat-field values between and across slices are due to differences in the effective pixel area, while bright (dark) periodic spectral banding in the vertical (dispersion) direction are due to the pixel flat fixing some residual fringing signal not fully corrected by the fringe flat.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Ratio of the count rate produced by identical observations of the MRS internal calibration lamps in 2023 June (blue points) and 2024 April (red points) to observations obtained in 2022 April. Light blue and red points indicate individual detector pixels, while the dark blue and red lines represent b-spline fits to the blue points at the spectral resolution of the MRS. The discontinuities at overlapping wavelength ranges represent jumps between individual spectral bands.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Relative count rate produced over time from identical observations of the MRS internal calibration lamps at the median wavelength of each of the 12 MRS spectral bands 1A–4C. Solid points show measured values while solid and dotted–dashed lines indicate the empirical model fits. Large gaps in time coverage appear when the MRS was offline in Fall 2022 for investigation of a (likely unrelated) grating wheel anomaly, and in Winter 2023 when multiple observations failed for unrelated reasons. Band “C” monitoring observations are missing prior to 2023 March due to an error in the PID 1518 program configuration, which complicates the fitting of a loss model without the corresponding Fall 2022 points.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Channel 2C spectrum of NGC 7027 (blue points) normalized by a continuum fit that interpolates over the 11.55–11.65 μm wavelength range. All detector pixels are plotted individually according to their native wavelength solution, resulting in a dramatic oversampling of the spectrum compared to the nominal spectral resolution of the instrument. The resulting spectrum (nicknamed the “bear claw”) shows strong evidence for systematic absorption due to GeO. The solid black line represents the cubic b-spline fit incorporated into the pixel flat field.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Default extraction aperture radius (blue line), and inner and outer background annulus radii (orange and green lines, respectively) for MRS point-source spectral extraction.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Flux-calibrated spectrum of O9 V star 10 Lac. Individual colored segments represent spectra from specific MRS bands while the solid black line represents the CALSPEC model. Note that the 10 Lac spectrum deviates systematically from the model as the MRS photometric calibration is normalized to the average of all standard stars.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: MRS aperture-correction factors for point-source aperture photometry with extraction radii of 1, 2, and 3 times the PSF FWHM. Approximately 5%–10% of the total flux is lost outside the IFU field of view.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Systematic repeatability for all 12 MRS spectral bands based on regular observations of HD 163466 (A7 Vm). Filled blue squares show the median flux ratio between repeated spectra in each band from 2022 June to 2024 July. Inset text values indicate the repeatability (defined as the rms scatter σs) between the individual measurements. The repeatability is below 1% in Channels 1A–3C, while the greater scatter in Channel 4 is driven by partly by increasing uncertainty in the background subtraction. The point highlighted in red was observed on 2024 February 28 during a major primary mirror tilt event in which the wave front error degraded to 327 nm; we exclude this point from our statistics.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Top panel: calibrated spectrum of the circumstellar disk SAO 206462 in Channels 3 and 4. Bottom panel: arbitrarily renormalized spectrum of the asteroid 515 Athalia (see text), overplotted with a best-fit T = 193.9 K blackbody model. In both plots the vertical dashed black line indicates the nominal Channel 4C wavelength cutoff of 27.9 μm, above which calibration quality decreases rapidly. The lower inset shows the ratio between the renormalized 515 Athalia spectrum and the best-fit model.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: 1D spectra of the A3 V standard star HD 2811 (top panel) and main-belt asteroid 515 Athalia (bottom panel) illustrating the impact of the 12 μm spectral leak, which manifests as a fraction of the signal at 6.1 μm being added to the 12.2 μm flux. An automated correction for this leak is available in the JWST calibration pipeline; while no correction is necessary for red sources such as 515 Athalia with minimal 6.1 μm flux, correction is essential for blue sources such as HD 2811.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: S/N ratio of the MIRI MRS spectrum of HD 163466 (A7 Vm) obtained by PID 1536. The solid blue and orange lines represent estimates provided by the JWST calibration pipeline corresponding to Builds 10.1 and 11.0 respectively, while the expected S/N based on the Cycle 3 ETC (v3.0) is shown as a green solid line. The solid black line represents an empirical estimate bootstrapped from rms variations with wavelength in the extracted spectrum, while the red filled squares represent empirical estimates based on repeated observations throughout the first 2 yr of the mission.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Continuum-normalized spectrum of 10 Lac (solid blue line) and the corresponding CALSPEC model (solid orange line, vertically offset for clarity). Note that many wavelengths show sinusoidal artifacts at the ∼0.5% level due to fringing that has not been completely corrected by the JWST calibration pipeline. Dashed gray lines indicate major H transition lines (labeled by quantum level), while dashed orange lines indicate He transitions. Note that the bottom panel has a larger vertical scale.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Stochastic noise for all 12 MRS spectral bands based on regular observations of HD 163466 (A7 Vm). Blue histograms represent the range of values about the median for each wavelength element in the extracted spectra, after correction for systematic per-band offsets. The rms of these histograms (σr) describes the effective noise in the spectra at a given wavelength across repeated observations.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Calibrated spectra and CALSPEC models for 10 Lac (O9 V; blue and orange lines, respectively) and μ Col (O9.5 V; green and red lines, respectively, scaled by a factor of 1.5) illustrating a broad emission feature in the 10 Lac spectrum that we identify as due to [Ne v] 14.3217 μm. This feature is not observed in μ Col, which has a similar spectral class.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: As Figure 8, but for Channel 4C using observations of main-belt asteroid 515 Athalia. In this case, however, the spline fit was performed in inverse-photon units to reduce artifacts that can occur when the effective response dips to near zero.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Relative calibration factor (averaged across 5–18 μm) derived from each spectrophotometric calibration star as a function of spectral class (colored diamonds). The average and rms distribution widths within each class are shown as filled squares (offset horizontally for clarity).
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Left panel: observed MIRI MRS brightness temperatures of Saturn in 2022 November. Data were zonally (i.e., east–west) averaged along Saturn’s central meridian from the equator to the north pole, and then convolved with the spectral response function of Cassini/CIRS (15 cm−1) to display as a function of wavelength. Right panel: difference in zonally averaged brightness temperature between 2022 MIRI MRS observations and 2017 Cassini CIRS observations.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Relative calibration factor derived from each spectrophotometric calibration star (colored diamonds) as a function of the maximum detector well depth, MJD of observation, and 10 μm flux density. The calibration factor does not have a trend with any of these variables, indicating both that the time-dependent count-rate loss model is working well and that there are no obvious detector-dependent systematics.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Ratio between the flux density observed by the MIRI MRS and Spitzer IRAC in the IRAC 5.8 μm and 8.0 μm band passes. Colored diamonds show values from individual stars, while filled squares (offset for clarity) represent the average and rms distribution within each band pass.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Continuum-normalized spectra (solid blue lines) and normalized CALSPEC models (solid orange lines) for each of the 10 observed standard stars in the wavelength range λ = 4.9–6.7 μm. Dashed vertical lines in all panels represent the wavelengths of major atomic hydrogen transitions.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Ratio between the stellar spectra observed by MIRI MRS and Spitzer IRS (colored lines). Note that both HD 163466 and HR 5467 have been trimmed at about 20 μm due to their low S/N at longer wavelengths.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: As Figure 25 but for the wavelength range λ = 16.0–27.0 μm. Note that the vertical scale is much larger than in Figures 25–27 to accommodate the lower S/N at long wavelengths.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: Ratio between the flux density observed by the MIRI MRS and the MIRI Imager in eight of the nine imaging band passes. Colored diamonds show values from individual stars, while filled squares (offset for clarity) represent the average and rms distribution within each band pass.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: As Figure 25 but for the wavelength range λ = 10.5–16.0 μm.
Paper: The James Webb Space Telescope Absolute Flux Calibration. III. Mid-infrared Instrument Medium Resolution Integral Field Unit Spectrometer
Authors: David R. Law, Ioannis Argyriou, Karl D. Gordon, G. C. Sloan, Danny Gasman, Alistair Glasse, Kirsten Larson, Leigh N. Fletcher, Alvaro Labiano, Alberto Noriega-Crespo
Figure caption: As Figure 25 but for the wavelength range λ = 6.7–10.5 μm.
Paper: Planetary Mass Determinations from a Simplified Photodynamical Model—Application to the Complete Kepler Dataset
Authors: Aviv Ofir, Gideon Yoffe, Oded Aharonson
Figure caption: Comparison of the mass estimates of objects with both literature and this work’s mass estimates that are significant to better than 3σ. The red symbols use older references (2014 and earlier), while the blue symbols use newer references (2015 and later). The recent estimates are more consistent with our own than earlier ones—demonstrating increasing agreement between different analyses of the same objects. We label systems in which the newer literature mass estimates differ from our own by more than 4σ. Note that there are duplicate entries: if multiple solutions are given in the paper, both appear here (with a common abscissa value). Also, if more than one literature source exists, all will be given (with a common ordinate value).
Paper: Planetary Mass Determinations from a Simplified Photodynamical Model—Application to the Complete Kepler Dataset
Authors: Aviv Ofir, Gideon Yoffe, Oded Aharonson
Figure caption: The mass–radius plane for all planets with significant mass in this study (maroon error bars). Note that a planet may appear more than once in the plot if more than one group of solutions is arrived at, and these points will share a common radius. Overplotted are lines of constant bulk density, as well as all planets with mass and radii determined to be better than 3σ from the NASA NExSci database (light gray points).
Paper: Planetary Mass Determinations from a Simplified Photodynamical Model—Application to the Complete Kepler Dataset
Authors: Aviv Ofir, Gideon Yoffe, Oded Aharonson
Figure caption: Relative mass error comparison for planets with significant masses both in this work as well as in the literature (the ones appearing in Figure 1). The literature median relative mass uncertainty is observed to be about ∼22% higher than the current study’s relative mass uncertainty.
Paper: An Ultrafast Image Simulation Technique with Spatially Variable Point-spread Functions
Authors: Zeyu Bai, Peng Jia, Jiameng Lv, Xiang Zhang, Wennan Xiang, Lin Nie
Figure caption: The method proposed in this study is delineated in this figure, which illustrates a two-stage procedure for image simulation. The first stage involves coefficient matrix generation, wherein the PSF basis is derived from empirical PSF data. The second stage encompasses the convolution and addition step, where the previously obtained PSF basis functions are convolved with the original image to generate image basis. These image bases are weighted by the coefficients in each pixel and added together to produce the final blurred image.