adsabs/AstroCLIMB huggingface dataset:
Paper: TOI 762 A b and TIC 46432937 b: Two Giant Planets Transiting M-dwarf Stars
Authors: Joel D. Hartman, Daniel Bayliss, Rafael Brahm, Edward M. Bryant, Andrés Jordán, Gáspár Á. Bakos, Melissa J. Hobson, Elyar Sedaghati, Xavier Bonfils, Marion Cointepas, Jose Manuel Almenara, Khalid Barkaoui, Mathilde Timmermans, George Dransfield, Elsa Ducrot, Sebastián Zúñiga-Fernández, Matthew J. Hooton, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Amaury H. M. J. Triaud, Michaël Gillon, Emmanuel Jehin, William C. Waalkes, Zachory K. Berta-Thompson, Steve B. Howell, Elise Furlan, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David Rapetti, Karen A. Collins, David Charbonneau, Christopher J. Burke, David R. Rodriguez
Figure caption: Additional follow-up light curves of TIC 46432937, shown as described in Figure 2.
Paper: TOI 762 A b and TIC 46432937 b: Two Giant Planets Transiting M-dwarf Stars
Authors: Joel D. Hartman, Daniel Bayliss, Rafael Brahm, Edward M. Bryant, Andrés Jordán, Gáspár Á. Bakos, Melissa J. Hobson, Elyar Sedaghati, Xavier Bonfils, Marion Cointepas, Jose Manuel Almenara, Khalid Barkaoui, Mathilde Timmermans, George Dransfield, Elsa Ducrot, Sebastián Zúñiga-Fernández, Matthew J. Hooton, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Amaury H. M. J. Triaud, Michaël Gillon, Emmanuel Jehin, William C. Waalkes, Zachory K. Berta-Thompson, Steve B. Howell, Elise Furlan, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David Rapetti, Karen A. Collins, David Charbonneau, Christopher J. Burke, David R. Rodriguez
Figure caption: Same as Figure 2, here we show the observations of TIC 46432937 together with our best-fit model. Additional follow-up light curves of TIC 46432937 are shown in Figure 5.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Mean relative error between MIRAGE input point source images and PSF models for the F115W and F150W bandpasses. Panels and color bars are the same as in Figure 7.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Mean relative error between MIRAGE input point source images and PSF models for the F444W filter. Panels and color bars are the same as in Figure 7.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Average execution time as a function of the output size of the PSF side length plotted on a log scale.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Evaluation of mean relative error between stars and PSF models for simulated mosaics in the F444W bandpass. The left panels show the median of the vignettes. The panels and color bars are the same as in Figure 9.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Average execution time as a function of the degree of the interpolating polynomial on (33, 33) PSF models plotted on a log scale.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Mean relative error between stars and PSF models for simulated mosaics in the F115W bandpass. The left panels show the median of the vignettes. The panels and color bars are the same as in Figure 9.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Distribution of ﹩{\chi }_{\nu }^{2}﹩ for real data mosaics. Not shown are two PSFEx ﹩{\chi }_{\nu }^{2}﹩ values greater than 100 and four ShOpt ﹩{\chi }_{\nu }^{2}﹩ values greater than 100.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Evaluation of mean relative error between stars and PSF models for simulated mosaics in the F277W bandpass. The left panels show the median of the vignettes. The panels and color bars are the same as in Figure 9.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Examples of mean average error (top panel) and χ 2 residual figures (bottom panel), shown here for the simulated mosaics in F115W.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Petal diagrams approximating different PSFs. Different k values correspond to PSF with different numbers of spikes. The A value determines how long the spikes are. Here, all of the pixels inside the petals (gray) are set to a constant value, and everything outside is 0.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Stream plots demonstrating how variables ﹩\left[s,{g}_{1},{g}_{2}\right]﹩ vary across the field of view (in astrometric coordinates (u, v)) for the F115W simulated mosaic image. Recall that s corresponds to size, and g 1, g 2 correspond to shear.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Evaluation of mean relative error between stars and PSF models for real data mosaics in the F277W bandpass. The panels and color bars are the same as in Figure 11.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Mean relative error between stars and PSF models for real data mosaics in the F115W and F150W bandpasses. The color bars are the same as in Figure 11.
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: Number distributions of galaxies in galaxy groups. The histograms indicate the distributions derived from the galaxy group sample in the SDSS.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Sample sequence within the AU Mic dTemp time series. A Gaussian-process fit to the data is shown as an overplot (top panel), with the residual to that fit in the bottom panel. One sees the envelope of the signal decaying in strength through the first half of the sequence as well as the notable presence of a strong second harmonic signal (secondary bump appearing around JD = 2459030). The small-scale magnetic field measurements form J.-F. Donati et al. (2023) are shown for comparison. dTemp and 〈B〉 show a remarkable agreement in their overall behavior, with a strong anticorrelation.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: (1) Model dTemp for different impact parameters for the HD 189733 system and the corresponding broadband light curves (2) integrated over the SPIRou bandpass. Low-impact-parameter transits would lead to first an apparent increase of temperature (planet occulting the limb) and a decrease of the mean temperature when the planet occults regions close to the disk center. Grazing transits lead to a positive excursion only. (3) For the nominal impact parameter (b = 0.69) and a 2.8% spot filling factor (D. K. Sing et al. 2011), we show the predicted dTemp signal through transit (3) as well as the corresponding broadband light curve (4).
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption:  dTemp time series of four HD189733b transit observed with SPIRou and phase-binned values. One notes the ∼1 K increase in the apparent temperature of the host star close to ingress and egress as cooler regions of the stellar disk are masked by the planet. The beige domain corresponds to the window between first and fourth contact for an impact parameter of 0.69.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption:  dTemp time series for ϵ Eridani at optical wavelength with HARPS. Rotation-induced variability is detected in the second half of the data set and is readily described by a semiperiodic GP fit (top). The residuals to the GP fit are at the 0.1 K level (bottom). In both time series, individual points have been binned on a nightly basis.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Cartoon representation of the toy model used to predict the amplitude of the dTemp effect in the HD 189733b transit data. The impact parameter of 0.69 corresponds to that of the system; the relative radii of the host star and planet correspond to literature values. Unocculted spots covering 2.8% of the disk are shown (filling factor from D. K. Sing et al. 2011).
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: 〈B〉 as a function of dTemp for the time series shown in Figure 5. An increase in temperature is associated with a decrease in the small-scale magnetic field. This is qualitatively understood as a decrease in the number of active regions on the observed hemisphere, leading to a smaller level of activity, fewer observed stellar spots, and hence a hotter average temperature. The correlation between the quantities (–0.924) is excellent, suggesting that they trace the same underlying physical processes. The 1σ envelope of Equation (8) is highlighted in purple.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption:  dTemp time series for Barnard’s star (top panel). As expected from the modest level of activity of this thick disk star, a much milder variability is observed than for AU Mic, but nonetheless one notes the rotation-induced variability. The residual to the GP fit (bottom panel) shows sub-K rms, consistent with the σ jit = ﹩{0.493}_{-0.040}^{+0.037}﹩ K reported in Table 2.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Same as Figure 5 over the entire time series.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: (Top panel) Sample average spectra at 500 K steps for SPIRou. The corresponding gradient spectra are shown on the bottom row. One can see that lines that change in depth in the top plot correspond to strong temperature gradient features in the bottom plot.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Reparameterization function. For any ellipticity vector ﹩\left[{e}_{1},{e}_{2}\right]﹩ the associated shear vector ﹩\left[{g}_{1},{g}_{2}\right]﹩ has a norm in [0, 1).
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Parameter space for fitting an analytic profile, with sample iterations of the algorithm converging toward a learned ﹩\left[s,{g}_{1},{g}_{2}\right]﹩. Note that the cylinder extends upward toward infinity but is bounded from below by 0.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Mean relative error between MIRAGE input point source images and PSF models for the F277W filter. The left panels show the median MIRAGE cutout; the center panels show the median PSF cutout. The right panels show the average relative error between the MIRAGE and PSF cutouts. The top two rows are ShOpt, and the bottom two rows are PSFEx. Color bars for left and center panels show pixel intensity values in units of MJy sr−1. The color bars in the right panels show the (dimensionless) relative error. The MREs defined in Equation (7) are displayed in the titles of the mean residual images.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Evaluation of mean relative error between stars and PSF models for simulated mosaics in the F150W bandpass. The left panels show the median of the vignettes. Center panels show the median PSF cutout. The right panels show the average relative error between the vignette cutouts and the PSF cutouts. The top is PSFEx, the middle is ShOpt, and the bottom is PIFF.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Distribution of ﹩{\chi }_{\nu }^{2}﹩ for simulated data mosaics. PSFEx values are shown in blue, ShOpt values are shown in orange, and PIFF values are shown in green. For clarity, the plot excludes two PSFEx ﹩{\chi }_{\nu }^{2}﹩ values greater than 100, one ShOpt                         ﹩{\chi }_{\nu }^{2}﹩ value greater than 100, and two PIFF χ 2 values greater than 100.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Pictoral representation of multithreading in ShOpt. In this example, all of the pixels in the upper left of the pixel-grid renderings are interpolated across the field of view in thread 1, and all of the pixels in the upper right of the pixel-grid renderings are interpolated across the field of view in thread 2, and so on.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Evaluation of mean relative error between stars and PSF models for real data mosaics in the F444W bandpass. The left panels show the median star vignette; the center panels show the median PSF model; and the right panels show the mean residuals of individual star-PSF vignettes. The top row is PSFEx, and the bottom row is ShOpt.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Schema illustrating the computation of summary statistics for PSF model assessment. Individual star-PSF model pairs are compared to produce residual images, which are then averaged into a mean residual image for the ensemble.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Size–magnitude diagram for objects detected in the A6 mosaic in F444W A6. Blue points represent all sources; orange points show stars selected by stellar locus parameter cuts.