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Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Left: stellar radius vs. effective temperature for stars in the KGPS I sample (blue) compared to the CLS (Rosenthal et al. 2021; gray). Stars for which we detected Jovian companions are ringed in magenta; other stars with nontransiting companions are ringed in green. The outlier in the giant branch is KOI-1241 (Kepler-56). Right: the continuous distribution function (CDF) of stellar metallicities from three different surveys: Raghavan et al. (2010), Rosenthal et al. (2021), and KGPS.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Left: the ﹩M\sin i﹩ values (measured or estimated from the Weiss & Marcy 2014 mass–radius relation) of all the transiting and nontransiting planets in KGPS I (orange histogram), and the maximum ﹩M\sin i﹩ value per star (blue histogram). Right: upper limits on ﹩M\sin i﹩ for Kepler stars with RVs. The upper limits are based on models in which a linear trend (dv/dt) is adopted.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1442 (Kepler-407). Left: the best-fit model includes a nontransiting planet, Kepler-407 c (orbital parameters inset in phase-folded panel). Right: the periodogram of the RVs after removing the signals from the transiting planet (top) and both planets (bottom).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1781 (Kepler-411). No nontransiting companions are detected, although the RV variability is higher than typical for our sample, likely because of high stellar activity.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-701 (Kepler-62). Left: this system has five transiting companions, for which the RVs provide only upper limits (not detections). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1241 (Kepler-56). Left: RVs are from HIRES (black circles) and HARPS-N (maroon triangles). The best-fit model has two nontransiting giant planets (details inset in RV panels, left).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1909 (Kepler-334). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1692 (Kepler-314). There is a marginal trend in the RVs.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1612 (Kepler-408). Left: there is a marginally significant long-term trend to the RVs consistent with a stellar-mass companion.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-623 (Kepler-197). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-719 (Kepler-220). No nontransiting companions are detected.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Components of L  ν  from nuclear reactions over the lifetime of an M ZAMS = 20 M ⊙ model for all six metallicities. The x-axis is the time to the onset of CC. Evolutionary phases are shown by the colored regions and labeled. Curves show the largest contributions by the burning processes and weak reactions listed in the legend.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Average electron neutrino energy for beta decays (top), and average electron antineutrino energy for inverse-beta decays (bottom) for the M ZAMS = 20 M ⊙ models across all six metallicities. Curves are smoothed with a 50 time step moving-average filter. The average pair-neutrino energy is shown by the black curve, with the gray band giving the lower 10% and upper 90% pair-neutrino energies. Phases of evolution are shown by the colored panels and labeled. The horizontal dashed line shows a representative ≃1.8 MeV detection threshold to inverse-beta decay of current neutrino detectors (e.g., Simpson et al. 2019; Harada et al. 2023). The average electron neutrino and antineutrino energies are to first order independent of Z.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Average electron neutrino energies for beta decay processes (top panel), average electron antineutrino energies for inverse-beta decay processes (second panel), Johnson–Cousins B − V and V − K colors (third and fourth panels), and neutrino light to mass ratio for a simple stellar population (bottom panel) for all six metallicities.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Tracks in a γHRD (left) and νHRD (right) from ZAMS to the onset of CC for the M ZAMS = 20 M ⊙ models across all six metallicities. Approximate locations of evolutionary phases are labeled or marked with a black dashed line. Luminosities are normalized to L ⊙ = 3.828 × 1033 erg s−1 (Prša et al. 2016).
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Fraction of E  ν  emitted at different phases of evolution for all six metallicities (colored circles). From top to bottom, the panels show ﹩{[E/{E}_{\mathrm{tot}}]}_{\nu }﹩ for H burning, He burning, C burning, O burning and Si burning to the onset of CC.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Cluster L  γ  and L  ν  light curves (top) and the ratio L  γ /L  ν  (bottom) using Equation (21) with M = 1 M ⊙ for all six metallicities.
Paper: Stellar Neutrino Emission across the Mass–Metallicity Plane
Authors: Ebraheem Farag, F. X. Timmes, Morgan T. Chidester, Samalka Anandagoda, Dieter H. Hartmann
Figure caption: Cluster L  γ  and L  ν  light curves from the evolution models for all six metallicities. Overlayed are quadratic fitting functions with the coefficients for each metallicity listed (see Equation (21)).
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: Five CL AGN example spectra of Hα (top left), Hβ (top right), Mg II (middle left), C III] (middle right), and C IV (bottom) found in DESI. In each figure, the top panel displays the spectral pseudophotometry with red (blue) “x” markers for DESI (SDSS) and the light curves from CRTS (stars), PS1 (triangles), PTF (pentagons), and ZTF (dots) when available. The bottom left panel shows the smoothed SDSS and DESI spectra, represented by the blue and red lines, respectively (the shaded region corresponds to the original spectrum). The spectra are derived from survey pipelines and have been corrected for galactic extinction and shifted to the rest frame (without [O III]-based calibration). Note that the DESI spectrum covers less flux from the host galaxy than SDSS in 221044.76+245958.0 (Figure 4). The gray line in the lower right panel represents the difference between the two spectra, obtained by subtracting the dim spectrum from the bright one. The black dashed vertical lines indicate the presence of Hα, Hβ, Mg II, C III], C IV, and Lyα lines. The red and green blocks represent the CL line features and candidate features, respectively.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: The histograms of the upper limits of the transition timescales for CL AGNs and CL candidates in observed frame (left panel) and rest frame (right panel). The dashed lines represent the median values of three samples. While it seems like C III] and C IV have lower rest-frame timescales than the other lines, the observed-frame histogram shows that that is partially due to a selection effect, since time dilation has made it impossible from our sample to detect carbon rest-frame lags longer than 3500 days.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: The DESI Legacy images for J164331.90+304835.5 (left), J221044.76+245958.0 (middle), and J221925.57+272806.4 (right). The blue and red circles represent the fiber diameters of SDSS and DESI.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: Two example spurious CL phenomena due to the SDSS (left) and DESI (right) flux calibration problem. The legends are same as in Figure 3. In the left (right) figure, the SDSS (DESI) spectrum does not match the calculated PS1 (ZTF) photometric magnitude (“x” markers) in the light curve, while the DESI (SDSS) spectrum aligns with the light curve. This suggests a discrepancy in flux calibration for this spectrum.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: The histograms of the upper limits of the transition timescales for Hα + Hβ (left panel), Mg II (middle panel), and C III] + C IV (right panel) CL AGNs and CL candidates in the rest frame (right panel). The dashed lines represent the median values of the samples.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: The same as Figure 3, but showing the CL candidates for Hα, Hβ, Mg II, C III], and C IV, respectively.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Photometry measured in the super catalog of this work compared against predicted fluxes from EA z Y in all 15 available bands, based on SFHz_CORR templates. In each panel, the difference in AB magnitude (ΔMag) as a function of observed magnitude is summarized by the log10-scaled 2D gray density histogram. Colored curves indicate binned medians with two-sided envelopes enclosing 68% of sources per bin. The overall median offset is labeled on each panel computed on all magnitudes up to the magnitude limit of the deepest 10% of the corresponding image indicated by the colored solid vertical line; that of the median depth is indicated by the colored dashed vertical line. The typical photometric error is indicated by the dotted gray curves.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Behavior of JWST/NIRCam as measured by the WFS on 2022 November 5, from which our JWST PSFs are derived, based on a grid of 144 PSF realizations generated with WEBBPSF. Top: the spatial dependence of the energy enclosed in 0.″32 apertures for NIRCam Module A5 (NRCA5) and B5 (NRCB5) in F444W relative to that of the average PSF. Middle: EE as a function of aperture size colored by distance from the respective module center. Bottom: EE as a function of aperture size relative to that of the average PSF for each module, colored as before. PSF variability across NIRCam for F444W is minimal with ΔEE ≲ 0.1% in even small 0.″32 apertures.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: EE of the PSFs reported by WebbPSF (blue), with drizzling (light blue), and those determined in this work by stacking stars (orange). Yet even after accounting for drizzling, our observed PSFs are still wider at fixed EE, e.g., 80% (colored dashed lines) and, equivalently, they have less EE at fixed aperture diameter, e.g., 0.″3 (vertical gray lines). The corresponding photometric difference, however, is relatively small: 0.01–0.02 AB for SW and ≲0.01 for LW.