adsabs/AstroCLIMB huggingface dataset:
Paper: Chemical Abundances of M and G Dwarfs in the Hyades and Coma Berenices Open Clusters from APOGEE Spectra
Authors: Deusalete Vilar, Diogo Souto, Katia Cunha, Anderson Andrade-Silva, Verónica Loaiza-Tacuri, Fábio Wanderley, Verne V. Smith, Vinicius Grilo, Cintia F. Martinez, Bárbara Rojas-Ayala, Zachary Way
Figure caption: Stellar metallicity as a function of galactocentric distance (kiloparsecs). Our metallicity results are represented by solid symbols for G dwarfs and hollow symbols for M dwarfs. The Hyades are red circles, and Coma Berenices are blue triangles, plotted alongside the data from L. Magrini et al. (2023), shown as small gray Xs. Different lines on the graph represent the abundance gradient slopes for various ages, as described by L. Magrini et al. (2023).
Paper: Experimental Absorption Cross Sections for ZrO
Authors: Léo Lavy, Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: Ratio of simulated to raw experimental intensity for the set of ZrO lines. The simulated intensity is from the Bernath2025 spectrum (dots) or from the McKemmish2018 spectrum (plus signs). The fitted calibration curve ﹩C(\widetilde{\nu })﹩ is shown as a black solid lines. Not all observations were considered to fit this curve: the insert shows the weights given to each Bernath2025 line in the fit.
Paper: Experimental Absorption Cross Sections for ZrO
Authors: Léo Lavy, Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: Experimental absorption cross sections of ZrO at 2700 K. Air wavelength axis is shown.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Experimental Absorption Cross Sections for ZrO
Authors: Léo Lavy, Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: Electronic states of ZrO as calculated by J. Tabet et al. (2019), experimentally observed states (horizontal solid lines) and unobserved (horizontal dashed lines) for the singlet (blue) and the triplet (gray) manifolds. Transitions are represented by solid arrows when observed in this work, and represented by dotted gray arrows when observed in other studies.
Paper: Experimental Absorption Cross Sections for ZrO
Authors: Léo Lavy, Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: Raw overview emission spectrum of ZrO with the y-axis in arbitrary units (a). Zoom on the baseline, with slight blackbody radiation (b).
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Images (left column), azimuthal surface brightness profiles (middle column, 0° corresponds to west), and radial surface brightness profiles (right column) of NGC 5005 in different energy bands. The images were rebinned to one-eighth of the native ACIS pixel scale and smoothed with a 3 pixel Gaussian. The PSF in each band was normalized to match the source counts in the innermost region.
Paper: Experimental Absorption Cross Sections for ZrO
Authors: Léo Lavy, Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: C1Σ+–X1Σ+ transition dipole moment functions calculated by ab initio methods. This work is shown in red, P. F. Bernath et al. (2024a) is shown in blue, A. N. Perri et al. (2023) is shown in purple, and S. R. Langhoff & C. W. Bauschlicher (1988) is shown in green.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Left panel: Chandra full-band image with overlaid pie-shaped extraction regions spanning radii of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5–8″ and divided into 36 angular bins (10° each), used to extract azimuthal surface brightness profiles from the merged data and simulated PSF model. Right panel: same image with 20 overlaid concentric annuli used to extract radial surface brightness profiles from an r = 8″ region.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Merged 1/8 subpixel Chandra/ACIS-S images of NGC 5005, smoothed with a 3 pixel Gaussian kernel and shown in the indicated energy bands. Nonnuclear point sources, which were excluded from the spatial and spectral analyses, are marked. In this and all other images displayed in this paper, north is up and east is to the left, with color bars shown in units of counts.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Full-band Chandra image of NGC 5005, rebinned to one-eighth of the native ACIS pixel scale. White contours show the HST F814W wide-band image. The diffuse X-ray excess detected in the data (see radial profiles in Figure 4) likely includes contributions from unresolved sources in the galaxy, such as X-ray binaries, supernova remnants, stellar sources, and hot ISM. The red square has dimensions of 5″ × 5″, as in Figure 4, for comparison.
Paper: Experimental Absorption Cross Sections for ZrO
Authors: Léo Lavy, Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: Detailed view of the calibrated spectrum from this work (black, upward and downward) compared to Bernath2025 simulated spectrum (transparent blue, upward) and McKemmish2018 simulated spectrum (transparent red, downward). Bernath2025 has Voigt profiles with ﹩{\rm{\Delta }}{\widetilde{\nu }}_{L}﹩ = 0.04 cm−1 and ﹩{\rm{\Delta }}{\widetilde{\nu }}_{D}﹩ = 4.24 ﹩\times 1{0}^{-6}\widetilde{\nu }﹩ cm−1, McKemmish2018 has Voigt profiles with ﹩{\rm{\Delta }}{\widetilde{\nu }}_{L}﹩ = 0.04 cm−1 and ﹩{\rm{\Delta }}{\widetilde{\nu }}_{D}﹩ = 0.06 cm−1.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Left: merged Chandra 0.3–7 keV image of NGC 5005, as shown in Figure 1. Right: simulated PSF generated with MARX, scaled to match the total number of counts within the central 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 radius. Both panels are displayed with the same color scale, binning (1/8 pixel), and Gaussian smoothing to enable direct comparison.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Left panels: X-ray spectrum of the core region (r < 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5), showing the best-fit phenomenological model (top) and best fit for a 1-photoionization + 1-thermal component model (bottom). The hard X-ray emission is modeled with an MYTorusL component for the Fe Kα line (pink) and an MYTorusS component for the scattered continuum (cyan). Right panel: X-ray spectrum of the extended region (1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 < r < 5″), with the same model structure. The hard X-ray emission is modeled with an absorbed pexrav reflection component (purple).
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Left: Chandra ACIS-S image of the 0.3–7 keV emission, rebinned to one-eighth of the native pixel scale and smoothed with a Gaussian kernel (σ = 1.5 pixels). The inner white circle (r = 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5) marks the Chandra core extraction region, while the surrounding orange annulus (1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 < r < 5″) corresponds to the extended emission region analyzed in Section 4. Right: same as in the left panel, but with the outer green annulus indicating the Swift extraction region (r = 20″), while the outermost yellow annulus corresponds to the NuSTAR extraction region (r = 30″).
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Summary of possible scenarios for the nature of the central engine in NGC 5005. The panels illustrate three hypotheses: (1) a heavily obscured AGN, in which strong absorption could suppress the intrinsic X-ray luminosity; (2) a recently switched-off AGN, where the central engine has faded but [O III] emission from the extended NLR persists; and (3) an intrinsically low-luminosity AGN, where the central source is faint due to low accretion activity. All three scenarios are considered to explain the low observed X-ray luminosity derived from our spectral modeling.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Color map derived from the HST F547M/F814W ratio, tracing the blue-to-red continuum variation across the central region of NGC 5005 (A. Trindade Falcão et al. 2025). Dark red regions indicate areas with significant dust extinction. The circle has a radius of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 and marks the Chandra core extraction region, while the black cross marks the position of the Chandra 0.3–7 keV centroid.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Left panel: excitation map constructed from HST narrowband imaging, showing spatially resolved emission-line diagnostics. Seyfert-like regions are shown in green, H II-like in blue, LINER-like in orange, and cocoon-like in white. Right panel: Chandra 0.3–7 keV image, binned to one-eighth of the native ACIS pixel scale. In both panels, the inner white circle marks the nuclear (core) spectral extraction region, while the outer annulus delineates the extended extraction region.
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Comparison between the AGN photoionization model tailored to NGC 5005 (magenta grid) and the observed LINER-classified pixels (red dots) on the S-BPT diagram (A. Trindade Falcão et al. 2025). The model grid includes lines of constant metallicity (from left to right: 12 + log(O/H) = 7.99, 8.28, 8.43, 8.54, 8.70, 8.80, 8.96, 9.09) and lines of constant ionization parameter (from bottom to top: log U = –4.0, –3.5, –3.0, –2.5).
Paper: The X-Ray Emission of NGC 5005: An Unobscured Low-luminosity Active Galactic Nucleus with a Weakly Accreting Broad-line Region
Authors: Anna Trindade Falcão, R. Middei, G. Fabbiano, M. Elvis, P. Zhu, W. P. Maksym, D. Ł. Król, L. Feuillet
Figure caption: Joint NuSTAR–Swift spectra of NGC 5005 and best-fit model, with residuals shown below. The individual model components are indicated.
Paper: Erratum: “Time-dependent Acceleration and Escape of Charged Particles at Traveling Shocks in the Near-Sun Environment” (2025, ApJ, 979, 50)
Authors: Thomas M. Do, Federico Fraschetti, Jozsef Kota, Joe Giacalone, Christina M. S. Cohen, David J. McComas
Figure caption: Top row: proton flux measured by PSP/IS⊙IS/Epi-Lo (Chan P, level 2, v5) during the 2022 September 5 event. The upper X-axis shows the heliocentric distance of the Parker Solar Probe (PSP). The shock crossed PSP at 17:27:20 UT (O. M. Romeo et al. 2023). Bottom row, left: comparison of the Epi-Lo energy range (or momentum) as a function of 〈tacc〉 in the escape case from Equation (9), in purple, and in the case of no escape (from Equation (C2), in green). Here, we used ﹩{\bar{\kappa }}_{1}=8\times 1{0}^{16}﹩ cm s−2, ﹩{\bar{\kappa }}_{2}={\bar{\kappa }}_{1}/20﹩, ﹩\bar{T}1=800﹩ s, ﹩{\bar{T}}_{2}=20\,{\bar{T}}_{1}﹩, r = 1.6, U1 = 1000 km s−1, Vsh = U1 + 500 km s−1 with an average upstream solar wind speed 500 km s−1, δ1 = δ2 = 1.3, γ1 = γ2 = 0.5. Bottom row, right: comparison of the Epi-Lo energy range (or momentum) as a function of time of arrival tarr at Epi-Lo (same colors as the left panel) in the case from Equation (12) with tacc(p0) = 0. The cyan solid line indicates a velocity profile that is nondispersive.
Paper: Early Stellar Flybys are Unlikely: Improved Constraints from Sednoids and Large-q Trans-Neptunian Objects
Authors: Qingru Hu, 清茹 胡, Yukun Huang, 宇坤 黄, Brett Gladman, Wei Zhu, 伟 祝
Figure caption: The histograms of the concentration parameter κ derived from both simulation (colored steps) and observation (gray-filled steps) for stellar masses of M⋆ = 0.3M⊙ (left panels) and M⋆ = 1M⊙ (right panels). The upper panels present results using all simulated sednoids for the calculation of κ, whereas the lower panels restrict the analysis to synthetic sednoids with inclinations i < 30°. The 95% confidence interval (ranging from 2.5% to 97.5%) of the observed κ distribution is indicated by black dashed lines.
Paper: X-Ray Polarimetry of Accreting White Dwarfs: A Case Study of EX Hydrae
Authors: Sean J. Gunderson, Swati Ravi, Herman L. Marshall, Dustin K. Swarm, Richard Ignace, Yael Nazé, David P. Huenemoerder, Pragati Pradhan
Figure caption: Diagram of the accretion column and scattering geometry in EX Hya. The observer is out of the page, looking at the accretion column perpendicularly. On the sky, this would be oriented 34﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 to the northwest.
Paper: X-Ray Polarimetry of Accreting White Dwarfs: A Case Study of EX Hydrae
Authors: Sean J. Gunderson, Swati Ravi, Herman L. Marshall, Dustin K. Swarm, Richard Ignace, Yael Nazé, David P. Huenemoerder, Pragati Pradhan
Figure caption: Protractor plot of our X-ray polarization measurement (specifically PCUBE; blue contours) in the 2–3 keV band. Contours are the 68%, 90%, and 99% confidence contours. The gray shaded region is the confidence in the optical polarization. The red shaded region is the direction of the magnetic field pole based on the optical polarization.
Paper: X-Ray Polarimetry of Accreting White Dwarfs: A Case Study of EX Hydrae
Authors: Sean J. Gunderson, Swati Ravi, Herman L. Marshall, Dustin K. Swarm, Richard Ignace, Yael Nazé, David P. Huenemoerder, Pragati Pradhan
Figure caption: Polarization degree Π in 0.25 phase bins for the 2–3 keV band against spin phase with 68% uncertainties (black histogram). MDP99 values for each bin are plotted in red.
Paper: Erratum: “Status Report on the Chicago-Carnegie Hubble Program (CCHP): Measurement of the Hubble Constant Using the Hubble and James Webb Space Telescopes” (2025, ApJ, 985, 203)
Authors: Wendy L. Freedman, Barry F. Madore, Taylor J. Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Peak MB magnitudes versus distance modulus for SNe Ia observed in galaxies with measured Cepheid distances from A. G. Riess et al. (2022). The orange line is a weighted orthogonal distance regression fit using the Python orthogonal-regression algorithm, scipy.odr. The T statistic (slope divided by the standard error) is 1.6.
Paper: Exploring One-point Statistics in HERA Phase I Data: Effects of Foregrounds and Systematics on Measuring One-point Statistics
Authors: Honggeun Kim, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Kai-Feng Chen, Zhilei Xu, Eleanor Rath, Vincent MacKay, Tyrone Adams, James E. Aguirre, Rushelle Baartman, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, David R. DeBoer, Eloy de Lera Acedo, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Nicolas Fagnoni, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Bryna J. Hazelton, Jack Hickish, Daniel C. Jacobs, Joshua Kerrigan, Piyanat Kittiwisit, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, David H. E. MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Miguel F. Morales, Tshegofalang Mosiane, Steven G. Murray, Hans Nuwegeld, Aaron R. Parsons, Nima Razavi-Ghods, James Robnett, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter van Wyngaarden, Haoxuan Zheng
Figure caption: Probability distribution of the fiducial (top row) and cold reionization (bottom row) models at specific redshifts for raw simulations (i.e., no instrumental effect). The dashed and solid vertical lines indicate the mean and median, respectively. At z = 12.5, both models exhibit asymmetric distributions due to heating, leading to a negative m3. As reionization advances, a prominent pileup at the zero bin becomes noticeable. In the fiducial model, efficient heating by star-forming galaxies raises the temperature of the IGM, resulting in a tail toward positive values and thus a positive m3 (top right panel). In the cold reionization model, the distribution at z = 10.0 centered around TB ∼ −250 mK exhibits negative tails. However, m3 transitions to positive values due to the ionized IGM at the zero bin (bottom center panel). As reionization progresses further, m3 becomes negative again as a large fraction of the IGM is ionized, leaving behind some negative IGM regions (bottom right panel).
Paper: Exploring One-point Statistics in HERA Phase I Data: Effects of Foregrounds and Systematics on Measuring One-point Statistics
Authors: Honggeun Kim, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Kai-Feng Chen, Zhilei Xu, Eleanor Rath, Vincent MacKay, Tyrone Adams, James E. Aguirre, Rushelle Baartman, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, David R. DeBoer, Eloy de Lera Acedo, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Nicolas Fagnoni, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Bryna J. Hazelton, Jack Hickish, Daniel C. Jacobs, Joshua Kerrigan, Piyanat Kittiwisit, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, David H. E. MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Miguel F. Morales, Tshegofalang Mosiane, Steven G. Murray, Hans Nuwegeld, Aaron R. Parsons, Nima Razavi-Ghods, James Robnett, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter van Wyngaarden, Haoxuan Zheng
Figure caption: Evolutionary history of m2 (equivalent to S2), m3, S3, and mean ionization fraction measured from raw simulations for the four distinct 21 cm models. Each line indicates the fiducial (Fid), cold reionization (CR), large halos (LH), and extended reionization (ER) models. Band 1 and Band 2 are highlighted in orange and blue shaded regions.
Paper: Exploring One-point Statistics in HERA Phase I Data: Effects of Foregrounds and Systematics on Measuring One-point Statistics
Authors: Honggeun Kim, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Kai-Feng Chen, Zhilei Xu, Eleanor Rath, Vincent MacKay, Tyrone Adams, James E. Aguirre, Rushelle Baartman, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, David R. DeBoer, Eloy de Lera Acedo, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Nicolas Fagnoni, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Bryna J. Hazelton, Jack Hickish, Daniel C. Jacobs, Joshua Kerrigan, Piyanat Kittiwisit, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, David H. E. MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Miguel F. Morales, Tshegofalang Mosiane, Steven G. Murray, Hans Nuwegeld, Aaron R. Parsons, Nima Razavi-Ghods, James Robnett, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter van Wyngaarden, Haoxuan Zheng
Figure caption: HERA stripe, displaying foreground emission, ranging from 1.5 to 14.5 hr centered at ﹩-30\mathop{.}\limits^{^\circ }7﹩ in decl. The map is created from observational data by connecting sky patches, which are made at every hour of LST with the size of 15 × 10 deg2. Emissions at around 3 hr are grating lobes of Fornax A, which is one of the brightest foreground radio sources.
Paper: Exploring One-point Statistics in HERA Phase I Data: Effects of Foregrounds and Systematics on Measuring One-point Statistics
Authors: Honggeun Kim, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Kai-Feng Chen, Zhilei Xu, Eleanor Rath, Vincent MacKay, Tyrone Adams, James E. Aguirre, Rushelle Baartman, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, David R. DeBoer, Eloy de Lera Acedo, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Nicolas Fagnoni, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Bryna J. Hazelton, Jack Hickish, Daniel C. Jacobs, Joshua Kerrigan, Piyanat Kittiwisit, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, David H. E. MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Miguel F. Morales, Tshegofalang Mosiane, Steven G. Murray, Hans Nuwegeld, Aaron R. Parsons, Nima Razavi-Ghods, James Robnett, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter van Wyngaarden, Haoxuan Zheng
Figure caption: PSF of HERA Phase I at 161.5 MHz (left) and a Gaussian fit (right). We forward model simulated maps using the PSF to capture pixel correlations. This PSF is integrated over 1 hr. FWHM of the Gaussian fit: ﹩1\mathop{.}\limits^{^\circ }11﹩ (major) and ﹩0\mathop{.}\limits^{^\circ }75﹩ (minor).