adsabs/AstroCLIMB huggingface dataset:
Paper: The Lyα Dependence on Nebular Properties from the HETDEX and MOSDEF Surveys
Authors: Óscar A. Chávez Ortiz, Gene C. K. Leung, Steven L. Finkelstein, Dustin Davis, Ralph S. Sutherland, David C. Nicholls, Mabel Stephenson, Erin Mentuch Cooper, Micaela Bagley, Karl Gebhardt, Lindsay R. House, Chenxu Liu, Robin Ciardullo, Caryl Gronwall, Gary J. Hill, Daniel Farrow, Donald P. Schneider
Figure caption: The CDFs for various galaxy properties from nebular line modeling algorithm are given in the top row and Bagpipes in the bottom row. The blue and red shaded curves correspond to the 1σ spread in the CDFs for the Lyα-detected and nondetected samples, respectively. The CDFs show clear evidence of physical differences between the two samples. The top row panels suggests differences between the ionization parameter [log10(Q)] and metallicity. In the bottom row, the differences are even more stark; there are physical differences between the two samples in terms of the Lyα equivalent width, stellar mass, dust attenuation, and specific star formation rate. The top row shows some tentative differences; the KS test returned p-values above 0.05, [Q: 0.25, p-val: 0.21, Z: 0.26, p-val: 0.16, E(B − V): 0.27, p-val: 0.34], indicating there is a high probability the two distributions are drawn from the same distribution. The Bagpipes-derived properties had the following KS statistics: W Lyα : 0.74, p-val: ﹩2.4\times {10}^{-13}﹩, Stellar mass: 0.39, p-val: 0.006, Av: 0.30, p-val: 0.06, sSFR: 0.26, p-val: 0.16. Indicating that a main contributor to the observability of Lyα is the stellar mass and lack of dust.
Paper: The Lyα Dependence on Nebular Properties from the HETDEX and MOSDEF Surveys
Authors: Óscar A. Chávez Ortiz, Gene C. K. Leung, Steven L. Finkelstein, Dustin Davis, Ralph S. Sutherland, David C. Nicholls, Mabel Stephenson, Erin Mentuch Cooper, Micaela Bagley, Karl Gebhardt, Lindsay R. House, Chenxu Liu, Robin Ciardullo, Caryl Gronwall, Gary J. Hill, Daniel Farrow, Donald P. Schneider
Figure caption: Left: Posterior distributions of the parameters in our nebular modeling code and line fluxes using all available lines in blue and only [O III]λ5007, Hβ, Ne III λ3870, and [O II]3729 in red for single sources. We achieve greater constraints on the physical properties when all available lines are used over a subset of lines. Right: We present the model grid used in our nebular modeling algorithm, comparing predictions for line flux ratios based on the best-fit results using only the “OHNO” lines as input vs. using all available lines. We can see that both model predictions overlap the observed data within the error bars; however, due to the tighter constraints on nebular line properties, we use the run using all available lines.
Paper: The Lyα Dependence on Nebular Properties from the HETDEX and MOSDEF Surveys
Authors: Óscar A. Chávez Ortiz, Gene C. K. Leung, Steven L. Finkelstein, Dustin Davis, Ralph S. Sutherland, David C. Nicholls, Mabel Stephenson, Erin Mentuch Cooper, Micaela Bagley, Karl Gebhardt, Lindsay R. House, Chenxu Liu, Robin Ciardullo, Caryl Gronwall, Gary J. Hill, Daniel Farrow, Donald P. Schneider
Figure caption: Histogram showing the velocity offset computed using Equation (7). Most of the Lyα-detected sources are redshifted from systemic with a median velocity offset of +178 km s−1, and we show the typical uncertainty in the velocity offset, which is 47.7 km s−1.
Paper: Revisiting the Chemical Composition of WD 1145+017: Impact of Circumstellar Disk Contamination on Photospheric Abundances
Authors: Érika Le Bourdais, Patrick Dufour, Siyi Xu, 偲艺 许
Figure caption: Selected regions of the 2018 May 18 HIRES spectrum. The contribution from the photosphere alone is in gray while the combined photospheric and circumstellar disk contributions are in orange.
Paper: Revisiting the Chemical Composition of WD 1145+017: Impact of Circumstellar Disk Contamination on Photospheric Abundances
Authors: Érika Le Bourdais, Patrick Dufour, Siyi Xu, 偲艺 许
Figure caption: Variation of average photospheric abundance for Fe, Si, Mg, and Ni in the optical (blue) and the UV (orange) for all epochs where at least two lines were used for fitting. A T indicates observations taken during a transit. The faded colored band represents the 1σ uncertainty (see Table 2) of the average value across all epochs.
Paper: Revisiting the Chemical Composition of WD 1145+017: Impact of Circumstellar Disk Contamination on Photospheric Abundances
Authors: Érika Le Bourdais, Patrick Dufour, Siyi Xu, 偲艺 许
Figure caption: Selected regions of the 2016 February 3 HIRES spectrum. The contribution from the photosphere alone is in gray while the combined photospheric and circumstellar disk contributions are in orange.
Paper: Revisiting the Chemical Composition of WD 1145+017: Impact of Circumstellar Disk Contamination on Photospheric Abundances
Authors: Érika Le Bourdais, Patrick Dufour, Siyi Xu, 偲艺 许
Figure caption: Selected regions of the 2023 May 10 GHOST spectrum. The contribution from the photosphere alone is in gray while the combined photospheric and circumstellar disk contributions are in orange.
Paper: A Rapidly Accreting Active Galactic Nucleus Hidden in a Dust-obscured Galaxy at z ∼ 0.8
Authors: Nathan Cristello, Fan Zou, William N. Brandt, Zhibo Yu, Fabio Vito, Shifu Zhu
Figure caption: The best-fit SED for J1324+4501. The observed photometry is shown by the green points, the AKARI upper limits are shown by the green downward-facing triangles, and the model spectrum (photometry) is shown by the gray line (black squares). The SED is decomposed into the galaxy components (red) and the AGN components (blue), and the reduced chi-squared of the fit is shown in the lower right. The bottom panel shows the χ residuals of the fit for points that are not upper limits.
Paper: A Rapidly Accreting Active Galactic Nucleus Hidden in a Dust-obscured Galaxy at z ∼ 0.8
Authors: Nathan Cristello, Fan Zou, William N. Brandt, Zhibo Yu, Fabio Vito, Shifu Zhu
Figure caption: Our sources in the L 6μm–L X, obs plane. Similar to Figure 4, J1324+4501 is plotted in pink, and our supplementary sample is plotted in purple. The open pink circle shows the intrinsic L X for J1324+4501. For reference, we also include the DOGs from Yu et al. (2024) in gray. The solid black line is the relation from D. Stern (2015), and the dashed black lines represent the 1σ deviation from this relation.
Paper: A Rapidly Accreting Active Galactic Nucleus Hidden in a Dust-obscured Galaxy at z ∼ 0.8
Authors: Nathan Cristello, Fan Zou, William N. Brandt, Zhibo Yu, Fabio Vito, Shifu Zhu
Figure caption: The N H–L X plane for several types of AGNs. Our primary source, J1324+4501, is plotted in pink. Our X-ray bright supplementary sample is plotted in purple. Reddened Type 1 quasars, DOGs, and Hot DOGs from the literature (see text) are plotted in light green, orange, and red, respectively. The median L X and N H values for each population are shown by the light green, orange, and red stars.
Paper: A Rapidly Accreting Active Galactic Nucleus Hidden in a Dust-obscured Galaxy at z ∼ 0.8
Authors: Nathan Cristello, Fan Zou, William N. Brandt, Zhibo Yu, Fabio Vito, Shifu Zhu
Figure caption: The unfolded joint observed-frame XMM-Newton/Chandra spectrum of J1324+4501. The best-fit AbsPow model is given by the cyan line, while the individual transmission and scattered components are shown by the red-dashed and blue-dotted lines, respectively. This spectrum is rebinned for visualization purposes, and this merged spectrum is presented only for illustration purposes. Our scientific analyses are based on jointly fitting the individual spectra.
Paper: A Rapidly Accreting Active Galactic Nucleus Hidden in a Dust-obscured Galaxy at z ∼ 0.8
Authors: Nathan Cristello, Fan Zou, William N. Brandt, Zhibo Yu, Fabio Vito, Shifu Zhu
Figure caption: The recovered SFH from our Prospector-α fit. The 50th percentile of the SFH is shown in black, while the 16th and 84th percentiles of the SFH are shown in gray.
Paper: A Rapidly Accreting Active Galactic Nucleus Hidden in a Dust-obscured Galaxy at z ∼ 0.8
Authors: Nathan Cristello, Fan Zou, William N. Brandt, Zhibo Yu, Fabio Vito, Shifu Zhu
Figure caption: A comparison between SFRMS and SFR for our sample. J1324+4501 is shown in pink, our supplementary sample in purple, and the X-ray detected DOGs from Yu et al. (2024) in gray. The black solid line represents the 1-to-1 line.
Paper: Challenges for Fast Radio Bursts as Multimessenger Sources from Binary Neutron Star Mergers
Authors: Mohit Bhardwaj, Antonella Palmese, Ignacio Magaña Hernandez, Virginia D'Emilio, Soichiro Morisaki
Figure caption: Derived constraints on the BNS ejecta mass (M ej) if FRB 20190425A is indeed associated with GW190425. Hatched regions are excluded using ejecta temperature (T ej)–dependent propagation effects, and shaded regions are excluded due to constraints that are independent of the ejecta temperature, as discussed in Section 3.
Paper: The Star-forming Main Sequence in JADES and CEERS at z > 1.4: Investigating the Burstiness of Star Formation
Authors: Leonardo Clarke, Alice E. Shapley, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer, Trinity Bento, Naveen A. Reddy, Emily Kehoe
Figure caption: Hα-based SFRs vs. stellar masses for the combined JADES and CEERS sample binned by redshift. The darker and lighter shaded regions denote the 1σ int and 2σ int intrinsic scatter intervals about the SFMS, respectively. The thick gray line shows the best-fit SFMS for the whole sample in the range 1.4 < z ≤ 7. The literature curves from I. Shivaei et al. (2015), P. Popesso et al. (2023), M. W. Topping et al. (2021), and J. S. Speagle et al. (2014) were shifted down in SFR by 0.32, 0.32, 0.37, and 0.32 dex, respectively, to match our low-metallicity Hα to SFR conversion. The slightly different shift for M. W. Topping et al. (2021) reflects the use of the C.-N. Hao et al. (2011) conversion, whereas the other works adopt the conversion from R. C. J. Kennicutt (1998).
Paper: Challenges for Fast Radio Bursts as Multimessenger Sources from Binary Neutron Star Mergers
Authors: Mohit Bhardwaj, Antonella Palmese, Ignacio Magaña Hernandez, Virginia D'Emilio, Soichiro Morisaki
Figure caption: Posterior distributions on the viewing angle θ  v  for GW190425 for both the low-spin (left panel) and high-spin (right panel) priors under the fixed sky location and fixed position assumptions as described in Section 2. For both cases, we also show the viewing angle posteriors computed using the results of B. Abbott et al. (2020) for reference.
Paper: The Star-forming Main Sequence in JADES and CEERS at z > 1.4: Investigating the Burstiness of Star Formation
Authors: Leonardo Clarke, Alice E. Shapley, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer, Trinity Bento, Naveen A. Reddy, Emily Kehoe
Figure caption: SED-based SFRs vs. stellar masses for the combined JADES and CEERS sample binned by redshift. The darker and lighter shaded regions denote the 1σ int and 2σ int intrinsic scatter intervals about the SFMS, respectively. The thick gray line shows the best-fit SFMS for the whole sample in the range 1.4 < z ≤ 7. The lower normalization of our sample compared to the literature is largely due to the fact that we assume an SMC dust law, whereas most literature studies have assumed a Calzetti dust law.
Paper: The Star-forming Main Sequence in JADES and CEERS at z > 1.4: Investigating the Burstiness of Star Formation
Authors: Leonardo Clarke, Alice E. Shapley, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer, Trinity Bento, Naveen A. Reddy, Emily Kehoe
Figure caption: UV-based SFRs vs. stellar masses for the combined JADES and CEERS sample binned by redshift. The darker and lighter shaded regions denote the 1σ int and 2σ int intrinsic scatter intervals about the SFMS, respectively. The thick gray line shows the best-fit SFMS for the whole sample in the range 1.4 < z ≤ 7. The lower normalization of our sample compared to the literature is largely due to the fact that we assume an SMC dust law, whereas most literature studies have assumed a Calzetti dust law.
Paper: The Star-forming Main Sequence in JADES and CEERS at z > 1.4: Investigating the Burstiness of Star Formation
Authors: Leonardo Clarke, Alice E. Shapley, Ryan L. Sanders, Michael W. Topping, Gabriel B. Brammer, Trinity Bento, Naveen A. Reddy, Emily Kehoe
Figure caption: Redshift distribution of the combined CEERS and JADES sample that we analyze consisting of 146 spectroscopically confirmed star-forming galaxies with robust SED measurements. Of these, 106 galaxies come from CEERS and 40 galaxies come from JADES.
Paper: Challenges for Fast Radio Bursts as Multimessenger Sources from Binary Neutron Star Mergers
Authors: Mohit Bhardwaj, Antonella Palmese, Ignacio Magaña Hernandez, Virginia D'Emilio, Soichiro Morisaki
Figure caption: Sky localization regions using both the low-spin (blue) and high-spin (yellow) posterior samples as reported in B. Abbott et al. (2020). We show both the 50% and 90% confidence intervals for each case and show the location of UGC 10667.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The number of cores per unit length (left column) and the number of class 0/1 YSOs per unit length (right column) of Perseus filaments plotted against their M lin and median σ  v  counterparts in the top and bottom rows, respectively. The symbols are the same as those in Figure 5. The gray dashed line represents the best-fitted linear regression model. The value of M lin,crit at 10 K is marked by the vertical dotted line in the top panels, with the shaded region representing the transcritical values of 0.5M lin,crit ≤ M lin ≤ 2M lin,crit.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The median ∣∇v LSR,⊥∣ (left column) and the ∣∇v LSR,∥∣ (right column) of the Perseus filaments plotted against their M lin and σ  v  counterparts, in the top and bottom rows, respectively. We note that σ  v  is the line-of-sight velocity dispersion derived directly from the spectral fits. The markers are the same as those in Figure 5. The gray dashed line represents the best-fitted linear regression models.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The Rayleigh test p-values for each filament’s ∇v LSR orientations plotted against their respective median σ  v , with the null hypothesis assuming the orientations are randomly distributed. The markers are the same as in Figure 5, and the shaded region shows where p > 0.001. The vertical dotted line shows the expected σ  v  value of NH3 for a 10 K gas with a sonic nonthermal component.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The median ∣∇v LSR,⊥∣ of each filament plotted against their respective number of Class 0/I YSOs. The markers are the same as in Figure 5. The gray dashed line represents the best-fitted linear regression model.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The NH3-derived vLSR maps of Perseus B5, IC348, and B1, in units of kilometers per second. The vLSR values of the component with the narrowest σ v (c1) are shown in the first row. The vLSR values of the widest-σ v component (c2) are shown in the second row, with the gray shaded region showing where NH3 is robustly detected.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The same as Figure 14, but vLSR showing maps of Perseus NGC 1333, L1448, and L1455, instead.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The same as Figure 14, but showing maps of σ v, in units of kilometers per second, instead.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The same as Figure 15, but showing maps of σ v, in units of kilometers per second, instead.
Paper: Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Michael Chun-Yuan Chen, James Di Francesco, Rachel K. Friesen, Jaime E. Pineda, Paola Caselli, Adam Ginsburg, Helen Kirk, Anna Punanova
Figure caption: The perpendicular component (left), the parallel component (center), and the magnitude (right) maps of ∇v LSR in the Perseus B5 filament.
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: UV and optical gas pressure diagnostics for the AGN narrow-line regions as predicted by AGN models with ﹩\mathrm{log}({E}_{\mathrm{peak}}/\mathrm{keV})=﹩−1.25, NHlow nitrogen scaling relation, and varying metallicity (﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=7.3,8.0,8.7,9.0,9.4﹩ correspond to colors from dark to bright) and varying ionization parameter (﹩\mathrm{log}(U)=-3.8﹩ in solid lines and log(U)=-2.2 in dashed lines).
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: UV and optical ionization parameter diagnostics for the AGN narrow-line regions as predicted by AGN models with ﹩\mathrm{log}(P/k)=7.0﹩, NHlow nitrogen scaling relation, and varying metallicity (﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=7.3,8.0,8.7,9.0,9.4﹩ correspond to colors from dark to bright) and varying peak energy in the AGN radiation field (﹩\mathrm{log}({E}_{\mathrm{peak}}/\mathrm{keV})=﹩−1.0 in solid lines and ﹩\mathrm{log}({E}_{\mathrm{peak}}/\mathrm{keV})=﹩−1.5 in dashed lines).
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: UV and optical E peak diagnostics for the AGN narrow-line regions as predicted by AGN models with ﹩\mathrm{log}(P/k)=7.0﹩, NHlow nitrogen scaling relation, and varying metallicity (﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=7.3,8.0,8.7,9.0,9.4﹩ correspond to colors from dark to bright) and varying ionization parameter (﹩\mathrm{log}(U)=-3.8﹩ in solid lines and log(U)=-2.2 in dashed lines).
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: External testing of the AGN metallicity diagnostics and ionization parameter diagnostics in this paper. The left-hand panel shows a comparison of optical AGN metallicity diagnostics [N II]/Hα and [N II]/[O II] from this paper and those from S. P. Carvalho et al. (2020) and C. S. Castro et al. (2017). The right-hand panel shows a comparison of AGN ionization parameter diagnostic C III]/C IV and [O III]/[O II] from this paper and those from O. L. Dors et al. (2019) and S. P. Carvalho et al. (2020). In both panels, the diagnostics from this paper are derived from AGN models with ﹩\mathrm{log}(P/k)=7.0﹩, ﹩\mathrm{log}({E}_{\mathrm{peak}}/\mathrm{keV})=﹩−1.5, and NHhigh nitrogen abundance scaling relation.
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: The effect of nitrogen scaling relation on optical metallicity diagnostics for the AGN narrow-line regions as predicted by AGN models with ﹩\mathrm{log}(P/k)=7.0﹩ and ﹩\mathrm{log}({E}_{\mathrm{peak}}/\mathrm{keV})=﹩−1.5. As in Figure 3, but with line styles representing the nitrogen scaling relation used in the AGN models (NHlow in solid lines and NHhigh in dashed lines).
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Comparing the metallicity measurements from six optical AGN metallicity diagnostics using NHhigh nitrogen scaling relation for 460 Seyfert galaxies observed in SDSS DR16. From left to right (from top to bottom), the x-axis (y-axis) represents the metallicity measurements from [N II]/Hα, [N II]/[O II], R(N2, S2, Hα), R(N2, S2, O3), ([N II]+Hα)/[O III], and [S II]/Hα. The metallicity measurements on SDSS spectra are shown in blue dots, with error bars indicating the measurement errors. The RMSEs are shown in every subplot.
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Comparing the metallicity measurements between (a) the two UV AGN metallicity diagnostics C III]/He II and C34/He II presented in this paper, (b) the C III]/He II metallicity and the metallicity measured in O. L. Dors et al. (2019), and (c) the C34/He II metallicity and the metallicity measured in O. L. Dors et al. (2019).
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Comparing the UV and optical metallicity diagnostics for AGN narrow-line regions (solid lines) and H II region (dashed lines) with varied ionization parameter (﹩\mathrm{log}(U)=﹩−3.8, −3.4, −3.0, −2.6, −2.2 correspond to colors from dark to bright). Both AGN and H II metallicity diagnostics are derived from models with the same gas pressure ﹩\mathrm{log}(P/k)=7.0﹩.
Paper: Theoretical Diagnostics for Narrow-line Regions of Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: The logical flowchart for determining metallicity for AGN narrow-line regions using theoretical diagnostics.
Paper: SCExAO/CHARIS Near-infrared Scattered-light Imaging and Integral Field Spectropolarimetry of the AB Aurigae Protoplanetary System
Authors: Erica Dykes, Thayne Currie, Kellen Lawson, Miles Lucas, Tomoyuki Kudo, Minghan Chen, Olivier Guyon, Tyler D. Groff, Julien Lozi, Jeffrey Chilcote, Timothy D. Brandt, Sebastien Vievard, Nour Skaf, Vincent Deo, Mona El Morsy, Danielle Bovie, Taichi Uyama, Carol Grady, Michael Sitko, Jun Hashimoto, Frantz Martinache, Nemanja Jovanovic, Motohide Tamura, N. Jeremy Kasdin
Figure caption: SCExAO/CHARIS AB Aur wavelength-collapsed, median-combined J (right), H (center), and K (left) Q  ϕ  images from 2020 January 4. J, H, and K passbands were taken to be channels 1–6 (1.15–1.37 μm), 7–15 (1.42–1.86 μm), and 16–22 (1.93–2.36 μm) of the PDI-reduced data cubes, respectively. All images are displayed in the same percentile-based stretch from Figure 1.