adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption:  χ 2 distribution of orientation angle (i) and half-opening angle (θ), derived from the modeled galaxy to the high spatial resolution (HST) described in Section 4.1. The heat map highlights clear preference for extremes of allowed parameters, preferring an almost perfectly face-on inclination of 10° and a large half-opening angle of 70°. Combinations of inclination and opening angle with the line of sight passing through the torus are heavily disfavored.
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption: The best-fit stellar-only model SED, fitted using the HST/WFC3 NSC photometry from Carson et al. (2015). We overplot the minimum and maximum archival ZTF photometry, which we argue represents a minimum and maximum state of the AGN in NGC 4395. The HST photometry for the NSC are consistent with the minimum ZTF points, giving reassurance that the photometry representing the NSC have negligible AGN contamination.
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Photospheric magnetograms (τ = 0.1). (a) Initial state (identical for all setups); (b)–(f) configuration found in setups (A)–(E) at the time of closest encounter. Setups (A) and (B) differ in terms of coherence of the moving spot and are analyzed in detail in this present paper. The red vertical lines indicate the positions of vertical cross sections presented in Figures 10 and 11. The blue contours highlight the PIL based on a smoothed magnetogram, the orange contours the cPILs. The spot centroids and collision distances are indicated by green dots and green dashed lines, respectively.
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Time evolution of cPIL length and collision distance for setups (A)–(E). Vertical dotted lines indicate the peak time of the flare (or the peak time of the strongest flare in case there was more than one flare) that was produced in each setup. See text for discussion.
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Buildup of magnetic free energy in setups (A)–(E). Panel (a) shows the time evolution of magnetic free energy integrated over the coronal volume of the simulation domain. Panels (b)–(f) show the time evolution of the horizontally averaged magnetic free energy for the individual cases. White contour lines indicate the height levels beneath which 25/50/75% of the magnetic free energy is stored.
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Evolution for flare ribbons for setup (B). In panels (a)–(e), we present synthetic GOES 15 soft-X-ray images at 1–8 Å bandpass with an overlay of the electron energy flux at a height of 1 Mm above the average τ = 1 level in the simulation. Panel (f) shows the integrated GOES 15 flux. Vertical dotted lines indicate the snapshots presented in panels (a)–(e). The snapshots shown correspond to the time steps 534,000, 542,000, 548,000, 565,000, and 600,000 in the animation provided with Figure 4.
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Post-flare evolution of GOES 15 X-ray and AIA EUV flux for setup (B). The secondary peak is present in both X-ray and EUV flux and the time delays are consistent with a typical cooling sequence. We show for the AIA channels the logT of the dominant temperature contributions.
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Synthetic GOES 15 X-ray flux computed for setups (A)–(E). The two strongest flares found in setups (A) and (B) reach a GOES flux peak level of M1.0.
Paper: The JWST Hubble Sequence: The Rest-frame Optical Evolution of Galaxy Structure at 1.5 < z < 6.5
Authors: Leonardo Ferreira, Christopher J. Conselice, Elizaveta Sazonova, Fabricio Ferrari, Joseph Caruana, Clár-Bríd Tohill, Geferson Lucatelli, Nathan Adams, Dimitrios Irodotou, Madeline A. Marshall, Will J. Roper, Christopher C. Lovell, Aprajita Verma, Duncan Austin, James Trussler, Stephen M. Wilkins
Figure caption: A comparison of HST vs. JWST. We show 13 galaxies in our sample that have observations in the four main CANDELS filters (left panel) and SW and LW filters in JWST (right panel). Faint features in CANDELS are generally very clear in JWST. In some cases only the central core of the galaxy is visible with the HST imaging. The classification label shown is derived from our JWST classifications.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Distribution of our M-dwarf sample as a function of spectral type: (a) exposure durations and (b) number of GALEX sources; (c) exposure durations and (d) number of XMM-OM sources. Black bars show all selected sources on the main sequence as described in Section 2. In the top panels, blue bars show the subgroup of GALEX sources detected over at least three exposures.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Gaia DR3 CMD plotted for stars from the (a) Gaia DR3 survey and (b) GALEX and XMM-OM crossmatched samples. The red curves demarcate the main-sequence bounds +0.65 < M  G  < −0.6 described in Section 2.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Flares in the GALEX sample with count rates reaching above 311 cps (shaded region), which is the nonlinearity regime of the NUV detector. From left to right, these are observed on the stars TIC 325273691, TIC 359185852, and TIC 142215003. The lower limits on flare energy and equivalent duration are shown in the plots.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Example of visually rejected flares in GALEX data (blue). The red highlights show visually accepted flares and the yellow highlights denote suspect regions that the algorithm did not qualify as flares (see Figure 5). The gray line denotes the estimated quiescent level. Lightcurves are artificially concatenated over exposure gaps for clarity. (A) shows a small flare with a clear impulse and decay, (B) is a typical quiet lightcurve segment, both blue regions in (C) are rejected for not having impulse or decay phases and being less than 3 times the quiescent and (D) is accepted as a flare for showing a decay phase.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Comparison of flare detection (shaded red) with our (a) algorithm and (b) FLAIIL for a GALEX source observed in just one visit. The dotted line denotes the estimated quiescent level, and the gray shaded area is the ±1σ interval. With FLAIIL, we replace the GP model for the quiescent with a clipped mean. FLAIIL fails to detect the flare and hence gives an erroneously high quiescent estimate.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: A flowchart detailing the flare identification algorithm used in this work. See the text for details.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Histogram of the standard deviation to quiescent flux ratio for sources in the GALEX data set after concatenation of lightcurves belonging to common sources.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Histogram of closest match separation of XMM-OM lightcurve positions crossmatched with the TIC sample. The maximum acceptable crossmatch is set at 4″, shown by the dashed black line.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Distribution of bin sizes in the GALEX sample. The shortest detectable flare duration is equal to the bin size as a flare can comprise a single lightcurve bin (see Section 3.1).
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: Overview of the SOL20141218T21:40 M6.9 flare. (a)–(d) Evolution of flare ribbons observed in UV 1600 Å by AIA. (e)–(h) PRFLs observed in the EUV 131 or 171 Å passbands by AIA. Images in all panels have been rotated to 21:00 UT and therefore co-aligned.
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: Degree of Alfvén-wave reflection, plotted as an amplitude ratio, as a function of a normalized rms density fluctuation. (a) For N = 1, we vary the shape factor s = 1 (black curve), s = 2 (blue curve), s = 3 (green curve). (b) For various values of N, we compare model results (see legend for curve colors and types) with data points extracted from numerical simulations. (c) Same as (b), but for different simulations. Reference abbreviations are vB16 (van Ballegooijen & Asgari-Targhi 2016), AT21 (Asgari-Targhi et al. 2021), Ma21 (Matsumoto 2021), Sh18 (Shoda et al. 2018), and Sh21 (Shoda et al. 2021).
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Gaia17bpp WISE-1 light curve fitted by an oblate solid disk model (top) and model residuals (bottom). In pink we show the maximum likelihood fit to the data. The gray points represent random draws from the posterior distribution.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Grid of blackbody mixture model including the radius and effective temperatures of the secondary star color-coded by the integrated SDSS u AB magnitude. The dashed line represents our limiting SDSS u-band magnitude. We assume that the primary star has a fixed radius of 58 R ⊙, an effective temperature of 3850 K, and a median distance of 8965 pc.
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: Coordinate system and vectors for the idealized MHD system of wave reflection and transmission. The wavenumber  k  (red) always remains in the x–z plane, and it is offset from the z-axis by a polar angle θ  k . Spherical coordinate angles α and β describe the magnetic field vector (blue).
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Violin plot displaying the posterior distribution of the generalized Gaussian distribution fitted for each photometric bandpass. The shape of each violin represents the KDE of the distribution, with the vertical black lines and white rectangles indicating the interquartile range. Solid lines at the violin end represent the minimum and maximum values of the KDE.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Normalized transit light curves of ϵ Aur analog systems ordered by event duration. Gaia17bpp (W1 bandpass) exhibits the longest and deepest duration event. We sort each dimming event from the shortest (top) to the longest (bottom) in the following order: ASASSN-21co (Rowan et al. 2021), VVV-WIT-08 (Smith et al. 2021), ϵ Aurigae (see Kloppenborg et al. 2012 and references therein), TYC 2505-672-1 (Lipunov et al. 2016), and Gaia17bpp.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: GP fits (gray lines) drawn from the posterior distribution for the Gaia G, Gaia RP, W1, and W2 light curves including their residuals at the bottom of each panel.
Paper: Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces
Authors: Steven R. Cranmer, Momchil E. Molnar
Figure caption: Illustration of how reflection from two parallel interfaces results in an infinite series of reflected components.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: Examination of the flux rope detected in situ by Parker Solar Probe using a characteristic length scale λ = 3.2 × 107 km (corresponding to a correlation time T  c  ∼ 6.4 hr with a nominal speed of 1000 km s−1). Stacked plots show (a) the magnetic field measured by the FIELDS instrument, (b) the PVI signal computed using a time lag of 60 s, and (c) the magnetic helicity at different scales. Black dashed vertical lines indicate the start and end of the identified flux rope structures; blue dashed vertical lines indicate discontinuities in the heliospheric magnetic field direction.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: The flare and CME associated with the eruption on 2022 September 5. Panel (a) shows the GOES (top) and STIX (bottom) X-ray lightcurves highlighting the flares associated with the active region rotating on-disk (gray shaded area in panel (a) and blue arrow in the left panels) and the flare associated with the eruption of the flux rope (red arrow in the left panels), both of which were observed by EUI/FSI (panel (c)). Panels (b) and (d) show running difference images highlighting the erupting CME as viewed by LASCO C2. The CME is first seen in C2 at 16:36 UT and exhibits two distinct lobes as highlighted by the red arrows and discussed in the text.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: SPICE spectra of the flux rope (blue) and a control quiet Sun region (red). These spectra are averaged over the boxed areas shown in Figure 1. The spectral positions of several Ne VIII and Mg VIII lines are indicated. The Mg VIII lines should be bright relative to the Ne VIII lines when there is a strong FIP effect in operation.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: ADAPT magnetogram from 12:00 UT on September 5 showing the field of view (black line) and subspacecraft point (blue cross) of Solar Orbiter. The red arrow indicates AR 13088 discussed here, with the white arrows indicating the location of the identified flux rope. The flux rope lies beneath the heliospheric current sheet, which could explain some of the complex structure observed in the in situ measurements.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: The small-scale evolution of the plasma flow along the observed flux rope structure on both 2022 September 4 (top) and 2022 September 5 (bottom). Left column shows the plasma evolution derived by recording pixels with a running ratio value greater than 1.3 at each time step. Middle column shows the locations of the cuts taken across the blue spine of the flux rope structure corresponding to the distance–time plots in the right column. The arrows indicate the orientation of the plasma flow corresponding to the red linear fits in the distance–time plots.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: Running difference images showing the apparent brightenings corresponding to a supposed global EUV wave. The white arrows indicate a large dimming region, which remains stationary with time, albeit with some evolution in size and shape. The red arrows indicate a feature propagating south away from the erupting active region, which corresponds to a global wave well observed by the STEREO-A spacecraft, but was behind the limb as seen from Solar Orbiter/EUI.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: 3DCORE model fit to the PSP/FIELDS magnetic field measurements assuming an elliptical flux rope cross section. The dashed colored lines show a specific fit from the ensemble run, with the shaded areas corresponding to the 2σ spread of the ensemble. The vertical dashed black lines show the start and the end of the flux rope as taken by 3DCORE.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: The temporal evolution of the plasma flow along the filament channel on 2022 September 4 (left) and 2022 September 5 (right). In each case, the distance–time evolution of the plasma has been fitted using a linear fit (indicated by the white line) to derive the velocity (given in the title).
Paper: High-redshift Galaxy Candidates at z = 9–10 as Revealed by JWST Observations of WHL0137-08
Authors: Larry D. Bradley, Dan Coe, Gabriel Brammer, Lukas J. Furtak, Rebecca L. Larson, Vasily Kokorev, Felipe Andrade-Santos, Rachana Bhatawdekar, Maruša Bradač, Tom Broadhurst, Adam Carnall, Christopher J. Conselice, Jose M. Diego, Brenda Frye, Seiji Fujimoto, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Intae Jung, Guillaume Mahler, Stephan McCandliss, Masamune Oguri, Marc Postman, Keren Sharon, M. Trenti, Eros Vanzella, Brian Welch, Rogier A. Windhorst, Adi Zitrin
Figure caption: Cutout images, best-fit spectral energy distributions (SEDs), and posterior redshift distributions for the high-redshift galaxy candidates WHL0137–ID08004 and WHL0137–ID09319. Top panels: 3″ × 3″ JWST cutout images spanning 0.9–4.5 μm centered on each candidate. Bottom left panels: Source photometry is shown as blue data points or triangle upper limits. Nondetections are plotted as upper limits at the 1σ level. The best-fit BAGPIPES spectral energy distribution (SED) model at high redshift (z ≥ 7) is shown in orange, with squares indicating the expected photometry in a given band. The best-fit BAGPIPES SED for a low-redshift (z < 7) solution is shown in gray. For WHL0137–ID08004, we also show the best-fit BEAGLE SED model (see Section 4.5) in green. Bottom right panels: Posterior probability distributions (P(z)) for the source photometric redshift derived using EAZYPY (using both the FSPS+ (Larson et al. 2022) and SFHZ template sets), BAGPIPES, and BEAGLE.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: Posterior plots for the masses of three of the galaxies in our sample. We do not place a direct prior on the galaxy masses, so priors here are calculated from the prior on the M/L distribution and σ  M/L . Ursa Major II and IC 1613 are the faintest galaxy that has GCs and the most luminous galaxy that does not have GCs, respectively. Their posteriors are both more constrained than the priors, but are centered on the prior values. The Milky Way is of particular interest due to the extent it has been studied. A stellar mass estimate from Licquia & Newman (2015) is plotted along with our posterior and prior.
Paper: High-redshift Galaxy Candidates at z = 9–10 as Revealed by JWST Observations of WHL0137-08
Authors: Larry D. Bradley, Dan Coe, Gabriel Brammer, Lukas J. Furtak, Rebecca L. Larson, Vasily Kokorev, Felipe Andrade-Santos, Rachana Bhatawdekar, Maruša Bradač, Tom Broadhurst, Adam Carnall, Christopher J. Conselice, Jose M. Diego, Brenda Frye, Seiji Fujimoto, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Intae Jung, Guillaume Mahler, Stephan McCandliss, Masamune Oguri, Marc Postman, Keren Sharon, M. Trenti, Eros Vanzella, Brian Welch, Rogier A. Windhorst, Adi Zitrin
Figure caption: JWST NIRCam detection image, comprised of a weighted sum of all NIRCam LW images (F277W, F356W, F410M, and F444W), of the nearby field (NIRCam A module), centered ﹩\sim 2\buildrel{\,\prime}\over{.} \,9﹩ from the WHL0137−08 cluster center. The field of view is ﹩\sim 2\buildrel{\,\prime}\over{.} \,3\times 2\buildrel{\,\prime}\over{.} \,3﹩ and the image is shown with north up and east left. The locations of the high-redshift candidates are indicated with red circles. The location of the lensed high-redshift candidate is shown in Figure 1.