adsabs/AstroCLIMB huggingface dataset:
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure 4 but for the 13CO emission.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure 8 but for the Gaussian ring model.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure 4 but for the 12CO emission.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Wide view of the velocity channel maps of the C18O J = 2–1 emission. The crosses indicate the positions of Ced110 IRS4A and IRS4B. The labels at the top left corners denote the LSR velocities. The filled ellipse at the bottom left corner represents the synthesized beam size.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure A1 but for the 13CO J = 2–1 emission.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Zoom-in view of the velocity channel maps of the C18O J = 2–1 emission. The contour levels are 3, 5, 7, 9... ×σ, where σ is the rms noise listed in Table 2. The dashed contours show negative emission. The crosses indicate the positions of Ced110 IRS4A and IRS4B. The labels at the top left corners denote the LSR velocities. The filled ellipse at the bottom left corner denotes the synthesized beam size.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure A4 but for the 12CO J = 2–1 emission.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure A4 but for the SO J  N  = 65–54 emission.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure A4 but for the 13CO J = 2–1 emission.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Moment zero maps of the other detected lines (color) overlaid with the 1.3 mm continuum map with a robust parameter of 2.0 (contours). The color scales are in units of mJy beam−1 km s−1. The contour level is 3σ, where σ is 0.018 mJy beam−1. The filled and opened ellipses at the bottom left corners represent the synthesized beam sizes of the line map and continuum map, respectively.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure 8 but for the broken power-law model.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure A1 but for the 12CO J = 2–1 emission with contour levels of 3, 6, 12, 24, ... ×σ.
Paper: Early Planet Formation in Embedded Disks (eDisk). V. Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
Authors: Jinshi Sai, Hsi-Wei Yen, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Kazuya Saigo, Yusuke Aso, Zhe-Yu Daniel Lin, Patrick M. Koch, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Woojin Kwon, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Leslie W. Looney, Shoji Mori, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams
Figure caption: Same as Figure 8 but for the power-law ring model.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Snapshots in multiple wave bands with the same FOV of 120″ × 120″ measured by CHASE/HIS (a) and (g), IRIS/SJI (c), SDO/AIA (c)−(f), and SDO/HMI (h) and (i). Blue and magenta contours outline bright kernels/features in Hα and AIA 94 Å hot channels. The pink box and two short cyan lines mark the flare region, and the dashed cyan line (S1) represents the slit of IRIS. The green (S2) curves outline the solar jet and are used to perform the time–distance maps in Figure 7. The red arrow indicates an enhancement of the white-light radiation. Two zoomed images show Fe I 6569.2 Å and HMI pseudointensity maps with a small FOV of about 30″ × 30″.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Moment analysis results (line intensity, Doppler velocity, and line width) from CHASE Hα spectra during the C9.6 flare. They all have a small FOV of 56″ × 56″, as outlined by the pink box in Figure 2(a). Blue and red contours represent the Hα line intensity and Fe I emission, respectively. Two cyan crosses (‘×’) and one box mark the locations of Hα spectra at flare kernels and the nonflare (background) region in Figure 4. The dashed cyan line represents the slit of IRIS.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: IRIS spectra at two FUV windows of “O I” (a) and “Si IV” (b) on 2022 August 27. The black profiles are line spectra at the flare kernel, as marked by the short black line on the left side of each panel, and the overplotted orange profiles represent their best-fitting results. The cyan and magenta lines are Fe XXI and C I, and the green line is the fitting background. The red vertical ticks labeled some other emission lines used in this study. The purple curve (after multiplication by 10) is the line spectrum at the nonflare location, as marked by the short purple line.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Hα spectra observed by CHASE/HIS in flare kernels (solid black) and the nonflare region (dashed black) at three times. The solid magenta curves indicate the Hα contrast line profiles, as normalized by the background spectrum. The dotted magenta lines represent emission levels, and the bisector velocities are indicated by solid dots.
Paper: Observational Signatures of Electron-driven Chromospheric Evaporation in a White-light Flare
Authors: Dong Li, Chuan Li, Ye Qiu, Shihao Rao, Alexander Warmuth, Frederic Schuller, Haisheng Zhao, Fanpeng Shi, Jun Xu, Zongjun Ning
Figure caption: Full-disk light curves from 13:00 UT to 13:30 UT on 2022 August 27. Panel (a): GOES SXR fluxes at wavelengths of 1−8 Å (red) and 0.5−4 Å (blue). The context image is the radio spectrogram observed by SWAVES. Panel (b): STIX count fluxes in the energy bands of 4−10 keV (black), 10−15 keV (orange), and 15−25 keV (green), and the normalized GECAM flux at 20−60 keV (cyan).
Paper: Mass Dependence of Galaxy–Halo Alignment in LOWZ and CMASS
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: Left: the fraction of central disk galaxies as a function of stellar mass for the LOWZ and CMASS samples. Middle: the misalignment angle σ  θ  as a function of stellar mass for central elliptical galaxies, central disk galaxies, and all the central galaxies in both the LOWZ and CMASS samples. The best-fit relations for the central elliptical galaxies are shown with solid lines. Right: the misalignment angle σ  θ  as a function of host halo mass for central elliptical galaxies. The best-fit relations are shown with solid lines. Open circles label the halo masses of the CMASS galaxies that are expected to grow to the LOWZ redshift, while the misalignment angles are assumed unchanged.
Paper: Mass Dependence of Galaxy–Halo Alignment in LOWZ and CMASS
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: The GI correlations of central elliptical galaxies and their host DM halos in different stellar mass bins for the LOWZ (left) and CMASS (right) samples. Dots with error bars show the measurements for central elliptical galaxies and lines show the GI correlations for their host DM halos from simulations. The GI correlation of all the central disk galaxies from the CMASS sample is also shown for comparison.
Paper: Mass Dependence of Galaxy–Halo Alignment in LOWZ and CMASS
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: Mean errors of the position angles of galaxies in LOWZ and CMASS as a function of stellar mass.
Paper: Mass Dependence of Galaxy–Halo Alignment in LOWZ and CMASS
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: Similar to Figure 1, the lines in this figure represent model predictions with the best-fit misalignment angles.
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption: Real vs. predicted (RvP) comparison for effective temperature T eff and surface gravity ﹩\mathrm{log}g﹩ for random forest training and testing on a single grid. No noise is assumed. Here, we show analysis for the grids B+97, B+06, M+11, and K+21. In each panel, the red dashed line indicates perfect agreement. Differences in the grid sizes, particularly for surface gravity, and corresponding effect on the accuracy of predictions can be seen.
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption: Examples of spectra from all of the model grids for a typical late-T dwarf with T eff = 800 K and ﹩\mathrm{log}g﹩ = 5. Left panel: cloud-free models. Right panel: cloudy models.
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption: Schematic flowchart describing the three applications of our supervised machine-learning method (random forest) in the current study: examining the information content of each model grid in isolation, comparing the information content of a pair of model grids, and finally performing atmospheric retrieval on measured spectra in the framework of Approximate Bayesian Computation.
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption: Retrieval outcomes for Gl 570 D (top), ϵ Indi Ba (middle), and ϵ Indi Bb (bottom). Left panels show the retrieved posterior median values (points) and 1 σ uncertainties (error bars) for each of the model grids. The flat line in each panel is a fit across the retrieved parameter values. Right panels show the median spectra for each individual grid compared to the original data (black dots). Note that for Gl 570 D, we use the SpeX spectrum from Burgasser et al. (2004) covering the wavelength range 0.8–2.5 μm with average spectral resolution of ∼100; For ϵ Indi Ba and Bb, we use spectra from King et al. (2010) obtained with the Very Large Telescope ISAAC spectrograph (Moorwood et al. 1998) which spans 0.6–5 μm at a resolution of λ/Δλ ≈ 5000, considerably higher than that provided by SpeX prism data. It should be noted that object-specific uncertainties have been considered according to Section 5.2, and are therefore data driven.
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption: RvP comparison for M+11c vs. B+06c grids, focusing on the influence of effective temperature range. The top panels show the RvPs when the full range of models are trained and tested; the bottom panels show the RvPs when models are restricted to overlapping effective temperatures. No noise is assumed.
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption: Same as Figure 3 but with grids enlarged through interpolation of surface gravity. No noise is assumed. Note the significant improvement in R 2 scores for both effective temperature (T eff) and surface gravity (log g).
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption:  R 2 scores for ﹩\mathrm{log}g﹩ (blue bands) and T eff (red bands) for random forests trained on the first model listed and tested on the second model listed. Values are shown for the restricted wavelength range of 1.2–2.45 μm. No noise is assumed.
Paper: Intercomparison of Brown Dwarf Model Grids and Atmospheric Retrieval Using Machine Learning
Authors: Anna Lueber, Daniel Kitzmann, Chloe E. Fisher, Brendan P. Bowler, Adam J. Burgasser, Mark Marley, Kevin Heng
Figure caption: Feature importance plots for the temperature T eff (red) and the surface gravity ﹩\mathrm{log}g﹩ (blue). All 14 different grids are shown. No noise is assumed.
Paper: COSMOS-Web: An Overview of the JWST Cosmic Origins Survey
Authors: Caitlin M. Casey, Jeyhan S. Kartaltepe, Nicole E. Drakos, Maximilien Franco, Santosh Harish, Louise Paquereau, Olivier Ilbert, Caitlin Rose, Isabella G. Cox, James W. Nightingale, Brant E. Robertson, John D. Silverman, Anton M. Koekemoer, Richard Massey, Henry Joy McCracken, Jason Rhodes, Hollis B. Akins, Natalie Allen, Aristeidis Amvrosiadis, Rafael C. Arango-Toro, Micaela B. Bagley, Angela Bongiorno, Peter L. Capak, Jaclyn B. Champagne, Nima Chartab, Óscar A. Chávez Ortiz, Katherine Chworowsky, Kevin C. Cooke, Olivia R. Cooper, Behnam Darvish, Xuheng Ding, Andreas L. Faisst, Steven L. Finkelstein, Seiji Fujimoto, Fabrizio Gentile, Steven Gillman, Katriona M. L. Gould, Ghassem Gozaliasl, Christopher C. Hayward, Qiuhan He, Shoubaneh Hemmati, Michaela Hirschmann, Knud Jahnke, Shuowen Jin, Ali Ahmad Khostovan, Vasily Kokorev, Erini Lambrides, Clotilde Laigle, Rebecca L. Larson, Gene C. K. Leung, Daizhong Liu, Tobias Liaudat, Arianna S. Long, Georgios Magdis, Guillaume Mahler, Vincenzo Mainieri, Sinclaire M. Manning, Claudia Maraston, Crystal L. Martin, Jacqueline E. McCleary, Jed McKinney, Conor J. R. McPartland, Bahram Mobasher, Rohan Pattnaik, Alvio Renzini, R. Michael Rich, David B. Sanders, Zahra Sattari, Diana Scognamiglio, Nick Scoville, Kartik Sheth, Marko Shuntov, Martin Sparre, Tomoko L. Suzuki, Margherita Talia, Sune Toft, Benny Trakhtenbrot, C. Megan Urry, Francesco Valentino, Brittany N. Vanderhoof, Eleni Vardoulaki, John R. Weaver, Katherine E. Whitaker, Stephen M. Wilkins, Lilan Yang, Jorge A. Zavala
Figure caption: An illustration of the deepest filters available in COSMOS-Web and their depths across the spectrum. At the top are the filter transmission profiles for existing COSMOS data sets that are ground-based (light gray), space-based (dark gray), and new additions from JWST for COSMOS-Web (blue). These filters are separated between those that have 5σ point-source depths between 24 and 26.5 mag (top subpanel), and those that reach depths beyond 26.5 mag (bottom subpanel; see Weaver et al. 2022b, for more details). We also include recent coverage from COSMOS-DASH at 1.6 μm (Mowla et al. 2019; Cutler et al. 2022). Note that narrowband and medium-band filters in the field are not shown (as they generally have depths shallower than ∼24 mag). At bottom, we illustrate the 5σ point-source depths from these same filters, highlighting the depth of COSMOS-Web JWST observations in solid blue at full four-integration depth; dashed lines show half two-integration depth (covering approximately half the mosaic, as detailed in Tables 1 and 2). Overlaid are several galaxy templates: Lyman break galaxies at z ∼ 7–13 (shades of lavender to dark purple), an M ⋆ ∼ 1010 M ⊙ z = 4 passive galaxy (dark green), and a z = 2 dusty starburst (light green).