adsabs/AstroCLIMB huggingface dataset:
Paper: A Dynamically Distinct Stellar Population in the Leading Arm of the Sagittarius Stream
Authors: Gwibong Kang, Young Sun Lee, Young Kwang Kim, Timothy C. Beers
Figure caption: Top panels: distribution of [Fe/H] (left) and [Mg/Fe] (middle) for RGB/MS stars and [Fe/H] (right) for RR Lyrae stars. The metallicity information for the RR Lyrae stars was obtained by cross-matching the RR Lyrae catalog of Ramos et al. (2020) with SDSS/LAMOST data. The blue, red, and green histograms in each panel indicate the LA, TA, and SC, respectively. Each histogram is normalized by the total number of stars in each category. Note that there are no [Mg/Fe] distributions for the RR Lyrae stars and no SC histogram in the right panel because there are no SC stars in the SDSS/LAMOST data. Bottom panels: same as the top panels but for the distribution of eccentricity for the RGB/MS (left), RR Lyrae (middle), and simulated Sgr stars with the LMC (right) from V21. We note the large fraction of low-e stars in the LA, and a similar behavior is observed in the model as well.
Paper: A Dynamically Distinct Stellar Population in the Leading Arm of the Sagittarius Stream
Authors: Gwibong Kang, Young Sun Lee, Young Kwang Kim, Timothy C. Beers
Figure caption: Distribution of heliocentric distance (d), V GSR, μ  α , and μ  δ  of the Sgr candidates as a function of the Sgr stream longitude (Λ). The gray dots represent the stars in −20° < B < 15°, where B is the Sgr stream latitude, d > 12 kpc, and L  Y  < − 0.3L  Z  − 2.5  × 103 kpc km s−1. The red line in each panel is the fiducial used to select the likely Sgr member stars, derived by a polynomial fit to the Sgr members in the catalog provided by V21. The black line delineates the ±3σ curve from the fiducial, except for the distance panel, considering the photometric distance error, which is set to ±4σ from the fiducial. The orange dots indicate the stars within the black curves in all four panels. The cluster around Λ = 0° and 360° is the SC. The stars with Λ < 180° belong to the LA, while the ones with Λ > 200° belong to the TA.
Paper: A Dynamically Distinct Stellar Population in the Leading Arm of the Sagittarius Stream
Authors: Gwibong Kang, Young Sun Lee, Young Kwang Kim, Timothy C. Beers
Figure caption: Angular momentum–energy (L–E) diagram for the RGB/MS stars (left panels), the RR Lyrae stars (middle panels), and a Sgr model with the LMC (right panels). The bottom panels are the stars with e < 0.4. Both the L and E quantities are rescaled to have zero at the location of the SC as in V21. The color code is the same as in Figure 2. Note that as the SC stars in the right panel are buried in the LA and TA, they are not clearly visible in the panel. We clearly see the offset of the LA from the TA and SC (top left), and we do not observe many stars with e < 0.4 in the TA and SC (bottom left). The RR Lyrae sample (bottom middle) exhibits the same pattern; qualitatively, a similar behavior is observed in the Sgr model with the LMC perturbation adopted from V21 (bottom right).
Paper: A Dynamically Distinct Stellar Population in the Leading Arm of the Sagittarius Stream
Authors: Gwibong Kang, Young Sun Lee, Young Kwang Kim, Timothy C. Beers
Figure caption: Metallicity profile of three regions (A, B, and C) as a function of Λ for the RGB/MS stars. Each point is a median value in a bin size of Λ = 5°; the error bar is the standard deviation. The color code represents the median eccentricity in each bin, and its scale is shown in the right color bar. The large open circles represent the median metallicity of the A, B, and C regions. Note that the LA is divided into two regions: metal-rich (A) and metal-poor (B). The red horizontal line indicates the median [Fe/H] of the TA. At the bottom of the figure, the fraction of stars with e < 0.4 in each region is listed.
Paper: A Dynamically Distinct Stellar Population in the Leading Arm of the Sagittarius Stream
Authors: Gwibong Kang, Young Sun Lee, Young Kwang Kim, Timothy C. Beers
Figure caption: Eccentricity distribution as a function of Λ. The cyan dots are the RGB/MS stars, while the magenta points indicate the RR Lyrae stars. The black background represents the number density produced by a Sgr model with the LMC, which is adopted from V21. The cluster around Λ ∼ 0° and 360° is the SC. We clearly observe that the eccentricity increases for the stars closer to the SC for the LA, while the opposite behavior is seen for the TA; the farthest stars from the SC have higher eccentricity.
Paper: Geometry and Kinematics of a Dancing Milky Way: Unveiling the Precession and Inclination Variation across the Galactic Plane via Open Clusters
Authors: Zhihong He, 治宏 何
Figure caption: The derived parameters from Equations (1) and (2) are presented with error bars accounting for uncertainties in OC sample age limitations. The parameters include: (a) inclination angle θ  i , (b) LON positions ϕ LON, (c) precession rate ﹩{\dot{\phi }}_{\mathrm{LON}}﹩, (d) inclinational variation rate ﹩{\dot{\theta }}_{i}﹩, (e) differential scale height ﹩{{\rm{d}}}_{{z}_{0}}﹩, and (f) uncertainty (from V ⊙) of ﹩{\dot{\phi }}_{\mathrm{LON}}﹩, plotted against Galactocentric radius R GC. The typical uncertainty resulting from V ⊙ for ﹩{\dot{\theta }}_{i}﹩ is 4.3 μas yr−1.
Paper: Geometry and Kinematics of a Dancing Milky Way: Unveiling the Precession and Inclination Variation across the Galactic Plane via Open Clusters
Authors: Zhihong He, 治宏 何
Figure caption: The edge-on views display Gaia-based OCs (colored dots) and CCs (black dots) from Skowron et al. (2019a) located at varying Galactocentric radii around R GC = 4, 6, 8, 10, 12, and 14 kpc, all within a width range of ±1 kpc. The gray dashed line shows the linear regression of the inclination angle on the line-of-sight anti-Galactic center. Young (<108 yr), middle-aged (108–109 yr), and old (>109 yr) OCs are identified by the blue, magenta, and red symbols, respectively. As the radius increases, the thickness of the OC/CC disks gradually increase, displaying flaring characteristics. Additionally, compared to younger open clusters, the older ones tend to have higher scale heights, as stated in Cantat-Gaudin et al. (2020). It is essential to note that the LONs are not situated at Y = 0 kpc, and the fitted θ  i  is visible in Figure 3(a).
Paper: Geometry and Kinematics of a Dancing Milky Way: Unveiling the Precession and Inclination Variation across the Galactic Plane via Open Clusters
Authors: Zhihong He, 治宏 何
Figure caption: The edge-on views of OCs in the inner (left upper panel) and outer (right upper panel) Galactic disk, along with their corresponding vertical velocity distributions (displayed in the lower panels) are presented. A linear regression is applied (gray dashed line) to demonstrate the smaller inclination angles of the inner disk for clear visualization. Even though the inner disk does not exhibit the same significant tilt as the outer disk, a noticeable negative V Z  is still observed, consistent with the direction of the tilt-induced velocity deviation. In the lower right panel, the black dashed line and cyan dashed line represent the vertical velocity when precession rate ﹩{\dot{\phi }}_{\mathrm{LON}}﹩ = 0 and 6.8 km s−1 kpc−1, respectively. It can be observed that the ﹩{\dot{\phi }}_{\mathrm{LON}}﹩ = 0 does not correspond to the observed V Z  distribution, as supported by the study conducted by Poggio et al. (2020) utilizing proper motions of giant stars.
Paper: Geometry and Kinematics of a Dancing Milky Way: Unveiling the Precession and Inclination Variation across the Galactic Plane via Open Clusters
Authors: Zhihong He, 治宏 何
Figure caption: The distribution of open clusters in the XY plane is depicted in both the face-on (a) and edge-on (b) views, with Galactocentric coordinates (ϕ, θ) also displayed. In the panel (a), the black arrow indicates the rotation direction of the Milky Way, and the position of the solar system is (−8.15, 0) kpc, according to Reid et al. (2019). Red dots represent distant open clusters from He et al. (2023b), while blue crosses denote other Gaia-based open clusters (Cantat-Gaudin et al. 2020; He et al. 2021; Castro-Ginard et al. 2022; He et al. 2022, 2023a). For comparison, the gray pluses signify the CC sample (Skowron et al. 2019a), showing a similar intuitive plot of the warp structure (based on CCs) from Chen et al. (2019) and Lemasle et al. (2022), except for the southern warp at ϕ ∼  270°, which still lacks OC samples there.
Paper: On the Sizes of Ionized Bubbles Around Galaxies During the Reionization Epoch. The Spectral Shapes of the Lyα Emission from Galaxies
Authors: Matthew J. Hayes, Claudia Scarlata
Figure caption: Left: the radii of the bubble inferred from Lyα modeling (R B), contrasted with that of the Strömgren sphere (R S). Right: the comparison of the LyC escape fraction (﹩{f}_{\mathrm{esc}}^{\mathrm{LyC}}﹩; inferred from the left plot) with the model-inferred EW of Lyα. We overplot the values measured at z ≃ 3 by Steidel et al. (2018) and at z ≃ 0.3 by Flury et al. (2022a). Redshift is color-coded in both cases.
Paper: On the Sizes of Ionized Bubbles Around Galaxies During the Reionization Epoch. The Spectral Shapes of the Lyα Emission from Galaxies
Authors: Matthew J. Hayes, Claudia Scarlata
Figure caption: Evolution of the bubble radius, R B (ordinate) with redshift (abscissa). Uncertainties refer to the 16th and 84th percentiles of the posterior. Absolute UV magnitude is color-coded. The shaded regions show the 10–90 percentile range of bubble sizes from the simulation of Giri & Mellema (2021).
Paper: Geometry and Kinematics of a Dancing Milky Way: Unveiling the Precession and Inclination Variation across the Galactic Plane via Open Clusters
Authors: Zhihong He, 治宏 何
Figure caption: Sketch map of scale height in the elliptical inclined galactic plane. The left panel displays the elliptical plane at different semimajor axes, represented by the function: x 2/a 2 + y 2/b 2 = 1, where f 1 (galactic center) and f 2 are the foci, and the eccentricity is set to 0.2. The right panel demonstrates the differential scale height of the f 2 and semiminor axis (galactic mid-plane), with the inclination angles (θ  i ) set at 0.5° (blue), 0° (magenta), and −0.5° (black).
Paper: Geometry and Kinematics of a Dancing Milky Way: Unveiling the Precession and Inclination Variation across the Galactic Plane via Open Clusters
Authors: Zhihong He, 治宏 何
Figure caption: Statistical distribution of velocity component errors presented in the Galactocentric coordinate system, using 1 km s−1 bin size for V Z  and 2.5 km s−1 bin size for V  ϕ  and ﹩{V}_{{R}_{\mathrm{GC}}}﹩.
Paper: The FRB 20190520B Sight Line Intersects Foreground Galaxy Clusters
Authors: Khee-Gan Lee, Ilya S. Khrykin, Sunil Simha, Metin Ata, Yuxin Huang, J. Xavier Prochaska, Nicolas Tejos, Jeff Cooke, Kentaro Nagamine, Jielai Zhang
Figure caption: Galaxy redshift distribution from our AAT/2dF-AAOmega spectroscopic observations, which targeted an approximately 2° field of view centered on FRB 20190520B. The FRB redshift (z frb = 0.241) is indicated by the vertical dashed line.
Paper: A Luminous Precursor in the Extremely Bright GRB 230307A
Authors: S. Dichiara, D. Tsang, E. Troja, D. Neill, J. P. Norris, Y.-H. Yang
Figure caption: Minimum variability timescale (top) and spectral peak energy (bottom) as a function of time. Red and gray crosses mark the evolution measured for GRB 230307A and 211211A, respectively. The shaded renormalized light curves (8–1000 keV) are GRB 230307A (red) and GRB 211211A (gray) (from Troja et al. 2022).
Paper: A Luminous Precursor in the Extremely Bright GRB 230307A
Authors: S. Dichiara, D. Tsang, E. Troja, D. Neill, J. P. Norris, Y.-H. Yang
Figure caption: The relationship between the average luminosity of an RSF and the strength of the magnetic field of the NS that produced it, assuming a 20% gamma-ray efficiency. The relationship is shown for several different values for the rate at which energy is transferred to the i-mode from the binary orbit (Equation (1)). The red dashed lines indicate the luminosity of GRB 230307A’s precursor, and the minimum magnetic field strength required to produce it.
Paper: A Luminous Precursor in the Extremely Bright GRB 230307A
Authors: S. Dichiara, D. Tsang, E. Troja, D. Neill, J. P. Norris, Y.-H. Yang
Figure caption: The i-mode frequency, which could produce an RSF with the duration of GRB 230307A’s precursor, showing how it varies with the mass of one object in the binary when assuming one of several different values for the mass of the other object. The solid lines are for a duration of 0.4 s, and the shaded regions vary this by the minimum variability timescale (±17 ms). Note that this is approximate, owing to simplifications made in the calculation of the resonance duration.
Paper: The Discrepancy between Observed and Predicted Heliospheric Energetic Neutral Atoms below Solar Wind Energy
Authors: André Galli, Igor I. Baliukin, Marc Kornbleuth, Merav Opher, Stephen A. Fuselier, Justyna M. Sokół, Konstantinos Dialynas, Maher A. Dayeh, Vladislav V. Izmodenov, John D. Richardson
Figure caption: The sky regions defined by Galli et al. (2022b), plotted on an ENA intensity map of IBEX-Lo energy bin centered at 0.9 keV averaged over all 11 yr, including ComptonGetting and ENA survival probability correction. V1 and V2 denote Voyager 1 and Voyager 2 directions. Figure taken from Galli et al. (2022b).
Paper: A Luminous Precursor in the Extremely Bright GRB 230307A
Authors: S. Dichiara, D. Tsang, E. Troja, D. Neill, J. P. Norris, Y.-H. Yang
Figure caption: Fermi/GBM Light Curves of GRB 230307A in two energy bands, soft (7–99 keV) and hard (883–38367 keV). The time bin is 16 ms. Bad time intervals (BTIs) are indicated by a dashed horizontal line. The insert zooms in on the first 2.5 s (marked by the thick horizontal bar) to highlight the different spectral properties of the first peak, identified as a possible precursor.
Paper: A Luminous Precursor in the Extremely Bright GRB 230307A
Authors: S. Dichiara, D. Tsang, E. Troja, D. Neill, J. P. Norris, Y.-H. Yang
Figure caption: Spectral fit of GBM data integrated over the precursor (from T 0−0.064 to T 0+0.320) using the three most illuminated NaI detectors (N6, N8, and N10) and the BGO (B1). The inset text shows the best-fit parameters obtained assuming a Band function.
Paper: NGDEEP Epoch 1: The Faint End of the Luminosity Function at z ∼ 9–12 from Ultradeep JWST Imaging
Authors: Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Pérez-González, Alexa Morales, Dale D. Kocevski, Guang Yang, 光 杨, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Óscar A. Chávez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg
Figure caption: Left: rest-frame UV luminosity function at z = 8.5–9.5. We show our luminosity function with red circles (open circles denotes bins where the completeness is <30%). We also show literature values from Bouwens et al. (2021, 2022a), Castellano et al. (2023), Donnan et al. (2023a, 2023b), Harikane et al. (2023), McLeod et al. (2016), and Pérez-González et al. (2023). We show our best-fit DPL function to the NGDEEP and CEERS data points in the red shaded regions. The dark (light) gray shaded regions show the DPL (Schechter) functions from Finkelstein & Bagley (2022) (Finkelstein et al. 2015) extrapolated to z = 8.5 (upper bound) and 9.5 (lower bound). Right: same as the left panel but for z = 9.5–12.0. We also show results from the two-epoch CEERS sample (S. Finkelstein et al. 2023, in preparation). The observed luminosity function at z = 9.5–12 is consistent with the upper end of the extrapolation, suggesting a more gradual evolution of the luminosity function at z ≳ 10. We measure a faint-end slope of –2.4 ± 0.4 at z ∼ 9 and –2.5 ± 0.2 at z ∼ 11, finding no significant evolution at the faint-end slope of the luminosity function.
Paper: NGDEEP Epoch 1: The Faint End of the Luminosity Function at z ∼ 9–12 from Ultradeep JWST Imaging
Authors: Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Pérez-González, Alexa Morales, Dale D. Kocevski, Guang Yang, 光 杨, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Óscar A. Chávez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg
Figure caption: Distribution of F277W magnitude and photometric redshift of our sample. We show objects in our sample with blue circles, along with photometric redshift samples in MDS (Pérez-González et al. 2023; orange asterisks) and Austin et al. (2023; green diamonds). We also show the sample from the completed CEERS NIRCam data set (Finkelstein et al. 2023; S. Finkelstein et al. 2023, in preparation), denoting source photometric redshift with red triangles and spectroscopic redshift with red triangles with black outlines. Even this first epoch of NGDEEP NIRCam imaging allows us to reach fainter magnitudes than CEERS by ∼1.5 mag. While MDS reaches ∼0.5 mag deeper than NGDEEP, we probe ∼1 mag fainter than the very early analysis of NGDEEP data by Austin et al. (2023), primarily due to our custom flat-field correction.
Paper: NGDEEP Epoch 1: The Faint End of the Luminosity Function at z ∼ 9–12 from Ultradeep JWST Imaging
Authors: Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Pérez-González, Alexa Morales, Dale D. Kocevski, Guang Yang, 光 杨, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Óscar A. Chávez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg
Figure caption: The two sources with photometric redshifts at z ≥ 12 in our sample. The top panel shows 1.″5 stamp images. The bottom left panel shows the observed photometry with black points, the best-fit EAZY model spectrum (photometry) with orange curves (open circles), and the best-fit z < 7 model spectrum (photometry) with blue curves (open circles). Observed fluxes with S/N < 2 are shown as 2σ upper limits. The bottom right panel shows the EAZY photometric redshift probability density function with a black curve. The best-fit and secondary redshifts are denoted by the orange and blue dashed vertical lines, respectively. The full sample is shown in the Appendix.
Paper: NGDEEP Epoch 1: The Faint End of the Luminosity Function at z ∼ 9–12 from Ultradeep JWST Imaging
Authors: Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Pérez-González, Alexa Morales, Dale D. Kocevski, Guang Yang, 光 杨, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Óscar A. Chávez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg
Figure caption: Galaxy cumulative surface density of sources with m F277W < 29.5 as a function of redshift. The black dashed line shows the completeness-uncorrected values, while the black solid line shows the completeness-corrected values. The light shaded region shows the 68% confidence intervals derived from Monte Carlo simulations sampling the F277W flux and photometric redshift distributions. The dark shaded region includes the Poisson uncertainty in the simulations. For the highest- and lowest-predicting models, we denote the 1σ spread in the predicted surface density due to cosmic variance with vertical error bars. We compare the observed results with predictions from theoretical models (see main text for details). Accounting for cosmic variance, our observed values are higher than those predicted by THESAN and the Santa Cruz SAM at all redshifts.
Paper: NGDEEP Epoch 1: The Faint End of the Luminosity Function at z ∼ 9–12 from Ultradeep JWST Imaging
Authors: Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Pérez-González, Alexa Morales, Dale D. Kocevski, Guang Yang, 光 杨, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Óscar A. Chávez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg
Figure caption: Same as Figure 3 but for the two sources found in our sample with a remarkably red color at ≳3 μm. The morphology is compact to pointlike. These properties are similar to a class of sources recently discovered with JWST (e.g., Furtak et al. 2022; Akins et al. 2023; Kocevski et al. 2023) whose origins have been attributed to dust-obscured galaxies or SMBH accretion. (Note that the model spectra are the best-fit combinations of EAZY templates considering only stellar emission.) The objects here are the first to be observed at z ∼ 9 and m F444W ∼ 28.
Paper: NGDEEP Epoch 1: The Faint End of the Luminosity Function at z ∼ 9–12 from Ultradeep JWST Imaging
Authors: Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Pérez-González, Alexa Morales, Dale D. Kocevski, Guang Yang, 光 杨, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Óscar A. Chávez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg
Figure caption: Comparison of our z = 9.5–12 rest-frame UV luminosity function with model predictions at z = 11, close to the volume-weighted average redshift of the observed sample of z = 10.7. Our best-fit DPL is shown by the red shaded region. Some models underpredict the number density of galaxies across the full studied range of luminosities, while others underpredict bright galaxies but reproduce the number of fainter galaxies, implying a different predicted luminosity function slope.
Paper: NGDEEP Epoch 1: The Faint End of the Luminosity Function at z ∼ 9–12 from Ultradeep JWST Imaging
Authors: Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Pérez-González, Alexa Morales, Dale D. Kocevski, Guang Yang, 光 杨, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Óscar A. Chávez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg
Figure caption: Color-composite (b = F115W+F150W, g = F200W+F277W, r = F277W+F356W) image of the NGDEEP field from our NIRCam mosaics. These fully reduced mosaics will be made publicly available following the NGDEEP release schedule. The NIRCam imaging reaches 29.9–30.4 AB mag, making it the deepest public JWST GO imaging data set at the time of writing.