adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
Authors: Kevin B. Burdge, Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, Deepto Chakrabarty, Emma Chickles, Matthew J. Graham, Erin Kara, S. R. Kulkarni, Thomas R. Marsh, Melania Nynka, Thomas A. Prince, Robert A. Simcoe, Jan van Roestel, Zach Vanderbosch, Eric C. Bellm, Richard G. Dekany, Andrew J. Drake, George Helou, Frank J. Masci, Jennifer Milburn, Reed Riddle, Ben Rusholme, Roger Smith
Figure caption: Constraints from joint fitting of the donor’s radial velocity semiamplitude and the observed period derivative. Black and red contours adopt priors of ﹩\dot{M}\sim { \mathcal N }(-8.5,0.5)﹩ and ﹩\dot{M}\sim { \mathcal N }(-7.3,0.5)﹩, respectively. The upper right panel shows how, for two different combinations of M wd and M donor that match the observed radial velocity amplitude, the predicted period derivative depends on the mass transfer rate. Mass transfer widens the orbit, so a larger ﹩\dot{M}﹩ requires higher masses to match the observed ﹩{\dot{P}}_{\mathrm{orb}}﹩.
Paper: Detection of a High-velocity Jet from MWC 349A Traced by Hydrogen Recombination Line Maser Emission
Authors: Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Izaskun Jimenéz-Serra, Jesus Martín-Pintado, Antonio Martínez-Henares, Alejandro Báez-Rubio
Figure caption: (a) The spectral profile plot for the H26α and H30α lines. The peak intensity for each spectral channel in the Band 6 and 7 data cubes was extracted as the amplitude from the centroid fit. Velocities are measured in the LSR reference frame in km s−1, and for both lines the velocity resolution is 1.26 km s−1. (b) The spatial distributions of H30α and H26α maser emission obtained by fitting elliptical Gaussians to the data cubes for the two recombination lines. Error bars include the standard deviation from the centroid fit and error contribution from the bandpass calibration (see the text for details). The H26α and the H30α distributions are offset from the position of the Band 7 and 6 continuum, respectively.
Paper: Detection of a High-velocity Jet from MWC 349A Traced by Hydrogen Recombination Line Maser Emission
Authors: Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Izaskun Jimenéz-Serra, Jesus Martín-Pintado, Antonio Martínez-Henares, Alejandro Báez-Rubio
Figure caption: Rotation curves for H30α and H26α masers in MWC 349A. (a) The projected distance is calculated as ﹩\sqrt{{({\rm{\Delta }}{\rm{R}}.{\rm{A}}.\cos (\mathrm{decl}.))}^{2}+{\rm{\Delta }}\mathrm{decl}{.}^{2}}﹩. (b) Distance to the polar axis is calculated as the perpendicular distance from the maser point to the line that is both orthogonal to the line of best fit for the disk masers and that intersects the best-fit line at the center. In both panels the color indicates the velocity of the masers in km s−1.
Paper: Detection of a High-velocity Jet from MWC 349A Traced by Hydrogen Recombination Line Maser Emission
Authors: Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Izaskun Jimenéz-Serra, Jesus Martín-Pintado, Antonio Martínez-Henares, Alejandro Báez-Rubio
Figure caption: Continuum emission of MWC 349A at 1.4 mm in Band 6 (panel (a)) and 0.87 mm in Band 7 (panel (c)) obtained with ALMA. Color indicates intensities in Jy beam−1, and the ellipse at the lower left corner marks the synthesized beam. The two overlaid points in panels (a) and (c) correspond to the two ends of the disk as seen in the maser distribution for that band. Panels (b) and (d) are zoomed-in areas of panels (a) and (c), respectively.
Paper: Detection of a High-velocity Jet from MWC 349A Traced by Hydrogen Recombination Line Maser Emission
Authors: Sirina Prasad, Qizhou Zhang, James Moran, Yue Cao, Izaskun Jimenéz-Serra, Jesus Martín-Pintado, Antonio Martínez-Henares, Alejandro Báez-Rubio
Figure caption: Total flux density and angular size as a function of frequency for the continuum emission of MWC 349A. The solid lines are the linear least-squares fits to the data from this study and data from previous studies; the dashed lines are the linear least-squares fits found by Tafoya et al. (2004).
Paper: Outflowing Helium from a Mature Mini-Neptune
Authors: Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno
Figure caption: Percent excess absorption from TOI 2134b as a function of time and wavelength (stellar rest frame). The dashed cyan line indicates the beginning of the white-light transit, while the solid cyan line indicates the end. The red lines show the wavelengths of planetary helium absorption. The white bars indicate gaps in the data. Note the variability in the stellar Si I line at 10830 Å and Na I line at 10838 Å, as well as the uncorrected telluric variability around 10836 Å. There is no stellar photospheric or telluric line near the 10833 Å helium absorption.(The data used to create this figure are available.)
Paper: Analytic Understanding of the Resonant Nature of Kozai–Lidov Cycles with a Precessing Quadrupole Potential
Authors: Ygal Y. Klein, Boaz Katz
Figure caption: Results of numerical integrations for (left panel) α = 0.01° and β ≈ 2.9, with initial conditions e  x  = j  x  = − j  y  =10−5, e  z  = 0.98, and (right panel) α = 5° and β = 2.5, with initial conditions e  x  ∼ −10−5, j  x  ∼ −0.28, j  y  ∼ − 0.186, e  z  ∼ 0.825. The blue solid lines are the result of the integration of the full secular equations, Equations (3) (with (2)), while the red dashed lines are the result of the averaged equations, Equations (21)–(24), and using Equation (33) (where it has real roots) to determine e min and e max using Equations (25) and (34). The two green horizontal lines in the bottom panel represent the extremum values of δ as determined from initial conditions and in the middle panel the maximal and minimal values of j  z  as determined from initial conditions using Equation (25) and the extremums of δ. ﹩\hat{\tau }﹩ is defined in Equation (12).
Paper: Analytic Understanding of the Resonant Nature of Kozai–Lidov Cycles with a Precessing Quadrupole Potential
Authors: Ygal Y. Klein, Boaz Katz
Figure caption: Upper panel: the potential V (Equation (30)) in blue and the constant energy E (Equation (29)) in black for the two optional shapes dependent on the constants C 1 (Equation (26)) and C 2 (Equation (27)). Lower panel: trajectories in the a − b vs. θ − ϕ plane for different values of C 1 at some C 2. Dashed black line mark the minimal value of C 1 for rotations. Red dashed lines mark the value of C 1 of the potentials in the upper panels. The left plots show a case where ﹩{C}_{1}\lt {C}_{1}^{\mathrm{crit}}﹩ and θ − ϕ is librating. The right plots are the case that is shown in the left panel of Figure 1 and show a case where ﹩{C}_{1}\gt {C}_{1}^{\mathrm{crit}}﹩ and θ − ϕ is rotating. Red circles (in all panels) mark the extremums of δ (which are also a − b extremums, see Equation (27)).
Paper: DELVE 6: An Ancient, Ultra-faint Star Cluster on the Outskirts of the Magellanic Clouds
Authors: W. Cerny, A. Drlica-Wagner, T. S. Li, A. B. Pace, K. A. G. Olsen, N. E. D. Noël, R. P. van der Marel, J. L. Carlin, Y. Choi, D. Erkal, M. Geha, D. J. James, C. E. Martínez-Vázquez, P. Massana, G. E. Medina, A. E. Miller, B. Mutlu-Pakdil, D. L. Nidever, J. D. Sakowska, G. S. Stringfellow, J. A. Carballo-Bello, P. S. Ferguson, N. Kuropatkin, S. Mau, E. J. Tollerud, A. K. Vivas
Figure caption: (Left) ﹩2^{\prime} \times 2^{\prime} ﹩ false-color image cutout centered on DELVE 6 based on griz DECam imaging, taken from the Legacy Survey Sky Viewer. A clustering of faint blue sources is visible amidst a number of foreground stars and background galaxies. We have increased the brightness of this cutout image to enhance the visibility of faint cluster member stars. (Right) Map of star clusters and dwarf galaxies in the Magellanic environment, plotted in the Magellanic Stream coordinate system from Nidever et al. (2008). Each black point corresponds to a star cluster included in the main cluster catalogs from Bica et al. (2008, 2020). Recently discovered ultra-faint star clusters in this region are shown as red dots, whereas candidate and confirmed ultra-faint dwarf galaxies potentially associated with the MCs are shown as blue triangles. We caution that some of these objects have uncertain classifications and/or tentative associations with the MCs. In addition, we plot the centroid position of the SMC northern overdensity (SMCNOD; Pieres et al. 2017) in orange. Lastly, DELVE 6 is shown as a yellow star positioned near B MS ∼ 0; this latitude falls along the projected track of the Magellanic Stream.
Paper: DELVE 6: An Ancient, Ultra-faint Star Cluster on the Outskirts of the Magellanic Clouds
Authors: W. Cerny, A. Drlica-Wagner, T. S. Li, A. B. Pace, K. A. G. Olsen, N. E. D. Noël, R. P. van der Marel, J. L. Carlin, Y. Choi, D. Erkal, M. Geha, D. J. James, C. E. Martínez-Vázquez, P. Massana, G. E. Medina, A. E. Miller, B. Mutlu-Pakdil, D. L. Nidever, J. D. Sakowska, G. S. Stringfellow, J. A. Carballo-Bello, P. S. Ferguson, N. Kuropatkin, S. Mau, E. J. Tollerud, A. K. Vivas
Figure caption: (Left) Spatial distribution of stars in a 0.°12 × 0.°12 (﹩7\buildrel{\,\prime}\over{.} 2\times 7\buildrel{\,\prime}\over{.} 2﹩) field centered on DELVE 6. Stars are colored by their probability of being a member of the candidate system, as determined through our ugali fit described in Section 2.2; stars with probabilities p < 0.1 are shown in gray. (Middle) CMD for the stars shown in the left panel. The best-fit isochrone with Z = 0.0001 and τ = 13.5 Gyr is shown in black, although see the discussion in Section 2.2 and Figure 3 for caveats about this model. (Right) Radial stellar density profile for DELVE 6. The best-fit Plummer model is shown as a solid blue curve, assuming the half-light radius reported in Table 1 and an ellipticity ϵ = 0. This ellipticity is approximately matched to the mode of the marginalized posterior distribution for ϵ derived from our MCMC analysis; however, our constraint on the system’s ellipticity (ϵ < 0.56 at 95% confidence) is relatively weak due to the small number of observed member stars.
Paper: DELVE 6: An Ancient, Ultra-faint Star Cluster on the Outskirts of the Magellanic Clouds
Authors: W. Cerny, A. Drlica-Wagner, T. S. Li, A. B. Pace, K. A. G. Olsen, N. E. D. Noël, R. P. van der Marel, J. L. Carlin, Y. Choi, D. Erkal, M. Geha, D. J. James, C. E. Martínez-Vázquez, P. Massana, G. E. Medina, A. E. Miller, B. Mutlu-Pakdil, D. L. Nidever, J. D. Sakowska, G. S. Stringfellow, J. A. Carballo-Bello, P. S. Ferguson, N. Kuropatkin, S. Mau, E. J. Tollerud, A. K. Vivas
Figure caption: (Left) 2D posterior probability distribution for the metallicity and age of DELVE 6. The blue shaded contours denote the 1σ, 2σ, and 3σ 2D confidence regions in this plane. (Right) CMD for all stars within 2r 1/2 of DELVE 6's centroid. Two isochrone models are shown. The blue model depicts an isochrone with [Fe/H] = −2.19 and τ = 13.5 Gyr, consistent with the posterior mode shown in the bottom right corner of the left panel, whereas the red model depicts a younger, more metal-rich isochrone corresponding to a fit lying within the medium-blue 2σ contour near the top center of the left panel. Here both models are fixed to the distance modulus reported in Table 1, despite small differences in distance between the corresponding samples. We highlight that one BHB candidate lies along the older, more metal-poor (blue) model, and one (likely nonmember) star lies near the RHB of the younger, more metal-rich (red) model.
Paper: DELVE 6: An Ancient, Ultra-faint Star Cluster on the Outskirts of the Magellanic Clouds
Authors: W. Cerny, A. Drlica-Wagner, T. S. Li, A. B. Pace, K. A. G. Olsen, N. E. D. Noël, R. P. van der Marel, J. L. Carlin, Y. Choi, D. Erkal, M. Geha, D. J. James, C. E. Martínez-Vázquez, P. Massana, G. E. Medina, A. E. Miller, B. Mutlu-Pakdil, D. L. Nidever, J. D. Sakowska, G. S. Stringfellow, J. A. Carballo-Bello, P. S. Ferguson, N. Kuropatkin, S. Mau, E. J. Tollerud, A. K. Vivas
Figure caption: Absolute magnitude (M  V ) vs. azimuthally averaged half-light radius (r 1/2) for a large sample of classical globular clusters, candidate and confirmed MW satellite galaxies, and recently discovered ultra-faint halo star clusters. The location of DELVE 6 in this plane is indicated by a yellow star. A complete reference list for this figure is available in Appendix B.
Paper: Symbiotic Star T CrB as an Extreme SU UMa–type Dwarf Nova
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Kiril A. Stoyanov
Figure caption: The smoothed light curve of T CrB in BV filters after the red giant contribution was removed. The blue lines indicate the start of superoutbursts, and the red lines indicate the times of normal dwarf nova outbursts (see the text).
Paper: Symbiotic Star T CrB as an Extreme SU UMa–type Dwarf Nova
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Kiril A. Stoyanov
Figure caption: The historical light curve of T CrB in UBV filters. The blue lines indicate the start of superoutbursts, and the red lines indicate the times of normal dwarf nova outbursts (see the text).
Paper: Symbiotic Star T CrB as an Extreme SU UMa–type Dwarf Nova
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Kiril A. Stoyanov
Figure caption: Same as Figure 2, but zoomed in on the most recent superoutburst. The maxima of suspected superhumps are marked with dashed lines.
Paper: Symbiotic Star T CrB as an Extreme SU UMa–type Dwarf Nova
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Kiril A. Stoyanov
Figure caption: Relationships between normal dwarf nova/short dwarf nova outbursts and superoutbursts/long dwarf nova outbursts properties (Otulakowska-Hypka et al. 2016). The SU UMa–type dwarf novae are plotted with the black points, the remaining dwarf novae are plotted with the gray points, and the measurements for T CrB are plotted with the red points (see the text).
Paper: Constraining Dark Energy from the Local Group Dynamics
Authors: David Benisty, Anne-Christine Davis, N. Wyn Evans
Figure caption: Top: bound on Λ from the Local Group dynamics (blue) compared to the measured value from Planck (green). The special case (orange) is for 5% for the mass and for the tangential velocity, with 2% for the other quantities. For this case, the upper bound on Λ is predicted to be 1.67 ± 0.79 times from the Planck value. Bottom: the reduced Δχ 2 for the current and the future local group measurements.
Paper: Constraining Dark Energy from the Local Group Dynamics
Authors: David Benisty, Anne-Christine Davis, N. Wyn Evans
Figure caption: Bound on the running gravitational constant ΔG/G from the Local Group dynamics vs. the Cassini bound (Bertotti et al. 2003) and Cepheids in the Large Magellanic Cloud (Desmond et al. 2021).
Paper: Constraining Dark Energy from the Local Group Dynamics
Authors: David Benisty, Anne-Christine Davis, N. Wyn Evans
Figure caption: The timing argument + cosmic bias prediction for the Local Group mass vs. the cosmological constant Λ value (blue). The red curve shows the latest updated mass of (3.2 ± 1.6) 1012 M ⊙ from Benisty et al. (2022).
Paper: A Luminous Red Supergiant and Dusty Long-period Variable Progenitor for SN 2023ixf
Authors: Jacob E. Jencson, Jeniveve Pearson, Emma R. Beasor, Ryan M. Lau, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Michael Engesser, Sebastian Gomez, Muryel Guolo, Emily Hoang, Griffin Hosseinzadeh, Saurabh W. Jha, Viraj Karambelkar, Mansi M. Kasliwal, Michael Lundquist, Nicolas E. Meza Retamal, Armin Rest, David J. Sand, Melissa Shahbandeh, Manisha Shrestha, Nathan Smith, Jay Strader, Stefano Valenti, Qinan Wang, Yossef Zenati
Figure caption: The SED of the SN2023 ixf progenitor candidate is shown in both panels, including phase-weighted average flux measurements from Spitzer and MMIRS (black diamonds) and the HST measurements reported by Kilpatrick et al. (2023; gray diamonds). Downward arrows indicate upper limits. In the left panel, the 20 best-fitting GRAMS models to the IR data points are shown as curves, where the color indicates χ 2 for the fit as indicated by the color bar. The best-fitting single model (T eff = 2300 K, ﹩\mathrm{log}L/{L}_{\odot }=5.07﹩) is indicated as the thick dashed curve, and the corresponding synthetic photometry in the four IR bands included in the fitting are shown as the red open square symbols. A warmer model (T eff = 3500 K, ﹩\mathrm{log}L/{L}_{\odot }=5.12﹩) at a secondary, relative minimum in the χ 2 distribution is shown as the thick dotted curve. In the right panel, we show two superwind models from Davies et al. (2022), with the same mapping of color to χ 2.
Paper: A Luminous Red Supergiant and Dusty Long-period Variable Progenitor for SN 2023ixf
Authors: Jacob E. Jencson, Jeniveve Pearson, Emma R. Beasor, Ryan M. Lau, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Michael Engesser, Sebastian Gomez, Muryel Guolo, Emily Hoang, Griffin Hosseinzadeh, Saurabh W. Jha, Viraj Karambelkar, Mansi M. Kasliwal, Michael Lundquist, Nicolas E. Meza Retamal, Armin Rest, David J. Sand, Melissa Shahbandeh, Manisha Shrestha, Nathan Smith, Jay Strader, Stefano Valenti, Qinan Wang, Yossef Zenati
Figure caption: Mid- and near-IR pre-explosion light curves of the SN 2023ixf progenitor candidate. Mid-IR [3.6] and [4.5] Spitzer light curves are based on image subtraction (filled gray circles and black squares, respectively) relative to PSF photometry on the 2004 Super Mosaics (open symbols). The J- and K  s /K cont-band light curves (orange pentagons and red diamonds, respectively) from ground-based NIRI and MMIRS imaging extend up to just 10.35 days before the SN discovery, indicated by the purple dashed line. The epoch of archival 2002 HST imaging reported by Soraisam et al. (2023a), Pledger & Shara (2023), and Kilpatrick et al. (2023) is indicated by the blue downward arrow.(The data used to create this figure are available.)
Paper: A Luminous Red Supergiant and Dusty Long-period Variable Progenitor for SN 2023ixf
Authors: Jacob E. Jencson, Jeniveve Pearson, Emma R. Beasor, Ryan M. Lau, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Michael Engesser, Sebastian Gomez, Muryel Guolo, Emily Hoang, Griffin Hosseinzadeh, Saurabh W. Jha, Viraj Karambelkar, Mansi M. Kasliwal, Michael Lundquist, Nicolas E. Meza Retamal, Armin Rest, David J. Sand, Melissa Shahbandeh, Manisha Shrestha, Nathan Smith, Jay Strader, Stefano Valenti, Qinan Wang, Yossef Zenati
Figure caption: HRD showing possible locations of the SN 2023ixf progenitor candidate. The result for the single best-fitting model from our SED analysis is shown as the large red star symbol, while the range of the 20 best models are shown by the small circles. The orange four-pointed star represents a secondary, local minimum in the χ 2 distribution at a more typical temperature for RSGs. The color of each point represents the χ 2 for the fit, as indicated by the color bar. The “x” symbols show the locations of the star assuming early, mid, and late M-type spectra and applying the K-band bolometric corrections of Davies & Beasor (2018) to the average K  s -band measurement. We show stellar evolutionary tracks from MIST (nonrotating, solar metallicity) for a set of massive stars in the range M = 8–26 M ⊙ as black curves for comparison. We also show the collection of directly detected SN progenitors of Types II (light gray squares) and IIb (dark gray circles; see text in Section 4.1).
Paper: A Luminous Red Supergiant and Dusty Long-period Variable Progenitor for SN 2023ixf
Authors: Jacob E. Jencson, Jeniveve Pearson, Emma R. Beasor, Ryan M. Lau, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Michael Engesser, Sebastian Gomez, Muryel Guolo, Emily Hoang, Griffin Hosseinzadeh, Saurabh W. Jha, Viraj Karambelkar, Mansi M. Kasliwal, Michael Lundquist, Nicolas E. Meza Retamal, Armin Rest, David J. Sand, Melissa Shahbandeh, Manisha Shrestha, Nathan Smith, Jay Strader, Stefano Valenti, Qinan Wang, Yossef Zenati
Figure caption: IR light curves (symbols are the same as in Figure 2) folded to a best-fitting period of P = 1119.4 days from a joint Lomb–Scargle analysis of the [3.6] and [4.5] data. A phase-weighted average magnitude has been subtracted out for each band. The ground-based near-IR data agree remarkably well with the pulsation cycle derived from the Spitzer measurements, without any additional fine-tuning of the parameters. The inferred phases of the explosion epoch and archival HST observations are indicated by the purple dashed line and blue downward arrow, as in Figure 2.
Paper: What Do Halo CMEs Tell Us about Solar Cycle 25?
Authors: Nat Gopalswamy, Grzegorz Michalek, Seiji Yashiro, Pertti Mäkelä, Sachiko Akiyama, Hong Xie
Figure caption: Solar wind parameters at 1 au (red lines with left-side y-axis) from the OMNI database: total pressure (Pt), magnetic field magnitude (B), proton density (N), proton temperature (T), and the Alfvén speed (V A). The blue lines (right-side y-axis) show the same parameters extrapolated from 1 au to the coronagraph field of view (20 Rs). The extrapolations assume that B, N, and T vary with the heliocentric distance R as R −2, R −2, and R −0.7, respectively. The blue bars denote the average values of the solar wind parameters over the first 37 months, roughly corresponding to the rise (RS) phase in each solar cycle. The maximum (MX) and declining (DCLN) phases of SCs 23 and 24 are also marked for completeness. The reduction in various parameters with respect to SC 23 in SC 24 (SC 25) are as follows: 40% (35%) in Pt, 23% (21%) in B, 30% (19%) in N, 25% (17%) in T, and 10% (13%) in V A.
Paper: A Luminous Red Supergiant and Dusty Long-period Variable Progenitor for SN 2023ixf
Authors: Jacob E. Jencson, Jeniveve Pearson, Emma R. Beasor, Ryan M. Lau, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Michael Engesser, Sebastian Gomez, Muryel Guolo, Emily Hoang, Griffin Hosseinzadeh, Saurabh W. Jha, Viraj Karambelkar, Mansi M. Kasliwal, Michael Lundquist, Nicolas E. Meza Retamal, Armin Rest, David J. Sand, Melissa Shahbandeh, Manisha Shrestha, Nathan Smith, Jay Strader, Stefano Valenti, Qinan Wang, Yossef Zenati
Figure caption: IR pre-explosion imaging of the site of SN 2023ixf. The source identified as the progenitor candidate is indicated by the white crosshairs at the center of each panel. In the left column, we show the Spitzer/IRAC [3.6] (top) and [4.5] (bottom) Super Mosaics. In the bottom center and right panels, respectively, we show the [4.5] image from 2015 June 18 and its corresponding difference image, where the Super Mosaic was used as the template for subtraction. The negative (white) flux at the position in the difference image indicates the source was fainter in 2015 than in 2004. The top center and right panels are the MMIRS J- and K-band images from 2023 April 2. The orientation and scale of each image are the same as indicated in the upper left panel.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: An RGB composite of the NGDEEP field after our reduction (R:F444W, G:F277W, B:F200W). Before we carry out our analysis, we mask the stars and other bright, foreground galaxies to obtain accurate depths and remove potential spurious detections from our catalogs. We note the locations of the commonly referred to modules A (left) and B (right).