adsabs/AstroCLIMB huggingface dataset:
Paper: Space Weathering Properties of Chang’e-6 Soils and Implication for Regolith Evolution of Young Lunar Maria
Authors: Xuejin Lu, Jian Chen, Haijun Cao, Changqing Liu, Ziyi Jia, Chengxiang Yin, Tianwei Wang, Xiaohui Fu, Le Qiao, Xiaojia Zeng, Jiang Zhang, Zongcheng Ling
Figure caption: Comparison of Chang’e-6 soil spectra with Apollo soil spectra. Laboratory measured reflectance (top), normalized reflectance at 750 nm (middle), and continuum-removed reflectance (bottom) of Chang’e-6 soils, Apollo mare soils (left), and Apollo highland soils (right) at various maturities were compared. These Apollo soil spectra are from the Lunar Soil Characterization Consortium (L. A. Taylor et al. 2001).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Space Weathering Properties of Chang’e-6 Soils and Implication for Regolith Evolution of Young Lunar Maria
Authors: Xuejin Lu, Jian Chen, Haijun Cao, Changqing Liu, Ziyi Jia, Chengxiang Yin, Tianwei Wang, Xiaohui Fu, Le Qiao, Xiaojia Zeng, Jiang Zhang, Zongcheng Ling
Figure caption: Fine-grained soils in optically mature veneer removed by Chang’e-6 rocket exhaust. Red arrows indicate the dust devil, raised fine-grained, and mature soil particles.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Representative example of a network jet observed in coordinated IRIS and SDO/AIA data set 1 to illustrate the (cooler) TR contamination in the AIA passbands. Predicted counts in different temperature bins obtained under isothermal approximation are shown for AIA 131 Å in panel (a), AIA 171 Å in panel (b), and AIA 193 Å in panel (c). The leftmost image in each of the panels shows the observed IRIS Si IV 1400 counts for comparison, and the “plus” marker serves as a guide for locating the same pixel across the different images. Note the different color bars in each of the images, which were intentionally chosen to optimize the visualization of the network jet. The size of each pixel is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩167 in the horizontal and vertical direction.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Temperature diagnostics with the filter-ratio method. Panel (a): ratio of the temperature response of the SDO/AIA 171 and 131 filters between logT[K] = [5.5, 6.0]. Panel (b), left to right: observed IRIS Si IV 1400 SJI intensities for network jet 1, predicted intensities using the total EM, and temperature map derived from the filter-ratio technique. Panels (c) and (d) are the same as panel (b) but for network jets 2 and 3. The FOV and the pixel size are the same as Figures 7, 8, and 9.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Same as Figure 7 but for a different network jet observed in data set 2.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Same as Figure 7 but for a different network jet observed in data set 1.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Zoom-in to the chromospheric Doppler shifts and lower coronal emission associated with spicular plasma for the bounded region indicated in Figure 4. Rows from top to bottom show Mg II k2 peak separation map, Doppler shift of the line core (k3), unsharped masked version of SDO/AIA 171, EMs computed using the method of sparsity, and Tikhonov regularization.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Coronal plane-of-sky velocities corresponding to the x–t maps of slit-1 from data sets 1 (top row) and 2 (bottom row) shown in Figures 1 and 2. The x-axis shows the time in seconds from the beginning of the observation. The dashed blue lines indicate the propagation for which the velocities are indicated. The two panels in each of the two rows correspond to SDO/AIA 171 Å and EM map derived using Tikhonov regularization.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Response functions for Si IV and SDO/AIA 131, 171, and 193 Å EUV channels. The response functions for the (selected) AIA channels are calculated using the routines available in SSWIDL, and the Si IV line is calculated using the method described in the appendix.
Paper: The Importance of Berry Phase in Solar Acoustic Modes
Authors: Armand Leclerc, Guillaume Laibe
Figure caption: Ray-tracing equations accounting for the Berry curvature are slightly deviated, correcting the frequencies of standing waves. Left: the polarization of the wave adds a Berry term in the ray-tracing equations, changing the bending of the ray between a scalar and fully vectorial theory. The resulting standing wave traced by the rays has a different frequency. Right: frequency estimates of solar acoustic modes for azimuthal degree ℓ = 25 significantly improve when accounting for the Berry phase, in particular for low radial orders n. The scalar and the two vectorial theories account for the phase function α(ω), the “vectorial (no Berry)” theory accounts for correction of Ω arising from spatial variation of background quantities, and the “vectorial (Berry)” theory further incorporates ϕB. For n ≤ 20, only the predictions accounting for ϕB match the observed frequencies to the current degree of precision of the 1D model (1%). The observational uncertainties (vertical bars) are indistinguishable at this scale (0.1% in F. Hill et al. 1996).
Paper: The Importance of Berry Phase in Solar Acoustic Modes
Authors: Armand Leclerc, Guillaume Laibe
Figure caption: The phase-space trajectories of solar standing acoustic waves enclose a specific amount of Berry curvature Fp, which gives rise to the Berry phase. A sharp feature appears close to the surface (z ∼ 140). Radial orders shown vary from n = 0 to n = 10 for ℓ = 25.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: MIRI LRS white-light curve of K2-18 b. The light curve is based on the time-series spectroscopic data binned between 4.8 and 10 μm, discarding the first 250 integrations. The top panel shows the white-light curve with and without binning, together with the median model fit. The lower panel shows the residuals after subtracting the model. The standard deviation of the residuals without binning is 471 ppm—corresponding to 1.25 times the expected noise level from photon noise and read noise.
Paper: Recent Star Formation in 0.5 < z < 1.5 Quiescent Galaxies
Authors: Michael J. Rutkowski, Bonnabelle Zabelle, Tyler Hagen, Anahita Alavi, Seth Cohen, Christopher Conselice, Norman Grogin, Yicheng Guo, Matthew Hayes, Sugata Kaviraj, Anton Koekemoer, Ray A. Lucas, Kameswara Bharadwaj Mantha, Alec Martin, Vihang Mehta, Bahram Mobasher, Nimish Hathi, Zhiyuan Ji, Kalina V. Nedkova, Robert O'Connell, Marc Rafelski, Claudia Scarlata, Harry I. Teplitz, Xin Wang, Rogier Windhorst, L. Y. Aaron Yung
Figure caption: Relevant archival parameters derived for the UVCANDELS sample of quiescent galaxies; throughout, filled circles indicate significantly (>3σ) F275W-detected quiescent galaxies. Left panel: UVJ color–color used for differentiating 0.5 < z < 1.5 quiescent galaxies (upper left) from SFGs; rest-frame UVJ colors from I. G. Momcheva et al. (2016). Center panel: physical size (kpc)–stellar mass distribution (M⊙) with the same CANDELS field galaxies (green contours), with the HST WFC3-IR/F160W PSF FWHM in physical units (z ≃ 1). Right panel: Sérsic profile index–star formation rate (M⊙ yr−1) distribution with the same for CANDELS field galaxies (red contours). In the center and right panels, physical size parameters are from A. van der Wel et al. (2012) and stellar parameters are from I. G. Momcheva et al. (2016).
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Spectral contributions from DMDS and DMS, also shown in Figure 4, as well as several other molecular species with significant cross sections in the mid-infrared considered in the maximal retrieval described in Section 3.1. All mixing ratios are set to 5 × 10−4.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Transit depth uncertainties of our MIRI transmission spectrum of K2-18 b with 0.2 μm bins. The solid and dotted green lines show the uncertainties for JExoRES, with and without using the GP model, respectively, as discussed in Appendix A.7. The solid orange line shows the uncertainties obtained with JexoPipe, as also discussed in Appendix A.7. The dotted line shows the expected uncertainties, obtained by propagating the photon and read noise.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Comparison of different limb-darkening assumptions on the MIRI transmission spectrum of K2-18 b. The wavelength-dependent model limb-darkening case is shown in pink, while the wavelength-independent empirical limb-darkening case is shown in dark gray. The model limb-darkening coefficients were obtained using an ATLAS9 model (F. Castelli & R. L. Kurucz 2003), computed via ExoCTK (M. Bourque et al. 2021).
Paper: Recent Star Formation in 0.5 < z < 1.5 Quiescent Galaxies
Authors: Michael J. Rutkowski, Bonnabelle Zabelle, Tyler Hagen, Anahita Alavi, Seth Cohen, Christopher Conselice, Norman Grogin, Yicheng Guo, Matthew Hayes, Sugata Kaviraj, Anton Koekemoer, Ray A. Lucas, Kameswara Bharadwaj Mantha, Alec Martin, Vihang Mehta, Bahram Mobasher, Nimish Hathi, Zhiyuan Ji, Kalina V. Nedkova, Robert O'Connell, Marc Rafelski, Claudia Scarlata, Harry I. Teplitz, Xin Wang, Rogier Windhorst, L. Y. Aaron Yung
Figure caption: Representative three-color images of UVJ-selected, quiescent galaxies in the UVCANDELS fields considered in this survey. We combine UVCANDELS and archival imaging in WFC3/UVIS F275W, ACS/WFC F606W, and WFC3/IR F125W (blue, green, red, respectively). The quiescent galaxy is centered in each image; a scale bar of length  ∼2﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 is provided (bottom left pane).
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Illustration of the correlation amplitude ρ (left) and the average autocorrelation function (right). The median fit is shown in solid green, while the 1σ and 2σ regions are shown in two lighter shades of green.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Posterior probability distributions of mixing ratios for a number of molecular species included in the maximal retrieval described in Section 3.1. We find that only one out of the 20 species considered, DMDS, has a well-constrained posterior, as shown. When DMDS is removed from the model, a peak in the posterior is found for DMS.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Posterior probability distribution for the canonical retrieval using the JExoRES spectrum. The diagonal panels show the posterior probability distribution for each parameter and the off-diagonal panels show the pairwise correlations. The horizontal error bars denote the median and 1σ intervals for each parameter.
Paper: Recent Star Formation in 0.5 < z < 1.5 Quiescent Galaxies
Authors: Michael J. Rutkowski, Bonnabelle Zabelle, Tyler Hagen, Anahita Alavi, Seth Cohen, Christopher Conselice, Norman Grogin, Yicheng Guo, Matthew Hayes, Sugata Kaviraj, Anton Koekemoer, Ray A. Lucas, Kameswara Bharadwaj Mantha, Alec Martin, Vihang Mehta, Bahram Mobasher, Nimish Hathi, Zhiyuan Ji, Kalina V. Nedkova, Robert O'Connell, Marc Rafelski, Claudia Scarlata, Harry I. Teplitz, Xin Wang, Rogier Windhorst, L. Y. Aaron Yung
Figure caption: Young stellar age and stellar mass fraction derived with CIGALE (see Section 4 above; M. Boquien et al. 2019) for UVJ-selected, quiescent galaxies with significant F275W (≥3σ) detections. Left panel: a two-dimensional heatmap histogram indicating CIGALE-“best” parameter estimation. Right panel: confidence intervals derived from the CIGALE-“Bayes” parameter estimation for all galaxies in each histogram cell. The upper (lower) row is formatted as follows as “x0 ± x1(x2)”, with x0 = mean, x1 = mean error, and x2 = standard deviation derived for the burst mass (fraction), respectively. Regions of parameter space not populated by galaxies in this sample are indicated by “—”; “xxx” indicates that the CIGALE best-fit SED was inconsistent with young stellar population. When a histogram cell is populated by a single galaxy, x2 ≡ 0.00 is excluded.
Paper: Recent Star Formation in 0.5 < z < 1.5 Quiescent Galaxies
Authors: Michael J. Rutkowski, Bonnabelle Zabelle, Tyler Hagen, Anahita Alavi, Seth Cohen, Christopher Conselice, Norman Grogin, Yicheng Guo, Matthew Hayes, Sugata Kaviraj, Anton Koekemoer, Ray A. Lucas, Kameswara Bharadwaj Mantha, Alec Martin, Vihang Mehta, Bahram Mobasher, Nimish Hathi, Zhiyuan Ji, Kalina V. Nedkova, Robert O'Connell, Marc Rafelski, Claudia Scarlata, Harry I. Teplitz, Xin Wang, Rogier Windhorst, L. Y. Aaron Yung
Figure caption: We implemented an MCMC logistic regression statistical analysis to determine the probability of an F275W detection for quiescent galaxies—a signpost for RSF (Section 4.3)—given the number of neighbors. We find the probability of a detection increases marginally with the number of neighbors. This weak environmental correlation likely indicates a reduced role for environmental processes (mergers, interactions), among the array of internal and ex situ processes, in the formation and evolution of quiescent galaxies.
Paper: Recent Star Formation in 0.5 < z < 1.5 Quiescent Galaxies
Authors: Michael J. Rutkowski, Bonnabelle Zabelle, Tyler Hagen, Anahita Alavi, Seth Cohen, Christopher Conselice, Norman Grogin, Yicheng Guo, Matthew Hayes, Sugata Kaviraj, Anton Koekemoer, Ray A. Lucas, Kameswara Bharadwaj Mantha, Alec Martin, Vihang Mehta, Bahram Mobasher, Nimish Hathi, Zhiyuan Ji, Kalina V. Nedkova, Robert O'Connell, Marc Rafelski, Claudia Scarlata, Harry I. Teplitz, Xin Wang, Rogier Windhorst, L. Y. Aaron Yung
Figure caption: The effective (half-light) radius–stellar mass distribution measured for UVJ-selected galaxies in three redshift bins as indicated in each panel. Here, UVJ-selected, F275W-detected quiescent galaxies are indicated with filled points. Overplotted are density contours (over the range 0%–100%, in 20% decrements) for size–mass distribution of the full UVJ-selected galaxies in the sample. For comparison, the local size–mass relation (black, dashed; S. Shen et al. 2003) is provided in each figure, with F125W FWHM in physical units (at z ∼ 1) indicated in cyan in the right panel.
Paper: Recent Star Formation in 0.5 < z < 1.5 Quiescent Galaxies
Authors: Michael J. Rutkowski, Bonnabelle Zabelle, Tyler Hagen, Anahita Alavi, Seth Cohen, Christopher Conselice, Norman Grogin, Yicheng Guo, Matthew Hayes, Sugata Kaviraj, Anton Koekemoer, Ray A. Lucas, Kameswara Bharadwaj Mantha, Alec Martin, Vihang Mehta, Bahram Mobasher, Nimish Hathi, Zhiyuan Ji, Kalina V. Nedkova, Robert O'Connell, Marc Rafelski, Claudia Scarlata, Harry I. Teplitz, Xin Wang, Rogier Windhorst, L. Y. Aaron Yung
Figure caption: Overplotted on the SED (magenta, filled circles) of this representative UVJ-selected, F275W-detected quiescent galaxy are the best-fit young and old stellar populations (green and red, respectively) with the dust-corrected, best-fit model (black) population. Without UVCANDELS F275W+F435W, the prominent very young (tyoung ≃ 10Myr), albeit minor (fm ≃ 0.01%), stellar population in this “quiescent” galaxy is difficult to characterize. In the top panel, the broadband filtercurves used are provided.
Paper: A Glimpse of the New Redshift Frontier through AS1063
Authors: Vasily Kokorev, Hakim Atek, John Chisholm, Ryan Endsley, Iryna Chemerynska, Julian B. Muñoz, Lukas J. Furtak, Richard Pan, Danielle Berg, Seiji Fujimoto, Pascal A. Oesch, Andrea Weibel, Angela Adamo, Jeremy Blaizot, Rychard Bouwens, Miroslava Dessauges-Zavadsky, Gourav Khullar, Damien Korber, Ilias Goovaerts, Michelle Jecmen, Ivo Labbé, Floriane Leclercq, Rui Marques-Chaves, Charlotte Mason, Kristen B. W. McQuinn, Rohan Naidu, Priyamvada Natarajan, Erica Nelson, Joki Rosdahl, Alberto Saldana-Lopez, Daniel Schaerer, Maxime Trebitsch, Marta Volonteri, Adi Zitrin
Figure caption: Most secure z ≳ 16 candidates from GLIMPSE. For each source we show 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 cutouts in all broad- and medium-band NIRCam filters, plus a detection (F277W+F356W+F444W) LW stack. On each cutout we overlay the extraction aperture (D = 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩2) in green. On the SED plot, we show the best-fit high-z vs. low-z EAZY models (maroon and blue, respectively), as well as the same for BEAGLE (dashed orange and green). The colored circles represent the integrated flux density for each solution. Detections are shown as black squares; 3σ upper limits are shown as downward-pointing arrows. We explicitly highlight the difference between a low-z interloper and high-z EAZY solution with a ΔBIC statistic in each panel, as discussed in Section 3.3. In the inset panel we show the p(z) for both EAZY and BEAGLE fits with a free redshift solution. Finally, we display the probability of these candidates being at z > 14 as derived from multiplying EAZY and BEAGLE redshift distribution.
Paper: A Glimpse of the New Redshift Frontier through AS1063
Authors: Vasily Kokorev, Hakim Atek, John Chisholm, Ryan Endsley, Iryna Chemerynska, Julian B. Muñoz, Lukas J. Furtak, Richard Pan, Danielle Berg, Seiji Fujimoto, Pascal A. Oesch, Andrea Weibel, Angela Adamo, Jeremy Blaizot, Rychard Bouwens, Miroslava Dessauges-Zavadsky, Gourav Khullar, Damien Korber, Ilias Goovaerts, Michelle Jecmen, Ivo Labbé, Floriane Leclercq, Rui Marques-Chaves, Charlotte Mason, Kristen B. W. McQuinn, Rohan Naidu, Priyamvada Natarajan, Erica Nelson, Joki Rosdahl, Alberto Saldana-Lopez, Daniel Schaerer, Maxime Trebitsch, Marta Volonteri, Adi Zitrin
Figure caption: Observed abundance of bright galaxies at z > 16. We report the approximate magnitude limits for a number of deep extragalactic surveys corresponding to the 2σ depth of the dropout filter—F200W, which is required for the Lyman break identification. In varying shades of gray, we show CEERS (M. B. Bagley et al. 2023; S. L. Finkelstein et al. 2024) and PRIMER (both COSMOS and UDS; C. T. Donnan et al. 2023) combined, JADES (Origins Field; D. J. Eisenstein et al. 2023), and NGDEEP (G. C. K. Leung et al. 2023; M. B. Bagley et al. 2024). The dashed line is a scaled version of the halo mass function that assumes a 30% SFE of the gas, no dust, and a continuous SFH. The dashed line is simply a toy model to illustrate how the UVLF at these redshifts could steeply decline.
Paper: A Glimpse of the New Redshift Frontier through AS1063
Authors: Vasily Kokorev, Hakim Atek, John Chisholm, Ryan Endsley, Iryna Chemerynska, Julian B. Muñoz, Lukas J. Furtak, Richard Pan, Danielle Berg, Seiji Fujimoto, Pascal A. Oesch, Andrea Weibel, Angela Adamo, Jeremy Blaizot, Rychard Bouwens, Miroslava Dessauges-Zavadsky, Gourav Khullar, Damien Korber, Ilias Goovaerts, Michelle Jecmen, Ivo Labbé, Floriane Leclercq, Rui Marques-Chaves, Charlotte Mason, Kristen B. W. McQuinn, Rohan Naidu, Priyamvada Natarajan, Erica Nelson, Joki Rosdahl, Alberto Saldana-Lopez, Daniel Schaerer, Maxime Trebitsch, Marta Volonteri, Adi Zitrin
Figure caption: High-z color–color selection. Our final high-z sample, which we also present in Figure 3, is shown with red diamonds. The color–color Lyman break selection is indicated with a black dashed line. Solid lines show the tracks followed by starburst galaxies at z ∼ 16 (J. Chevallard & S. Charlot 2016) with varying levels of attenuation AV = 0–0.5 (shown with blue to green). We highlight low-redshift quiescent galaxies (M. Polletta et al. 2007), whose Balmer break could mimic the Lyman break at higher redshifts, as dashed lines. Extreme dusty starbursts (R. P. Naidu et al. 2022; P. Arrabal Haro et al. 2023; J. A. Zavala et al. 2023) at z ∼ 4.5–5.5 (orange squares) look quite similar to a high-z galaxy with this selection alone (see Section 3.3 for why these are disfavored). Finally, cool stars and brown dwarfs (G. Chabrier et al. 2000; F. Allard et al. 2001) are shown in purple.
Paper: A Glimpse of the New Redshift Frontier through AS1063
Authors: Vasily Kokorev, Hakim Atek, John Chisholm, Ryan Endsley, Iryna Chemerynska, Julian B. Muñoz, Lukas J. Furtak, Richard Pan, Danielle Berg, Seiji Fujimoto, Pascal A. Oesch, Andrea Weibel, Angela Adamo, Jeremy Blaizot, Rychard Bouwens, Miroslava Dessauges-Zavadsky, Gourav Khullar, Damien Korber, Ilias Goovaerts, Michelle Jecmen, Ivo Labbé, Floriane Leclercq, Rui Marques-Chaves, Charlotte Mason, Kristen B. W. McQuinn, Rohan Naidu, Priyamvada Natarajan, Erica Nelson, Joki Rosdahl, Alberto Saldana-Lopez, Daniel Schaerer, Maxime Trebitsch, Marta Volonteri, Adi Zitrin
Figure caption: The abundance of bright sources at cosmic dawn. We trace the possible evolutionary paths of our objects from z ∼ 16, while factoring in the redshift uncertainty, to some of the brightest spectroscopically confirmed high-z objects at z ≃ 11–14 (P. Arrabal Haro et al. 2023; A. J. Bunker et al. 2023; E. Curtis-Lake et al. 2023; S. Carniani et al. 2024b; M. Castellano et al. 2024). Shown are the tracks (with 1σ uncertainty represented by shaded regions) of constant star formation at ∼1 M⊙ yr−1 (purple) and a ΛCDM-limited maximal possible accretion scenario (pink line; A. Dekel & M. R. Krumholz 2013), where all gas is converted to stars. The overabundance of bright galaxies observed at high z so far is fully consistent with our observations. We only show the MUV uncertainties that are larger than the marker size.
Paper: A Glimpse of the New Redshift Frontier through AS1063
Authors: Vasily Kokorev, Hakim Atek, John Chisholm, Ryan Endsley, Iryna Chemerynska, Julian B. Muñoz, Lukas J. Furtak, Richard Pan, Danielle Berg, Seiji Fujimoto, Pascal A. Oesch, Andrea Weibel, Angela Adamo, Jeremy Blaizot, Rychard Bouwens, Miroslava Dessauges-Zavadsky, Gourav Khullar, Damien Korber, Ilias Goovaerts, Michelle Jecmen, Ivo Labbé, Floriane Leclercq, Rui Marques-Chaves, Charlotte Mason, Kristen B. W. McQuinn, Rohan Naidu, Priyamvada Natarajan, Erica Nelson, Joki Rosdahl, Alberto Saldana-Lopez, Daniel Schaerer, Maxime Trebitsch, Marta Volonteri, Adi Zitrin
Figure caption: GLIMPSE field overview. Positions of the high-z candidates are overlaid on top of the red, green, and blue image constructed from all available JWST broad bands. All of the high-z candidates are located in the full-coverage (six primary dithers) area of Module A (left). We additionally overlay a z = 16 critical curve in red.