adsabs/AstroCLIMB huggingface dataset:
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Evolution of the cosmic stellar mass density, ρ *, in galaxies from 4 < z < 10. The lines show pre-JWST constraints from Finkelstein (2016) and Madau & Dickinson (2014). The data points show recent measurements of ρ * at z > 6 from the literature (Kikuchihara et al. 2020 [Ki20], Bhatawdekar & Conselice 2021 [Bh21], Stefanon et al. 2021 [St21], and Santini et al. 2022 [Sa22]), which largely follow the pre-JWST constraints. The shaded regions show maximally allowable stellar mass density assuming galaxies experience a burst at z = 100 followed by “normal” star formation. Constraints lacking JWST/MIRI coverage to rest-frame 1 μm allow for a stellar mass density that is up to 0.8 dex higher at z = 4 and 1.4 dex higher at z = 10. Including MIRI 5.6 and 7.7 μm data lowers the maximum allowed by up to a factor of 5.
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Comparison of the median and relative SED for each galaxy, both for the case that MIRI data are used (top panel) and when the MIRI data are excluded (middle panel). The individual lines are the median SED model fit to each galaxy in the sample, shifted to the rest-frame. The large data points show the median rest-frame magnitude at 1600 Å, 2800 Å, and U, B, V, and I. The error bars show the scatter in the sample. All models have been normalized to the 1600 Å magnitude (which accounts for the lack of scatter at that wavelength). The bottom panel shows the difference in color (Δm) between the models with and without the MIRI data. The error bars show the range of the 16th–84th percentiles of the sample. The change in the color at the reddest wavelengths probed (about the rest-frame I-band) corresponds to a Δm ≈ 0.4 mag.
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Comparison of stellar masses derived for galaxies with and without early bursts (at z  f  = 100). The top row shows the results that lack MIRI data. The top left panel shows the stellar masses derived from the delay-τ models only (labeled “no burst”) compared to the models that include the burst (labeled “allowed in burst”). The top right panel shows the difference between the stellar masses as a function of redshift. The bottom row shows the same results for the galaxies including the MIRI data. In the left panels, the dashed lines show the one-to-one relation and the solid lines show the median offsets. In the right panels, the large rectangles show the medians in the two bins of redshift (4 < z < 6 and 6 < z < 9) these are given in Table 7. Adding the MIRI data reduces the amount of stellar mass allowed in the burst components.
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Testing the impact of sources with “crowded” IRAC photometry. The plots in this figure are similar to those in Figure 6, and they compare the stellar masses and SFRs derived from the SED modeling for galaxies including the MIRI F560W and F770W data and without the MIRI data. In both panels, the results show the difference between the mass (SFR) derived without MIRI data and the mass (SFR) derived including the MIRI data. In this figure, we have excluded objects that have a neighbor with r ≤ 3″ and MIRI [5.6] ≤ 26.7 mag. This eliminates 11 objects and allows us to test if crowding in the IRAC data (which has lower angular resolution) impacts object photometry in the IRAC bands. We do not observe any significant offset compared to the results in Figure 6: the median offsets in stellar mass and SFR change by ≈0.1 dex. Therefore, we conclude that blended IRAC photometry does not significantly impact the results here.
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Comparison of the redshifts for galaxies in our sample with and without the MIRI data. The data points show the relative difference between the photometric redshifts (derived from our BAGPIPES fits) for the galaxies excluding MIRI (z no MIRI) and when including MIRI (z MIRI) as a function of the prior photometric redshift from Finkelstein et al. (2022a). Annotated points indicate objects with ﹩\left|{z}_{\mathrm{no}\ \mathrm{MIRI}}-{z}_{\mathrm{MIRI}}\right|\gt 0.2﹩. These objects indicate shifts in their photometric redshift, where this is at least in part because of nebular emission in one or more bands.
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Comparison of redshift posterior probability densities, P(z), derived from the BAGPIPES fits to three of the galaxies in the sample (as labeled). These three galaxies each have a change of more than 0.2 between the respective median redshifts when including the MIRI F560W and F770W data in the fit vs. when they are excluded. For the case of galaxy IDs 35896 and 7818, the IRAC−MIRI colors are blue, indicating redshifted emission lines (likely Hα+[O III] and Hα) inhabit both IRAC bands while the MIRI data probe the galaxy continua. In the case of galaxy ID 12514, the MIRI F560W band clearly shows boosted emission, likely from redshifted Hα at z = 7.6–8.
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Illustration of galaxy spectra (in relative units of erg s−1 cm−2 Å−1) compared to the broadband data for the observations in this work. The bottom panel shows the relative transmission functions for the HST/ACS and WFC3 filters (ACS F606W and F814, and WFC3 F125W and F160W), Spitzer/IRAC 3.6 μm (Ch1) and 4.5 μm (Ch2), and JWST/MIRI F560W and F770W. The top panel shows model spectra of star-forming galaxies at z = 5.1 and z = 8.7, which match two galaxies with spectroscopic redshifts in this sample. Key emission lines and features are labeled. The MIRI data probe the shape of the galaxy spectral energy distributions to the 8000 Å rest frame, even for galaxies with z = 9.
Paper: Negligible Effects of Baryons on the Angular Momentum Scaling Relations of Galactic Dark Matter Halos
Authors: S. Michael Fall, Vicente Rodriguez-Gomez
Figure caption: Specific angular momentum j h plotted against mass M h for halos in the TNG100 DMO and FP runs (left and right panels, respectively) at redshifts z = 0 and z = 2 (upper and lower panels, respectively). The color scale indicates the number of halos in each 2D bin. The red lines represent the best-fit linear relations, while the black lines represent the running median relations and 16th–84th percentile ranges. Note the close similarity of the halo j–M relations in the DMO and FP runs and the slightly flatter slopes at z = 2 than at z = 0.
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption: (a) Unfiltered continuum MeerKAT image of the Sgr E H II complex G358.7-0.0 at 20 cm showing a cluster of discrete H II regions surrounding a dark cavity coincident with the Sgr E molecular cloud (Heywood et al. 2022). The outline of 13CO (2-1) line emission from the Sgr E cloud is shown as white contour (Anderson et al. 2020). The range of gray scale is [-5e-4, 7e-4] Jy beam−1. (b) Similar to (a) except filtered continuum image is displayed (Yusef-Zadeh et al. 2022a). The range of gray scale is [-2e-5, 7e-5] Jy beam−1. (c) Same as (b) except that identified filaments are drawn in red. The range of gray scale is [-2e-5, 7e-5] Jy beam−1. (d) A histogram of filament PAs in Sgr E shows that most filaments PA are distributed within ∼40°. Red line shows a Gaussian fit to the histogram of the Galactic plane.
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption: (a) The clump of points near GPA = 270° with GPA ﹩\mathrm{GPA}={{\tan }}^{-1}l/b)\lt 270^\circ ﹩ identify shorter-filament PAs that are mostly below the radial trend (orange line). Those with GPA >270° (fourth quadrant) have PAs that are generally above the radial trend with steeper values, suggesting that they are close to the Galactic plane. On the other hand, at GPA <270° (third quadrant) filament PAs are generally flatter, running away from the Galactic plane. (b) The same as (a) except for long filaments. (c) A diagram showing the PAs of short filaments within a cone pointed toward the direction of Sgr A*.
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption: A schematic diagram of a jet-driven outflow with an opening angle 2θ along the Galactic plane.
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption: Top panel: the PAs of filaments with L > 66″, represented by a point, is shown as a function of Galactic longitude. A clustering of PAs slightly greater and slightly less than 0° are located near Galactic longitudes l ∼ 0.°2 and ∼ − 0.°3, respectively. Bottom panel: similar to top except that the filament PAs are restricted to L < 66″. Excluded regions shown in Figure 1 are applied before top and bottom panels were constructed.
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption: Top panel: similar to Figure 3 top panel, except for short filaments (L < 66″). Bottom panel: similar to Figure 3 bottom panel, except for short filaments (L < 66″).
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption:  Top panel: a histogram of the PA distribution of filaments with lengths L > 66″. Galactic north has PA = 0°. Bottom panel: similar to top except for the spectral index distribution. Known SNRs and H II regions have been masked.
Paper: True Polar Wander of Lava Worlds
Authors: Wanying Kang, Francis Nimmo, Feng Ding
Figure caption: Panel (a) shows the air temperature T  a  (red, left), pressure P  a  (black, left), velocity V  a  (blue, left), surface temperature (red dashed, left), mass transport flux Φ (green, right), condensation D (cyan, right) and surface mass flux F (magenta, right) for an example case, where T  s0 = 3000 K, M  p  = 0.02 M  e  and M ⋆ = 10 M Sun. Other stellar parameters can be derived from T  s0 and M ⋆ following formula given in Table 1. Panel (b) shows the mass load profile. Mass deposited to the planetary surface by atmospheric flow out of the magma ocean can be sustained by the lithosphere, as shown by solid curves. Within the magma ocean edge (T  s  > T  f  = 1600 K), the total mass-loss rate per area is assumed to be evenly distributed, as shown by the vertical locations of the solid dots. The horizontal locations are set to the magma ocean edge minus 10°. Panel (c) compares the measured e-folding scale of the mass load out of the magma ocean l  L  against the theoretical prediction π RT  s0/g. For panels (b) and (c), color indicates the temperature at the substellar point of the planet and line width, symbol size reflects the size of the planet; stellar mass M ⋆ is set to 10 M Sun.
Paper: True Polar Wander of Lava Worlds
Authors: Wanying Kang, Francis Nimmo, Feng Ding
Figure caption: (a) shows the equilibrium height of the load (assuming M ⋆ = 10 × solar mass, other solar masses yield similar results). (b)–(d) show the nondimensional load size Q as a function of insolation level (measured by the substellar point temperature T  s0) and planetary mass M  p , for M ⋆ = 1, 3, and 10 M Sun, respectively. Red contours denote positive Q  L  and black contours denote negative Q  L . The black shading in (b)–(d) marks the parameter combinations where the timescale for a specific planet to get tidally locked τ lock is greater than 10% of the lifespan of the star τ star. The colorful shading overlaid shows atmospheric escape rate obtained from the analytical model in Kang et al. (2021). Red color corresponds to escape rate beyond 1012 kg s−1 and blue color corresponds to escape rate below 102 kg s−1. With an escape rate of 107 kg s−1, it will take 0.2 Gyr to completely vaporize a planet of 0.01 M  e . In panels (b)–(d), areas encompassed by the bold 0-contour are likely to undergo TPW.
Paper: True Polar Wander of Lava Worlds
Authors: Wanying Kang, Francis Nimmo, Feng Ding
Figure caption: Radiative equilibrium surface temperature profiles assuming various substellar temperatures and stellar masses.
Paper: True Polar Wander of Lava Worlds
Authors: Wanying Kang, Francis Nimmo, Feng Ding
Figure caption: Geometry from the point of view of an observer at the surface of the planet. The side view demonstrates the geometric relationship between the planet (gray) and the star (orange). The bird’s-eye view demonstrates the shadow (red shading) cast by stellar disk (orange shading) on the horizon plane (gray shading). The red circle is the projected stellar disk, with key intersections marked in the same color as the side-view schematics. Orange circle is the unprojected stellar disk (orange shading in side view) overlaid rotated to the horizontal plane. See the main text for more details.
Paper: An Extremely Compact, Low-mass Galaxy on its Way to Quiescence at z = 5.2
Authors: Victoria Strait, Gabriel Brammer, Adam Muzzin, Guillaume Desprez, Yoshihisa Asada, Roberto Abraham, Maruša Bradač, Kartheik G. Iyer, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris Willott, Katriona Gould, Tess Grindlay, Jasleen Matharu, Gregor Rihtaršič
Figure caption: Photometrically calibrated observed spectrum (dark gray) with 1σ noise (light gray shaded areas) and posterior spectrum from BAGPIPES (blue) for MACS0417-z5BBG. Top panel shows f  λ ; bottom panel shows f  ν . Emission lines are labeled in green. Inset is a zoomed-in version of the spectrum surrounding the detection of Hα. Note that although BAGPIPES fits an [S II] line, we do not detect it in our spectrum.
Paper: An Extremely Compact, Low-mass Galaxy on its Way to Quiescence at z = 5.2
Authors: Victoria Strait, Gabriel Brammer, Adam Muzzin, Guillaume Desprez, Yoshihisa Asada, Roberto Abraham, Maruša Bradač, Kartheik G. Iyer, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris Willott, Katriona Gould, Tess Grindlay, Jasleen Matharu, Gregor Rihtaršič
Figure caption: JWST/NIRCam images of MACS0417-z5BBG and nearby system from Asada et al. (2023). From left to right: F090W, F200W, F444W, and RGB (red: F356W+F410M+F444W; green: F200W+F277W+F356W; blue: F090W+F115W+F150W) image of MACS0417-z5BBG. All images have 40 mas pixels and are non-PSF-homogenized. Field of view (FOV) is 2″ × 2″. NIRSpec slit configuration is shown in the F444W image. Approximate critical curve, as well as the multiple images of MACS0417-z5BBG (labeled M9.1 and M9.2) and galaxies from Asada et al. (2023) are shown in the RGB image.
Paper: An Extremely Compact, Low-mass Galaxy on its Way to Quiescence at z = 5.2
Authors: Victoria Strait, Gabriel Brammer, Adam Muzzin, Guillaume Desprez, Yoshihisa Asada, Roberto Abraham, Maruša Bradač, Kartheik G. Iyer, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris Willott, Katriona Gould, Tess Grindlay, Jasleen Matharu, Gregor Rihtaršič
Figure caption: Star formation history posteriors from BAGPIPES. Median star formation history is the solid blue line; all other possibilities are gray. Inset is a zoomed-in version of the same plot, <20 Myr before observation. MACS0417-z5BBG peaked in star formation ∼10–30 Myr ago, and the SFR has declined precipitously since then. Median magnification factor of 43 is assumed. 85% of the solutions are found within the less peaky solution.
Paper: An Extremely Compact, Low-mass Galaxy on its Way to Quiescence at z = 5.2
Authors: Victoria Strait, Gabriel Brammer, Adam Muzzin, Guillaume Desprez, Yoshihisa Asada, Roberto Abraham, Maruša Bradač, Kartheik G. Iyer, Nicholas Martis, Lamiya Mowla, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris Willott, Katriona Gould, Tess Grindlay, Jasleen Matharu, Gregor Rihtaršič
Figure caption: Top row: one observed multiple image of MACS0417-z5BBG, M9.2, followed by the model and normalized residuals from Lenstruction. The hexagonal structure in the images comes from the JWST PSF. Bottom row: the same, for the second image, M9.1. Right: modeled source-plane image.