adsabs/AstroCLIMB huggingface dataset:
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: The left panel shows an F150W − F356W vs. F356W color–magnitude diagram. The overall population of galaxies in the CEERS sample is shown in a gray-scale density map (cut to F356W < 28 mag). The markers show the color-selected, F150W − F356W > 1.5 mag (horizontal dashed gray line) sample divided into HST-faint (light circles) and HST-dark (dark hexagons) galaxies with magnitudes brighter and fainter than F150W = 26 mag, respectively. Diagonal dashed gray lines at 26, 28, 30, and 32 mag are shown. Nearly 70% of the HST-dark galaxies are undetected in previous HST/WFC3-based surveys (∼90% of those with F150W > 27 mag). Cyan circles and blue stars indicate galaxies within our sample detected in the far-IR and radio/submillimeter wavelengths, and green circles show the sample of HST-dark galaxies from Alcalde Pampliega et al. (2019). The middle panel shows the same plot with colored lines presenting the redshift dependence (marked with vertical lines) in color and magnitude for six different galaxy types with stellar masses ﹩\mathrm{log}{M}_{\star }/{M}_{\odot }=11﹩ and 10, thin and thick lines, respectively. The typical SEDs and rest-frame UVJ colors of each type are indicated in the bottom and top panels on the right. The templates correspond to star-forming galaxies with low (blue tones) and high (magenta/purple) levels of obscuration, a quiescent galaxy template (red), and an extreme starburst spectrum with high equivalent width lines (black).
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Example of a two-dimensional photometric redshift determination for one of our extended sources (identified as two galaxies at different redshifts; see text for more details). The upper-left panel shows an RGB 8″ × 8″ postage stamp of nircam2-7122, using NIRCam filters F115W, F150W, and F200W. The top-right thumbnails show individual images of the source in all HST/ACS and JWST/NIRCam filters used in this work. The images have been PSF-matched to the F444W image. The red ellipse marks the aperture used for the integrated photometric measurements, and the blue ellipse depicts the aperture containing half of the total flux in F356W. On the bottom left, we show the histogram of the most probable photometric redshifts for all pixels with enough S/N (see text for details) within the integrated aperture. The combined redshift probability distribution function (zPDF) for all these pixels is shown in red, while the most probable redshift and its uncertainty for this source are marked and written in red. The inset shows the photometric redshift map. On the bottom right, we show the SEDs of two circular apertures positioned on the central region of the source and the northern part, respectively (see circular regions marked in the RGB image insets). In red, we show the sum of all photometric redshift templates fitting the corresponding pixels (offset to the average redshift of the region for clarity). The bottom-right insets in these SED plots show the individual probability distribution functions for all pixels within the aperture, plotted with a transparency parameter.
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Rest-frame U − V vs. V − J diagram at different redshifts for the galaxies in the CEERS sample (color gray-scale) and the color-selected sample divided into HST-faint and -dark (light and dark colors). MIPS24 emitters are marked with a cyan circle, submillimeter and radio galaxies with a blue star, quiescent galaxies by sSFR with a red square, and XELG-z6 with green triangles. The green circles show quiescent galaxies at z > 3 from Carnall et al. (2023). HST-dark galaxies make up the bulk of the sample at z > 4 while HST-faint ones dominate in number at 〈z〉 = 2.5, and there is an even split between them at 〈z〉 = 3.5. The average color, extinction, and stellar mass are indicated in the top-left corner of each plot. Overall color-selected galaxies are predominantly massive, dusty, or quiescent galaxies in agreement with the goal of the selection criteria in Figure 1. Furthermore, there is a clear downward trend in extinction and stellar mass ranging from 〈A  V 〉 ∼ 2.2 mag and ﹩\langle \mathrm{log}{M}_{\star }/{M}_{\odot }\rangle \sim 10.5﹩ at z < 3 to 〈A  V 〉 ∼ 1.2 mag and ﹩\langle \mathrm{log}{M}_{\star }/{M}_{\odot }\rangle =10﹩ at z > 4. The cutouts on the bottom show the 5″ × 5″ images of the MIPS and submillimeter/radio galaxies marked with letters in the UVJ diagram, also providing IDs and redshifts. From bottom to top, the images are color composites of three HST bands and three JWST bands, short and long wavelengths, respectively.
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Main-sequence (SFR vs. stellar-mass, SFMS) plots for our sample of galaxies with red near-to-mid-IR colors, compared to the CANDELS sample. From left to right, each panel shows the SFMS in different redshift bins, selected to exemplify the range dominated by HST-faint galaxies (F150W < 26 mag), 2 < z < 3; HST-dark sources (F150W > 26 mag), 4 < z < 7; and a transition range. In each panel, our sample is shown with hexagons (HST-dark) and circles (HST-faint). MIPS24 emitters are marked with a cyan circle, submillimeter and radio galaxies with a blue star, quiescent galaxies with a red square, and XELG-z6 with green triangles. The hexmap shows the distribution of galaxies in the CANDELS catalog (Stefanon et al. 2017), with SFRs estimated with the method explained in Barro et al. (2019). The colored lines depict the SFMS at z = 2–7 from Schreiber et al. (2015), Santini et al. (2017), and Barro et al. (2019). The cutouts on the bottom show the 5″ × 5″ images of the quiescent galaxies marked with letters in the SFMS, also providing IDs and redshifts. From bottom to top, the images are color composites of three HST bands and three JWST bands, short and long wavelengths, respectively.
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Results of our pixel-by-pixel SED-modeling procedure for the example source presented in Figure 2. In this figure, we just keep the southern component of the source, which we identify as a distinct galaxy that meets our selection criteria and lies at a different redshift than the northern region of the source. The top four panels show maps of the stellar-mass surface density, the mass-weighted age, the SFR averaged over the last 25 Myr of the SFH of the galaxy, and the dust attenuation in the V band. The centroid of the galaxy calculated with the stellar-mass map is marked with a gray star. The striped circle depicts the FWHM of the data. On the bottom left, we show the integrated SFH and its uncertainty obtained by adding the results for all pixels, after applying an aperture correction based on the average flux ratio between the sum of all pixels used in the 2D analysis and the integrated aperture. On the bottom-center panel, we show a UVJ diagram for all pixels used in our analysis, color-coded by distance to the galaxy centroid. Average uncertainties in both axis as a function of radius are plotted in the top-left (uncertainties in V − J) and bottom-right (in U − V) corners of the panel. The position of the integrated colors of the galaxy is marked with a black circle. On the bottom-right panel, we show color maps using the closest observed filters to the UVJ rest-frame colors considering the redshift of the galaxy (z = 3.7), namely F150W − F277W for U − V and F277W − 1.5 × F444W for V − J (the multiplicative factor being applied to account for the extrapolation to probe the J band).
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Star formation main-sequence plot for our sample of mid-IR-bright, near-IR-faint galaxies constructed with SFRs derived from our 2D stellar population synthesis analysis through the calculation of the dust-absorbed stellar emission. The energy extincted by dust in the UV/optical is assumed to be reemitted in the mid- to far-IR, from 8 to 1000 μm. The luminosity in this wavelength range is then converted to SFR using the Kennicutt (1998) factor. Symbols in gray show the SFRs obtained from the average of the integrated SFHs in the last 20 Myr. Blue curves depict literature main-sequence relationships (same as in Figure 5).
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: The left panel shows the stellar-mass vs. photometric redshift diagram for all the galaxies in the CANDELS catalog (gray-scale density map) and the color–magnitude-selected sample divided into HST-dark (dark hexagons) and HST-faint (light circles). MIPS24 emitters are marked with a cyan circle, submillimeter and radio galaxies with a blue star. The central and right panels show the photometric redshift and stellar-mass distributions for the HST-dark and HST-faint galaxies (with the same color scheme) and the whole sample (gray histogram). Some statistical information (median and quartiles) for the HST-faint and HST-dark subsamples are provided.
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Left: average and scatter of the SFHs (in terms of the age of the universe and corresponding redshift) for all the galaxies in our sample (black), quiescent galaxies (red), and star-forming galaxies (blue). The latter types have been divided into two subsamples based on their redshifts, roughly with an equal number of sources in each subgroup. We also depict the SFH for the XELGs-z6 type (green). Right: gray lines show the evolution of the specific SFRs of our galaxies according to the 2D-based SFHs. The black-border symbols show the positions of our galaxies at the epoch of observation, hexagons for HST-dark and circles for HST-faint galaxies. Quiescent galaxies in our sample are marked with red squares, dusty star-forming galaxies detected by MIPS and (sub)millimeter surveys with cyan circles and blue stars, respectively, and XELG-z6 sources with a green triangle. The black thick line corresponds to inverse specific SFRs (i.e., doubling times) equal to the age of the universe. The average tracks for types of galaxies shown in the left panel are also shown. Comparison samples are depicted in color, using literature estimations of the redshift, stellar mass, and SFR. Yellow points correspond to the CANDELS catalog. Purple pointing-down triangles depict ALMA-detected galaxies (Scoville et al. 2016; Bowler et al. 2018; Tadaki et al. 2020; Burgarella et al. 2022; Schouws et al. 2022). Orange crosses show near-IR-faint, mid-IR-bright sources (i.e., red galaxies) discovered in the Spitzer/HST era (Huang et al. 2011; Wang et al. 2016; Alcalde Pampliega et al. 2019). Magenta diamonds depict the high-z red (and tentatively massive) galaxies discovered by JWST in comparison with HST data (Barrufet et al. 2022; Carnall et al. 2023; Labbe et al. 2022; Nelson et al. 2022). Pink stars correspond to z > 9 JWST-selected galaxies (Atek et al. 2022; Finkelstein et al. 2022; Naidu et al. 2022; Rodighiero et al. 2023; Santini et al. 2023).
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Left: gray lines show the evolution of the stellar mass of our galaxies according to the 2D-based SFHs. The black-border symbols show the positions of our galaxies at the epoch of observation, hexagons for HST-dark and circles for HST-faint galaxies. Quiescent galaxies in our sample are marked with a red square, dusty star-forming galaxies detected by MIPS and (sub)millimeter surveys with cyan circles and blue stars, respectively, and XELG-z6 sources with a green triangle. The average tracks for quiescent galaxies, dusty starburst (both types divided by redshift, with lower/higher redshifts depicted with dashed/continuous lines), and XELG-z6 are also shown. Comparison samples are also depicted, using literature estimations of the redshift and the stellar mass, and with the same colors mentioned in Figure 9. On the top-right panel, we show the distribution of redshifts where our galaxies have formed 1, 5, and 25% of their observed stellar mass. In the bottom-right panel, we show the histograms of redshifts where our galaxies have already formed 108, 109, and 1010 M ⊙ in stellar mass.
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Radial distribution of the main stellar population properties for our sample of HST-faint and HST-dark galaxies, divided into four samples: quiescent galaxies (QGs, red), star-forming galaxies at z < 4 and z > 4 (in cyan and blue), and XELG-z6 sources (green). From top to bottom, we show attenuations in the V band, mass-weighted ages, redshift at which each pixel formed 5% of its current stellar mass, and stellar-mass surface density. In the left column, we plot these properties as a function of absolute galactocentric distances in kiloparsec. In the middle-column panels, we normalize the distances using the effective radius calculated in the stellar-mass maps. In the right column, we show histograms of all properties, jointly with median and quartiles.
Paper: Coplanar Circumbinary Planets Can Be Unstable to Large Tilt Oscillations in the Presence of an Inner Polar Planet
Authors: Anna C. Childs, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Aaron M. Geller
Figure caption: Critical radii as a function of a p1 (top left), m p1 (top right), e b (lower left), and m 2/m 1 (lower right). The default parameters from our numerical solutions are used for all other parameters besides the parameter we vary in each panel. The red and blue lines mark r c1 and r c2 (Equations (9) and (10), respectively). The gray shaded region between these two curves denotes where an initially coplanar outer planet is librating with an inner polar planet. The points show our numerical results.
Paper: Coplanar Circumbinary Planets Can Be Unstable to Large Tilt Oscillations in the Presence of an Inner Polar Planet
Authors: Anna C. Childs, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Aaron M. Geller
Figure caption: Contour plot of the maximum inclination of the outer planet as a function of the outer planet semimajor axis and the initial inclination of the inner Jupiter-mass planet. The outer planet has an initial inclination of 0°.