adsabs/AstroCLIMB huggingface dataset:
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: Left: color composite image of J1044+0353 constructed from the DECalS g, r, and z images. The stretch is an inverse hyperbolic sine function. The yellow circle (SB) is the Sloan-like circular aperture with a radius of 1.″5 covering this galaxy’s SB region. The three red circles (FEN, MEN, and NEN) identify lower surface brightness stellar associations. The furthest is 4.″9 (1.4 kpc) east of the SB. The blue circle represents the background galaxy identified by C. L. Martin et al. (2023, in preparation). Right: the extracted spectrum of each stellar association.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: The positions of stellar associations lie in the EW space constructed by BEAGLE’s mock galaxy spectra. The composite SFH model ranges from 106 to 108.5 yr. For both panels (left: Hγ; right: Hδ), the EW of the emission portion is on the x-axis, and the EW of the absorption portion is on the y-axis. The marker for each stellar association is shown as a diamond (MEN), an inverted-triangle (NEN), a square (FEN), and a star (SB), respectively. For both panels, the absorption EWs of the SB region cannot be accurately measured due to its weak absorption troughs. Therefore, we assume the absorption EWs of the BEAGLE mock profile at the corresponding age (i.e., 106.48 yr) to be the upper limits for those of the SB region. The circular points are BEAGLE mock galaxies that are color coded by their ages. Within each panel, the upper right corner displays the representative error bars of the measured emission and absorption EWs for the mock galaxies.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: Fittings of the Balmer lines Hβ, Hγ, and Hδ for each stellar association labeled in Figure 1. For each stellar association, the best-fitting model (red dashed line) is plotted with the observed line profile (black solid line) in the first row. For double-Gaussian or GL fittings, the broad and narrow components are shown as the blue dashed line and the cyan dashed line, respectively. The gray areas represent the 1σ uncertainties of the raw data. The residual (i.e., (data – model)/error) plot is included in the second row. The two red dashed lines in the residual plot represent residual = ±1.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: The observed Hβ/Hγ line ratio map. Some regions surrounding the northern part of SB region exhibit unphysical extinction values when their observed ratios are compared to the intrinsic ratio for Case B (red contours) or Case A (white contours). These optically thin regions, corresponding to holes in the H I distribution, might reveal escape channels for ionizing photons.
Paper: Is It Possible to Measure the Lense–Thirring Orbital Shifts of the Short-period S Star S4716 Orbiting Sgr A*?
Authors: Lorenzo Iorio
Figure caption: LT shifts per orbit, in arcseconds per revolution (″ rev−1), of S4716 according to Equations (8)–(9) plotted as functions of i • and ε •. For ﹩{J}_{\bullet }={\chi }_{{\rm{g}}}\,{M}_{\bullet }^{2}\,G/c﹩, the values χ g = 0.5 and M • = 4.1 × 106 M ⊙ (Peißker et al. 2020, 2022) were adopted.
Paper: Discovery of the Elusive Carbonic Acid (HOCOOH) in Space
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres
Figure caption: Selected transitions of cis-trans HOCOOH identified toward the G+0.693 molecular cloud (listed in Table 1). The result of the best LTE fit is shown with a red solid line, while the blue line shows the expected molecular emission from all of the molecular species identified to date in our survey. The observed spectra are plotted as gray histograms. The structure of cis-trans HOCOOH is also depicted (carbon atoms in gray, oxygen atoms in red, and hydrogen atoms in white).
Paper: Discovery of the Elusive Carbonic Acid (HOCOOH) in Space
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres
Figure caption: Selected transitions of c-HCOOH identified toward the G+0.693 molecular cloud. The best LTE fit computed with MADCUBA is depicted as a red solid line, while the expected molecular emission from all of the molecular species identified in our spectral survey is shown in blue (observed spectra plotted as gray histograms).
Paper: Discovery of the Elusive Carbonic Acid (HOCOOH) in Space
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres
Figure caption: The LTE simulation of the cis-cis HOCOOH emission at the 3σ upper limit column density derived toward G+0.693 using the physical parameters shown in Table 2 (in red) together with the expected molecular emission from all of the molecular species identified to date in our survey (in blue), both overlaid on the observations (black line and gray histogram). The features depicted correspond to the 31,3–20,2 rotational transition. The structure of cis-cis HOCOOH is also shown.
Paper: Discovery of the Elusive Carbonic Acid (HOCOOH) in Space
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres
Figure caption: Selected transitions of CH3COOH identified toward the G+0.693 molecular cloud. The best LTE fit computed with MADCUBA-SLIM is depicted as a red solid line, and the predicted molecular emission from all of the molecules identified in our spectral survey is shown in blue (observed spectra plotted as gray histograms).
Paper: Discovery of the Elusive Carbonic Acid (HOCOOH) in Space
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres
Figure caption: Abundance ratio between formic and acetic acid toward different astronomical environments
Paper: Discovery of the Elusive Carbonic Acid (HOCOOH) in Space
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Sarah Massalkhi, Belén Tercero, Pablo de Vicente, Sergio Martín, David San Andrés, Miguel A. Requena-Torres
Figure caption: Rotational diagram of cis-trans HOCOOH using the unblended transitions (depicted by red dots) reported in Table 1. The gray dotted line corresponds to the best linear fit to the data points. The derived values for the molecular column density, N, and the excitation temperature, T ex, are shown in blue.
Paper: Constraining Cosmology with Machine Learning and Galaxy Clustering: The CAMELS-SAM Suite
Authors: Lucia A. Perez, Shy Genel, Francisco Villaescusa-Navarro, Rachel S. Somerville, Austen Gabrielpillai, Daniel Anglés-Alcázar, Benjamin D. Wandelt, L. Y. Aaron Yung
Figure caption: “All” clustering of z = 0 SAM galaxies with stellar mass greater than 1 × 109 M ⊙ and randomly downsampled to 0.005 h 3 cMpc−3, with SAM parameters allowed to vary (top) or held at fiducial values (bottom).
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Model atmospheric temperature profiles (left-hand side) and thermal emission spectra (right-hand side) for HD 86226 c assuming mixed volatile/rock-vapor compositions. In the top, middle, and lower panels, the volatile component consists of 80% H2O + 20% CO2, 100% H2O, and 67% O2 + 33% CO2, respectively. In each panel, lighter colors correspond to lower rock-vapor fractions and higher volatile fractions. Simulated JWST observations are shown for the most volatile-rich cases assuming five NIRSpec G395H eclipses and five MIRI LRS eclipses. Temperature profiles are shown up to the pressure corresponding to the base of the 0.2–50 μm photosphere. Key spectral features are labeled in gray.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Similar to Figure 5 but for 55 Cnc e. Simulated JWST observations are shown for the most volatile-rich cases assuming five NIRCam F444W eclipses and one MIRI LRS eclipse. The light gray diamond and error bars show the existing Spitzer observation using the latest reanalysis from Mercier et al. (2022). Key spectral features are labeled in gray.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Retrieved thermal emission spectra for the simulated JWST observations shown in Figures 5, 6, and 7 for HD 86226 c (top row), HD 3167 b (middle row), and 55 Cnc e (bottom row), respectively. The simulated observations correspond to an atmospheric composition with 1% rock vapor and 99% volatiles, where the volatile composition is either 80% H2O + 20% CO2 (left-hand column), 100% H2O (middle column) or 67% O2 + 33% CO2 (right-hand column). Purple points and error bars show the simulated observations, while solid-blue lines show the ‘true’ underlying model. The medium retrieved spectra and 1σ/2σ contours are shown as orange lines and dark/light orange shading, respectively. Note that the bottom row spans a different wavelength range to the top two rows.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Absorption cross sections weighted by volume mixing ratio. Panels, from left to right, show the dominant opacity sources for three atmospheric compositions, which have elemental abundances corresponding to: 100% rock vapor (left panels), 50% rock vapor + 40% H2O + 10% CO2 (middle panels), and 1% rock vapor + 79% H2O + 10% CO2 (right panels). Top and bottom rows show weighted cross sections corresponding to a temperature of 2500 K and 3000 K, respectively, and a pressure of 1 mbar.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Same as Figure 5 but for HD 3167 b. Simulated JWST observations are shown for the most volatile-rich cases assuming five NIRSpec G395H eclipses and five MIRI LRS eclipses.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Retrieved atmospheric temperature profiles for HD 86226 c (top row), HD 3167 b (middle row), and 55 Cnc e (bottom row), respectively, given the simulated JWST observations shown in Figures 5, 6, and 7. The simulated observations correspond to an atmospheric composition with 1% rock vapor and 99% volatiles, where the volatile composition is either 80% H2O + 20% CO2 (left-hand column), 100% H2O (middle column) or 67% O2 + 33% CO2 (right-hand column). Solid purple lines show the ‘true’ model temperature profile. The medium retrieved temperature profiles and 1σ and 2σ contours are shown as orange lines and dark/light orange shading, respectively.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Planetary radius relative to the radius expected for an Earth-like interior composition, as a function of the ESM. The color scale shows the substellar temperature for each planet. Larger points with error bars show planets with a substellar temperature >1700 K, which are therefore hot enough for the dayside to be partially molten. Smaller points denote planets with substellar temperatures cooler than 1700 K. The case studies explored in this work (HD 86226 c, HD 3167 b and 55 Cnc e), other lava worlds with ESM > 5 (pi Men c, TOI-500 b, TOI-561 b), and planets scheduled for JWST Cycle 1 observations (GJ 367 b, K2-141 b and 55 Cnc e) are labeled and outlined with bold black circles.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: A schematic of the model framework used. We consider mixed atmospheric compositions consisting of volatiles and rock vapor. The atmospheric temperature profile and thermal emission spectrum of the planetary dayside are then calculated under the assumptions of radiative-convective, thermochemical, and hydrostatic equilibrium. We simulate JWST observations corresponding to the model thermal emission spectrum and perform atmospheric retrievals to quantify the observability of key chemical species.
Paper: Rocky Planet or Water World? Observability of Low-density Lava World Atmospheres
Authors: Anjali A. A. Piette, Peter Gao, Kara Brugman, Anat Shahar, Tim Lichtenberg, Francesca Miozzi, Peter Driscoll
Figure caption: Equilibrium chemical abundances as a function of pressure corresponding to isothermal temperature profiles of 2000 K (top panel) and 3000 K (bottom panel). The elemental abundances correspond to a 1% rock-vapor fraction (99% volatiles) and a volatile composition consisting of 80% H2O + 20% CO2, as described in Section 2.1.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Locations of strong lens candidates from this work (red) and previous searches (black) collected in the Master Lens Database (Moustakas et al. 2012) augmented by the results from recent searches using DECaLS (Huang et al. 2020, 2021; Dawes et al. 2022; Storfer et al. 2022), the extended Baryon Oscillation Spectroscopic Survey (eBOSS; Talbot et al. 2021), and HSC (Sonnenfeld et al. 2018, 2020; Chan et al. 2020; Jaelani et al. 2020, 2021; Cañameras et al. 2021; Shu et al. 2022; Wong et al. 2022). Lens candidates are overplotted on the DELVE DR1 griz footprint (blue). The DELVE DR2 griz footprint (turquoise) is shown for reference, but the search was conducted only on the DR1 data set. The DES footprint is outlined with solid blue lines (DES Collaboration et al. 2021), while the DECaLS region is outlined with solid green lines (Dey et al. 2019). The Galactic plane (b = 0°) is shown as a solid black curve, while the two dashed black curves show b = ±10°. The sky map is shown using an equal-area Thomas–McBryde flat polar quartic projection in celestial equatorial coordinates.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Training data examples. Left: negative examples were taken from a random collection of galaxies in DELVE DR1. Right: the same random collection of galaxies with simulated strong lens images generated by deeplenstronomy. Cutouts are approximately 11.″8 × 11.″8.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Output scores of our CNN classifier applied to Grade A, B, and C lens candidates identified in Huang et al. (2020, 2021). We indicate candidates that pass our color–magnitude preselection (Section 2) in blue and those that fail our selection in purple. The red dashed line indicates the CNN cutoff score that was used to select our candidate list.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Distributions of stellar mass and photometric redshift for both the target data set in this work and the full sample of galaxies in DECaLS DR9, based on the Zou et al. (2022) catalog. Galaxies in our target data set are generally more massive and lie at lower redshift relative to the full distribution of galaxies in DECaLS DR9.