adsabs/AstroCLIMB huggingface dataset:
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: Page 2 of grade C candidates identified in this work. Previously discovered lens candidates are outlined in red. 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: Page 1 of grade C candidates identified in this work. Previously discovered lens candidates are outlined in red. 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: Page 3 of grade C candidates identified in this work. Previously discovered lens candidates are outlined in red. 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: Grade B candidates identified in this work. Previously discovered lens candidates are outlined in red. 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: Grade A candidates identified in this work. Previously discovered lens candidates are outlined in red. Cutouts are approximately 11.″8 × 11.″8.
Paper: Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia
Authors: Leon Ofman, Scott A. Boardsen, Lan K. Jian, Parisa Mostafavi, Jaye L. Verniero, Roberto Livi, Michael McManus, Ali Rahmati, Davin Larson, Michael L. Stevens
Figure caption: The temporal evolution for Case 1 with the initial parameters of E11 at 2022 February 25 21:50:50 UT with A  p  = 4.3, A  α  = 1.6, n  α /n  p  = 0.007, and V  d  = 0.3V A of (a) the α particle temperature anisotropy, (b) the proton temperature anisotropy, (c) the α particle perpendicular kinetic energy W ⊥,i  (red) and parallel kinetic energy W ∥,i  (blue), (d) the proton perpendicular kinetic energy W ⊥,p  (red) and parallel kinetic energy W ∥,p  (blue), and (e) the drift velocity V  d .
Paper: Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia
Authors: Leon Ofman, Scott A. Boardsen, Lan K. Jian, Parisa Mostafavi, Jaye L. Verniero, Roberto Livi, Michael McManus, Ali Rahmati, Davin Larson, Michael L. Stevens
Figure caption: The temporal evolution of the proton VDF for Case 3 with the initial parameters of E10 at 2021 November 22 02:42:10 UT with A  p  = 0.19, A  α  = 0.85, n  α /n  p  = 0.013, and V  d  = 0.62V A. (a) The temporal evolution of the α particle temperature anisotropy (note the small range of the y-axis). (b) The temporal evolution of the proton temperature anisotropy (note the small range of the y-axis). (c) The proton VDF in the V  x –V  z  plane at ﹩t=600{{\rm{\Omega }}}_{p}^{-1}﹩ (top), and the cut along V  x  through the peak of the proton VDF (lower panel). (d) The α particle VDF in the V  x –V  z  plane at ﹩t=600{{\rm{\Omega }}}_{p}^{-1}﹩ (top), and the cut along V  x  through the peak of the α particle VDF (lower panel).
Paper: Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia
Authors: Leon Ofman, Scott A. Boardsen, Lan K. Jian, Parisa Mostafavi, Jaye L. Verniero, Roberto Livi, Michael McManus, Ali Rahmati, Davin Larson, Michael L. Stevens
Figure caption: The dispersion relations obtained from the 2.5D hybrid modeling results. (a) Case 1, with the initial parameters of E11 at 2022 February 25 21:50:50 UT, with A  p  = 4.3, A  α  = 1.6, n  α /n  p  = 0.007, and V  d  = 0.3V A. The LH resonant proton and α as well as the nonresonant RH polarized dispersion branches are marked with arrows and labeled. (b) Case 2, on 2022 February 25 at 18:56:38, with the initial parameters A  p  = 3.4 and A  α  = 2.0. The power is shown on a log10 intensity scale, indicating that the dominant power is in the proton resonant branches. (c) The modeled total perpendicular magnetic energy for Case 1 (solid) and Case 2 (dashes).
Paper: Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia
Authors: Leon Ofman, Scott A. Boardsen, Lan K. Jian, Parisa Mostafavi, Jaye L. Verniero, Roberto Livi, Michael McManus, Ali Rahmati, Davin Larson, Michael L. Stevens
Figure caption: The temporal evolution for Case 2 with the initial parameters of E11 at 2022 February 25 18:56:38 UT with initial A  p  = 3.3, A  α  = 2, n  α /n  p  = 0.007, and V  d  = 0.42V A of (a) the α particle temperature anisotropy, (b) the proton temperature anisotropy, (c) the α particle perpendicular kinetic energy W ⊥,i  (red) and parallel kinetic energy W ∥,i  (blue), (d) the proton perpendicular kinetic energy W ⊥,p  (red) and parallel kinetic energy W ∥,p  (blue), and (e) the drift velocity V  d .
Paper: Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia
Authors: Leon Ofman, Scott A. Boardsen, Lan K. Jian, Parisa Mostafavi, Jaye L. Verniero, Roberto Livi, Michael McManus, Ali Rahmati, Davin Larson, Michael L. Stevens
Figure caption: The results of the 3D hybrid modeling run with the parameters of Case 1 of E11. The left panel shows the temporal evolution of the temperature anisotropy for protons (solid) and α particles (dashes). The right panels show the α particle VDF at ﹩t=0,50,300{{\rm{\Omega }}}_{p}^{-1}﹩ in the V  x –V  z  plane (upper panels) and the cuts of the VDF along V  x  (lower panels).
Paper: Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia
Authors: Leon Ofman, Scott A. Boardsen, Lan K. Jian, Parisa Mostafavi, Jaye L. Verniero, Roberto Livi, Michael McManus, Ali Rahmati, Davin Larson, Michael L. Stevens
Figure caption: The results of the 3D hybrid modeling run with the parameters of Case 1 of E11. The panels show the proton VDF in the V  x –V  z  plane (upper panels) and the cuts of the VDF along V  x  (lower panels) at ﹩t=0,50,300{{\rm{\Omega }}}_{p}^{-1}﹩.
Paper: Observations and Modeling of Unstable Proton and α Particle Velocity Distributions in Sub-Alfvénic Solar Wind at Parker Solar Probe Perihelia
Authors: Leon Ofman, Scott A. Boardsen, Lan K. Jian, Parisa Mostafavi, Jaye L. Verniero, Roberto Livi, Michael McManus, Ali Rahmati, Davin Larson, Michael L. Stevens
Figure caption: The temporal evolution of the temperature anisotropy of α particles (solid) and protons (dashes) for Case 4 with the initial parameters of E12 at 2022 June 3 04:17:01 UT with A  p  = 1.86, A  α  = 1.0, n  α /n  p  = 0.007, and V  d  = 0.32V A.
Paper: Neutrino-driven Winds in Three-dimensional Core-collapse Supernova Simulations
Authors: Tianshu Wang, Adam Burrows
Figure caption: Left: the density profiles of all progenitors. The 9, 9.25, 9.5, 11, and 60 M ⊙ models are taken from Sukhbold et al. (2016), and all other progenitors are from Sukhbold et al. (2018). Right: the average shock radii during the first 1.5 s. The shock velocities can be found in Table 1.
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: The evolution of c/a, the angular momentum of 11 satellites, and their dispersion. We consider 11 satellites, which are the red dots surrounded by a dotted box in Figure 6, and we obtain the evolution of their individual angular momentum, θ, and the dispersion of their angular momentum (σ  θ ). The upper panel shows the evolution of σ  θ , where prograde and retrograde satellites are treated equally. The middle panel shows the evolution of angular momentum θ for each individual satellite. Here θ is measured between the angular momentum of a satellite and an arbitrary fixed direction vector. The lower panel shows the evolution of c/a of the satellite plane composed of 11 (blue line) and full 14 (orange line) satellites. The orange line starts at lookback time = 9.5 Gyr because one of the 14 satellites did not form until then; see the caption of Figure 6. Note that only here we consider all 14 satellites. The four vertical dotted lines (with black, green, red, and purple color) indicate the epochs when the 1st, 5th, 10th, and the 11th (the last) satellite are accreted by the model galaxy, respectively. The accretion time is defined as the time when the satellite first crossed the halo virial radius. Actually, the 11th satellite never crossed the virial radius, but it was within 300 kpc at z = 0. It is also worth noting that, in the middle panel, the satellites represented by the three solid lines (with θ ∼ 150°) at the top are retrograde in the plane, and others are prograde. It is seen that for most of the lookback time, the angular momentum of satellites is almost kept fixed since their accretion.
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: The large-scale structure around the model galaxy and its evolution. The view of this figure is rotated so that the normal of the satellite plane is aligned with the Z axis. Each column shows the projection to the X-Y, X-Z and Y-Z planes. Each row is for different epoch (redshift: 5.85, 3.28, 2.32, 0, or cosmic age: 0.96, 1.94, 2.84, 13.8 Gyr) of the evolution. The green cross and the red dots represent the central galaxy and satellites (top 14 brightest), respectively. In all panels, only subhalos with total mass ≥4.5 × 108 M ⊙ are shown. The blue, orange, and green circles indicate the virial radii of “Centaurus A/M83 group,” “M31,” and the model galaxy. Red dots surrounded by a dotted rectangle in the upper-left panel fell on the model galaxy along a sheet plane and are analyzed in Figure 7. It is worth noting that only 13 red dots were shown in the first three rows, as one of the 14 satellites formed very recently until z = 1.41 or cosmic age = 4.5 Gyr. The thickness of all slices (panels) are 3 cMpc.
Paper: A Rotating Satellite Plane around Milky Way–like Galaxy from the TNG50 Simulation
Authors: Yingzhong Xu, Xi Kang, Noam I. Libeskind
Figure caption: The  k  − Δ  k   curve, computed using Equation (4) without flipping the angular momentum of retrograde satellites. All data points are similar to Figure 2.
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: (a) Redshift vs. bolometric luminosity. The bolometric luminosities are adopted from Krawczyk et al. (2013). (b) Redshift distribution of our sample.
Paper: Formation of CO2 Driven by Photochemistry of Water Ice Mixed with Carbon Grains
Authors: Alexey Potapov, Dmitry Semenov, Cornelia Jäger, Thomas Henning
Figure caption: IR spectra before (black) and after (red) UV irradiation of 13C grains at 150 K.
Paper: Formation of CO2 Driven by Photochemistry of Water Ice Mixed with Carbon Grains
Authors: Alexey Potapov, Dmitry Semenov, Cornelia Jäger, Thomas Henning
Figure caption: IR spectra before (black) and after (red) UV irradiation of 13C/H2O mixtures at 10, 100, 125, and 150 K.
Paper: Modeling the Central Supermassive Black Hole Mass of Quasars via the LSTM Approach
Authors: Seyed Sajad Tabasi, Reyhaneh Vojoudi Salmani, Pouriya Khaliliyan, Javad T. Firouzjaee
Figure caption: The total number of objects available in the QuasarNET+QUOTAS data is 37,648. As a result of data-correction methods, 34,403 objects were removed (red dots). The accepted data are the final flux- and volume-limited samples, consisting of 3245 objects (blue dots).
Paper: Formation of CO2 Driven by Photochemistry of Water Ice Mixed with Carbon Grains
Authors: Alexey Potapov, Dmitry Semenov, Cornelia Jäger, Thomas Henning
Figure caption: Evolution of the column density of 13CO2 at different temperatures with the UV fluence.
Paper: Constraints on the Abundance of Primordial Black Holes from X-Ray Quasar Microlensing Observations: Substellar to Planetary Mass Range
Authors: A. Esteban-Gutiérrez, E. Mediavilla, J. Jiménez-Vicente, J. A. Muñoz
Figure caption: Dark matter fraction of PBHs inferred from microlensing (light blue) from OGLE, EROS, and HSC collaborations, GWs/pulsars (red) from LIGO-Virgo and NANOGrav collaborations, and dynamical constraints (orange) from ultra-faint dwarf galaxies and wide binaries constraints on MACHOs in terms of their mass, assuming a monochromatic mass function (data taken from PBHbounds). The gray curve represents the quasar microlensing results for the visible and X-ray measurements, taking into account the upper limits at the 90% confidence level.
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: A summary of the 1σ  rMSE errors we find on our five parameters when using “all” clustering (the 2ptCF, VPF, and CiC at z = {0.0, 0.1, 0.5, 1.0}) across our various galaxy selections. The color of each point indicates the property we selected by: halo mass (black), stellar mass (magenta), SFR (cyan), or sSFR (blue). The shape of each marker indicates what density we downsampled to after the selection: 0.001 h 3 cMpc−3 (downward-pointing triangle), 0.005 h 3 cMpc−3 (upward-pointing triangle), or no density downsampling (star). The plus sign markers in deeper colors indicate the rMSE constraints found by having a neural network focus only on the single parameter (see Appendix D); these symbols have been shifted slightly left for clarity. The gray dashed–dotted lines indicate the mean of the parameter’s prior space; errors around this value indicate poor to no constraints found by the neural networks. The density plotted on the x-axis is the z = 0 value averaged across the five CV simulations after applying each selection, but before randomly downsampling. See Tables 4, 5, and 7 for complete details.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: Simulated ALMA maps constructed using the same observing parameters as in Figure 4 but at 135 GHz (Band 4), 100 GHz (Band 3), and 42 GHz (Band 1) for the most active lower redshift (z  =  .016) BH. Top panel: mock ALMA tSZ maps for no feedback. Second panel: the corresponding S/N maps, Third panel: same maps, but now for the no-jet feedback mode. Fourth panel: the S/N maps corresponding to the third panel. See Tables 1 and 2 for feedback nomenclature and BH properties. The ALMA results are summarized in Table 4.
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: Our best cosmological constraints with CAMELS-SAM, using “all” N-body only halo clustering and the LFI loss function. Here, we selected halos with mass greater than 2 × 1011 M ⊙, downsampled to a density of 0.005 h 3 cMpc−3 at z = {0.0, 0.1, 0.5, 1.0}.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: Simulated ALMA maps constructed using the same observing parameters as in Figure 4 but at 135 GHz (Band 4), 100 GHz (Band 3), and 42 GHz (Band 1) for the most massive lower redshift (z  =  .016) BH. Top panel: mock ALMA tSZ maps for the no-feedback case. Second panel: the corresponding S/N maps. Third panel: same maps, but now for the no-jet feedback mode. Fourth panel: S/N maps corresponding to the third panel. We note that the lower frequency maps reveal more structure at lower redshift. See Tables 1 and 2 for feedback nomenclature and BH properties.
Paper: Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array
Authors: Avinanda Chakraborty, Suchetana Chatterjee, Mark Lacy, Soumya Roy, Samrat Roy, Rudrani Kar Chowdhury
Figure caption: Simulated ALMA maps constructed using the same observing parameters as Figure 4 but at 135 GHz (Band 4), 100 GHz (Band 3), and 42 GHz (Band 1) for the most active high redshift (z = 1) BHs. Top panel: mock ALMA tSZ maps for no feedback. Second panel: the corresponding S/N maps, Third panel: same maps, but now for the no-jet feedback mode. Fourth panel: the S/N maps corresponding to the third panel. See Tables 1 and 2 for feedback nomenclature and BH properties.