adsabs/AstroCLIMB huggingface dataset:
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: Drift plot of the quadratic bias parameters fit to three simulations: (i) the low-resolution 960 h−1 Mpc (purple), (ii) the reconstructed 960  h−1 Mpc box (blue); and (iii) the input high-resolution 80 h−1 Mpc simulation (gray). We show the best-fit 1D and 2D marginalized posteriors using a maximum wavenumber of ﹩{k}_{\max }=1\,h\,{\mathrm{Mpc}}^{-1}﹩ (﹩{k}_{\max }=2\,h\,{\mathrm{Mpc}}^{-1}﹩) for the fits of the large (small) boxes. We find promising agreement in the higher-order EFT bias parameters, but note that the linear bias parameters (b1 and bη) yield discrepant results at the 2σ–3σ level. The quality of the fits is shown in Figure 8 in the Appendix.
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: The probability density (PDF, left panel) and 1D power spectrum (P1D, right panel) of Lyα flux in redshift space for four related simulation volumes: the high- and low-resolution Nyx simulations, the resized target, and our network output. The gray band in the residual highlights the 10% error range around the smaller, 80  h−1 Mpc high-resolution simulation from our validation data set. The strong P1D agreement demonstrates that small- and intermediate-scale fluctuations are well captured; in contrast, discrepancies in the PDF arise because the model’s limited correlation length prevents reconstruction of correct large-scale phases and spatial correlations.
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: Illustration of the process for creating training data target fields from high-resolution simulations. Fields are iteratively Gaussian blurred and subsampled until they match the grid size (and data footprint) of the low-resolution simulations. This method preserves most fine structures while dramatically reducing the memory necessary to store the density fields on our computer.
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: Illustration of the effects of resolution on Lyα absorption features. We plot slices of baryon density ∼30 Mpc wide for high-resolutions, low-resolution, and reconstructed fields, visualized in log-space. Notice that absorption features are spectrally sharpest in the high-resolution simulation but that some spectral detail is recovered by our ML model.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: Imaging and light profiles considered for two example events: FRBs 20240312D (top panels) and 20220725A (lower panels), along with the FRB positions (1σ total uncertainty; magenta ellipses). The smaller panels represent the Galfit surface-brightness profile model (“Profile”), residual image (“Residual”), and 2D synthetic globular cluster distribution models (“GC Ellipsoidal,” “GC Spherical”); the production of these images is described in Sections 4.1–4.2. We denote the preferred model for each FRB with a white check mark. The images are oriented with north up and east to the left and span ≈﹩1^{\prime} ﹩ on a side. It is clear that the GC models extend to larger radii, representative of their more extended spatial distribution compared to stars. The host of FRB 20240312D has a face-on orientation, with no apparent difference in the two GC models, while the effects of the host inclination on the GC distributions can clearly be seen for the host of FRB 20220725A.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of the SMBH mass, M• (top), the total luminosity of the jets, ﹩{L}_{{\rm{jet}}}=\eta [1/2{\dot{M}}_{\bullet }{v}_{{\rm{jet}}}^{2}+3/2({\dot{M}}_{\bullet }/{m}_{p})kT]﹩ (middle), and evolution of jet extent, Rjet. Rjet is represented by the median distance of the farthest 20% of the jet particles at a moment in time, sampled every 30 Myr. The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Face-on galaxies in 60 kpc x 60 kpc frames from LBH and EBH sequences shown for each 2 Gyr from z = 3.7 to z = 0. Stars are blue, and gas is overplotted on the stars in orange, both colored by 2D projected density and rotated based on the angular momentum vector of stars inside 3 kpc. The first four columns represent the LBH sequence galaxies, from ϵ0 to ϵ50, and the next four columns represent the EBH sequence.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of galactic SFR within 0.1Rvir for three similar ϵ5 models (top frame) and two ϵ0 models (bottom frame). Top: the LBH model (black solid line), the EBH model with enhanced SN feedback (blue dotted line), and the comparison ϵ5,EBH(test) model with the same SN feedback as in the LBH models (red dashed line). The ϵ5,EBH model differs from the other two by increased strength of the SN feedback, increased range of the SN feedback to 700 pc, and a reduced 10 Myr energy deposition timescale. Bottom: two models without AGN. The EBH model has enhanced SN feedback (see Section 2). The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of galactic SFR within 0.1Rvir for LBH (top) and EBH (bottom) models. Each curve represents a different AGN feedback model. The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of the gas fraction, fgas, within the galactic radii, 0.1Rvir, for all models, LBH (top) and EBH (bottom). The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: SFR vs. molecular mass, MH2, within the galactic radius 0.1Rvir for LBH models (top frame) and EBH models (bottom frame). Points represent each 100 Myr of evolution during z = 3–0. Those corresponding to z = 0 for each model are highlighted with a yellow outline. Marker color shows the accretion efficiency: lime green for ϵ0, red for ϵ5, blue for ϵ15, and black for ϵ50. Marker type indicates time, namely, circles correspond z = 3–2, squares to z = 2–1, and x’s to z = 1–0. The dashed lines are median lines that provide linear fits for z ≲ 1 markers. The markers converge to median lines after z ∼ 2.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Galaxies from Figure 10 shown edge-on with LBH (left four columns) and EBH (right four columns) sequences shown at z = 1.9 and z = 0. Stars (first and third rows) and gas (second and fourth rows) are separated. Stars are blue, and gas is orange. Both are colored by 2D projected density and rotated based on the angular momentum of stars inside 3 kpc. Frames are 60 kpc × 60 kpc.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of ﹩{M}_{{{\rm{H}}}_{2}}﹩ inside 0.1Rvir, for LBH (top) and EBH (bottom). The black arrows indicate the seeding time of the SMBHs.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: Spectrum summary figure for α Cen in the same style as Figure 3 with an additional panel to show the spectra of each component of the binary separately.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: Spectrum summary figure for ﹩{ \mathcal E }﹩ Eri in the same style as Figure 3.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: Spectrum summary figure for κ1 Ceti in the same style as Figure 3.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for κ1 Ceti in the same style as Figure 2.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for ﹩{ \mathcal E }﹩ Eri in the same style as Figure 2.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for α Cen A in the same style as Figure 2.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for ξ Boo A in the same style as Figure 2.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for α Cen B in the same style as Figure 2.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: Spectrum summary figure for Procyon in the same style as Figure 3.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: An example of targeted quasar field SDSSJ0819 and its ALMA detections. Upper panel: SCUBA-2 850 μm map where white circles indicate the ≥4σ detections at 850 μm reported by F. Arrigoni Battaia et al. (2023). Magenta squares represent the ALMA targets presented in this work. Targets with CO detections are labeled in red with their corresponding names. Lower panels: integrated CO emission maps integrated over channels within the FWHM of the detected emission line. White circles illustrate the beam size and shape of the corresponding targets. Images featuring only black contours indicate that the lines are better described by single-Gaussian models (Section 3.1), with the contours representing 3σ–6σ of the stacked maps. Conversely, images with blue and red contours represent emission lines that are better fitted by double-Gaussian (DG) models. Blue and red contours denote 3σ–6σ of the stacked map based on each of the two components of the DG models, respectively. Figures for the rest of the detections are shown in Appendices A–B.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Completeness (COM) and false detection rate (FDR) based on our Monte Carlo simulations using ALMA USB cubes. Upper panels: COM with different signal-to-noise ratio (SNR). The corresponding SNRs from the right to left panels are 7.0, 7.5, 8.0, and 8.7 (the minimum SNR among primary sources). The white curves show the COM at 10%, 30%, 50%, 70%, and 90% levels from thin to thick. Lower panels: FDR at different SNR cuts. The white pixels represent the locations where no sources can be detected. Additionally, in panels with SNRs ≥ 8.0 (our detection threshold), we plot the primary (orange points) and supplementary (red points) sources that exceed the corresponding SNR threshold.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Spectra of the detected sources and their fitting results of SDSSJ0819. The gray region depicts the noise for each channel. Fitting results for both the single-Gaussian (SG) and double-Gaussian (DG) models are shown on the figure: the black dotted lines represent the best-fit SG models, while the black solid line represents those for DG, with the two components displayed separately as blue and red solid lines. Figures for the rest of the detections are shown in Appendix C.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: The results of the curve-of-growth analyses. Gray lines represent CO intensity of each sample SMG extracted using various beam sizes, normalized to that of original beam size. The orange and red line represent the mean and median normalized CO intensity value, respectively. Both the mean and median converge to 2.0 at sufficiently large aperture sizes (≳2 beams).
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: SED for SDSSJ0819_SMG 1.1: one example of the MBB fitting results for the primary sample. Black points represent the flux density for ALMA and JCMT/SCUBA-2 (from left to right, 450, 850 μm (SCUBA-2), 3 mm (ALMA)), while green points represent those for Herschel (from left to right, 250, 350, 500 μm). The blue line represents the fitting result. The fitting results of the rest of the sample can be found in Appendix E.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: Spectrum summary figure for ξ Boo in the same style as Figure 3 with an additional panel to show the spectra of each component of the binary separately.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: The DEM-generated EUV spectra produced by this work are plotted with each star in the labeled panels compared to the SIRS of that in T. N. Woods et al. (2009) in gray, scaled to a distance of 1 au.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for ξ Boo B in the same style as Figure 2.
Paper: Calcium Excess in Novae: Beyond Nuclear Physics Uncertainties
Authors: Mallory K. Loria, Pavel A. Denissenkov, Chris Ruiz, Falk Herwig
Figure caption: Comparison of observed abundances in novae of uncertain type (CO or ONe) with predicted abundances from multizone nova models. Observational data for V1224 Oph (J. Andrea et al. 1994), V603 Aql (S. Pottasch 1959), RR Pic (S. Pottasch 1959), and GK Per (S. Pottasch 1959) are shown with blue and green symbols. Model predictions are represented by purple, pink, yellow, orange, and red symbols connected by solid lines.
Paper: Calcium Excess in Novae: Beyond Nuclear Physics Uncertainties
Authors: Mallory K. Loria, Pavel A. Denissenkov, Chris Ruiz, Falk Herwig
Figure caption: Comparison of observed abundances in CO novae V705 Cas (V. P. Arkhipova et al. 2000), GQ Mus (C. Morisset & D. Pequignot 1996), V977 Sco (J. Andrea et al. 1994), V443 Sct (J. Andrea et al. 1994), and DQ Her (S. Pottasch 1959) with predicted abundances from Model 1 and Model 2. Observational data are shown with blue and green symbols, while model predictions are represented by pink and purple circles and diamonds connected by a solid line.
Paper: Calcium Excess in Novae: Beyond Nuclear Physics Uncertainties
Authors: Mallory K. Loria, Pavel A. Denissenkov, Chris Ruiz, Falk Herwig
Figure caption: Comparison of elemental mass fractions from our multizone nova models (MESA and MPPNP simulations in the Nova framework, solid-color lines) with those of the Barcelona group (black dashed and dotted lines). Models selected from the Barcelona group have parameters closest to ours for both CO and ONe novae (J. José & M. Hernanz 1998). The gray dashed and dotted lines represent more recent models from J. José et al. (2020).
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: The physical properties of misaligned galaxies and aligned controls. (a) The galaxy distribution in a two-dimensional plane of M* and Dn4000. The black contour shows the distribution of SDSS galaxies. The black dashed line separates galaxies into the SF sequence and the QS sequence. The blue and gray squares represent SF misaligned galaxies and aligned controls. The red and gray triangles represent QS misaligned galaxies and aligned controls. (b) Stellar mass distribution. (c) Dn4000 distribution. (d) Inclination angle distribution. (e) Redshift distribution. In panels (b), (c), (d), and (e), the pink and gray histograms represent the distributions of misaligned galaxies and aligned controls, respectively. The pink and gray bars on the top show the corresponding median values.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: An example of misaligned galaxies MaNGA 1-418253. (a) The DESI g, r, z image. The purple hexagon shows the MaNGA bundle. (b) Stellar velocity field. The black dashed line shows the kinematic position angle the stellar disk. (c) Gas velocity field. The black dashed line shows the kinematic position angle of the gas disk. In panels (b) and (c), the blue and red colors represent velocities approaching and receding from the galactic center.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: Examples of H I profiles. (a) Star-forming (SF) misaligned galaxy and aligned control with single-peaked H I profiles. (b) SF misaligned galaxy and aligned control with double-horned H I profiles. (c) Quiescent (QS) misaligned galaxy and aligned control with single-peaked H I profiles. (d) QS misaligned galaxy and aligned control with double-horned H I profiles. Blue (red) lines represent the SF (QS) misaligned galaxies, and gray lines represent the aligned controls. Each profile is normalized by its peak flux.
Paper: Spatial Distribution of Secondary Electrons’ Synchrotron Emission: Property and Implication
Authors: Qi-Zuo Wu, Ruo-Yu Liu
Figure caption: Left: the morphology of emission in hadronic scenario. Right: the corresponding SBPs and photon index profiles along the x-axis in hadronic (black lines) and leptonic (green lines) scenarios. From top to bottom, (a) 25–100 TeV γ-ray emission (b) 2–7 keV X-ray emission.
Paper: Diverse Pathways for Supermassive Black Hole–Galaxy Coevolution
Authors: Bryan A. Terrazas, James Aird, Alison L. Coil
Figure caption: The z = 0.5 and z = 2 MBH–Mstar relations for the fiducial model and model variations 3 and 4, similar to Figure 9. The z = 0 (J. E. Greene et al. 2020) relations are shown by the dotted lines for comparison in every panel. Similar to our findings comparing model variations 1 and 2, the differences in the method for assigning z = 0 MBH distributions across the galaxy population result in similar relations at z = 2. However, for model variation 3, the distinction at z = 2 between galaxies that will be star-forming or quiescent at z = 0 is stronger, with the star-forming galaxies all either moving outside the limits of the plot or falling in the f0 regime, while quiescence by z = 0 is strongly associated with a high MBH at z = 2. Model variation 4 exhibits significantly less scatter at z = 2 than the other models, a negligible f0, and no distinction based on the z = 0 galaxy star formation properties. All models result in a flatter MBH–Mstar relation at z = 2.