adsabs/AstroCLIMB huggingface dataset:
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Left: an example of calculated AMD for multi-ion UFOs with MHD winds assuming Γ = 2, θ = 40°, p = 1.2, f  D  = 1, α OX = 1.5, and λ ion = 0.05. Local hydrogen-equivalent columns (expressed in the left ordinate) are shown for major ions: Fe XXVI (green), Fe XXV (cyan), S XVI (orange), Si XIV (yellow), Mg XII (dark blue), Ne X (red), and O VIII (dark) along with the LOS wind velocity v out/c (purple; expressed in the right ordinate). A majority of the column is highly blueshifted (v out/c > 0.1 in the light-yellow region) for many ions. Right: schematics of AMD with velocity profiles v out(ξ) for different ionizing photons corresponding to the ionic column (dark for less ionizing photons and red for more ionizing photons). Filled blue circle denotes where a local column is maximally produced. Open circle corresponds to the column produced at the innermost wind layer where ξ value is the highest in each case. Note that the wind under higher ionization (in red) produces a lower column of near-relativistic blueshift (v out/c > 0.1 in squared domain) yielding slower UFOs in comparison with the lower ionization case (in the shaded domain).
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Left: schematic diagram showing a comparison of characteristic absorption profiles among various wind-driving mechanisms: Gaussian/Voigt profiles (dashed), thermal driving (green), line driving (cyan), and MHD driving (red). Right: spectral change in Fe XXV/Fe XXVI lines due to disk truncation at the inner launching radius parameterized by q  T .
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Upper: simulated 100 ks XRISM/Resolve spectrum (the dark line) for θ = 35°, p = 1.25, Γ = 2, α OX = 1.5, f  D  = 0.1, and λ ion = 0.08 with the best-fit composite model (the red line). See Table 2 for the best-fit model parameters. Middle: unfolded best-fit model spectrum. Lower: residuals in the form of a data/model ratio in the absence of the UFO component (mhdwind).
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Left: sample comparison of AMD, similar to Figure 1, with (solid) and without (dashed) SE flux in the injected SED for selected ions assuming θ = 40°, p = 1.3, α OX = 1.5, f  D  = 1, and λ ion = 0.05. Right: theoretical multi-ion absorption spectra (ratio to the continuum) for different SE normalization of K SE = 6 × 10−7 (strong in the red line) and 3 × 10−8 (moderate in blue) in comparison with the absence of SE (the dark line) assuming θ = 30°, p = 1.3, α OX = 1.5, f  D  = 0.1, and λ ion = 0.05.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Theoretical multi-ion absorption spectra (ratio to the continuum) for different photon index Γ with θ = 30°, p = 1.3, f  D  = 1, α OX = 1.5, and λ ion = 0.1.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Zoom-in on simulated 100 ks XRISM/Resolve spectrum for Γ = 2, α OX = 1.5, λ ion = 0.08, p = 1.3, f  D  = 0.1, and θ = 35° showing the residual (ratio) from the best-fit composite model (composite; the red line) in the absence of MHD UFO component (mhdwind).
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Simulated 100 ks XRISM/Resolve spectra for different photon index Γ with θ = 30°, p = 1.3, α OX = 1.5, f  D  = 1, and λ ion = 0.1. Inset shows a close-up of Fe K absorbers.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Theoretical multi-ion absorption spectra (ratio to the continuum) for different inclination θ with Γ = 2, α OX = 1.5, p = 1.3, f  D  = 1, and λ ion = 0.1.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Confidence contours of (θ, f  D ) for different values of wind density factor f  D  derived from the best-fit models with θ = 35° showing 68% (red), 90% (green), and 99% (blue) levels. Left: XRISM/Resolve 100 ks exposure. Right: Athena/X-IFU 10 ks exposure.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Theoretical multi-ion absorption spectra (ratio to the continuum) for different density slope p with θ = 30°, Γ = 2, α OX = 1.5, f  D  = 1, and λ ion = 0.1.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Theoretical multi-ion absorption spectra (ratio to the continuum) for different ionizing luminosity ratio λ ion with θ = 30°, Γ = 2, p = 1.3, f  D  = 1, and α OX = 1.5.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Simulated 100 ks XRISM/Resolve spectra for different X-ray strength α OX with θ = 30°, p = 1.3, f  D  = 1, Γ = 2, and λ ion = 0.1.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Theoretical multi-ion absorption spectra (ratio to the continuum) for different X-ray strength α OX with θ = 30°, Γ = 2, p = 1.3, f  D  = 1, and λ ion = 0.1.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Simulated 100 ks XRISM/Resolve spectra for different ionizing luminosity ratio λ ion with θ = 30°, p = 1.3, f  D  = 1, Γ = 2, and α OX = 1.5.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Zoom-in on simulated 10 ks Athena/X-IFU spectrum for Γ = 2, α OX = 1.5, λ ion = 0.1, p = 1.2, f  D  = 0.1, and θ = 35° showing the residual (ratio) from the best-fit composite model (composite; the red line) in the absence of MHD UFO component (mhdwind).
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Simulated 100 ks XRISM/Resolve spectra for different density slope p with θ = 30°, Γ = 2, α OX = 1.5, f  D  = 1, and λ ion = 0.1.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Simulated 100 ks XRISM/Resolve spectra for different inclination θ with Γ = 2, p = 1.4, α OX = 1.5, f  D  = 1, and λ ion = 0.1.
Paper: Tell-tale Spectral Signatures of MHD-driven Ultrafast Outflows in AGNs
Authors: Keigo Fukumura, Mauro Dadina, Gabriele Matzeu, Francesco Tombesi, Chris Shrader, Demosthenes Kazanas
Figure caption: Similar to Figure 6 but in the presence of the reflection component.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: Various parameters as functions of the Alfvénic Mach number M for A = 1 (black curves), A = 0.5 (red curves), and A = 0.1 (blue curves). Top left: the magnetic compression R = B  d /B  u . Top right: the normalized downstream pressure ﹩{{\rm{\Pi }}}_{{xx}}={p}_{d,{xx}}/{\rho }_{u}{V}_{u}^{2}﹩. Bottom left: the density compression N = n  d /n  u . Bottom right: the ratio of the magnetic compression to the density compression R/N . The shock angle is θ  u  = 60° and β = 0.5.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: Various parameters as functions of the Alfvénic Mach number M for A = 1 (black curves), A = 0.5 (red curves), and A = 0.1 (blue curves). Top left: the magnetic compression R = B  d /B  u . Top right: the normalized downstream pressure ﹩{{\rm{\Pi }}}_{{xx}}={p}_{d,{xx}}/{\rho }_{u}{V}_{u}^{2}﹩. Bottom left: the density compression N = n  d /n  u . Bottom right: the ratio of the magnetic compression to the density compression R/N. The shock angle is θ  u  = 40° and β = 0.5.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: Top: the magnetic field magnitude, normalized to the upstream magnetic field magnitude. Middle: the three eigenvalues of the ion temperature tensor, normalized to the upstream ion temperature. Bottom: the three eigenvalues of the electron temperature tensor, normalized to the upstream electron temperature. The smallest eigenvalue is in blue, while the largest one is in black. The measurements are conducted in burst mode. See the text for more details.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: The normalized magnetic field magnitude ∣B∣/B  u  (black) and the ratio of the largest to smallest eigenvalues of the temperature tensor ﹩{T}_{\max }/{T}_{\min }﹩ (blue) for two MMS-observed shocks. The thin black line corresponds to T max/T min = 1.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: Various parameters as functions of the Alfvénic Mach number M for A = 1 (black curves), A = 0.5 (red curves), and A = 0.1 (blue curves). Top left: the magnetic compression R = B  d /B  u . Top right: the normalized downstream pressure ﹩{{\rm{\Pi }}}_{{xx}}={p}_{d,{xx}}/{\rho }_{u}{V}_{u}^{2}﹩. Bottom left: the density compression N = n  d /n  u . Bottom right: the ratio of the magnetic compression to the density compression R/N. The shock angle is θ  u  = 60° and β = 1.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: The parallel (blue) and perpendicular (black) temperatures of ions normalized to the upstream ion temperature.
Paper: Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals
Authors: Zhiwei Chen, Youjun Lu, Yuetong Zhao
Figure caption: The normalized evolution of merger rate density as a function of redshift. Here  R (z s) represents the merger rate density at redshift z s and  R  total is the integration of the merger rate density over redshift. Cyan, blue, and orange lines represent the results obtained by assuming that all sBBHs are produced by the EMBS, dynamical, and AGN-MBH channels, respectively.
Paper: Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals
Authors: Zhiwei Chen, Youjun Lu, Yuetong Zhao
Figure caption: The fraction of lensed GW sBBH events P(H∣GW) that can have their host galaxies identified as lensed by a sky galaxy survey with the limiting magnitude of ﹩{m}_{\mathrm{lim}}﹩. Solid, dashed, and dotted–dashed lines represent the i band of CSST, the J band of RST, and the VIS band of Euclid, while cyan, blue, and orange lines show the results obtained by assuming that all the sBBH mergers originate from the EMBS, dynamical, and AGN-MBH channels, respectively. The limiting magnitude of each telescope at the given band is also indicated by the purple, red, and brown dotted lines.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: Various parameters as functions of the Alfvénic Mach number M for A = 1 (black curves), A = 0.5 (red curves), and A = 0 (blue curves). Top left: the magnetic compression R = B  d /B  u . Top right: the normalized downstream pressure ﹩{{\rm{\Pi }}}_{{xx}}={p}_{d,{xx}}/{\rho }_{u}{V}_{u}^{2}﹩. Bottom left: the density compression N = n  d /n  u . Bottom right: the ratio of the magnetic compression to the density compression R/N. The shock angle is θ  u  = 10° and β = 0.5.
Paper: Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals
Authors: Zhiwei Chen, Youjun Lu, Yuetong Zhao
Figure caption: Distributions of redshift z s and stellar mass ﹩\mathrm{log}({M}_{* }/{M}_{\odot })﹩ of the identifiable source galaxies in the simulated host samples for the lensed sBBH GW events, resulting from the EMBS (left), dynamical (mid), and AGN-MBH (right) channels. The limiting magnitude for the survey to identify the lensing signatures of the host galaxies is set to be m  i  = 25. The dashed lines and the solid contours indicate the 16%, 50%, and 84% percentiles for each parameter.
Paper: Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals
Authors: Zhiwei Chen, Youjun Lu, Yuetong Zhao
Figure caption: Spatial distribution of the lensed GW sBBH events in units of the effective radius R e of their host galaxies. The limiting magnitude ﹩{m}_{\mathrm{lim}}﹩ for the galaxy survey to identify the hosts as lensed is assumed to be 24 (top left), 25 (top right), 26 (bottom left), and 27 mag (bottom right). In each panel, the cyan, blue, and orange lines show the results of EMBS, dynamical, and AGN-MBH channels, respectively.
Paper: Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals
Authors: Zhiwei Chen, Youjun Lu, Yuetong Zhao
Figure caption: The cumulative probability distribution of the GW localization errors for those lensed sBBH mergers detected by third-generation ground-based GW detectors. The orange, blue, and cyan solid lines show the results obtained by the ET with xylophone design, CE, and the network of CE and ET with xylophone design, respectively.
Paper: Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Michael Gedalin, Michal Golan, Nikolai V. Pogorelov, Vadim Roytershteyn
Figure caption: The number of DOF ν as a function of B  d /B  u  and θ  u .
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Evolution of thermodynamic states of the wind for the NEI-SR run. The density, temperature, and velocity of the wind are shown in the left, middle, and right panels. The mass and energy injection push the background CGM further and further with time and finally set up a steady-state flow at ≳20 Myr. The injection region is at R ≤ 200 pc, where the density and temperature are roughly constant. Different line styles show results for different runs in the steady state (dotted: PIE, dashed–dotted: PIE-SR, dashed: NEI, and solid: NEI-SR). The lines superpose each other except for the temperature panel. The dashed gray line in the right panel shows the circular velocity corresponding to the assumed gravitational potential.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Output spectra at 200 pc (left panel) and at 10 kpc (right panel). The top panel shows the spectral evolution with time for the NEI-SR run. The bottom panel compares the photon number spectra (total number of photons above certain energy) from all the four runs at t = 28 Myr. The black dotted lines represent the HM12 background radiation field. The dashed lines represent runs without considering self-radiation of the wind itself, and the solid lines show results for the cases with self-radiation of the wind included.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Total mass (left panel), mechanical power (middle panel), and radiation energy (right panel) output from the stellar synthesis code STARBURST99 for a given SFR of 10 M ⊙ yr−1. The input radiation spectra in the simulation use a coarser frequency containing only 56 frequency bins than shown here. The injection rates become roughly constant after ∼30 Myr when the wind attains a steady-state solution.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: [Regions found for all radial distances. Excludes Encounter 1.] 2D histograms of RTN bulk velocity unit vectors and velocity magnitude. Figure 7(a) represents the ﹩\hat{R}﹩ component of the velocity unit vector in RTN coordinates. 7(b) is the ﹩\hat{T}﹩ component. Figure 7(c) is the ﹩\hat{N}﹩ component. Figure 7(d) is the magnitude of the solar wind velocity in km s−1.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: Superposed epoch analysis of electron properties inside and near wave-active quiescent regions. Figure 10(a) shows the measured component of the strahl width. Figure 10(b) shows the sunward drift of the thermal core electrons. Figure 10(c) shows the electron core temperature (average of parallel and perpendicular temperatures). Figure 10(d) shows the electron core temperature anisotropy.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: [Regions found at all R  s ] 2D histograms of RTN bulk velocity unit vectors and velocity magnitude. Figure 8(a) represents the ﹩\hat{R}﹩ component of the velocity unit vector in RTN coordinates. 8(b) is the ﹩\hat{T}﹩ component. 8(c) is the ﹩\hat{N}﹩ component. Figure 8(d) is the magnitude of the solar wind velocity in km s−1. SPC fits have been used to calculate the velocity for Encounter 1.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: Histograms of proton temperature components and proton temperature anisotropy. Figure 9(a) is a 2D histogram over time of the component of the proton temperature perpendicular to the ambient magnetic field, normalized to the total temperature measured in the instrument frame. Figure 9(b) is the parallel component, also normalized to the total temperature. Figure 9(c) shows the temperature anisotropy.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: Distribution of electron core sunward drift values for each solar encounter (blue) and distribution of electron core sunward drift during wave-active quiescent regions identified within each encounter (orange).
Paper: Cosmological Simulation of Galaxy Groups and Clusters. II. Studying Different Modes of Feedback through X-Ray Observations
Authors: Rudrani Kar Chowdhury, Suchetana Chatterjee, Ankit Paul, Craig L. Sarazin, Jane Lixin Dai
Figure caption: X-ray maps for different exposure times. Top left: X-ray map of a system at z = 1 including all the AGN feedback modes, observed for an exposure time of 200 ks (same as shown in top left panel of Figure 6). Top right: X-ray map of the same system observed for 2 Ms. Bottom left: X-ray map of a system at z = 0.016 including all the modes of feedback from AGNs, observed for an exposure time of 200 ks (same as shown in the top left panel of Figure 7). Bottom right: X-ray map of the same system observed for a longer exposure time of 2 Ms. Color bars represent photon number counts per pixel in all the panels. An increase in S/N is observed for the longer exposure time as expected.
Paper: Simulated Bars May Be Shorter but Are Not Slower Than Those Observed: TNG50 versus MaNGA
Authors: Neige Frankel, Annalisa Pillepich, Hans-Walter Rix, Vicente Rodriguez-Gomez, Jason Sanders, Jo Bovy, Juna Kollmeier, Norm Murray, Ted Mackereth
Figure caption: Comparing bar properties between TNG50 and MaNGA observations with the distributions of pattern speeds, corotation radii, bar sizes derived from the light, and ﹩{ \mathcal R }\,=\,{R}_{\mathrm{corot}}/{R}_{{\rm{b}}}﹩ values for observed and simulated barred galaxies. These are from the MaNGA (filled brown) and the TNG50 (green line) matched samples. Contributions from the highly inclined MaNGA systems (i > 60°) are separated out in black. TNG50-obtained bar sizes are emulated to observations. The mean values of pattern speeds, Ω P , and corotation radii, R corot, agree within 15% whereas the mean bar sizes, R b, and ﹩{ \mathcal R }﹩ value differ by ∼50%. The averages and their uncertainties are annotated at the top of each panel for the simulations and observations respectively. Averages over observed properties also include the highly inclined systems.