adsabs/AstroCLIMB huggingface dataset:
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Image comparison of dI/dθo for each pixel generated by Jipole. Panel (a): dI/dθo computed using the FD method, shown in symmetric logarithmic scale. Panel (b): dI/dθo computed using AD, shown in symmetric logarithmic scale. Panel (c): absolute difference between the FD and AD results, in logarithmic scale; the NMSE (Equation (26)) is indicated in the top-right corner. Panel (d): relative difference between the FD and AD results, in logarithmic scale.
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Convergence analysis of both parameters using conjugate gradient optimization for the blurred analytical model. Panel (a) shows the convergence of the observer’s inclination θo. The dashed black line represents the targeted value of θo = 60°. Panel (b) depicts the convergence of the dimensionless spin parameter a. The dashed black line represents the targeted value of a = 0.9. Panel (c) showcases the mean square error for the fittings. The dashed black line represents the tolerance level to stop the iteration at ∼6 × 10−19.
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Convergence of the joint fitting of spin and inclination using conjugate gradient optimization for the analytical Model 5. Panel (a): evolution of the dimensionless spin a during iterative fitting, starting from two initial conditions—a = 0.99 (blue) and a = 0.30 (red)—and converging toward the reference value a = 0.9 (dashed black line). Panel (b): evolution of the inclination angle θo during iterative fitting, starting from two initial conditions—θo = 90° (blue) and θo = 20° (red)—and converging toward the reference value θo = 60° (dashed black line). Panel (c): the MSE during the joint fitting, showing convergence to the tolerance threshold of 4 × 10−17 (dashed black line).
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Convergence of the value of the observer’s inclination fitting using conjugate gradient optimization for the analytical Model 5. Panel (a): evolution of the inclination angle θo during iterative fitting, starting from two initial conditions—θo = 80° (blue) and θo = 5° (red)—and converging toward the reference value of 60° (dashed black line). Panel (b): the MSE during the θo fitting, showing convergence to the tolerance threshold of 4 × 10−17 (dashed black line).
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Convergence of the spin parameter fitting using conjugate gradient optimization for the analytical Model 5. Panel (a): evolution of the dimensionless spin a during iterative fitting, starting from two initial conditions—a = 0.99 (blue) and a = 0.20 (red)—and converging toward the reference value a = 0.9 (dashed black line). Panel (b): the MSE during the a fitting, showing convergence to the tolerance threshold of 4 × 10−17 (dashed black line).
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Evolution of the conjugate gradient fitting for blurred, noisy images with three different signal-to-noise ratios: 15 (blue), 1 (red), and 0.05 (green). The black dashed lines indicate the reference values for θo and a. Panel (a): evolution of the observer inclination over the iterations. Panel (b): evolution of the dimensionless spin over the iterations. Panel (c): evolution of the MSE over the iterations.
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Blurred image intensity colormap for the analytical Model 5 described in Section 4.2 with parameters θo = 60° and a = 0.9.
Paper: Jipole: A Differentiable ipole-based Code for Radiative Transfer in Curved Spacetimes
Authors: Pedro Naethe Motta, Ben S. Prather, Alejandro Cárdenas-Avendaño
Figure caption: Resulting noisy images for the blurred analytical model described in Section 4.2. The blurring is applied according to Equations (36), and noise is added following the procedure in Section 5.3. Panels (a)–(c) show the resulting images for signal-to-noise ratios of 15, 1, and 0.05, respectively.
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Characterization of multicomponent accretion states. (Top) Schematics illustrating available combinations of thin disk (blue) and ADAF (red) components. (Bottom-left) Critical accretion rates for the full binary (﹩{\dot{m}}_{0,{\rm{crit}}}﹩; solid), primary (﹩{\dot{m}}_{1,{\rm{crit}}}﹩; dashed), and secondary (﹩{\dot{m}}_{2,{\rm{crit}}}﹩; dotted–dashed) as a function of the binary mass ratio 1/q and mass supply rate ﹩{\dot{m}}_{0}﹩. The Roman numerals indicate the regions of ﹩{\dot{m}}_{0}-q﹩ space corresponding to different accretion geometries as illustrated in the schematics above. The vertical gray band shows our fiducial choice of mass ratio for Section 3. (Right) The colormap shows the secondary accretion rate ﹩{\dot{m}}_{2}﹩, and the thin white band indicates when the secondary starts accreting above its Eddington limit (top, blue regions) under the assumed form of λ(q). ﹩{\dot{m}}_{2}﹩ only ever mildly exceeds its Eddington limit, such that this effect is not significant for our analysis (see text).
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Characteristic cooling profiles for Bremsstrahlung, synchrotron, and inverse Compton emission from the ADAF self-similar solutions for a 107M⊙ binary with a 6 month period (upper panel) and a 1010M⊙ binary with a 10 yr period (lower panel) as a function of radius in units of binary semimajor axes. Both panels are for an outer mass supply rate ﹩5\times 1{0}^{-3}{\dot{M}}_{{\rm{Edd}}}﹩. Dashed lines show an equivalent binary with one-sixth the period. The gray region shows typical scales of the circumbinary cavity such that regions to its left are generally part of the circumsingle flows (mds) and to the right part of the circumbinary flow (cbd). The solid gray line illustrates the characteristic inflow time for hot, advection-dominated solutions, which we regard as a lower limit (see text).
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Critical accretion rates evaluated at the inner edge of a circumbinary disk (r = 2ab) for binaries with mass M and period Pb (and viscosity α = 0.3α0.3). Below the indicated ﹩{\dot{m}}_{{\rm{crit}}}﹩, hot advection-dominated solutions are available. Binaries that would contribute to the GWB at redshift z = 0.3 are highlighted in blue. Gray pluses represent fiducial binary systems used throughout.
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Case study of the binary candidate PG1302-102 fit with our multicomponent three-disk model (in red, dashed) in Region II to a binary of total mass 109.4M⊙, mass ratio 0.3, and rest-frame period Pb = 4 yr. Observed data are shown as the black markers (NASA/IPAC Extragalactic Database (NED) (2019)). PG1302 is a blazar, so we include in purple (dotted) a simple jet model that we emphasize is primarily illustrative. In green (dotted–dashed), we include a cold dust component to capture the infrared bump. The full SED is shown in blue (solid) and captures the predominant features of the system, including the thermal blue bump and high-energy emission.
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: SED decomposition into contributions from the circumbinary disk (cbd), the primary minidisk (md1), and the secondary minidisk (md2) for the binary with M = 1010 M⊙ and Pb = 10 yr. The solid gray line shows the total SED. The accretion rate and associated Region are indicated in the top left of each panel.
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Full broadband SEDs for the fiducial binaries from our multicomponent three-disk model: (Left) M = 107M⊙, Pb = 6 months, and (Right) M = 1010M⊙, Pb = 10 yr. Dashed lines are for a period a factor of 6 shorter (1 month and ∼1.5 yr, respectively).
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Characteristic cooling times evaluated at the typical truncation radius for an equal-mass binary (r ≃ 0.3a) for a 1 yr period binary with indicated mass and outer accretion rate. Tiles rightward and upward of the white tiles (with green/blue hues) have characteristic cooling times shorter than the binary orbital period and could source periodic variability around a binary component. Those leftward and downward (with orange/red hues) radiate too slowly to source a distinct periodic emission at Pb. Gray crosses indicate the tiles associated with the models in Figures 3 and 5.
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Sensitivity of our model SEDs to intrinsic parameters s, β, δ, and f. The colors correspond to the same accretion rates in Figure 3.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: The confirmed bar candidates using the residuals of the single Sérsic fitting in band F277W. Each image is ﹩6\mathop{.}\limits{^{\prime\prime} }5\times 6\mathop{.}\limits{^{\prime\prime} }5﹩.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: The nonparametric metrics of the bright (SFR>175M⊙ yr−1) and faint groups (SFR<175M⊙ yr−1), marked by red and dark green, respectively.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: Results of the single Sérsic fitting: distribution of Sérsic index and effective radius for JWST bands.
Paper: Witnessing Magnetic Reconnection in Tangled Superpenumbral Fibrils around a Sunspot
Authors: Hechao Chen, 何超 陈, Hui Tian, 晖 田, Eric R. Priest, Christopher B. Prior, Chun Xia, 莼 夏, Anthony R. Yeates, Xiaoli Yan, 晓理 闫, Yadan Duan, 雅丹 段, Zhenyong Hou, 振永 侯, Zhenghua Huang, 正化 黄, Oliver E. K. Rice
Figure caption: Magnetic field extrapolation and topology analysis. (a) and (d)–(f): top views of the NLFFF results with different background images. Black lines represent the background field, and the green-colored lines depict the magnetic field lines of the braided bright threads simulated by the NLFFF model. The background images are the AIA EUV 171 Å taken at 09:46 UT in (a), the radial component of the HMI vector magnetogram taken at 06:12 UT in (b), the field line magnetic helicity in (d), the mean twisting T(γ) in (d), and the current helicity Hc(γ) in (f), respectively. Magnified views of the mean twisting and the current helicity at the northern footpoint region, where the extrapolated magnetic field lines are rooted, are presented in the lower left insets of panels (e) and (f), respectively. (c1) and (c2) present four sets of distinctive colored field lines within the braided structure, shown from side and 3D viewpoints, respectively. Arrows in panels (c1) and (c2) highlight the locations of the braid knots.
Paper: Witnessing Magnetic Reconnection in Tangled Superpenumbral Fibrils around a Sunspot
Authors: Hechao Chen, 何超 陈, Hui Tian, 晖 田, Eric R. Priest, Christopher B. Prior, Chun Xia, 莼 夏, Anthony R. Yeates, Xiaoli Yan, 晓理 闫, Yadan Duan, 雅丹 段, Zhenyong Hou, 振永 侯, Zhenghua Huang, 正化 黄, Oliver E. K. Rice
Figure caption: (a) 3D view of the NLFFF results. The background images display the radial component of the vector magnetogram obtained by HMI at 06:12 UT, saturated at ± 500 G. (b) Long-term photospheric horizontal flow fields, as depicted by green arrows, averaged over the time period from 06:00 UT to 12:00 UT, with a maximum and median horizontal velocities of 1.30 and 0.20 km s−1, respectively. Red circles indicate the footpoint regions of the bright threads. (c) Short-term photospheric horizontal flow fields, derived over a 12 minute period, at the south footpoint region of the bright threads.
Paper: The Shape of the Solar Tachocline
Authors: Sarbani Basu, Sylvain G. Korzennik
Figure caption: The model of the tachocline. The tachocline parameters used in this figure are marked at the top of the figure.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: High-resolution 12CO moment 0 (integrated intensity) maps of confirmed dual AGN in major mergers. When resolved, upper-bound and lower-bound estimates of SMBH SoI are overlaid as cyan and yellow circles, respectively. If only the SoI upper bound is resolved, we only show the upper bound. For systems with unresolved SoIs, we mark the AGN position with a white star. Here, we analyze 12CO(1–0) for ESO 253-G003 emission, whereas the remaining systems only have 12CO(2–1) detections. Note that the color map is shown on a logarithmic scale.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: High-resolution 12CO(2–1) moment 0 (integrated intensity) maps of a single AGN in major mergers. For the AGN, the upper-bound and lower-bound estimates of the SMBH SoI are overlaid as cyan and yellow circles, respectively. The white star indicates an unresolved SoI. For the non-AGN SMBH, we mark the upper bound of the SoI with a magenta circle (lower bounds were unresolved). Note that the color map is shown on a logarithmic scale.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: 12CO(2–1) Moment 8 (spectral line peak) map of Mrk 739. In addition to the prominent 12CO emission from Mrk 739W, the circumnuclear ring of Mrk 739E is faintly visible to the left-hand side. The SMBHs have unresolved SoIs, and we mark their positions with white stars. Note that the color map is shown on a logarithmic scale.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Bolometric luminosity (LBol) with respect to the nonrotating molecular gas mass (Mmol/M⊙) within the SMBH SoI at both the SoI lower bound (left panel) and upper bound (right panel). Both axes are on a logarithmic scale. Upper limits (shown as black arrows) are for unresolved SoI and/or 12CO nondetections. We find no significant correlation.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Eddington ratio (LBol/LEdd) with respect to the nonrotating molecular gas mass (Mmol/M⊙) within the SMBH SoI at both the SoI lower bound (a) and upper bound (b). Both axes are on a logarithmic scale. Upper limits (shown as black arrows) are for unresolved SoI and/or 12CO nondetections.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: NGC 6240 corner plot output from 30,000 iterations of our KinMS-implemented MCMC model fitting.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: ESO253-G003 NE corner plot output from 65,000 iterations of our KinMS-implemented MCMC model fitting.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Mrk 463E corner plot output from 35,000 iterations of our KinMS-implemented MCMC model fitting.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Mrk 463W corner plot output from 40,000 iterations of our KinMS-implemented MCMC model fitting.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Mrk 739E corner plot output from 30,000 iterations of our KinMS-implemented MCMC model fitting.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Mrk 739W corner plot output from 30,000 iterations of our KinMS-implemented MCMC model fitting.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: UGC 4211 corner plot output from 30,000 iterations of our KinMS-implemented MCMC model fitting.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Mrk 975 corner plot output from 40,000 iterations of our KinMS-implemented MCMC model fitting. Vmax was constrained to Vmax ≤ 1500 km s−1 (the maximum velocity range of the inputted data cube) to ensure physically meaningful results.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: ESO253-G003 SW corner plot output from 60,000 iterations of our KinMS-implemented MCMC model fitting.