adsabs/AstroCLIMB huggingface dataset:
Paper: Accelerating Giant-impact Simulations with Machine Learning
Authors: Caleb Lammers, Miles Cranmer, Sam Hadden, Shirley Ho, Norman Murray, Daniel Tamayo
Figure caption: Comparison between the performance of the orbital-outcome regressor (top row) and a non-ML baseline model (bottom row) on the validation set of 103,404 three-planet systems. Predicted orbital elements (i.e., semimajor axis, eccentricity, and inclination) for the new, merged planets are plotted against their true orbital elements. The ML model predicts orbital elements with somewhat less scatter and bias about the true values than the baseline model, approaching the accuracy limits imposed by chaos (see Table 1).
Paper: Accelerating Giant-impact Simulations with Machine Learning
Authors: Caleb Lammers, Miles Cranmer, Sam Hadden, Shirley Ho, Norman Murray, Daniel Tamayo
Figure caption: Performance of the collision-classifier model on 200 random validation systems. The probabilities of a collision occurring between planets 1–2, 2–3, and 1–3, as predicted by the ML model, are plotted against the true fraction of collisions that occur between the planet pairs, determined by performing 250 shadow integrations of each system. The model accurately predicts collision probabilities with a scatter of ∼10% and very little bias about the true fractions (σ is the rms error and b is the mean of the residuals). For comparison, all baseline models we considered performed poorly (see Appendix B).
Paper: Accelerating Giant-impact Simulations with Machine Learning
Authors: Caleb Lammers, Miles Cranmer, Sam Hadden, Shirley Ho, Norman Murray, Daniel Tamayo
Figure caption: Same comparison as Figure 3, now for the three postcollision orbital elements of the surviving planet that is not involved in the merger. The orbital-outcome regressor predicts semimajor axis, eccentricity, and inclination with less scatter and bias than the non-ML baseline model, approaching the limit imposed by chaos (see Table 1).
Paper: Accelerating Giant-impact Simulations with Machine Learning
Authors: Caleb Lammers, Miles Cranmer, Sam Hadden, Shirley Ho, Norman Murray, Daniel Tamayo
Figure caption: Schematic of our ML model. The collision classifier takes the mean and standard deviation of the three planets’s orbital elements from a short N-body integration as input and predicts which pair of planets will collide (in the form of three collision probabilities). The orbital-outcome regressor takes the orbital elements, as well as a choice for which two planets to combine, and predicts the orbital elements of the two resulting postcollision planets.
Paper: An Intermediate-mass Black Hole Hidden behind Thick Obscuration
Authors: Peter G. Boorman, Daniel Stern, Roberto J. Assef, Abhijeet Borkar, Murray Brightman, Johannes Buchner, Chien-Ting Chen, Hannah P. Earnshaw, Fiona A. Harrison, Gabriele A. Matzeu, Ryan W. Pfeifle, Claudio Ricci, Jiří Svoboda, Núria Torres-Albà, Ingyin Zaw
Figure caption: (Top) The coadded Chandra data and corresponding texrav-based fit, folded with the instrument response. The background has been subtracted for visual clarity but was not subtracted during fitting. The total posterior model range is shown in green, together with the posterior constraint on the Fe Kα and tentative silicon emission lines shown in pink and red hatched shaded regions, respectively. The instrument background is plotted with gray shading at the bottom of the panel. (Bottom) Difference in the cumulative posterior model-predicted counts and cumulative measured data counts are plotted as a function of energy with green shading. Simulated posterior predictive checks, showing the range expected if the derived posterior were true, are shown in gray. Since the green posterior is broadly bounded by the gray-shaded region, we deem the fit as acceptable.
Paper: An Intermediate-mass Black Hole Hidden behind Thick Obscuration
Authors: Peter G. Boorman, Daniel Stern, Roberto J. Assef, Abhijeet Borkar, Murray Brightman, Johannes Buchner, Chien-Ting Chen, Hannah P. Earnshaw, Fiona A. Harrison, Gabriele A. Matzeu, Ryan W. Pfeifle, Claudio Ricci, Jiří Svoboda, Núria Torres-Albà, Ingyin Zaw
Figure caption: The Eddington ratio posteriors derived for IC 750 plotted against line-of-sight column density. The Eddington ratio posteriors were derived using the unabsorbed 2–10 keV luminosities predicted from the physically motivated obscuration modeling while propagating uncertainties in black hole mass and bolometric correction. The boundaries representing the effective Eddington limits on dusty gas in the regime of radiation trapping and the single-scattering UV-thin regime from W. Ishibashi et al. (2018) are plotted with dotted (red) and dashed (blue) lines, respectively. The sample of NuSTAR-studied megamaser AGN from M. Brightman et al. (2016) is plotted as dark gray squares with error bars.
Paper: An Intermediate-mass Black Hole Hidden behind Thick Obscuration
Authors: Peter G. Boorman, Daniel Stern, Roberto J. Assef, Abhijeet Borkar, Murray Brightman, Johannes Buchner, Chien-Ting Chen, Hannah P. Earnshaw, Fiona A. Harrison, Gabriele A. Matzeu, Ryan W. Pfeifle, Claudio Ricci, Jiří Svoboda, Núria Torres-Albà, Ingyin Zaw
Figure caption: Left: coadded 177 ks exposure Chandra image in the 0.5–7 keV passband. Center: coadded Chandra image in the 6.1–6.6 keV passband. The central AGN produces significant flux consistent with Fe Kα. Right: optical Hubble Space Telescope/F606W image centered on the nucleus of IC 750. All panels are matched in coordinates and oriented such that north is up and east is to the left.
Paper: An Intermediate-mass Black Hole Hidden behind Thick Obscuration
Authors: Peter G. Boorman, Daniel Stern, Roberto J. Assef, Abhijeet Borkar, Murray Brightman, Johannes Buchner, Chien-Ting Chen, Hannah P. Earnshaw, Fiona A. Harrison, Gabriele A. Matzeu, Ryan W. Pfeifle, Claudio Ricci, Jiří Svoboda, Núria Torres-Albà, Ingyin Zaw
Figure caption: (Left) The distribution of Iron Kα equivalent widths from the Compton-thick sample of P. G. Boorman et al. (2018) with upper limits shown as solid green arrows. The large error bar at the top of the panel shows the texrav-based equivalent width measurement of Iron Kα for IC 750 from this work. (Right) The distribution of 295 intrinsic luminosity measurements for 30 unique Compton-thick AGN in DoCTA within D < 50 Mpc (P. G. Boorman et al. 2024).
Paper: An Intermediate-mass Black Hole Hidden behind Thick Obscuration
Authors: Peter G. Boorman, Daniel Stern, Roberto J. Assef, Abhijeet Borkar, Murray Brightman, Johannes Buchner, Chien-Ting Chen, Hannah P. Earnshaw, Fiona A. Harrison, Gabriele A. Matzeu, Ryan W. Pfeifle, Claudio Ricci, Jiří Svoboda, Núria Torres-Albà, Ingyin Zaw
Figure caption: Unfolded spectral posteriors for each physically motivated obscuration model fit to the coadded Chandra data of IC 750. Lower panels show the difference in the cumulative (and normalized) model, and data counts as a quantile–quantile difference plot. The gray oval-shaped regions present the 90% confidence range expected by simulating the posterior model many times with the instrumental setup of the coadded data.
Paper: An Intermediate-mass Black Hole Hidden behind Thick Obscuration
Authors: Peter G. Boorman, Daniel Stern, Roberto J. Assef, Abhijeet Borkar, Murray Brightman, Johannes Buchner, Chien-Ting Chen, Hannah P. Earnshaw, Fiona A. Harrison, Gabriele A. Matzeu, Ryan W. Pfeifle, Claudio Ricci, Jiří Svoboda, Núria Torres-Albà, Ingyin Zaw
Figure caption: Two-dimensional posterior contours on intrinsic 2–10 keV AGN luminosity versus line-of-sight column density. The vertical dotted–dashed line shows the upper limit on 2–10 keV luminosity predicted from the mid-infrared 6 μm luminosity, whereas the horizontal dashed line shows the Compton-thick threshold. Though the predicted intrinsic luminosities are very discrepant among different models, all converge on a Compton-thick line-of-sight column density to >99% confidence.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The influence of BH spin, BH charge, and observation inclination angle on the redshift (maximum blueshift point). Left panel: the BH charge varies from 0 to 0.5 with a step size of 0.05, while the spin is fixed at a = 0.5 and the observation angle at θ 0 = 75 deg. Middle panel: the BH spin varies from 0 to 0.98 with a step size of 0.05, while the charge is fixed at a = 0.3 and the observation angle at θ 0 = 75 deg. Right panel: the observation angle varies from 0 to 180 deg with a step size of 15 deg, while the BH charge is set to 0.2 and the spin is set to 0.8.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The redshift distribution of direct images under prograde disk. Left panel: observation angle θ 0 = 17 deg. Middle panel: observation angle θ 0 = 75 deg. Right panel: observation angle θ 0 = 150 deg. From top to bottom, the spin of the KN BH is a = 0.8, a = 0.8, and a = 0.94, with a charge of Q = 0.3, Q = 0.5, and Q = 0.3. Set the mass of the BH to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The image of the KN BH surrounded by a prograde thin accretion disk at 230 GHz. Left panel: observation angle θ 0 = 17 deg. Middle panel: observation angle θ 0 = 75 deg. Right panel: observation angle θ 0 = 150 deg. From top to bottom, the spin of the KN BH is a = 0.8, a = 0.8, and a = 0.94, with a charge of Q = 0.3, Q = 0.5, and Q = 0.3. The mass of the BH is set to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The intensity distribution of a KN BH surrounded by a prograde thin accretion disk at 230 GHz. Top panel: intensity distribution along the x-axis scenario. Bottom panel: intensity distribution along the y-axis.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The intensity distribution of a KN BH surrounded by a retrograde thin accretion disk at 230 GHz. Top panel: intensity distribution along the x-axis. Bottom panel: intensity distribution along the y-axis.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The redshift distribution of lensing images under prograde disk. Left panel: observation angle θ 0 = 17 deg. Middle panel: observation angle θ 0 = 75 deg. Right panel: observation angle θ 0 = 150 deg. From top to bottom, the spin of the KN BH is a = 0.8, a = 0.8, and a = 0.94, with a charge of Q = 0.3, Q = 0.5, and Q = 0.3. Set the mass of the BH to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The same as Figure 11, but the disk is retrograde.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The same as Figure 17, but the disk is retrograde.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The same as Figure 10, but the disk is retrograde.
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Electron-scattering cross sections in different regions of magnetosphere parameter space. The x- and y-axes represent the FRB isotropic luminosity and the distance from the magnetar, respectively. The regions where 1 < a 0 < ω  B /ω, 1 < ω  B /ω < a 0, and ω  B /ω < 1 < a 0 are marked in gray, blue, and green, respectively. The red dashed line represents the light cylinder radius, which also serves as the boundary between the blue and green regions. Scattering is most severe in the blue region, while it is relatively weak in the gray and green regions. The parameters ν = 109 Hz, B s = 1015 G, and the magnetar spin period P = 2.95 s are adopted.
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: A coordinate system established in the lab frame (left panel). An FRB is propagating along the z-axis. The electric field and magnetic field of the FRB are along the x- and y-axes, respectively. The background magnetic field is in the y–z-plane. The angle between the wavevector and the background magnetic field is θ. A coordinate system is established in the frame ﹩{K}^{{\prime} }﹩ (right panel), which is defined as a frame that slides along the background magnetic field line with a Lorentz factor ﹩{\gamma }_{f}=1/\sin \theta ﹩ in the lab frame. The FRB propagation direction is assumed to be along the ﹩{z}^{{\rm{{\prime} }}}﹩-axis. The electric field and magnetic field are along the ﹩{x}^{{\rm{{\prime} }}}﹩- and ﹩{y}^{{\rm{{\prime} }}}﹩-axes, respectively. In the frame ﹩{K}^{{\prime} }﹩, the background magnetic field has the same direction as the magnetic field of the FRB.
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: The value of ζ as a function of γ ±.
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: The motion of a test particle in an FRB. The Lorentz factor of the particle as a function of time (upper left panel). The Lorentz factor of the velocity along the field line ﹩{\gamma }_{\mathrm{bg}}\equiv {\left(1-{\beta }_{\mathrm{bg}}^{2}\right)}^{-1/2}﹩ as a function of time (upper middle panel) and its zoomed-in view (upper right panel). The trajectory of the particle in the y–z-plane (lower left panel) and in the plane perpendicular to the field line (lower middle panel). The blue dashed lines and dots indicate the direction of the field line. The distance that the particle travels along the field line with respect to time (lower right panel). Before entering the FRB, the particle has an initial Lorentz factor γ  i  = 1000 along the field line. As time goes by, the Lorentz factor corresponding to the velocity along the field line drops rapidly and finally reaches a stable value ﹩{\gamma }_{\mathrm{bg}}\approx 1/\sin \theta ﹩. The parameters a 0 = 2000 and ω  B /ω = 40 are adopted, which are equivalent to an FRB with isotropic luminosity L iso ≈ 1.3 × 1041 erg s−1 and distance from the magnetar r ≈ 4.1 × 109 cm. The other adopted parameters are θ = 10−1 rad, ν = 109 Hz, and B  s  = 1015 G.
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: The motion of a test particle in an FRB observed in the frame ﹩{K}^{{\prime} }﹩. The Lorentz factor of the particle as a function of time (upper left panel). The time evolution of the Lorentz factor of the velocity along the field line (upper middle panel) and its zoomed-in view (upper right panel). The dimensionless momentum of the particle along the field line as a function of time (lower left panel). The trajectory of the particle in the ﹩{x}^{{\prime} }\mbox{--}{z}^{{\prime} }﹩-plane (lower middle panel). The blue dots indicate the direction of the field line. The distance that the particle travels along the ﹩{y}^{{\rm{{\prime} }}}﹩-axis with respect to time (lower right panel). At the beginning, the particle has an initial Lorentz factor ﹩{\gamma }_{i}^{{\prime} }\approx 50﹩ (corresponding to γ  i  = 1000 in the lab frame) along the field line. As time goes by, the velocity of the particle along the field line drops rapidly and then nearly vanishes. The adopted parameters are ﹩{a}_{0}^{{\prime} }=2000﹩, ﹩{\omega }_{B}^{{\prime} }/{\omega }^{{\prime} }\approx 400﹩, ﹩{\theta }^{{\prime} }=\pi /2\ \mathrm{rad}﹩, and ﹩{\nu }^{{\prime} }=6.3\times {10}^{8}\ \mathrm{Hz}﹩, which are transformed from those parameters adopted in Figure 4 from relativistic transformations (Equation (19)).
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: The constraints on the value of θ as a function of distance r in various approaches. The physically allowed regions in different approaches are highlighted by different colors. The vertical dashed line represents the light cylinder radius. The horizontal dashed lines represent θ = 10−2 and 10−1 rad. The adopted parameters are ξ = 103, ζ = 10−3, ν = 109 Hz, L iso = 1042 erg s−1, B  s  = 1015 G, P = 2.95 s, and ﹩{ \mathcal D }={{ \mathcal D }}_{\mathrm{cr}}﹩.
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Three different regimes of constraints on the radiation-cone half-opening angle for various emission radii of an FRB in a magnetar magnetosphere (left panel). The orange part represents the region outside the critical transverse spatial size determined by Equation (45). The red dots represent various emission radii of FRBs. The critical radiation-cone half-opening angle as a function of the luminosity and emission radius of FRBs (right panel). The two horizontal black dashed lines represent θ  j,cr = 10−3 and 10−2 rad, respectively. The gray part represents the region outside the light cylinder. The parameters ξ = 103, ζ = 10−3, ν = 10−9 Hz, B s = 1015 G, P = 2.95 s, and θ = 10−1 rad are adopted.
Paper: Fast Radio Bursts with Narrow Beaming Angles Can Escape from Magnetar Magnetospheres
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: A schematic illustration of the motion of an electron in an x-mode FRB pulse in the lab frame. The pulse (gray) propagates at an angle θ relative to the background magnetic field (blue). The directions of the electric and magnetic fields of the pulse are marked with a green arrow. The transverse spatial size of the pulse is denoted as ﹩{ \mathcal D }﹩. In addition to the cyclotron motion, the electron is nearly sliding along the magnetic field line with a constant velocity β bg.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: SFHs for the galaxies in our sample, derived with Prospector (B. D. Johnson et al. 2021). We mark the panels with different colors to highlight galaxies with similar SFHs showing a similar trend in the [O II] spatial and kinematic maps (see Section 5.2 for more details). A different scale is used for the y-axis of the top three right-hand panels to better display the data. Light-blue shaded regions show the errors on the SFH. Time is displayed on a logarithmic scale to emphasize the recent SFH. Indeed, on a linear scale, the young bursts are so impulsive they are nearly invisible against the y-axis. The mean light-weighted age of the stellar populations younger than ∼1 Gyr is reported at the bottom right-hand of each panel. The [O II] σ map is shown for each galaxy in the upper right-hand inset as presented in Section 4.4. The color bars show the σ in km s−1.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Mg II and [O II] spatially integrated continuum-subtracted spectra for each galaxy in our sample. Left-hand panels: Weak Mg II emission and strong blueshifted absorption are observed in each galaxy. The black-solid line shows the integrated spectrum over the full extent of the nebula, and the purple-solid line shows the integrated spectrum over the nebula’s core, i.e., the central 5 × 5 central spaxels. The vertical pink band represents the spectral region used to integrate the continuum-subtracted spectrum in each spaxel used to construct the Mg II SB map. Center panels: Strong [O II] emission is observed in each galaxy. The black-solid line shows the spectrum integrated over the full extent of the nebula, and the magenta-solid line shows the total Gaussian fit to the [O II] emission doublet. Blue and orange lines show the fits to the individual [O II] doublet lines for the narrow and broad components, respectively. Right-hand panels: Same as the central figures, where here the data and fits are shown for the spectrum integrated over the core of the nebula, i.e., the central 5 × 5 central spaxels.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Left-hand panel: Outflow velocity, v, vs. light-weighted age. Center panel: [O II] radius enclosing 90% of the SB, R 90 vs. ΣSFR. Right-hand panel: Outflow dynamical time vs. light-weighted age. The filled circles represent the galaxies studied in this work and the filled star is the galaxy Makani (see legend in the first panel). The tilted line in the central panel illustrates outflow timescales that match 1:1 the light-weighted age.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: [O II] and stellar kinematics for four galaxies in our sample that show an [O II] emission velocity gradient J0944 (left-hand two panels), J1107 (second two panels), J1341 (third two panels) and J1500 (right-hand two panels). In every two panels, we show at the top the [O II] central velocity (v 50) and at the bottom the stellar v 50. All velocities of the ionized gas are relative to the systemic redshift of the source. The color bars show the velocity in km s−1. The axes are labeled in kpc from the brightest spaxel.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: [O II] kinematics for the galaxy J0826. All velocities of the ionized gas are relative to the systemic redshift of the source. We show in the top left-hand panel the [O II] central velocity (v 50); in the top right-hand panel the [O II] velocity dispersion (σ), in the bottom left-hand panel the [O II] maximum redshifted velocity (v 02); in the bottom right-hand panel [O II] maximum blueshifted velocity (v 98). All velocities of the ionized gas are relative to the systemic redshift of the source. The color bars show the velocity in km s−1. The axes are labeled in kpc from the brightest spaxel.