adsabs/AstroCLIMB huggingface dataset:
Paper: The Potential of the SPHEREx Mission for Characterizing Polycyclic Aromatic Hydrocarbon 3.3 μm Emission in Nearby Galaxies
Authors: Edward Zhang, Andreas L. Faisst, Brendan P. Crill, Hanae Inami, Thomas Lai, Youichi Ohyama, Jeonghyun Pyo, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Richard M. Feder, Yongjung Kim, Bomee Lee, Daniel Masters, Gary Melnick, Roberta Paladini, Michael W. Werner
Figure caption: Examples of simulated spectra for sources in the wide-field area (top four panels) and the deep-field area (bottom four panels). The two areas differ in the number of scans per pixel (see Section 3.2) and thus number of observations (gray points). The sources are chosen to have a detected PAH 3.3 μm band emission at z = 0.1 and z = 0.3 bracketing E(B − V) values of 0.1 and 0.5 mag. The input model is shown as a thick blue line, and intrinsic measurements are shown as gray points. We also show the measurements binned at 0.1 μm (wide field) and 600 Å (deep field) in red (errors computed from bootstrapping). The insets show the wavelength around the PAH 3.3 μm band, as well as a fit (magenta line) to the binned data. We note that the significant increase in scatter around 3.45 μm rest frame (z = 0.1) is due to a lower sensitivity in detectors 5 and 6.
Paper: The Potential of the SPHEREx Mission for Characterizing Polycyclic Aromatic Hydrocarbon 3.3 μm Emission in Nearby Galaxies
Authors: Edward Zhang, Andreas L. Faisst, Brendan P. Crill, Hanae Inami, Thomas Lai, Youichi Ohyama, Jeonghyun Pyo, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Richard M. Feder, Yongjung Kim, Bomee Lee, Daniel Masters, Gary Melnick, Roberta Paladini, Michael W. Werner
Figure caption: Summary of SFR vs. observed K-band magnitude (proxy for stellar mass; contours) parameter space for three different redshift bins in which SPHEREx is able to measure the PAH 3.3 μm emission band (indicated by the light-red hatched region). The hexagonal background shows galaxies in the COSMOS field and from SDSS in the given redshift bins color-coded by average stellar mass.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Impact of the dipole magnetic field strength Bd and magnetar initial spin period Pi on supernova bolometric LCs. The dashed lines represent the central-engine heating rate.
Paper: The Potential of the SPHEREx Mission for Characterizing Polycyclic Aromatic Hydrocarbon 3.3 μm Emission in Nearby Galaxies
Authors: Edward Zhang, Andreas L. Faisst, Brendan P. Crill, Hanae Inami, Thomas Lai, Youichi Ohyama, Jeonghyun Pyo, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Richard M. Feder, Yongjung Kim, Bomee Lee, Daniel Masters, Gary Melnick, Roberta Paladini, Michael W. Werner
Figure caption: Comparison of input and measured PAH 3.3 μm total flux for the wide-field (top panel) and deep-field (bottom panel) survey configuration. The gray areas show an error of 30% (dark gray) and a factor of two (light gray) around the 1-to-1 line (dashed). The dashed horizontal lines show the median 1σ detection limits.
Paper: The Potential of the SPHEREx Mission for Characterizing Polycyclic Aromatic Hydrocarbon 3.3 μm Emission in Nearby Galaxies
Authors: Edward Zhang, Andreas L. Faisst, Brendan P. Crill, Hanae Inami, Thomas Lai, Youichi Ohyama, Jeonghyun Pyo, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Richard M. Feder, Yongjung Kim, Bomee Lee, Daniel Masters, Gary Melnick, Roberta Paladini, Michael W. Werner
Figure caption: Impact of different model assumptions (SFH, dust, and AGN) on the PAH 3.3 μm emission flux (resulting change with respect to the basis model in dex).
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Impact of the mass of 56Ni MNi on supernova bolometric LCs.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Impact of the heat source distribution. The heating is uniformly mixed out to xheat on supernova bolometric LCs.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Radial temperature profiles T(r) from our time-dependent diffusion model, evaluated at multiple epochs as indicated by the color bar.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Impact of the ejecta mass Mej and initial kinetic energy EK on supernova bolometric LCs.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Bolometric LC of SN 1993J compared with our TransFit model. The open circles with error bars represent the observed bolometric data from M. W. Richmond et al. (1994). The solid black line shows the best-fit model, while the shaded blue region indicates the 1σ credible interval derived from the MCMC posterior. The individual model components are also shown: the dashed orange curve is the contribution from shock-cooling emission alone (assuming MNi = 0), while the dashed green curve is the pure 56Ni heating component (assuming ETh,in = 0). The combined model successfully reproduces both the initial shock-cooling peak and the subsequent radioactively powered main peak.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Left: normalized ejecta density profiles ηej(x) vs. normalized radius ﹩r/{R}_{{\rm{\max }}}﹩ for five models: uniform, exponential, broken power law, W7, and DDT100. Right: corresponding bolometric LCs. At default parameters, the peak luminosity and decline rate are nearly independent of the density profile; only the early rise time and late-time tail show modest variations. The dashed black line indicates the instantaneous radioactive heating rate.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Corner plot showing the posterior probability distributions for the physical parameters of SN 1993J obtained with our MCMC analysis using TransFit. The diagonal panels display the marginalized one-dimensional distributions for each parameter, with vertical dashed lines indicating the median and the central 68% credible interval (1σ).
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Our TransFit model fits to the multiband optical LCs of SN 2007gr. The points show the observational data from D. J. Hunter et al. (2009), while the solid lines and shaded regions represent our best-fit models and their 1σ uncertainties, respectively. The LCs are vertically shifted for clarity as noted in the legend.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Corner plot showing the posterior probability distributions for the physical parameters of SN 2007gr obtained with our MCMC analysis using TransFit.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Theoretical LC and temperature evolution. Top: absolute magnitudes in the u, g, r, i, and z bands (offset vertically for clarity) as a function of time. Bottom: evolution of the effective temperature Teff (solid black line) alongside the band-specific temperatures at peak luminosity (dashed horizontal lines).
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Compares bolometric LC predictions from TransFit (solid blue line), the one-zone model (dotted green), and the Arnett model (dashed orange). The left panel shows a radioactive-decay-powered scenario, while the right panel illustrates a magnetar-powered scenario.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Impact of the the initial thermal energy ETh,in and initial progenitor radius R0 on supernova bolometric LCs.
Paper: TransFit: An Efficient Framework for Transient Light-curve Fitting with Time-dependent Radiative Diffusion
Authors: Liang-Duan Liu, Yu-Hao Zhang, Yun-Wei Yu, Ze-Xin Du, Jing-Yao Li, Guang-Lei Wu, Zi-Gao Dai
Figure caption: Impact of the opacity κ on supernova bolometric LCs.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: The [O III] λ5007 profiles across different spatial regions in Mrk 110. We chose these regions to display the diversity in the [O III] line profiles across the FoV. The left panel is a white light image generated by collapsing the data cube over a spectral region centered on the [O III] λ5007 line. The horizontal axis has been stretched to account for the rectangular pixel sizes in the reduced data cube. The y-axis of the FoV corresponds to a PA of 80°, which was the orientation of KCWI when we observed this object. The second object near region E3 is a foreground star. In the right panel, we have marked the core component of [O III] (magenta), which is used in calculations of the bulge velocity dispersion σgas. Velocities displayed are measured relative to the host galaxy redshift.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: Optical HST (SDSS for Mrk 315) image together with three moment maps (i.e., surface brightness, centroid velocity, and velocity dispersion) of the ionized gas component, and the kinematic maps (v⋆, σ⋆) of the stellar component, for five objects in the sample as derived from our KCWI data. Images used in the first column are the same as those from Figure 1, but resampled with North up and East to the left. The red plus sign denotes the location of the AGN point source, as derived from the peak emission in the imaging data. In other panels, the black plus sign denotes the location where the AGN continuum emission is brightest. The surface brightness is plotted in units of ﹩{\mathrm{log}}_{10}{S}_{\,\rm{[O III]}\,}﹩, while velocity and dispersion are plotted in units of km s−1. The magenta and green lines on the velocity maps denote the measured PA of [O III] and the stars, respectively. In each velocity map, the thicker line corresponds to the PA of the velocity field shown in that panel. We masked out several spaxels in Zw 535–012 and Mrk 110, where the spectra were dominated by foreground stars.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: Spectral decompositions illustrating the variety in emission profiles across our sample. The spectral decompositions are for single spaxels near the nucleus, where AGN features (e.g., broad emission lines, power-law continuum, Fe II blends) and the host galaxy could be reliably constrained. Emission associated with the narrow-line region is displayed in blue, host galaxy templates in green, Fe II templates in gray, and power laws as red dashed lines. Broad emission lines are colored separately, with Hβ in pink, He II in cyan, and He I in orange.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: Surface brightness and ionized gas kinematics for the four galaxies with separable components. Component G1 refers to the narrow core of the [O III] profile, while G2 refers to the broad asymmetric wing.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: The KCWI FoV plotted as rectangles over optical imaging data from HST (blue) and SDSS (green) for each of the targets. The red plus sign represents the position of the AGN point source, corresponding to the peak of the galaxy emission. North is up and East is to the left.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: Same as Figure 5, but for the remaining objects in the sample. The masked regions in RX J2044.0+2833 correspond to foreground stars located ≲5″ south of the nucleus.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: Comparison of [O III] line width and σ⋆ for the flux-weighted dispersions (blue circles, left panel) and the fits to the aperture-summed spectra (purple squares, right panel) within an elliptical aperture. Data points based on measurements on local Seyfert 1 galaxies from V. N. Bennert et al. (2018) are shown as green diamonds. We adopt the velocity dispersion values of the two-Gaussian fit to [O III] (σ[O III],D) for σgas. The dashed line is the 1:1 relation. For both methods of measuring the velocity dispersion, the majority of galaxies fall below the 1:1 line, suggesting that σgas underestimates σ⋆.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: [O III]/Hβ flux ratio (top) and [O III] surface brightness (bottom) as a function of projected distance from the nucleus. The black points represent the flux ratio or surface brightness in a spatial bin whose centroid is located some distance from the nucleus. Each red point denotes the mean flux ratio for all black points in a given 0.25 kpc bin from the nucleus. The red error bars are the standard deviations calculated from all the black points in a given distance bin. The blue dashed line represents the threshold of [O III]/Hβ = 3 or S[O III] = 10−16 erg s−1 cm−2 arcsec−2.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: The RNLR − L[O III] relation for our sample. Our data points based on the [O III]/Hβ ratio are plotted as black circles and gray arrows (for lower limits), with the best-fit relation as the solid black line. Our points based on the [O III] surface brightness cutoff are plotted as blue squares, with the best-fit relation as the dotted blue line. The pink lines connect measurements associated with the same galaxy. For comparison, we plot the A. Trindade Falcão et al. (2024) relation based on HST imaging data as the green dotted–dashed line, and the J. Chen et al. (2019) relation from SDSS/MaNGA integral-field data as the solid red line.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: MBH–σ data points with [O III] line widths (blue squares) and stellar velocity dispersions (orange stars) compared against data used in the analysis of J.-H. Woo et al. (2015). The dashed line is the best-fit MBH–σ⋆ relation to a joint sample of quiescent galaxies from J. Kormendy & L. C. Ho (2013) and reverberation-mapped AGN in J.-H. Woo et al. (2015). Plots in the top row correspond to the flux-weighted measurements σw, while those in the bottom row correspond to σa. The green diamonds are from the RM sample, while the gray squares correspond to the quiescent sample. Our σgas tend to be lower than the range of the literature values for a fixed black hole mass.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: [O III] Surface brightness maps of Mrk 110 and Mrk 315 within 60 km s−1 bins. The inner 2″ of Mrk 110 are masked to better display the extended [O III] emission. Similar to Figures 5 and 6, surface brightness is plotted in units of ﹩{\mathrm{log}}_{10}{S}_{[{\rm{O}}\ {\rm{III}}]}﹩.
Paper: Spatially Resolved [O III] Emission Line Kinematics of Reverberation-mapped Active Galactic Nuclei with the Keck Cosmic Web Imager
Authors: Raymond P. Remigio, Vivian U, Aaron J. Barth, Nico Winkel, Vardha N. Bennert, Tommaso Treu, Matthew A. Malkan, Sebastian Contreras, Peter R. Williams, Jordan N. Runco, Liam Hunt
Figure caption: Comparison between the flux-weighted and aperture-summed measurements of velocity dispersion for the gas (left panel) and the stars (right panel). The dashed line represents equality between σw and σa. We denote targets where σ measurements between both methods are notable outliers from the 1:1 relation.
Paper: The Dust Echo Emission of Fast Blue Optical Transients and Application to the Near-infrared Excess of AT 2018cow
Authors: Jing-Yao Li, 京谣 李, Yun-Wei Yu, 云伟 俞, Liang-Duan Liu, 良端 刘, Ming-Yan Xiao, 明燕 肖
Figure caption: Left: the size evolution of dust grains for different initial sizes. The solid, dotted–dashed, dashed, and dotted lines represent the distances to the FBOT source of 2 × 1016 cm, 8 × 1016 cm, 3 × 1017 cm, and 1 × 1018 cm, respectively. Right: the evaporation radius for different size of dust grains, inside which the dusts of a size less than a can be evaporated completely within a short time.
Paper: The Dust Echo Emission of Fast Blue Optical Transients and Application to the Near-infrared Excess of AT 2018cow
Authors: Jing-Yao Li, 京谣 李, Yun-Wei Yu, 云伟 俞, Liang-Duan Liu, 良端 刘, Ming-Yan Xiao, 明燕 肖
Figure caption: Left: fitting to the multiwavelength light curves of AT 2018cow. Right: a comparison between the model-predicted spectra and observational ones at seven time points. The dashed and dotted lines represent the FBOT and dust echo emission, respectively.
Paper: The Dust Echo Emission of Fast Blue Optical Transients and Application to the Near-infrared Excess of AT 2018cow
Authors: Jing-Yao Li, 京谣 李, Yun-Wei Yu, 云伟 俞, Liang-Duan Liu, 良端 刘, Ming-Yan Xiao, 明燕 肖
Figure caption: The bolometric light curves of the FBOT (solid blue) and dust echo (solid red) emission for parameters derived from the fitting of AT 2018cow. The dotted lines show the UV (1015–17 Hz) and IR (1011–13 Hz) components of the FBOT. The dashed line is the echo of the FBOT emission only before its peak.
Paper: The Dust Echo Emission of Fast Blue Optical Transients and Application to the Near-infrared Excess of AT 2018cow
Authors: Jing-Yao Li, 京谣 李, Yun-Wei Yu, 云伟 俞, Liang-Duan Liu, 良端 刘, Ming-Yan Xiao, 明燕 肖
Figure caption: The schematic diagram of the model (not to scale).
Paper: The Dust Echo Emission of Fast Blue Optical Transients and Application to the Near-infrared Excess of AT 2018cow
Authors: Jing-Yao Li, 京谣 李, Yun-Wei Yu, 云伟 俞, Liang-Duan Liu, 良端 刘, Ming-Yan Xiao, 明燕 肖
Figure caption: Parameter posteriors of the fittings of AT 2018cow.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: Full sample of MaNGA galaxies with spatially offset BLRs coincident with optical detections from the SDSS imaging. For each galaxy, the panels contain (from left to right) the SDSS g + r + i color composite images (with the MaNGA IFS fiber bundle hexagon shown in magenta), the MaNGA IFS maps and BPT classifications using the [N II]-based criteria (pink = “AGN,” orange = “composite,” and green = “star-forming”) and [S II]-based criteria (pink = “Seyfert,” purple = “LINER,” and green = “star-forming”), and the [N II] and [S II] BPT diagrams. In the BPT plots, the solid red lines denote the pure AGN demarcation, while the dashed red lines denote the pure star formation ([N II]) and LINER ([S II]) demarcations. The log-scale density map denotes spaxels from the full MaNGA map (only for spaxels with BPT classifications). The cyan dots denote the subset of the spaxels associated with the BLRs, selected to be within a box (centered on the BLR centroid) of size 2 × σspax (to include extended NLR emission around the BLR) but not including the spaxels that have detected broad emission lines (since the MaNGA pipeline does not account for them). The BLR positions are indicated by the cyan circles with radii of 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 + σspax (radius used for matching with optical counterparts; Section 3). The white scale bar indicates 4″.