adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for Converging Flows of Atomic Gas onto a Molecular Cloud
Authors: Mark Heyer, Paul F. Goldsmith, Robert Simon, Rebeca Aladro, Oliver Ricken
Figure caption: Images of [C II], 12CO, and H I 21 cm line emission. From left to right: integrated intensity; longitude–velocity image; latitude–velocity image. The longitude–velocity images show spectra averaged over Galactic latitudes 4.°213 to 4.°303 and the latitude–velocity images show spectra averaged over Galactic longitudes 109.°806 to 109.°900. (Top row) representations of [C II] emission. The scaling of the [C II] integrated intensity image begins at 0.75 K km s−1 that corresponds to 3σ uncertainty. Pixels with values below this threshold are dark and uniform. (Middle row) representations of 12CO emission. The contours show the SCUBA 850 μm emission observed by Di Francesco et al. (2008). The contour levels are 0.15, 0.25, 0.35, 0.45 Jy beam−1. (Bottom row) representations of H I 21 cm emission.
Paper: Searching for Converging Flows of Atomic Gas onto a Molecular Cloud
Authors: Mark Heyer, Paul F. Goldsmith, Robert Simon, Rebeca Aladro, Oliver Ricken
Figure caption:  PDR Toolbox models of line emission. (a) Image of the logarithm of [C II] intensities over a range of radiation fields and gas densities. The red lines show contours of the logarithms of the observed 3σ detection limit (−5.14) and maximum [C II] intensity (−4.14) (in units of ergs s−1 cm−2 sr−1). (b) Same as (a) for 12CO emission. Contours are the logarithm of the observed 3σ detection limit (−7.98) and maximum intensity of 12CO emission (−7.02). (c) Same as (a) for the ratio [C II]/12CO. Blue lines denote the logarithms of the 3σ (2.42) and maximum (3.41) ratio values. (d) Same contours in (a), (b), and (c). The gray shading marks subset area bounded by the contours of acceptable values of I C II , I  CO , and I CII/I CO. This area provides the range of model radiation field and gas density values that are consistent with the observations.
Paper: Searching for Converging Flows of Atomic Gas onto a Molecular Cloud
Authors: Mark Heyer, Paul F. Goldsmith, Robert Simon, Rebeca Aladro, Oliver Ricken
Figure caption: [C II] spectra averaged over 60 pixels along the horizontal (left) and vertical (right) cuts of the cross map. Blueshifted wing emission over the interval −50 to −43 km s−1 (filled in gray) is evident. Angular offsets from the center of the map are shown in each spectrum. The measured brightness temperatures and velocity overlap with the absorption feature shown in Figure 2 suggest that this [C II] wing emission reflects CNM gas that is present throughout the BKP 7323 cloud.
Paper: Searching for Converging Flows of Atomic Gas onto a Molecular Cloud
Authors: Mark Heyer, Paul F. Goldsmith, Robert Simon, Rebeca Aladro, Oliver Ricken
Figure caption: H I 21 cm spectra at the position of the extragalactic source G109.65+4.24 (filled in gray) and at the offset position at l = 109.°70, b = 4.°24 . The absorption feature occurs over the velocity interval [−48,−42] km s−1 and indicates the presence of cold, neutral, atomic gas in the vicinity of the BKP 7323 molecular cloud.
Paper: Searching for Converging Flows of Atomic Gas onto a Molecular Cloud
Authors: Mark Heyer, Paul F. Goldsmith, Robert Simon, Rebeca Aladro, Oliver Ricken
Figure caption:  12CO spectrum averaged over the 0.°1  ×  0.°1 field shown in Figure 1. The solid horizontal line marks T mb = 0 and the horizontal dotted lines mark T mb = ±3σ. No 12CO emission is found within a 3σ limit of 0.18 K over the velocity interval [−50, −44] km s−1 (shaded in blue) that coincides with the blueshifted wing of [C II] emission.
Paper: Searching for Converging Flows of Atomic Gas onto a Molecular Cloud
Authors: Mark Heyer, Paul F. Goldsmith, Robert Simon, Rebeca Aladro, Oliver Ricken
Figure caption: Atomic hydrogen volume densities over the velocity interval [−50, −43] km s−1 derived from Equation (2) for each average spectrum shown in Figure 3. The blue and red points correspond to average spectra long the horizontal and vertical cuts, respectively.
Paper: Searching for Converging Flows of Atomic Gas onto a Molecular Cloud
Authors: Mark Heyer, Paul F. Goldsmith, Robert Simon, Rebeca Aladro, Oliver Ricken
Figure caption: Integrated H I 21 cm line emission over the velocity intervals (left) [−50,−43], (middle) [−43,−38], and (right) [−38,−31] km s−1. The black contour is the 5 K km s−1 isophote of CO J = 1–0 emission. The white contour in the [−50,−43] km s−1 image corresponds to an atomic column density of 8 × 1020 cm−2.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption:                         Type IV: the spectral evolutions of flares are hard-to-soft-to-hard (anti-intensity tracking). Symbols are as in Figure 1.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption: The distribution of I (the ratio of the maximum value to the minimum value of the spectral index).
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption: The spectral evolution intensity I vs. peak flux F peak.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption: The spectral evolution intensity I vs. peak time T peak.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption: The spectral evolution intensity I vs. FWHM.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption: The distribution of spectral index evolution slopes.
Paper: The Spectral Evolution Patterns and Implications of Gamma-Ray Burst X-Ray Flares
Authors: Lian-Zhong Lü, En-Wei Liang, Bertrand Cordier
Figure caption:                         Type III: the spectral evolutions of flares are soft-to-hard. Symbols are as in Figure 1.
Paper: Searching for Propionamide (C2H5CONH2) toward Sagittarius B2 at Centimeter Wavelengths
Authors: Caden Schuessler, Anthony Remijan, Ci Xue, Joshua Carder, Haley Scolati, Brett McGuire
Figure caption: Graphical representation of possible molecular structures by subsequent methyl (CH3) and/or amine (NH2) addition starting with formaldehyde (H2CO). Note that these are only illustrations of structures and not true representations of possible formation routes.
Paper: Searching for Propionamide (C2H5CONH2) toward Sagittarius B2 at Centimeter Wavelengths
Authors: Caden Schuessler, Anthony Remijan, Ci Xue, Joshua Carder, Haley Scolati, Brett McGuire
Figure caption: Absorption features of NH2CHO detected in the PRIMOS data (black trace). The best-fit model to the PRIMOS observations toward Sgr B2(N), including all velocity components, are shown with red traces with a best-fit T ex of 5.8 K and N T of ∼8.5 × 1014 cm−2. Simulated spectra of the three velocity components are show in: blue (the LMH region with a velocity of +63 km s−1 and a source size of 3″), purple (the K6 region with a velocity of +63 km s−1 and a frequency-dependent source size), and cyan (the K5 region with a velocity of +82 km s−1 and a source size of 11″), as described in Section 3.1. Transition quantum numbers and upper state energy levels (in kelvin) are at the bottom of each spectrum.
Paper: Searching for Propionamide (C2H5CONH2) toward Sagittarius B2 at Centimeter Wavelengths
Authors: Caden Schuessler, Anthony Remijan, Ci Xue, Joshua Carder, Haley Scolati, Brett McGuire
Figure caption: The observed and synthetic spectra of C2H5CONH2. Simulated C2H5CONH2 absorption features (blue trace) overlaid on the PRIMOS observations (black trace) toward Sgr B2(N). A single velocity component of +64 km s−1 was used to model the transitions. The quantum numbers and upper state energy of each transition are shown. Nearby transitions belonging to other species are labeled. The synthetic spectra for the Sgr B2(N) component (blue trace) were generated from the physical conditions and observing parameters described in Section 3.2, that is, T ex = 5.8 K, source size = 20″, N T ∼ 1.8 × 1014 cm−2.
Paper: Searching for Propionamide (C2H5CONH2) toward Sagittarius B2 at Centimeter Wavelengths
Authors: Caden Schuessler, Anthony Remijan, Ci Xue, Joshua Carder, Haley Scolati, Brett McGuire
Figure caption: Diagram of the potential energy surface for the formation routes to propionamide starting from formamide and the ethyl radical (blue) and acetamide and the methyl radical (red). All stationary points are labeled by their energy in kJ mol−1 relative to the products, propionamide and a hydrogen atom.
Paper: Using Gravitational Waves to Distinguish between Neutron Stars and Black Holes in Compact Binary Mergers
Authors: Stephanie M. Brown, Collin D. Capano, Badri Krishnan
Figure caption:                     ﹩\mathrm{ln}{ \mathcal B }﹩ for all combinations of parameters and detectors as a function of the signal-to-noise ratio. The right and left plots correspond to the constant and variable equation of state cases. In each plot, the right panel shows the results for the maximum likelihood equation of state and the left panel shows the stiff equation of state. The marker color corresponds to the detector, and the marker shape indicates the mass of the black hole. The black horizontal line shows the cutoff of ﹩\mathrm{ln}{ \mathcal B }=10﹩.
Paper: Using Gravitational Waves to Distinguish between Neutron Stars and Black Holes in Compact Binary Mergers
Authors: Stephanie M. Brown, Collin D. Capano, Badri Krishnan
Figure caption: IMRPhenomNSBH and SEOBNRv4_ROM_NRTidalv2_NSBH waveform strain amplitude as a function of frequency plotted along with the Cosmic Explorer 1 amplitude spectral density. Both panels show waveforms with a black hole mass of 20 M ⊙. The red line corresponds to the Λ = 0 case (the waveform of a binary black hole; Matas et al. 2020), and the gray line corresponds to a waveform with a stiff equation of state (Λ = 369). The top panel shows unphysical dependence of the postmerger amplitude on Λ.
Paper: Using Gravitational Waves to Distinguish between Neutron Stars and Black Holes in Compact Binary Mergers
Authors: Stephanie M. Brown, Collin D. Capano, Badri Krishnan
Figure caption: Comparison between the IMRPhenomD_NRTidal, IMRPhenomNSBH, and SEOBNRv4_ROM_NRTidalv2_NSBH waveform approximants. For each detector, the variable equation of state analysis is on the left (circle marker) and the constant equation of state analysis is on the right (square marker). Each point corresponds to the average value of 10 runs with different noise realizations, and the error bars are 2 standard deviations. The horizontal black line indicates the cutoff of ﹩\mathrm{ln}{ \mathcal B }=10﹩.
Paper: Using Gravitational Waves to Distinguish between Neutron Stars and Black Holes in Compact Binary Mergers
Authors: Stephanie M. Brown, Collin D. Capano, Badri Krishnan
Figure caption: Natural Log Bayes factor plotted as a function of black hole mass for all six detectors considered using the IMRPhenomNSBH waveform approximant. All data points are at d = 40 Mpc and have a stiff equation of state (Λ = 369).
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Solar neutrino flux (left) and components defining the neutrino flux observed in a telescope from the solar disk at θ  z  = 135° and atmospheric background at the same zenith inclination (right).
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Maximum neutrino flux from DM annihilation consistent with the bounds on ﹩{\sigma }_{\chi N}^{\mathrm{SI}}﹩ (left) and ﹩{\sigma }_{\chi N}^{\mathrm{SD}}﹩ (right) from direct searches for the three annihilation channels that we have considered.
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Gamma and neutron fluxes (left) and integrated CR shadow from the solar disk (right); the dots correspond to the HAWC observation (Enriquez-Rivera & Lara 2015).
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Total neutrino flux from the solar disk versus atmospheric background for the Sun in two different zenith inclinations (left). Signal to background ratio for ν  e  and for the sum of all flavors (right).
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Gamma-ray flux from the solar disk (data from Fermi-LAT; Linden et al. 2018).
Paper: The Solar Disk at High Energies
Authors: Miguel Gutiérrez, Manuel Masip, Sergio Muñoz
Figure caption: Muon shadow of the Sun at different muon energies (left) or slant depths (right).
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: A demonstration of the detectability of contraction in nearby Sag-like systems. The figure is based on Au16-9, which is similar to the left plot of Figure 6 but shows the ﹩{v}_{y}^{\prime} ﹩ velocity component. Each bin contains 300 star particles. The left panel is based on bound member stars without including observational errors. Observational errors are incorporated in the middle panel. In the right panel, observational errors are included and tracers are selected according to their kinematics, which includes some unbound particles in the outskirts. We only show the ﹩y^{\prime} ﹩ component of the tangential velocities along the major and minor axes of the dwarf. The black horizontal dashed lines of y = 0 are to guide the eyes.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Red circles denote besting-fitting vs. true masses within 150 pc. The true masses are obtained by extrapolating the true density profiles to the very center based on the double power-law functional form. The best-fitting mass within 150 pc is based on tracer dynamics beyond 185 pc, which is the softening scale of the simulation at z = 0. Black empty triangles are best-fitting vs. true masses between 200 and 300 pc, which are exactly the same as the red circles in the left plot of Figure 2. Red circles with a green star on top denote star-forming dwarf systems with prominent galactic winds. Red circles with a blue diamond on top denote dwarfs with no zero but low star formation rates, and we do not see prominent galactic winds for them. Red circles with a cyan square on top denote nearby Sag-like systems. The y- and x-axes errors reflect the 1σ uncertainties of the best fits and of the extrapolated inner profiles. Errors for the black empty triangles are comparable to or smaller than the symbol size, and thus are not shown.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Similar to Figure 4. Green dots with error bars denote the true total density profiles of the six Sag-like systems, and magenta solid curves denote the best fits based on the double power-law functional form for the underlying potential (errors not modeled). These are exactly the same as in Figure 4. We further include realistic observational errors (1–10 km s−1 of errors in line-of-sight velocities and Gaia DR3 proper motion and parallax errors), and the tracer stars are selected according to their difference in kinematics with respect to the dwarf centers (see Section 2.2 for details). Blue dashed curves denote the best fits based on tracer star particles selected after including the observational errors. Cyan and yellow dashed curves denote best fits based only on line-of-sight velocities and only on proper motions, respectively, with observational errors included.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: A demonstration of the detectability of outflows in a dwarf at a distance of ∼130 kpc. The figure is based on ∼4000 wind particles in Au23-2. Each bin contains 300 particles. Observational errors are included in the right plot, but not in the left plot. We only show the ﹩y^{\prime} ﹩-component tangential velocities along the major and minor axes of the dwarf, and the trend is the same for the ﹩x^{\prime} ﹩-component tangential velocities. The black dots show prominent expansions, while the green dots show some rotations. The black horizontal dashed line at y = 0 is to guide the eye.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: Comparison of the predictions from the extended-medium model of Lee & Jokipii (1975b) with computed autocorrelation functions for our 12 pulsars. The predictions are plotted as solid lines for indices of α corresponding to the best-fitting models. The ACFs are plotted as data points with different symbols for each of the pulsars listed on the upper right.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: The true inner slopes vs. the true (left) and best-fitting (right) masses enclosed within 150 pc. The true inner slopes and true masses within 150 pc are computed by extrapolating the actual density profiles down to the very center, using a double power-law function. The best-fitting mass within 150 pc is based on tracer dynamics beyond 185 pc. The meanings of the different symbols are the same as those in Figure 12.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: Dynamic spectra of four pulsars analyzed in this paper. The color-coded intensity as a function of time and frequency is given in arbitrary units in the bar on the right side of each spectrum.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Similar to Figure 10, but shows the results after incorporating CSST proper motion errors for only Au16-9.
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption: [O III]λ λ4960, 5008 (left) and [S II]λ λ6718, 6733 (right) emission with the exposure-corrected 0.7–2 keV Chandra contours (red) and Hα + [N II]λ6584 contours (blue) overlaid. The position of the centroid of the optical host is indicated with a red cross. The 1 arcsec2 extraction regions, L, C, F1, and F2, for the BPT diagram in Figure 5 are shown as black dashed squares. Chandra contours were smoothed with a 1.5″ Gaussian kernel radius and drawn in red at 0.25  ·   10−15 erg cm−2 s−1. Hα + [N II]λ6584 contours were drawn at 5, 10, 20, 50, and 100 times the rms. Region L marks the region co-spatial with the northeastern radio lobe.
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption: Hα + [N II]λ6584 flux in velocity bins of 100 km s−1, with 8.4 GHz VLA (black) and exposure-corrected 0.7–2 keV Chandra (blue) contours overlaid. MUSE images have a pixel size of 0.″2 pixel−1. 8.4 GHz VLA contours were drawn at 5, 20, and 50 times the rms level of the background. Chandra contours were smoothed with a 1.″5 Gaussian kernel radius and drawn in red at 0.25  ·  10−15 erg cm−2  s−1. The centers of the velocity bins are shown on the top right corners. The main features are labeled in the figures, with L denoting the region co-spatial with the northeastern radio lobe, F1 and F2 denoting the blue and red filaments that appear to surround the southwestern radio lobe, A being the arched emission that appears to trace the inner edge of the X-ray cavity, F3 marking an additional filament not co-spatial with the X-ray cavity, and R being the region polluted by the redward component.
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption: Location of 3CR 196.1 regions core, northeastern radio lobe and blue and red filaments (C, L, F1 and F2, respectively) in the BPT diagnostic diagrams. The size of the regions was chosen to match the seeing of MUSE observations (i.e., ∼1″). The extraction regions are shown in Figure 4. The red solid curves represent the Kewley et al. (2001) theoretical upper bound for pure star formation, the red straight line shows the Kewley et al. (2006) separation between AGN and LINERs, while the dashed red curve in the [N II]λ6584 BPT is the Kauffmann et al. (2003) empirical classification separating star-forming galaxies and AGN. Contours represent the isodensities of all Sloan Digital Sky Survey Data Release 7 emission line galaxies (Capetti & Baldi 2011). Extended ionized gas structures in 3CR 196.1 have an ionization state compatible with the LINER region of the BPT diagnostic diagrams, while the ionization state at the optical host position is compatible with Seyfert-like ionization.