adsabs/AstroCLIMB huggingface dataset:
Paper: Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
Authors: N. B. Xiang, X. H. Zhao, L. H. Deng, F. Y. Li, Y. J. Wang, X. W. Tan
Figure caption: Global wavelet power spectra (solid line) and the 99.9% confidence level (dashed line) of the IMFs of three typical examples of the daily radio flux at 245 (left panel), 2695 (middle panel), and 8800 (right panel) MHz during the considered time interval.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Subaru spectra (this work) scaled to the AKARI and Spitzer spectra (S. Baba 2018; S. Baba et al. 2018) of U5101, N4418, and IR08572 NW. The spectra of IR08572 NW are reprinted from S. Onishi et al. (2021). The low-resolution spectra of AKARI (R ∼ 160) and Spitzer (R ∼ 80) and the Subaru spectra, which are convolved to R ∼ 160 and flux scaled, are colored blue, green, and red, respectively. The dashed black lines and orange dots are, respectively, the continuum determined from the AKARI and Spitzer spectra and the pivots used to estimate it. The adopted continuum values for IR08572 NW and N4418 are the same as those of S. Baba et al. (2018) and S. Baba (2018), respectively, whereas the continuum of U5101 is not. After this flux-scaling process, we rescaled the flux levels of N4418. (See the text for the details.)
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Derived spectra of IR01250 and U5101 normalized with the continuum (top panel) and the telluric transmission (bottom panel). Top panel: normalized flux values of each target are shown as a solid blue line, and flux errors are shown as a solid orange line. The continuum level is unity. The rest wavelength of the HI Pfβ and H2 v = 0 → 0 S(9) lines is denoted by the vertical olive-green arrows. The excluded bad data points with large flux error or small telluric transmission are colored gray. (See text for the thresholds.) The rest wavelength of the CO rovibrational absorption lines is denoted by the vertical arrows. Note that the wavelength range of ∼4.53–4.62 μm has not been observed and has no data points in U5101. Bottom panel: telluric transmission at the corresponding wavelength ranges corrected by the redshift.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Schematic illustration of the geometry of the dust-sublimation layer (the continuum source) and the absorbing clumps that cause CO rovibrational absorption lines (reprinted from S. Onishi et al. 2021).
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Adopted continuum of IR01250. The observed high-dispersion spectrum and that convolved to R ∼ 180 are colored blue and red, respectively. The dashed black lines and orange dots represent the adopted continuum and the pivots used to estimate it, respectively.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Decomposed spectrum of the gaseous CO rovibrational absorption lines in IR01250. The abscissa is the rest wavelength. The ordinate is the normalized flux. Components (a)–(d) and their sum are denoted with red, orange, green, dark-blue, and sky-blue lines, respectively. In addition, component (d) of 13CO absorption lines are shown with dark-blue dashed lines. The black and purple arrows denote the rest wavelength of each 12CO and 13CO rovibrational transition, respectively. Because the 13CO transitions are detected only in component (d) with J ≤ 19, the purple arrows denote the transitions in the J range. The HI Pfβ and H2 v = 0 → 0 S(9) emission lines are colored olive-green. Decomposed spectrum of the gaseous CO rovibrational absorption lines in IR01250. The abscissa is the rest wavelength. The ordinate is the normalized flux. Components (a)–(d) and their sum are denoted with red, orange, green, dark-blue, and sky-blue lines, respectively. In addition, component (d) of 13CO absorption lines are shown with dark-blue dashed lines. The black and purple arrows denote the rest wavelength of each 12CO and 13CO rovibrational transition, respectively. Because the 13CO transitions are detected only in component (d) with J ≤ 19, the purple arrows denote the transitions in the J range.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Population diagrams of each velocity component inside the sphere of influence mentioned in Section 5.1.2. The column densities, whose upper limits are set, are colored in gray. The blue solid lines denote the best-fit RADEX models with the median value of the posterior distribution of each parameter, and the orange areas illustrate 95% confidence bands. We herein adopt the RADEX model because it is preferable to a simple two-temperature model to reproduce the level populations. See Section 5.2.2 for the details.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Velocity spectra and decomposed velocity components of some gaseous 12CO rovibrational transitions as representative examples. The transitions shown here are selected so that low and high rotational levels are covered, and all detected velocity components are visible in the figures for each target. The abscissa is the LOS velocity relative to the systemic velocity (V − V sys). The ordinate is the normalized flux. Components (a), (b), (c), (d), and (e) are shown with red, orange, green, dark-blue, and pink lines, respectively. The sum of the detected velocity components are shown with sky-blue lines. The features other than gaseous 12CO are colored gray. In particular, the absorption transitions of 13CO are shown with dashed lines, and the emission transition of H2 v = 0 → 0 S(9) (visible in P(3) panel of IR01250) and the absorption transitions of ice are shown with solid lines.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Spectra of the R-branch (red) and P-branch (blue) in each rotational level. In principle, we show spectra in rotational levels J = 0, 1, 8, 12, and 16, so that they cover the entire range of J observed toward all targets in common. (See Table 2 for observed J ranges for each target.) When the rotational level is unobservable from the ground due to the telluric transmission, its adjacent levels are shown here. The abscissa is the LOS velocity relative to the system. The ordinate is the normalized flux. The vertical dashed lines denote the visually inspected valley position of each velocity component: V − V sys ∼ (−200, −70, −10, 0), (−240, −10, +30), (0), (−160, 0, +65, +100) km s−1 for IR01250, U5101, N4418, and IR08572 NW, respectively. Exact positions are estimated with the velocity decomposition in Section 4.2.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Schematic image of the geometry of the velocity components in the molecular torus. Components (c) and (d) are excluded here because they are unlikely to be related to the molecular torus according to their small velocity dispersions of σ  V  ∼ 15 km s−1 as mentioned in Section 5.1.2. The image of IR08572 NW is adapted from S. Onishi et al. (2021) because changes of analyses do not make difference in the estimate of the radii of rotation.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Best-fit model of the gaseous CO rovibrational absorption lines in U5101. The abscissa is the rest wavelength. The ordinate is the normalized flux. Components (a)–(c) and their sum are denoted with red, orange, green, and sky-blue lines, respectively. The black arrows denote the rest wavelength of each CO transition. The HI Pfβ and the H2 v = 0 → 0 S(9) emission line are colored in olive-green. Ice features of H2O, ﹩{{\rm{OCN}}}^{-}﹩, CO, and OCS are denoted with solid gray lines.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Relationship between the number of velocity components considered and the difference between the AIC and its minimum (ΔAIC) for IR01250, U5101, N4418, and IR08572 NW. The name of the target in each panel is shown in the legend. The dashed horizontal line denotes the 0.1% rejection threshold (ΔAIC = 14). Note that for IR01250 the model with five velocity components gives ΔAIC = 61, which exceeds the rejection threshold. The adopted number of velocity components is denoted by a black arrow.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Optical spectrum of IR01250. The spectrum is colored black, and the best-fit model is colored orange. Lines with less than 3σ detections are denoted by question marks.
Paper: Systematic Study of the Inner Structure of Molecular Tori in Nearby U/LIRGs Using Velocity Decomposition of CO Rovibrational Absorption Lines 
Authors: Shusuke Onishi, Takao Nakagawa, Shunsuke Baba, Kosei Matsumoto, Naoki Isobe, Mai Shirahata, Hiroshi Terada, Tomonori Usuda, Shinki Oyabu
Figure caption: Derived spectra of N4418 and IR08572 NW normalized by the continuum (top panel) and telluric transmission (bottom panel). Notations are the same as those in Figure 4.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: Comparison of the analysis of the simulated sources with SkyLLH and the hierarchical_nu framework presented in this work. The gray contours show the 68%, 90%, and 99% confidence intervals computed by assuming Wilk’s theorem with 2 degrees of freedom. The purple shaded contours show the Bayesian 68%, 90%, and 99% credible regions of highest posterior density.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: The marginal posterior distributions for ﹩{\bar{n}}_{\nu }﹩ from all six point sources for the three example cases discussed in Section 3.3.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: The marginal posteriors for L, γ s, and ﹩{\bar{n}}_{j}﹩ for all six point sources, shown by the different colors. The upper, middle, and lower rows show the results for cases (1), (2), and (3), respectively. The true values are indicated as solid vertical lines and the priors are shown in gray, where relevant.
Paper: A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Francesca Capel, Julian Kuhlmann, Christian Haack, Martin Ha Minh, Hans Niederhausen, Lisa Schumacher
Figure caption: Distribution of observed and posterior predictive data. Shaded bands show 30%, 60%, and 90% quantiles from darkest to lightest.
Paper: CME Arrival Time Prediction Based on Coronagraph Observations and Machine-learning Techniques
Authors: Yucong Li, Yi Yang, Fang Shen, Bofeng Tang, Rongpei Lin
Figure caption: The normalized F-score of 11 physical parameters.
Paper: CME Arrival Time Prediction Based on Coronagraph Observations and Machine-learning Techniques
Authors: Yucong Li, Yi Yang, Fang Shen, Bofeng Tang, Rongpei Lin
Figure caption: The configuration for each layer of the CNN model used in this study.
Paper: CME Arrival Time Prediction Based on Coronagraph Observations and Machine-learning Techniques
Authors: Yucong Li, Yi Yang, Fang Shen, Bofeng Tang, Rongpei Lin
Figure caption: Scatter plot between model prediction results and actual CME transit times. The left-hand panel is the optimal CNN network prediction result of Model A, and the right-hand panel is the prediction result adding the constraint of physical parameters (Model B).
Paper: CME Arrival Time Prediction Based on Coronagraph Observations and Machine-learning Techniques
Authors: Yucong Li, Yi Yang, Fang Shen, Bofeng Tang, Rongpei Lin
Figure caption: Examples of the running differential images from CDAW.
Paper: CME Arrival Time Prediction Based on Coronagraph Observations and Machine-learning Techniques
Authors: Yucong Li, Yi Yang, Fang Shen, Bofeng Tang, Rongpei Lin
Figure caption: An example CNN input image (a) and the output feature maps by three CNN blocks (b)–(d), respectively.
Paper: CME Arrival Time Prediction Based on Coronagraph Observations and Machine-learning Techniques
Authors: Yucong Li, Yi Yang, Fang Shen, Bofeng Tang, Rongpei Lin
Figure caption: The decrease in average MAE on the training and validation sets.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: The effect of the decorrelation between CHIME and the Galt telescope on the amplitude of the holography measurement. Each row depicts a different source, in order from highest decl. at the top to lowest at the bottom. In the left column we show the amplitude of the decorrelation as a function of HA, referenced to 1 at transit. The black vertical lines in these panels indicate the span (±30°) of the HA grid used for all data presented in this paper; within this range the effect is approximately linear but becomes nonlinear in the very far sidelobes. We do not consider this regime here but use the full result of the calculation when correcting the data. In the right column, we show the dependence of the decorrelation strength on transit as a function of feed along the cylinders (color-coded), referenced to the first feed. Each cylinder behaves in the same way: the slope becomes more severe at larger zenith angles and flips sign across zenith.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: The Hubble constant (left) and expansion rate (right) inferred using multispectral sirens (i.e., the TwoSpin model) and the traditional spectral sirens (PP and PS models) with 42 events (SNRs > 11). In the left panel, the pink and green bands represent the Hubble constant measured from the cosmic microwave background (CMB; Planck Collaboration et al. 2020) and that measured in the local universe (A. G. Riess et al. 2019), respectively. The dotted histogram shows the results adopted from R. Abbott et al. (2023a), and the dotted lines represent the prior distribution. In the right panel, the shaded regions and solid lines are for 90% credible intervals and median values, respectively.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: Waterfall plots (in feed index vs. sky degrees) of the stacked Vir A data. For each cylinder data are taken from 717 MHz. The top two rows show copolar data while the bottom two rows show cross-polarization. The one-dimensional slices above each image panel show the median along the respective cylinders. Relative to Cyg A, the focal-line support legs are not as pronounced in cross-polarization. There is some apparent feed-dependent structure in the copolarized sidelobes in the form of roughly symmetric horizontal bands in YY which appear asymmetric in XX as if coupling to a neighboring cylinder. We measure a slightly wider beamwidth for a handful of feeds at the southern end of the cylinder (feed index 0).
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Hubble constant, matter density, and the parameters for the population models recovered by the TwoSpin (in orange) and NoSpin (in blue) models with 50 mock detections in O3. The solid lines represent the injections, and the contours mark the central 50% and 90% posterior credible regions, respectively; the values are for 90% credible intervals.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: Waterfall plots (in frequency vs. sky degrees) of the stacked Vir A data. Note the different behavior of the sidelobes as a function of frequency and HA (degrees on-sky) at this decl.; the checkerboard pattern is largely replaced by diagonal striping whose extent over the band appears to be polarization dependent.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Posterior distributions for H 0 obtained by combining the measurements from multispectral sirens/spectral sirens with 42 events (SNR > 11) and measurement from the bright standard siren GW170817 (B. P. Abbott et al. 2017c).
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Hubble parameters recovered by the TwoSpin (in orange) and NoSpin (in blue) models with 50 mock detections in O3. The dotted lines represent the injections. The shaded regions and solid lines are for 90% credible intervals and median values, respectively.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Hubble constant, matter density, and the parameters for the population models recovered by the TwoSpin model with five independent sets of mock detections in O3. The solid lines represent the injections, and the contours mark the central 50% and 90% posterior credible regions, respectively. The values are for 90% credible intervals.
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Central entropy of the ICM measured at a radius of 10 kpc (K 10 kpc) vs. luminosity of the [O II] lines (L [O II]) measured as in Figure 4. Detections are shown in blue, and upper limits are shown in red. For the first time, we show that the entropy threshold (shown here as a vertical dashed line) below which the hot ICM can condense into multiphase gas and trigger star formation persists to high (z ∼ 1) redshifts.
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Multiwavelength images for one of the clusters in our sample (SPT-CL J0000-5748), showing smoothed X-ray data from Chandra (left panel), optical data from the Dark Energy Survey (middle panel), and radio data from ATCA (right panel), with beam size shown in the bottom left. From the X-ray data, we can quantify how much hot (T ∼ 107 K) gas is cooling out of the ICM to subsequently fuel both star formation onto the BCG that ionizes warm (T ∼ 104 K) gas at optical wavelengths, as well as accretion onto the BCG’s central AGN which we can see at radio wavelengths. The BCG (selected as described in Section 2.2.1) is marked in all panels with a cross (+). ATCA contours are shown at [6, 50, 90, 130, 170] × σ rms, where σ rms ∼ 32 μJy beam−1.