adsabs/AstroCLIMB huggingface dataset:
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Spectral index maps of bent radio AGNs in the cluster sample. Each pixel corresponds to a 1.″5 × 1.″5 region of the sky. The 6″ LoTSS beam is shown as a gray circle in the bottom-right corner of each image. The 3σ FIRST contours are shown. Although most images are shown at the same size (≈ 0.′45 × 0.′45 centered on the radio core), a few of the images are scaled differently to encompass the entire radio AGN. We use a uniform color bar to show the value of the spectral index. We see examples of both core-dominated and lobe-dominated sources within our sample. Despite showing values of the spectral index for each individual pixel (the pixels are highly correlated because the pixel size is smaller than the beam size), we limit our analysis to larger structures and only identify the cores and lobes of our radio AGNs (see Table 3).
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Spectral index error maps of bent radio AGNs in the cluster sample. Each pixel corresponds to a 1.″5 × 1.″5 region of the sky. The 6″ LoTSS beam is shown as a gray circle in the bottom-right corner of each image. The black contours show the 3σ FIRST contours. All images show the same region as in Figure 20. While we see a roughly uniform error, we do use a uniform color bar to show our measure of the error in the value of the spectral index. As with the spectral index maps, we again note that the pixels are highly correlated because the pixel size is smaller than the beam size.
Paper: AMUSE-Antlia. I. Nuclear X-Ray Properties of Early-type Galaxies in a Dynamically Young Galaxy Cluster
Authors: Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Kelley M. Hess, Ralph P. Kraft, William R. Forman, Paul E. J. Nulsen, Sarrvesh S. Sridhar, Andra Stroe, Junhyun Baek, Aeree Chung, Dirk Grupe, Hao Chen, Jimmy A. Irwin, Christine Jones, Scott W. Randall, Elke Roediger
Figure caption: Multiwavelength images of the galaxies that host nuclear X-ray sources, 10″ ≃ 1.7 kpc. For each galaxy, from left to right, are images of CTIO r band, Chandra X-ray in the energy band of 0.5–8 keV, and broad bandwidth L-band radio continuum image from MeerKAT. The X-ray image is binned into twice the original pixel size. The name of each galaxy at the upper right corner of the CTIO r image is adopted from Ferguson & Sandage (1990). The NGC name is also shown if available. The cyan circle centered on each X-ray source has a radius of 50% PSF. All galaxies have a corresponding radio source except Antlia 105.
Paper: AMUSE-Antlia. I. Nuclear X-Ray Properties of Early-type Galaxies in a Dynamically Young Galaxy Cluster
Authors: Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Kelley M. Hess, Ralph P. Kraft, William R. Forman, Paul E. J. Nulsen, Sarrvesh S. Sridhar, Andra Stroe, Junhyun Baek, Aeree Chung, Dirk Grupe, Hao Chen, Jimmy A. Irwin, Christine Jones, Scott W. Randall, Elke Roediger
Figure caption: DSS J band image of the central region of the Antlia cluster, ﹩10^{\prime} \simeq 102\ \mathrm{kpc}﹩. The fields of the Chandra observations presented in this study are marked in white. Green circles indicate the detected nuclear X-ray sources. NGC 3268 and NGC 3258 are marked with a red “×” and a blue “⋆,” respectively.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Spectral index error maps of bent radio AGNs in the noncluster sample. As in Figure 22, each pixel corresponds to a 1.″5 × 1.″5 region of the sky, and the images cover the same region as those in Figure 21. We use the same color bar as in Figure 22.
Paper: AMUSE-Antlia. I. Nuclear X-Ray Properties of Early-type Galaxies in a Dynamically Young Galaxy Cluster
Authors: Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Kelley M. Hess, Ralph P. Kraft, William R. Forman, Paul E. J. Nulsen, Sarrvesh S. Sridhar, Andra Stroe, Junhyun Baek, Aeree Chung, Dirk Grupe, Hao Chen, Jimmy A. Irwin, Christine Jones, Scott W. Randall, Elke Roediger
Figure caption: The PDFs of the weighted bootstrap replications. Note that the Field refers to the AMUSE-Field sample. As a result, the outcome occupation fraction of the AMUSE-Antlia, AMUSE-Field, AMUSE-Virgo, and Fornax samples are 45% ± 10%, 38% ± 6%, 13% ± 4%, and 20% ± 8%, respectively. In conclusion, the AGN activity is similar in AMUSE-Antlia and AMUSE-Field samples, but both are higher than AMUSE-Virgo and Fornax.
Paper: AMUSE-Antlia. I. Nuclear X-Ray Properties of Early-type Galaxies in a Dynamically Young Galaxy Cluster
Authors: Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Kelley M. Hess, Ralph P. Kraft, William R. Forman, Paul E. J. Nulsen, Sarrvesh S. Sridhar, Andra Stroe, Junhyun Baek, Aeree Chung, Dirk Grupe, Hao Chen, Jimmy A. Irwin, Christine Jones, Scott W. Randall, Elke Roediger
Figure caption: The occupation fraction of AMUSE-Antlia, AMUSE-Field, AMUSE-Virgo, and Fornax in four mass bins. The data are restricted to nuclear X-ray sources with ﹩\mathrm{log}({L}_{{\rm{X}}}/\mathrm{erg}\,{{\rm{s}}}^{-1})\geqslant 38.9﹩ in the 0.5–8 keV band and logarithmic galaxy stellar masses of 8–8.9, 8.9–9.8, 9.8–10.7, and 10.7–11.6. The occupation fractions of Antlia and Field samples are higher than Virgo and Fornax.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Probes of the symmetry of the lobes of bent radio AGNs. The top panels shows the projected physical size (kpc) of each lobe when compared to the opposite lobe. The left-hand side is a direct comparison of the projected physical size, while the right-hand side shows a histogram of the ratios of the lengths of each lobe. For the ratio, we compare the smallest lobe length and largest lobe length regardless of which lobe is lobe 1 or lobe 2. Red points are bent AGNs in the cluster candidate sample. Blue points are bent AGNs in the noncluster sample. A gray dashed line in each of the left-hand panels shows a one-to-one trend. The bottom panels similarly show the projected physical area (Mpc2) of each radio lobe when compared to its opposite lobe. It follows the same conventions as the top panel with the left side showing a direct comparison, and the right side showing a histogram of the ratio of the areas of each lobe. Both plots comparing the radio lobes indicate that most of the lobes have similar projected physical sizes and areas when compared to their opposite lobe. Although no overall trend with the total projected physical size or area is found, when we compare the ratio of the projected physical sizes and projected physical areas, the two most asymmetric sources are in noncluster environments.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Examples of the two bands used to create spectral index maps. The left two images show LoTSS and FIRST images of COBRA145023.3+340123, while the right two images are from COBRA104641.5+282028. In the LoTSS images, the red contours show the 10σ, 20σ, and 50σ contours, while in the FIRST images, the red contours show 3σ, 5σ, and 10σ. The blue circle identifies the location of the core. Each FIRST image is smoothed and regridded to match LoTSS (6″ resolution and 1.″5 pixels). We specifically highlight two sources with slight differences in the components. For COBRA145023.3+340123, the west component is not as strongly identified in FIRST, while for COBRA104641+282028, the core is not detected at the 10σ level in LoTSS.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The ratio of the projected physical areas of the radio lobes as a function of the offset from the cluster center. The offset from the cluster centers is measured in GM19 and presented in GM21 and is based on the surface density of red sequence galaxies. Richer cluster candidates, with a combined overdensity greater than 3.5σ, are shown in red boxes. Bent radio AGNs hosted by BCGs are shown in blue boxes. We find no overall trend between the symmetry of radio lobes and the offset from the cluster center.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The ratio of the projected physical areas of the radio lobes as a function of the significance of the combined overdensity from GM19, our cluster richness proxy, for the cluster candidates. We plot the m*+1 i − [3.6] cluster candidates (the most statistically robust sample in the initial analysis) in black circles, the magnitude-limited i − [3.6] cluster candidates in pink diamonds, the magnitude-limited [3.6] − [4.5] cluster candidates in blue triangles, and the m*+1 r − i cluster candidates in red squares. We find a weak correlation with little evidence to reject the null hypothesis for the entire sample (r  s  = 0.266, p = 0.256). While we find a stronger correlation in the m*+1 i − [3.6] sample, we again find no evidence to reject the null hypothesis, making this trend statistically improbable (r  s  = 0.643, p = 0.119).
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Spectral index maps of bent radio AGNs in the noncluster sample. As in Figure 20, each pixel corresponds to a 1.″5 × 1.″5 region of the sky. Although most images are scaled the same (≈ 0.′45 × 0.′45 centered on the radio core), a few are scaled differently to encompass the entire radio AGN. We use the same color bar as in Figure 20.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The radio luminosity (L 144 MHz) as a function of the combined overdensity for the cluster candidate sample is shown in the top panel and the total projected physical area (Mpc2) as a function of the combined overdensity is shown in the bottom panel. Each subsample is identified following the same legend as Figure 13. We find no evidence of any correlations between the combined overdensity and the radio luminosity. Although we see no trend between the projected physical size and combined overdensity for the entire sample, we do find a strong trend with weak to moderate evidence to reject the null hypothesis for the m*+1 i − [3.6], magnitude-limited i − [3.6], and m*+1 r − i cluster samples.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: 3.6 μm Spitzer IRAC Cutouts of the 20 bent, double-lobed radio sources in the COBRA cluster candidate sample observed by LoTSS. Each image shows the same FOV as in Figure 2, and the three red contours show the same 10σ, 20σ, and 50σ contours based on the measurement of the LoTSS rms noise in each image. Here, the blue circle identifies the host galaxy. The black line shows 0.′5.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The ratio of the projected physical area of the radio lobes as a function of the LoTSS opening angle. While there is no clear distinction between the two populations, we find that narrower bent AGNs are generally more commonly in clusters, as expected.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: 3.6 μm Spitzer IRAC Cutouts of the 15 bent, double-lobed radio sources in the noncluster sample observed by LoTSS. Each image shows the same FOV as in Figure 3. The red contours show the same contours as in Figure 3, while the blue circle identifies the host galaxy.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The log of the normalized projected physical area as a function of the log of the offset from the cluster center. The offsets from the cluster center are reported in GM21. The normalization of the fit from Moravec et al. (2019) is shown in the gray dashed line.
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: MUSE total intensity image of JO36 with the contours of the stellar disk (black contour, from Gullieuszik et al. 2020) and the emission-only Hα emission (red-to-yellow filled).
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: Left: example of five random trajectories on the phase-space diagram, color coded for the value of R  tr , and the 5%, 10%, and 15% scatter regions around the phase-space coordinates of JO36; Right: resulting normalized distributions with a Gaussian fit. The vertical dashed line corresponds to the observed radius, and the gray shaded area indicates the Gaussian fit 1σ confidence region. In the legend are reported the number of solutions of each distribution, and Gaussian centroid, μ, and dispersion, σ.
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: Hα kinematics of JO36. Left: position–velocity slice along the galaxy’s major axis, extracted from the MUSE data. The yellow squares show the rotation curve determined with the envelope-tracing method. The bright regions at velocities ∣v∣ > 400 km s−1 are due to the [N II] doublet entering the velocity range of the data cube. Intensity contours are drawn at 3 × 2 N  (N ≥ 0) times the rms noise (solid lines). A negative contour at −3 times the rms noise is also shown with gray-dashed lines. Right: the corresponding rotation curve. The approaching and receding sides are shown separately as blue and red squares, respectively. The black circles show the mean rotation velocity.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Histograms of the spectral index values of the entire radio AGN, the radio core, and the radio lobes. The radio AGNs in the cluster sample are shown in red and the radio AGNs in the noncluster sample are shown in blue. The median value of each distribution is shown as the vertical red and blue lines. While the total number of radio AGNs in each sample is 20 and 15, respectively, there are sources in each sample where the core region is smaller than the beam size. While we have included them here, they are flagged in Table 3.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The LoTSS opening angle as a function of the combined overdensity (top panel) and the FIRST opening angle as a function of the combined overdensity (bottom panel). Unlike the trend shown in GM21, we find slightly weaker trends between the samples using the LoTSS images and very weak to no statistical evidence to reject the null hypothesis. However, we do find a moderate trend with weak evidence to reject the null hypothesis in the FIRST sample.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: A comparison of the opening angle measurements from FIRST (GM21) with the opening angle measurements from LoTSS DR2 for the cluster sample. The black lines shows a one-to-one trend, while the two gray dashed lines highlight a 10% difference between the opening angles. We overlay colored squares on all bent AGNs where the opening angles differ by more than 10%. For the majority of our sources, these measurements are very similar.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The radio luminosity of bent radio AGNs (L 144 MHz ) as a function of the total projected physical area of each bent radio AGN. The cluster candidates are shown in red, and the noncluster candidates are shown in blue. We find a moderate trend with strong evidence to reject the null hypothesis for the cluster sample, but only a moderate trend with no evidence to reject the null hypothesis for the noncluster sample.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Examples of our measurement of the opening angle for the LoTSS images. The red contours are the same contours as in Figure 2. The yellow dashed lines show L 1 and L 2 from Equation 1, while the blue lines show our estimate of the opening angle using the largest physical extent of each radio source. In some cases, the opening angles are nearly identical, while most slightly differ. However, some give a dramatically different value, as is the case for COBRA171330.9+423502, in the far right panel.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Radio contours for COBRA164611.2+512915. Here we show our fiducial divide of the radio source (the blue line) through the radio core that we use to divide the radio AGNs into lobe 1 and lobe 2. As in Figure 2, the blue circle shows the AGN core, and the red contours show 10σ, 20σ, and 50σ values.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The projected physical size and area distributions of the bent radio AGNs in the cluster and noncluster sample. We see that each sample spans a similar range of sizes and areas.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Cutouts of the 15 bent, double-lobed radio sources in the noncluster sample observed by LoTSS DR2. While most of the cutouts are 1.′3 × 1.′3, some of the images are slightly larger due to the larger angular size of the radio AGNs. All contours, lines, and circles are the same as in Figure 2 (the location of the core for COBRA104641.5+282028 comes from the optical/IR host and the FIRST contours; see Figure 19 for the host galaxies).