adsabs/AstroCLIMB huggingface dataset:
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: Effects of the slow luminosity dip driven by thermal pulses. Left panel: sketch of the luminosity evolution as a function of time between two consecutive thermal pulses, with interpulse period τ ip. The labels indicate a few relevant stages: the quiescent luminosity L CMLR, the rapid dip L B and peak L C, and the slow dip L D. The time axis is stretched around the the first TP, from ﹩L{{\prime} }_{\mathrm{CMLR}}﹩ to L D. These short-lived stages typically cover ≲ 0.1 of the interpulse period. Middle panel: probability distribution (purple histogram) of the luminosity along the slow dip from L D to L CMLR. The width of the luminosity bins is set to 0.01 dex. We consider a TP-AGB star with solar metallicity, M  c  = 0.6 M ⊙, L CMLR ≃ 8000 L ⊙, and L D ≃ 3400 L ⊙. Right panel: statistical (positive only) uncertainty of the core mass derived from the CMLR, due to the probability that a star intercepts the observed luminosity while evolving on a slow dip of a TP at higher M  c . The uncertainty is shown as a function of the core mass in the range 0.5 ≤ M  c /M ⊙ ≤ 0.9. The corresponding quiescent luminosity in the asymptotic regime spans the interval 4600 ≲ L CMLR/L ⊙ ≲ 26,400. See the text for more details.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: Same as Figure 8, but adopting cluster ages and visual extinctions from the work of Dias et al. (2021). Luminosity and core mass of all objects are rederived accordingly. Note that the stars Case 473, IRAS 19582+2907, HD 292921, and IRAS 09251−5101 are absent, as their host clusters are not included in the catalog.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: PLD of the LPVs in open clusters from Table 7, color-coded by initial mass according to Cantat-Gaudin et al. (2020). The source Case 121 is indicated by the black symbol, as its initial mass according to Cantat-Gaudin et al. (2020;  ∼ 7 M ⊙) is substantially larger compared to all other sources. The spectral type is indicated by symbol shapes (triangles: M type; diamonds: MS type; squares: S type; circles: C type). For the source IRAS 23455+6918 we show both the pulsation period and the long secondary period, connected by a dashed line. For visual reference, primary periods of LPVs in the LMC from OGLE-III (Soszyński et al. 2009) are displayed as gray circles in the background. Solid lines represent the best fits to period–luminosity relations A, B, C′, C, and D derived by Soszyński et al. (2007) for O-rich LPVs in the LMC, whereas dashed lines correspond to the best fits to C-rich LPVs on sequences C′ and C. No parallax correction was applied to sources in the left panel, while in the middle and right panels, respectively, we have adopted the L21 and G21 parallax corrections.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: Same as Figure 10, but with the TP-AGB stars identified by their names, consistently with other figures in the paper. The absolute magnitude ﹩{M}_{{K}_{s}}﹩ of each star is corrected for interstellar reddening. The results are shown for the three options of parallax ZP correction, as indicated on the top of each panel.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: NIR-bright stars of open clusters in the Gaia−2MASS diagram. The absolute ﹩{M}_{{K}_{s}}﹩ magnitude is corrected for interstellar extinction, derived from A  V  of each cluster. Dashed lines show the approximate boundaries of main stellar branches, defined by Lebzelter et al. (2018). Left panels: all stars from the catalog of Cantat-Gaudin & Anders (2020) with cluster membership probability p ≥ 0.5. The stars are marked according to their spectral type if known (otherwise, they are indicated by gray circles), age, and turnoff mass of the host cluster. Right panels: AGB star candidates in open clusters, brighter than the RGB tip. From top to bottom the stars are color-coded as a function of the spectral type (when unknown, the gray color is used), cluster’s age, and initial mass. The top panel distinguishes between E-AGB (triangles) and TP-AGB (circles) stars, based on PARSEC stellar isochrones. It also includes the full list of MS, S, and C stars. See the text for more details.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: CMLR of TP-AGB stars. TP-AGB model sequences (crosses) show the evolution of the core mass and luminosity during the quiescent stages of the TP cycles, for a few values of the initial stellar mass in the interval ﹩1.0\lesssim {M}_{{\rm{i}}}^{\mathrm{AGB}}/{M}_{\odot }\lesssim 6.5﹩ and metallicities close to the solar value (0.01 ≤ Z ≤ 0.02). Each model (cross) is taken at the pre-flash luminosity maximum, just before the occurrence of an He-shell thermal instability. Various sources are included: Karakas et al. (2002; green), Cristallo et al. (2011; orange—FRUITY database), Addari (2020; blue—models computed with the MESA code). The solid black line running over the entire M  c  range is an analytic fit to the asymptotic CMLR for Z = 0.014, given by Equations (3a)+(3b). Overplotted to the TP-AGB models we show the predictions (black lines) obtained with the synthetic CMLR (Equations (3a)+(3b)+(3c)), including the pre-pulses and assuming the same M  c  , 1TP, L 1TP, Z, and M  c , as in the stellar models.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: Effect of the Gaia EDR3 parallax zero-point corrections considered in this work (no ZP correction, Lindegren et al. 2021a, and Groenewegen 2021) applied to the carbon star V* V493 Mon and its candidate hosting cluster Trumpler 5. The blue curves describe the parallax distributions of the cluster members in the form of the density distribution function (calculated using the kernel density estimation method—KDE), normalized by the total area. The solid, dashed, and dotted blue lines mark, respectively, the median and the 68th and 95th confidence intervals of the distributions. The parallax central value and the ± 1σ errors for V* V493 Mon are also shown (red solid and dashed lines).
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: Visual example of membership assessment for the target star MSB 75 with respect to the cluster NGC 7789. The blue circles in the top panels refer to the cluster members (with p > 0.7) according to Cantat-Gaudin et al. (2020), while the red circle marks the target star. The blue curves in the middle and bottom panels are the density distribution functions of each astrometric parameter (calculated using the KDE method, similar to the one adopted in Figure 3), with the solid, dashed, and dotted blue lines indicating the median and the 68th and 95th percentiles, respectively. The red lines denote the central values (solid lines) and the 1σ errors (dashed lines) of MSB 75 parameters. Our analysis indicates that MSB 75 is a member of NGC 7789. The bottom right panel shows the CMD using the three optical Gaia passbands. The parameters of each star are updated to Gaia EDR3 and the parallaxes corrected for the zero-point offset (in this example using Groenewegen 2021).
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: SED fitting of TP-AGB stars of type M, S, and C in Milky Way open clusters. Interstellar extinction A  V  is taken from the catalog of Dias et al. (2021). Each star is placed at the distance given by its own Gaia EDR3 parallax (no ZP correction). Photometric data (with error bars) from various sources are displayed with colored symbols. Upper limits (denoted with filled triangles) are not considered in the fits. Note that all sources are consistent with being TP-AGB stars, except for NIKC 3-81, which is probably an R-hot star, placed below the RGB tip.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: Light curves of the 18 sources for which we determined a period in filters of Gaia (G, G BP, G RP), ASAS-SN (V, g), and ZTF (g, r).
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Examples of radio morphology categories. The lowest level of the red/cyan/white (configuration A/B/C or D) radio contours corresponds to 5× rms noise (σ rms) in the image and the subsequent contours increase by a factor of 2. The corresponding rms noise and restoring beam size of the elliptical Gaussian for each source can be found in Table 1. The black cross depicts the position of the radio center of the galaxy.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Example of the calibrated, final total-intensity image of the giant elliptical galaxy NGC 4472 in the upgraded VLA A configuration data observed in 2015. The red contour levels are created at [1, 2, 4, 8, 16, …] ×  5 σ rms up to peak intensity at 1.5 GHz (S peak). The rms noise and peak intensity values are 22 μJy beam−1 and ﹩\left(2.79\pm 0.11\right)\times \,{10}^{-2}\,\mathrm{Jy}﹩ (Table 1). The red ellipse in the white box represents the restoring beam of the final image. The black cross shows the position of the radio center of the giant elliptical galaxy.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Example of determining the spectral index for NGC 4472 from a red circle with a diameter of 0.7 kpc. Top: the CASA output “alpha image” and its corresponding uncertainty values. In CASAVIEWER, we extracted the mean spectral index of (−0.55 ± 0.05). Bottom: the manual fitting of four frequency chunks and their corresponding flux densities gives a final spectral index value for NGC 4472 of −0.64, which is comparable with the mean spectral index from the CASA “alpha image”.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Top: relation between radio power at ∼1.5 GHz (P 1.5GHz) versus the X-ray luminosity (L Xray) within 10 kpc from the center of the galaxy shows no correlation. Bottom: significant correlation (Spearman and Pearson coefficient of 0.71 with p-value of 0.004) is seen when we compare the radio power at ∼1.5 GHz (P 1.5GHz) with the luminosity of the central X-ray point sources (L Xray_AGN) (Lakhchaura et al. 2018) detected only in a subset of our main sample of early-type galaxies. Error bars on the radio power are mostly smaller than the plotted symbol size. The correlation coefficients and corresponding p-values are given in Table 2. The black line represents the linear fit of the distribution, while the shaded area shows the 1σ confidence region for the correlation.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: The radio power (P 1.5GHz) plotted against the entropy (top) and cooling time (bottom) of the hot X-ray-emitting gas measured within r < 10 kpc shows no correlation. Error bars on the radio power are mostly smaller than the plotted symbol size.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Top: no correlation is found between the radio power (P 1.5 GHz) and the jet power (P jet; top), the Hα + [N II] luminosity (﹩{L}_{{{\rm{H}}}_{\mathrm{alpha}}+[{{\rm{N}}}_{\mathrm{II}}]};﹩ middle) as well as the supermassive black hole mass (M BH; bottom). The nuclear (nucHα), extended (extHα), undetected (noHα) and unknown (unkHα) Hα +[N mathscII] emission are distinguished. The correlation coefficients and corresponding p-values are given in Table 2. Error bars on the radio power are mostly smaller than the plotted symbol size.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: The total flux density at 1.5 GHz (S 1.5 GHz) is plotted against the largest linear size (LLS) of the radio source. A positive correlation with a linmix correlation coefficient of ﹩{0.67}_{-0.09}^{+0.08}﹩ is determined. The brighter the radio source, the larger its linear extent. The correlation coefficients and corresponding p-values are given in Table 2. The black line represents the linear fit of the distribution, while the shaded area shows the 68% confidence region for the correlation.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Total integrated radio flux-density histogram with two morphologically different categories: point sources and extended sources. The fainter sources fall into the point sources category, whereas the brighter galaxies are the extended ones.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Radio spectral indices for a subset of our sample. Approximately, three-quarters of the sources have steep spectra (α > −0.5) and the rest have flat and inverted radio spectra (α ≤ −0.5). The vertical blue dashed line indicates the spectral index of −0.5.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Widening of the radio contours visible for 3C 449, IC 4296, NGC 315 and NGC 4261. The radio contour levels are drawn at 5 × rms noise, increasing by factors of 2 up to the peak intensity. The rms noise and peak intensity values can be found in Table 1. The black cross depicts the radio center of the galaxy.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: The Chandra X-ray images smoothed to enhance the X-ray tail enclosed by the radio jets of 3C 449 (top) and IC 4296 (bottom). The black cross indicates the position of the radio center of the galaxy and yellow circles show the cross-cone region between the jets with the X-ray tail.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Chandra images with overlaid black X-ray contours and a black “X” to mark the central X-ray brightness peak. The innermost X-ray contour is drawn by estimating the peak of the average count value of the Chandra image with the DS9 (Joye & Mandel 2003) projection region tool. The subsequent contour levels are decreasing as a power of 2. The brown cross shows the core of the radio emission from VLA A configuration data, and the blue cross represents the position of the optical center from Pan-STARRS in each image (estimated from the innermost optical contour). The offset of the observed radio core emission with respect to the central peak of the optical emission is shown by cyan lines. Small offsets (within 0.5 kpc) are seen for NGC 3923, NGC 4486, NGC 5129 and NGC 5846.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Top: VLA D configuration total-intensity image of NGC 4125 with overlaid radio isophots in white. The contours in cyan and black represent the emission from the TGSS at 148 MHz and WSRT at 1.4 GHz, respectively. In all cases the contour levels are at [1, 2, 4, 8, 16, …] ×  5 ·  σ rms. The corresponding rms noise levels (σ rms) for the VLA D configuration, TGSS and WSRT data is 67 μJy, 1.7 mJy and 60 μJy, respectively. The restoring beam (resolution) for each observation can be found in the bottom-right corner of the image in the white box. The optical (Hubble Space Telescope) center of the galaxy is shown as a green cross and is consistent with the X-ray center (Chandra; a yellow cross) and the radio center, most prominent in the WSRT image at 1.4 GHz. Bottom: the spectral index map between 148 MHz (TGSS) and 1.4 GHz (WSRT).
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Top: the total-intensity image of NGC 533 in VLA A configuration at 1–2 GHz. Bottom left: its corresponding in-band spectral index map with measurement uncertainties produced by the multiterm “cleaning” algorithm in CASA. Bottom right: the morphological structure of NGC 533 is similar to the structure in the COMP2CAT source J132031.47-012718.5.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: Left: the total-intensity image of NGC 1600 in VLA A configuration at 1–2 GHz has a morphology resembling the (right) FR II radio source J1423+2501 from the FRIICAT catalog (Capetti et al. 2017b).
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: The Chandra-smoothed (with a 2″ Gaussian kernel) images overlaid by 1.5 GHz VLA A, AB/B, and C/D configuration contours in the red, cyan and white, respectively. In all cases, the contours are created at 5  ×  σ rms and increase by the power of 2 up to the peak intensity. The center of the galaxy is represented by a black “+” sign. Rms noise (σ rms) and peak intensity values are given in Table 1.
Paper: Very Large Array Radio Study of a Sample of Nearby X-Ray and Optically Bright Early-type Galaxies
Authors: Romana Grossová, Norbert Werner, Francesco Massaro, Kiran Lakhchaura, Tomáš Plšek, Krisztina Gabányi, Kamlesh Rajpurohit, Rebecca E. A. Canning, Paul Nulsen, Ewan O'Sullivan, Steven W. Allen, Andrew Fabian
Figure caption: The X-ray Chandra-smoothed (with a 2″ Gaussian kernel) images overlaid by 1.5 GHz VLA A, AB/B, and C/D configuration contours in the red, cyan and white, respectively. In all cases, the contours are created at 5  ×  σ rms and increase by the power of 2 up to the peak intensity. The center of the galaxy is represented by a black “+” sign. Rms noise (σ rms) and peak intensity values are given in Table 1.