adsabs/AstroCLIMB huggingface dataset:
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Comparison between the simulated QSLs at the solar surface and the EUV images at two moments. The top row is for SDO/AIA 304 Å, and the bottom row is for 1600 Å. The left column is for 10:08 UT, and the right column is for 10:39 UT. The pink ovals highlight the QSLs corresponding to the flare ribbons.
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: CMD of NGC 3201 (gray dots) with the 67 surveyed BSSs marked as blue circles, and a set of BaSTI isochrones (Pietrinferni et al. 2021) with ages ranging from 1 to 9 Gyr overplotted as blue lines. The BSSs in common with SP14 are encircled.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Sketch illustrating the eruption and lateral drifting of the filament. The cyan and pink tubes represent the flux rope carrying the filament material and the ambient arcades, respectively. The yellow asterisk locates the regions where interchange magnetic reconnection may occur. The gray translucent contours represent the filament material.
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Proper-motion-selected and differential-reddening-corrected CMD of NGC 3201 (black dots), with the spectroscopic targets discussed in the paper highlighted as solid colored circles: the 67 BSSs are marked in blue, while the reference sample of MS, SGB, RGB, and AGB stars are plotted in red.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Comparison between the initial flux rope (green) at 10:00 UT and that after reconnection (purple) at 10:50 UT.
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Radial velocities (in kilometers per second) of the target stars as a function of their distance from the cluster center (in arcseconds). The stars belonging to NGC 3201 are shown as black circles, while the objects belonging to the Galactic field are colored in gray.
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: From top left to bottom right: distribution of the surveyed BSSs in the CMD of NGC 3201, rotational velocity distributions as a function of the (V − I) color, the V magnitude, and the distance from the cluster center. In all the panels, the FRs are plotted as red circles with increasing size for increasing rotational velocity, while the BSSs spinning at ﹩v\sin (i)\lt 40﹩ km s−1 are marked as small blue circles. A set of single-mass evolutionary tracks (Pietrinferni et al. 2021) for stars between 0.9 and 1.3 M ⊙ are also overplotted as red solid lines in the top left panel.
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Left panel: difference between the rotational velocities obtained in this work (﹩v\sin (i)﹩) and those determined by SP14 (﹩v\sin {(i)}^{\mathrm{SP}14}﹩) for the 29 BSSs in common, as a function of our measures. Right panel: as in the left panel but for the rotational velocities of SP14 computed from the Mgb triplet line alone (﹩v\sin {(i)}^{\mathrm{SP}14,\ \mathrm{Mgb}}﹩).
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Cumulative distributions of the (V − I) color (left panel) and V magnitude (right panel) for the sample of FRs (i.e., BSSs with ﹩v\sin (i)\geqslant 40﹩ km s−1; red lines) and slow rotators (blue lines). The Kolmogorov–Smirnov probability to be extracted from the same parent distribution p is marked in each panel. Note that the statistical significance of the Kolmogorov–Smirnov test is somehow overestimated in this case due to the need of introducing a free parameter (namely the 40 km s−1 threshold).
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Distributions of the rotational velocities measured for highly evolved, giant stars (red histogram in the upper panel), mildly evolved (SGB and MS) stars (green histogram in the central panel), and BSSs (blue histogram in the bottom panel).
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Distribution of magnitude as a function of the distance from the cluster center (in arcseconds) for the observed sample of BSSs. Symbols have the same meaning as Figure 8.
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Percentage of FRs (i.e., number of BSSs with ﹩v\sin (i)\gt 40﹩ km s−1 over the total number of surveyed BSSs) as a function of the central density of the parent cluster for NGC 3201 (blue circle) and the other GCs (namely, M55, ω Centauri, M4, 47 Tucanae, M30, NGC 6752, and NGC 6397; gray circles) studied in Ferraro et al. (2023).
Paper: Fast-rotating Blue Straggler Stars in the Globular Cluster NGC 3201 
Authors: Alex Billi, Francesco R. Ferraro, Alessio Mucciarelli, Barbara Lanzoni, Mario Cadelano, Lorenzo Monaco, Mario Mateo, John I. Bailey, Megan Reiter, Edward W. Olszewski
Figure caption: Comparison between the observed spectra (gray lines) and the best-fit synthetic spectra (black lines) for four BSSs with different rotational velocities, ranging from 5 to 82 km s−1.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Snapshots of the erupting flux rope viewed from the side at (a) 10:04 UT, (b) 10:14 UT, (c) 10:23 UT, and (d) 10:50 UT. Field lines with different topology connectivity are distinguished in color, where the yellow shows the initially inserted flux rope, the cyan and orange show the newly formed flux ropes with magnetic reconnection, and the pink indicates the background field. Side images in the x–z and y–z planes represent the synthesized EUV images in 171 Å and 335 Å integrated along the y- and x-axes, respectively. Panels (e) and (f) display the synthesized EUV 171 and 335 Å images with the zoomed-in views of the pink rectangles in panel (a).
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: (a) CHASE/HIS observation in Hα red-wing image at 10:55 UT, where the black dashed line (Cut 3) represents the cut to make the time–distance map in panel (c), and the yellow asterisk represents the point to show the Hα spectrum profile in panel (d). (b) SDO/AIA 304 Å image at 10:55 UT. (c) Time–distance diagram along Cut 3 in panel (a). (d) Hα spectrum profile (red solid line) at the asterisk in panel (a). The black solid line represents the reference profile observed from the quiet Sun, and the vertical dashed line is the reference line center (6562.8 Å).
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: [C II] spectrum of J0109–3047 in the central pixel (defined as the FIR peak, upper panel) and the optimal r = 0.″5 aperture (lower panel), using the combined new high-resolution data and archival low-resolution observations. The error per frequency channel (defined as the σ-clipped rms per pixel in each channel and scaled by the square root of the number of pixels in the aperture) is shown in red, a single Gaussian fit is overplotted in blue. The best-fit parameters and errors of the Gaussian fit are indicated in the top right corners. The frequency, amplitude, and FWHM of the [C II] line are consistent with that of the previous observations, and we find no evidence for an additional broad component in the [C II] emission line profile.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: The posterior distribution for the dispersion-dominated model without SMBH, where I 0 is the central [C II] emission in janskys beam−1, R  d  is the scale length of the exponentially declining [C II] profile in kiloparsecs, and σ  v  the spatially constant velocity dispersion in kilometers per second. To make the graph less crowded, we do not show the posterior for the 3D center of the source (x, y, Δv), which is tightly constrained to the observed center of the [C II] emission.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Curve of growth of the dust continuum (left) and [C II] velocity-integrated emission (right). The flux density reported in Venemans et al. (2020) is recovered at an aperture size of r = 0.″5 (e.g., 2 kpc at z = 6.7). The flux difference between the low- and high-resolution data is only <10% and the fluxes agree within the 1σ uncertainty, indicating that little or no diffuse emission (θ ≳ 0.″05) is lost in the high-resolution data. We note that the errors shown here are only statistical (using the rms in the map and scaling for the aperture size) and do not include the ∼10% amplitude calibration uncertainty.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: The velocity dispersion of the [C II] line in J0109–3047 (top left) and best-fit models for given black hole masses between 108 − 109  M ⊙ (first row). The residuals of the models are shown in the second row. The data, models, and residuals are only shown for pixels in which the velocity-integrated [C II] emission exceeds 3σ (as in Figure 1). The reduced χ 2 statistic (adjusted for the kernel size) for the three models are, in order, ﹩{\chi }_{\mathrm{red}}^{2}=1.097,1.097,1.101﹩.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: GCS reconstruction for the CME observed by the white-light coronagraphs of (a) STEREO A/COR2 and (b) SOHO/LASCO C2. The blue wireframe depicts the CME flux rope structure.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: CHASE/HIS observations in Hα line center (panels (a)–(c)), Hα red wing (panels (d)–(f)), and the derived velocity maps (panels (g)–(i)). The green contours in panel (g) represent the flare ribbons observed in the Hα line-center image at the same moment.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Side views of the typical flux rope filed lines and the distributions of the squashing factor (Q) on the planes of x = −44 Mm and x = 15 Mm at 10:08 UT (panels (a)–(c)) and 10:39 UT (panels (d)–(f)).
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Same as Figure 7 but for the top view.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Integrated mass (left) and velocity (dispersion) profiles as a function of galactocentric radius for the SMBH and gas component of the galaxy. The integrated gas mass profile is derived from the radially averaged dust profile, assuming a gas-to-dust ratio of 100 ± 50. The velocity dispersion is calculated by approximating the gas as virialized. To first order, the velocity dispersion derived from the gas mass is consistent with that observed and is constant.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Velocity dispersion of the [C II] line for different “dispersion-dominated+SMBH+gap” model for various central gap sizes. The model is constructed as a dispersion-dominated source with a central 109  M ⊙ SMBH, and a central gap in the intensity profile (r gas). The central increase in the velocity dispersion due to the SMBH can be decreased if the gap is large >200 pc, but such configurations are excluded as our observations resolve these scales, and the [C II] emission does not present a central dip.
Paper: Dependence of Stellar Differential Rotation on Effective Temperature and Rotation: An Analysis from Starspot Transit Mapping
Authors: Alexandre Araújo, Adriana Valio
Figure caption: Strong negative correlations for the dependence of ΔΩ on the mean rotation period (right) and a weak correlation for the dependence of ΔΩ on the effective temperature of the stars (left).
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Same as Figure 6 but for the dispersion-dominated+SMBH+gap model. This model has an exponentially declining intensity profile with a central gap and fixed black hole mass of 1.1 × 109  M ⊙.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Same as Figure 7, but for the dispersion-dominated model including an SMBH with mass 1.1 × 109  M ⊙ (fixed) and a central gap (given in kiloparsecs) in the [C II] emission profile.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Same as Figure 7, but for the dispersion-dominated model including an SMBH.
Paper: The Contribution and FIP Bias of Three Types of Materials inside ICMEs Associated with Different Flare Intensities
Authors: Hui Fu, Xinzheng Shi, Zhenghua Huang, Youqian Qi, Lidong Xia
Figure caption: The numbers (left panel), speeds (middle panel), and scales (right panel) of NFCs, and three types of FCs. The error bars in panels (b) and (c) represent the standard deviations of speeds and scales of ICMEs. It is clear that the speeds and scales of ICMEs are increased significantly with flare intensities.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Comparison between the observed [C II] emission and the best-fit dispersion-dominated model. This spherically symmetric model has an exponentially declining intensity profile and a constant dispersion velocity. The contours start at 3σ and increase in steps of 3.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Same as Figure 7, but for a thin disk model. The maximum rotation velocity (﹩{v}_{\max }﹩, in kilometers per second) is constrained to be <4.3 km s−1 at the 2σ level.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Same as Figure 6 but for the best-fit thin disk model.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Same as Figure 6 but for the dispersion-dominated+SMBH model.
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: Radio continuum images of the JO36-GIN 049 system. Top-left: 144 MHz (rms = 110 μJy beam−1, resolution = 8.6 × 4.6 arcsec2); top right: 675 MHz (rms = 110 μJy beam−1, resolution = 13.6 × 8.2 arcsec2). Bottom left: 144 MHz (rms = 159 μJy beam−1, resolution = 11.3 × 5.2 arcsec2). The gray-dashed polygon defines the extended region (see Section 3.1). Bottom right: 675 MHz (bottom right, rms = 40 μJy beam−1, resolution = 5.4 × 2.8 arcsec2). The relevant parameters used to produce the images with WSCLEAN are reported in Table 1. We show the −3, 3, 6, 12, 24, 48, 96 × rms levels (gray), and the contour of the stellar disk of JO36 (black). The silver rectangular regions in the top panels indicate the FOV of the lower panels.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: (a) GOES SXR light curves between 10:00 UT and 11:40 UT on 2022 August 18, in which the peak times are marked with dashed lines. (b) Composite image of AIA 171 Å (red), 193 Å (green), and 304 Å (blue) of the pre-eruptive filament at 09:33 UT on 2022 August 18. (c) Hα line-center image of the pre-eruptive filament observed by CHASE/HIS at 09:33 UT. (d) Line-of-sight magnetic fields (gray scale) in the source region of the pre-eruptive filament.
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: SDSS gri image of A160 overlaid with the 3, 6, 9, 12, 15, 18, 21, 24, 48, 80, 160, 320, 550 × rms levels of the 144 MHz radio emission (rms = 127 μJy beam−1, resolution = 10.6 × 5.2 arcsec2) and stellar disk of JO36 (gold contour). In the top-left and bottom-right inserts, we present a zoom-in of JO36 and GIN 049, respectively.
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: Spectral index maps between 144 and 675 MHz (left), and corresponding uncertainties (right). The angular resolution, from top to bottom, is 9″, 17″, and 30″. For each angular resolution, we report the 3, 6, 12, 24, 48, 96, 192 × rms contours of the corresponding LOFAR image.
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: Left panel: ETG XLF for AMUSE-Antlia (black error bar), AMUSE-Field (green error bar), AMUSE-Virgo (yellow error bar), and Fornax sample (pink error bar). The leftmost luminosity bin is under the median sensitivity of AMUSE-Antlia, so we focus on the right three bins. We present the 90% upper limit as a downward arrow for the non-detection of the third bin of Antlia XLF. The y-axis is logL X number density divided by the total stellar mass of galaxies M T in each sample. Right panel: the stellar mass distributions of the four samples. Also, we plot the standard ETG stellar mass function (Moffett et al. 2016) with the blue long-dashed line. Below a certain detection limit, high-mass galaxies can have more AGN detections due to Eddington incompleteness, so for the left panel we divide the XLF by M T. Generally speaking, the AGN XLF in Antlia is consistent with the Field, while both are much higher than Virgo and Fornax.