adsabs/AstroCLIMB huggingface dataset:
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Results of a plane-wave collapse (Zel’dovich pancake) test problem with grid (left) and glass (right) initial conditions. We display the velocity along the plane wave, the gas temperature, and the normalized density at z = 0. The grid panel includes all simulation particles, with the lack of scatter indicating that the planar symmetry is preserved throughout the volume. For the glass setup, we show the median values in narrow distance bins perpendicular to the plane of collapse. In black, we include outputs from a high-resolution 1D simulation taken from Hopkins (2015), which the CRK-HACC runs converge toward.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Stacked radial profiles showing baryon density (top), temperature (center), and entropy (bottom) for three M/M * bins indicated in the legend. The radial profiles have been transformed in the x-axis by ﹩{\left(M/{M}_{* }\right)}^{-1/3}﹩ and scaled in the y-axis using a procedure that minimizes the L1-norm between the three curves.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Comparison of the T eff (top row), ﹩\mathrm{log}g﹩ (middle row), and [Fe/H] (bottom row) values of APOGEE DR17 with those of GALAH DR3 (black, left columns) and with those of RAVE DR6 (black, right columns). The red points are similar to the black points, except that the T eff, ﹩\mathrm{log}g﹩, and [Fe/H] estimates in the GALAH and RAVE catalogs are calibrated to match the APOGEE scales (see Section 2.2). The ordinates (residuals) are defined in the sense of APOGEE minus GALAH or APOGEE minus RAVE, whereas the abscissas correspond to GALAH or RAVE. The horizontal lines indicate perfect consistency. The mean offset and standard deviation of the residuals are shown in each panel, with the colors having the same meaning as those of the data points.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Left: comparison of radii determined from the SED fitting with those from asteroseismology. The blue squares indicate dwarfs and subgiants from Serenelli et al. (2017), while the red circles indicate giants from Pinsonneault et al. (2018). The median formal uncertainties of the two sets of radii are shown in the top panel, and the mean ratio of the seismic to SED fitting radii and its standard deviation are given in the bottom panel. The dashed lines represent perfect consistency. Right: similar to the left panels, except for the seismic radii replaced by those from Berger et al. (2020).
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Top panel: comparison of bolometric flux derived from the SED fitting with that computed from the HST CALSPEC/STIS spectrophotometry of flux standards (red circles; Bohlin et al. 2014) and with that calculated from bolometric corrections (blue squares; Casagrande & VandenBerg 2018). The dashed line marks the one-to-one relation. Bottom panel: bolometric flux ratio as a function of our bolometric flux estimates. The red and blue dashed lines show the mean ratios, while the gray dashed line denotes perfect one-to-one agreement. The numbers in the legend indicate the offsets and the scatters.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Comparison of angular diameters from the SED fitting with those from CHARA interferometry. Top: angular diameters compared for the 83 dwarfs and subgiants (﹩\mathrm{log}g﹩ > 3.5; blue squares) and the 33 giants (﹩\mathrm{log}g﹩ ≤ 3.5; red circles). The one-to-one line (perfect match) is shown in black. Bottom: angular diameter ratio (SED/CHARA) shown for the same set of populations, but color-coded by Hipparcos H  P  magnitude. The mean and the standard deviation of the ratios are also labeled.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Left: comparison of luminosity determined from the SED fitting with those from asteroseismology. The symbols, line, and text have the same meaning as in Figure 5, now for luminosity. Right: similar to the left panels, except for the seismic luminosity replaced by those from Berger et al. (2020). Our SED luminosities are computed from our bolometric fluxes and Gaia-based distances (Bailer-Jones et al. 2021), while the luminosities from asteroseismology and Berger et al. (2020) were derived from their radii and temperatures.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Top: histograms of the heterogeneous uncertainties of T eff (left), ﹩\mathrm{log}g﹩ (middle), and [Fe/H] (right) of APOGEE DR17 (blue), GALAH DR3 (orange), and RAVE DR6 (green). Bottom: similar to the top panels, but now for the rescaled uncertainties that contain the calibration uncertainties and the intrinsic uncertainties (see Section 2.2).
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Comparison of extinctions determined from the SED fitting with those from asteroseismology. The symbols, line, and text have the same meaning as in Figure 5. No extinctions were provided for dwarfs and subgiants by Serenelli et al. (2017).
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Comparisons between extinctions derived from the SED fitting and those from Queiroz et al. (2020) and Green et al. (2019). In each panel, the orange diamonds show the mean values in each bin, and the red line is a fitted linear model to the orange diamonds, with its slope and intercept values annotated. The scatter value is the dispersion of the A  V  measurements with respect to the fitted linear model. The blue dashed line indicates the one-to-one correspondence.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Dereddened Gaia color–magnitude diagram of high-extinction, high-luminosity red giants (A  V  > 5 mag), using A  V  from (a) Green et al. (2019), (b) this work, and (c) Queiroz et al. (2020). The red text indicates the data and models used for deriving A  V  in each work. Overplotted are MIST evolutionary tracks of the AGB phase of different reasonable masses and metallicities: dashed, solid, and dotted lines for [M/H] = 0.3, 0, and −0.3, respectively, and red, orange, and blue lines for M = 0.8, 1.0, and 1.2 M ⊙, respectively. The purple line corresponds to a stellar track of M = 1.0 M ⊙ and [M/H] = 0 that has representative properties of the sample shown here.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Spatial distributions of the extinctions of NGC 6791 with respect to the cluster center (R.A., decl.) = (295.32283, 40.19639) and of NGC 6819 with respect to the cluster center (R.A., decl.) = (295.32283, 40.19639). The black circles indicate the cluster star members (Cantat-Gaudin et al. 2020) in our sample that are used to probe differential extinction as shown with the filled contours. The margin at the bottom of the right panel is not covered by any stars. For comparison, our field windows shown here are chosen to be the same as in Brogaard et al. (2012) for NGC 6791 and in Platais et al. (2013) for NGC 6819.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Hertzsprung–Russell (H-R) diagram. The black circles mark MS stars, and the orange circles denote our SB2 candidates. The red and blue circles are SB2 and SB3 candidates/binaries compiled from the literature, respectively. The yellow dashed line indicates the gap between the SB2 sequence and the MS (green line; see the text).
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Comparison of extinctions of 184 Gaia open clusters that have been investigated by Cantat-Gaudin et al. (2020) and that have at least three members each in our sample. The color code indicates the number of members of each cluster. Two open clusters, NGC 6791 and NGC 6819, that are subject to extensive asteroseismic analysis are highlighted with red open circles. The red dashed line shows the one-to-one relation. The mean difference (−0.09) and its standard deviation (0.34) are indicated, where the literature extinction scale is on average less than ours.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Top: extinction map in Galactic coordinates, traced by the footprint of APOGEE DR17, GALAH DR3, and RAVE DR6. The Kepler field, TESS Northern and Southern Continuous Viewing Zones (NCVZ, SCVZ), and PLATO North and South Long-duration Observation Phase fields (LOPN, LOPS) are schematically highlighted. The sky region that has not been observed by the three spectroscopic surveys is shown in black. Bottom: similar to the top panel, except for highlighting the Galactic plane using the stars with A  V  > 2 mag (note the different A  V  scales of the color bars).
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Radius vs. T eff diagram, color-coded by the normalized number density. Radius estimates are derived from our SED fitting, while effective temperatures are adopted from APOGEE DR17, GALAH DR3, and RAVE DR6. Some key features are highlighted.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Uncertainty distributions of angular radius, bolometric flux, extinction, radius, and luminosity (from left to right). The numbers shown in red are the median uncertainties.
Paper: Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE
Authors: Jie Yu, Shourya Khanna, Nathalie Themessl, Saskia Hekker, Guillaume Dréau, Laurent Gizon, Shaolan Bi
Figure caption: Similar to Figure 8, except for the color code replaced by spectroscopic metallicities from APOGEE DR17, GALAH DR3, and RAVE DR6, available for stars with T eff ≳3500 K.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: Fourier spectra (the first column), illustration of the method to estimate the significance of Fourier spectral power peaks (the second column), global wavelet spectra (the third column), and local wavelet spectra (the fourth column) for different angular widths of daily CMEs. In the Fourier spectra, the dashed red lines correspond to the 95% confidence level. The second column displays the logarithm of the cumulative probability of the spectra vs. power for the actual daily CME counts and the randomized sequence. In the global wavelet spectra, the dashed red lines correspond to the 95% confidence level against the red-noise background. Moreover, regions where the local wavelet spectral power is statistically significant at the 95% level against the red-noise backgrounds, are contoured by black, thick lines. From top to bottom the first/second/third/fourth/fifth rows show all/halo/partial-halo/normal/narrow CMEs, respectively.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: The daily occurrence rate of CMEs (CDAW catalog). The panels from top to bottom show all/halo/partial-halo/normal/narrow CMEs, respectively.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: The daily occurrence rate of CMEs (CDAW catalog) in the northern and southern hemispheres. The left column is for the northern hemisphere. The right column is for the southern hemisphere. From top to bottom the panels show all/partial-halo/normal/narrow CMEs, respectively.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: Global wavelet spectra and local wavelet spectra for different angular widths of daily northern CMEs for SC23 (the first and second columns) and SC24 (the third and fourth columns). From top to bottom the first/second/third/fourth rows show all/partial-halo/normal/narrow CMEs, respectively.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: Global wavelet spectra and local wavelet spectra for different angular widths of daily CMEs for SC23 (the first and second columns) and SC24 (the third and fourth columns). From top to bottom the first/second/third/fourth/fifth rows show all/halo/partial-halo/normal/narrow CMEs, respectively.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: Fourier spectra (left column), global wavelet spectra (middle column), and local wavelet spectra (right column) for different angular widths of daily CMEs in the northern hemisphere. From top to bottom the first/second/third/fourth rows show all/partial-halo/normal/narrow CMEs, respectively.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: Upper panels: Comparison of the total observed proper-motion dispersions from Cantat-Gaudin et al. (2020) (member stars were crossmatched to Gaia EDR3) and this work; the x-axis in the left plot presents a logarithmic-scale parallax, and the right plot shows the histograms. Bottom panels: Same as the upper panels but for the apparent radius; the black and blue dashed lines indicate the angular size corresponding to 5 and 15 pc, respectively.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: Same as Figure 9 but for the line-of-sight extinction.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: Left: Histograms of the cluster ages in H22b and in this work. Right: Galactic longitude–age (only SC candidates in this work and in H22b) distributions, color-coded by parallax, where the colored dashed lines show the median ages at the different longitudes.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: Distribution of the newly found candidate (crosses) and known (dots) OCs (ϖ < 0.8 mas) in the Galactic fields. The colors indicate the parallax of each cluster.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: Hertzsprung–Russell diagram for the 48,714 member stars in 1656 new cluster candidates, which are divided into nine age intervals.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: The left panel shows a histogram of the parallaxes. Orange: Sample of Gaia DR2 OCs. Blue: The sample found in this work. The right panel shows the proportion of increase in the number of Gaia DR2 OCs at the different parallaxes.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: Histogram of the RV dispersion for 328 new cluster candidates with more than one matched member star in the Gaia DR3 RV database.
Paper: Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: Zhihong He, 治宏 何, Xiaochen Liu, 效臣 刘, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Qingquan Jiang, 青权 蒋
Figure caption: Same as Figure 3, but for the new globular cluster candidate CWNU 1944.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: The time–frequency grid for parallel calibration. The blue blocks represent the RTFs. The phase parts of the gain solutions are interpolated on a common time slice, as shown by the dark gray cells. The orange blocks represent the time and frequency slices where differential intensity self-calibration is performed. Bandpass and polarization calibrations are performed for individual coarse channels, which are marked by green. The pink dotted lines demarcate the 1.28 MHz wide coarse channels.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: Demonstration of the flagging of bad data based on the solar dynamic spectrum. Top: the dynamic spectra of r a. Middle: the visibility amplitude for a time slice without any RFI/instrumental issue is plotted against the uv-distance. Bottom: the visibility amplitude for a time stamp, 01:25:33.75 UTC, which is affected by RFI/instrumental issues, is plotted against the uv-distance. This time slice is marked by the red box in the top left panel. In all rows, the left and right panels represent the XX and YY polarizations, respectively.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: Dynamic spectrum of the image rms. The spectral and temporal spans of the dynamic spectrum are 1.28 MHz and 240 s, respectively. There is significant temporal variation in the image rms, while that along the spectral axis is barely evident.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: Schematic diagram of P-AIRCARS, highlighting its main modules.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: Flowchart describing the calibration block of P-AIRCARS. The major stages of the calibration block are shown by the colored boxes.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: Global wavelet spectra and local wavelet spectra of different angular widths of daily southern CMEs for SC23 (the first and second columns) and SC24 (the third and fourth columns). From top to bottom the first/second/third/fourth rows show all/partial-halo/normal/narrow CMEs, respectively.
Paper: Quasiperiodic Variations of Coronal Mass Ejections with Different Angular Widths
Authors: Xia Li, Hui Deng, Feng Wang, Linhua Deng, Ying Mei
Figure caption: Fourier spectra (left column), global wavelet spectra (middle column), and local wavelet spectra (right column) for different angular widths of daily CMEs in the southern hemisphere. From top to bottom the first/second/third/fourth rows show all/partial-halo/normal/narrow CMEs, respectively.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: The alignment of the solar radio disk center with the optical solar disk center. Left: the image after phase-only self-calibration. The center of the optical solar disk, shown by the blue dot, is not at the center of the radio disk. Middle: the mask of the solar disk, with the red dot representing the center of the radio disk. Right: the final image after alignment. The centers of the optical and radio disks coincide after the alignment.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: Variation of the calibration time with the available number of CPU threads. The green, orange, blue, and red points represent the expected runtimes for different combinations of temporal and spectral spans. The black cross and the magenta square show the runtimes from a real data set using 20 and 30 CPU threads, respectively.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: Flowchart describing the imaging block of P-AIRCARS. A single imaging block is shown inside the blue shaded box.
Paper: Tackling the Unique Challenges of Low-frequency Solar Polarimetry with the Square Kilometre Array Low Precursor: Pipeline Implementation
Authors: Devojyoti Kansabanik, Apurba Bera, Divya Oberoi, Surajit Mondal
Figure caption: Demonstration of ankflag on MWA data. The flagging is done on a single time–frequency slice using uv-bin mode. The gray squares and blue points show the flagged and unflagged data, respectively.