adsabs/AstroCLIMB huggingface dataset:
Paper: A Simple Method for Predicting N H Variability in Active Galactic Nuclei
Authors: Isaiah S. Cox, Núria Torres-Albà, Stefano Marchesi, Xiurui Zhao, Marco Ajello, Andrealuna Pizzetti, Ross Silver
Figure caption: The TPR as a function of ΔN H. The left panel shows inclination angle θ inc = 45°. The right panel shows inclination angle θ inc = 87°. The colors show different count levels and the line styles show different sensitivity levels. This plot shows that the TPR increases with the number of counts and ΔN H. For observations with ≳5000 counts (orange line), we would expect to detect all variable events at 90% confidence, or a threshold ﹩{\chi }_{{\rm{c}}}^{2}﹩ of 2.706 (solid line) in both cases.
Paper: A Simple Method for Predicting N H Variability in Active Galactic Nuclei
Authors: Isaiah S. Cox, Núria Torres-Albà, Stefano Marchesi, Xiurui Zhao, Marco Ajello, Andrealuna Pizzetti, Ross Silver
Figure caption: The HRs of simulated spectra for a range of N H values and different count levels. All spectra here were simulated as described in Section 5. The colors are the same as in Figure 8.
Paper: A Simple Method for Predicting N H Variability in Active Galactic Nuclei
Authors: Isaiah S. Cox, Núria Torres-Albà, Stefano Marchesi, Xiurui Zhao, Marco Ajello, Andrealuna Pizzetti, Ross Silver
Figure caption: Confusion matrices for all three models at the 99.999% confidence level (﹩{\chi }_{{\rm{c}}}^{2}=19.511﹩). The small number of FPs (top right) show that, at this sensitivity, almost none of the nonvariable sources in a sample will be flagged. However, this comes at the expense of not selecting a larger number of variable sources (bottom left).
Paper: A Simple Method for Predicting N H Variability in Active Galactic Nuclei
Authors: Isaiah S. Cox, Núria Torres-Albà, Stefano Marchesi, Xiurui Zhao, Marco Ajello, Andrealuna Pizzetti, Ross Silver
Figure caption: Confusion matrices for all three models at the 90% confidence level (﹩{\chi }_{{\rm{c}}}^{2}=2.706﹩). These show that the method is good at avoiding FNs, meaning that most of the variable sources in a sample will be flagged. However, this comes at the expense of flagging as variable more sources that are not variable (top right).
Paper: A Simple Method for Predicting N H Variability in Active Galactic Nuclei
Authors: Isaiah S. Cox, Núria Torres-Albà, Stefano Marchesi, Xiurui Zhao, Marco Ajello, Andrealuna Pizzetti, Ross Silver
Figure caption: Direct comparison of the best-fit N H values from UXCLUMPY to the NuSTAR HR. As can be seen, the HR is able to predict N H variability in NGC 4388 and nonvariability in 3C 105 and NGC 7319.
Paper: A Simple Method for Predicting N H Variability in Active Galactic Nuclei
Authors: Isaiah S. Cox, Núria Torres-Albà, Stefano Marchesi, Xiurui Zhao, Marco Ajello, Andrealuna Pizzetti, Ross Silver
Figure caption: Confusion matrices for all three models at the 99% confidence level (﹩{\chi }_{{\rm{c}}}^{2}=6.635﹩). These show that at this sensitivity, the method does a decent job overall at flagging variable sources while avoiding nonvariable sources.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: Mass growth histories of relevant merger tree branches from the COCO simulation with M(z = 0) ≃ 109.5 M ⊙. Red and blue solid lines show the evolution of the main and minor branches, respectively, in a randomly chosen tree of this mass that meets our “ghost galaxy” criteria. The solid black line shows the halo mass corresponding to the cooling threshold described in the text. The sharp increase in the threshold mass at z = 10 corresponds to our fiducial model of reionization (V cut = 30 km s−1). We associated this tree with a ghost galaxy at z = 0 because the minor branch crosses the cooling threshold (up to z above = 10, m above ∼ 108 h −1 M ⊙) while the main branch does not. The two branches merge at z merge ≈ 2.4 (dashed line), at which point their mass ratio is m merge/M merge ∼ 10%. Shaded areas show the 10th–90th percentile range of mass histories for main branches (red) and minor branches (blue) in all such trees, for this choice of final mass.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: A cartoon of the “ghost galaxy” formation scenario. Time runs down the page. Dark matter halos above and below the hydrogen cooling threshold are indicated by solid and dotted circles, respectively, with radii indicating their mass. Two branches in the merger tree of a present-day halo merge at z merge. At this time, the less massive (minor) progenitor contains stars, whereas the more massive (main) progenitor does not. As sketched in the inset graph, this is possible if the minor branch grows faster at higher redshift, briefly exceeding the hydrogen cooling threshold up to a time z above (thick lines). The main branch is always below this threshold. The (possible) result at the present day is a dark matter halo that is underluminous for its mass and contains only an LSB, stellar halo-like component, comprising the stellar debris of the accreted minor branch.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: Comparisons between our measurements and those from the literature, between different measurement methods. The vast majority of literature metallicity measurements come from medium-resolution studies, particularly those leveraging the CaT metallicity calibration. The ground-based CaHK narrowband measurements are from the Pristine study of Dra II (Longeard et al. 2018).
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: The fraction of merger trees for dark matter halos of a given mass that host ghost galaxies at z = 0, for V cut = 30 km s−1. The result based on EPS trees is shown in green, and the result based on trees from the COCO simulation is shown in blue. The probability of finding ghosts in the field peaks at ∼5% around a halo mass ≈4 × 109 h −1 M ⊙.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: Stellar metallicities used for fitting the mean and dispersion (Section 3.2) of our MDFs as a function of brightness across our entire sample of galaxies. The measurements shown here are specifically for the process of fitting the MDFs, and may not fully reflect the final reported measurements (e.g., asymmetric uncertainties, upper limit constraints). The uncertainties shown here also take into account the systematic uncertainties we adopt as discussed in Appendix B.5, and statistical uncertainties for our brighter stars are often smaller. (Top panel) Metallicity measurements as a function of absolute magnitude, where absolute magnitude is a stand-in for the stellar evolutionary phase. (Bottom panel) Metallicity measurements as a function of apparent magnitude.
Paper: Ghostly Galaxies: Accretion-dominated Stellar Systems in Low-mass Dark Matter Halos
Authors: Chung-Wen Wang, Andrew P. Cooper, Sownak Bose, Carlos S. Frenk, Wojciech A. Hellwing
Figure caption: The shaded gray region (same in both panels) shows the 10th–90th percentile range of mass growth histories for the main branches of all halos in the COCO simulation with M(z = 0) ≃ 109.5 M ⊙. Shaded orange and blue regions, repeated from Figure 2, show the corresponding range for main (left) and minor (right) branches in the subset of these halos that host ghost galaxies.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: HST data of the M92 GC, a monometallic population, that we use to determine systematic uncertainties for our metallicity measurements. (Left) CMD of M92 in F475W–F814W. (Right) The position of M92 members on the CaHK diagram. The majority of these stars lie between the [Fe/H]= −3 and [Fe/H]= −2 tracks.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: Comparing MIST and BaSTI stellar evolution models in CaHK space for α-enhanced, 13 Gyr RGB (left) and MS (right) stars.
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: Kinematics of CME1 (left) and CME2 (right) using the GCS model on the coronagraphic observations. Top panel: the measurements of the heliocentric distance (h) of the leading edge of the flux rope (FR) and its radius (R). Middle panel: propagation speed (v) and expansion speed (v  e ) derived by taking the three-point derivatives of h and R, respectively. Bottom panel: propagation acceleration (a) and expansion acceleration (a  e ) derived by taking the derivative of v and v  e , respectively. The red vertical lines at each data point show the error bars derived by considering an error of 10% in the measurements of the flux rope’s leading-edge height (h).
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: For the CME1: Variation of the polytropic index (Γ), average heating rate (dQ/dt), average temperature ﹩(\bar{T})﹩, and average proton number density (﹩{\bar{n}}_{p}﹩) of the CME with the heliocentric distance of the CMEs leading edge (h) is shown in the top left, top right, bottom left, and bottom right, respectively. The red vertical lines at each data point show the error bars derived by considering an error of 10% in measurements of the flux rope’s leading-edge height (h).
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: For the CME2: variation of the Polytropic index (Γ), average heating rate (dQ/dt), average temperature ﹩(\bar{T})﹩, and average proton number density (﹩{\bar{n}}_{p}﹩) of the CME with the heliocentric distance of the CMEs leading edge (h) is shown in the top left, top right, bottom left, and bottom right, respectively. The red vertical lines at each data point show the error bars derived by considering an error of 10% in measurements of the flux rope’s leading-edge height (h).
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: Schematic of a flux rope CME in the cylindrical coordinate system (i:e r,ϕ, z) showing the propagation speed (v  c ) of the axis of the flux rope, expansion speed (v  e ), and poloidal speed (v  p ).
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: GCS-model-fitted wireframe in green and pink overlay on the contemporaneous coronagraphic images of the CME1 shown in left (left: STEREO-A/COR2, center: LASCO-C3, right: STEREO-B/COR2) and for CME2 shown in the right (left: STEREO-A/COR2, right: LASCO-C2).
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: Profile of R/L for CME1 and CME2 from the measurements (black; left-hand side of Equation (1)), model-fitted result for this parameter (blue; right-hand side of Equation (1)), and relative errors (red) (MPE: mean percentage error).
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: Multiwavelength view of magnetic flux rope as seen in different wave bands of SDO/AIA. Top row (panels (a)–(c)): the hot flux rope formed above an active region, AR 11302, as shown by SDO/HMI line-of-sight magnetograms (panel (a)). The SDO/AIA 304 Å image depicts the absence of flux rope/eruption (panel (b)). Panel (c) indicates the presence of a hot flux rope (8–15 MK) in the DEM map. Middle row (panels (d)–(f)): it shows the distinct feature of the magnetic flux rope in its eruptive phase. The cyan dotted lines show the cool compression front, followed by the dark cavity region of the flux rope, which best appears at coronal temperature (0.6–2 MK) in AIA 171, 193, and 211 Å wave bands. Bottom row (panels (g)–(i)): the hot channel of the flux rope is shown via dotted red lines in the hotter wave bands of AIA (2.5–10 MK, i.e., 94, 131, and 335 Å). It should be noted that cool coronal images (middle panel) show the very faint signature of this hot channel of the flux rope.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: R Lep HF long baseline synthesized images for the continuum emission at Bands 8 and 9 in the top and bottom, respectively. The left and right panels are the images before and after phase self-cal (using the continuum), respectively. The solid line contours start from 3σ  level, increased by a factor of a power of 2, and the dashed line contour represents the −3σ level. The contour levels are shown on the upper side of each panel. The image peak value and rms noise are indicated at the top and bottom of each panel, respectively. The ellipse in the lower left represents the synthesized beam. Note that the synthesized beam size of the continuum self-cal image at Band 9 becomes broader compared to that of the original images because phase self-cal solutions were not obtained for some of the more distant antennas and the data for these were flagged in applying the solutions.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Top: (u, v) coverage of R Lep in B-08–B-10 from the left, middle, and right, respectively. Bottom: visibility amplitude of the continuum as a function of (u, v) distance of R Lep in B-08–B-10 from the left, middle, and right, respectively. The visibility data were first vector averaged in time and two polarization pairs. Then the data are scalar averaged in each 2 Mλ bin. The color represents each spectral window. In Band 9, one of the spectral windows in BB-3 (LSB; light blue color) has a systematically higher amplitude and deviation compared to the other spectral windows because a cluster of atmospheric O3 absorption lines exists (Pardo et al. 2022) in the bandwidth.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Experiment schedule of the B-09 B2B phase referencing test. Black bars represent HF band scans in Band 9, while gray bars represent LF band scans in Band 4. The horizontal axis is the experiment date and time in UTC. The observed sources, bands (in parentheses), and scan intents (in square brackets) are found in the left part of the panels.
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: FRIS-model-derived average internal forces, such as Lorentz force, Thermal pressure force, and Centrifugal force, that is responsible for the radial expansion of the flux rope of CME1 (left) and CME2 (right). The red vertical lines at each data point show the error bars derived by considering an error of 10% in measurements of the leading-edge height of the flux rope (h). The solid and dash lines show the power-law fitted values for the model-derived internal forces.
Paper: Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Authors: Soumyaranjan Khuntia, Wageesh Mishra, Sudheer K. Mishra, Yuming Wang, Jie Zhang, Shaoyu Lyu
Figure caption: Top row (panels (a)–(c)): the sequence of images of GONG/H α  shows the gradual eruption of a quiescent filament on 2018 August 20. It is associated with an elongated filament channel containing no cool component but a hot plasma channel. Middle row (panels (d)–(f)): temporal evolution of coronal plasma channel (hot filament channel) lying between two coronal holes as observed by SDO/AIA 211 Å. Bottom row (panels (g)–(i)): the formation of flux rope and its eruption lying over the coronal plasma channel is shown in STEREO-A/EUVI 171 Å on 2018 August 20.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Cross-correlation spectrum for the HCN maser at 890.8 GHz, from the J = 10−9 transition between the (1110) and (0400) vibrationally excited states, for the shortest projected baseline antenna pair with the (u, v) distance of 5259–5290 kλ. The horizontal axis represents the radial velocity in ﹩{v}_{{}_{\mathrm{LSRK}}}﹩ (kilometers per second), and the vertical axis represents the cross-correlated flux density (jansky). The black and blue lines represent the XX and YY polarization pairs, respectively. The line profile was obtained by scalar averaging in time.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Rms phase as a function of baseline length of the 120 s Go/NoGo checks for J0423-0120 just before the experiments. The horizontal axis denotes the baseline length, and each open circle denotes the phase rms value in degrees at ﹩{\nu }_{{}_{\mathrm{HF}}}﹩ for a single baseline. The flux density of J0423-0120 was bright (6.4, 3.4, and 2.6 Jy at Bands 3, 7, and 9, respectively) and the thermal phase noise is negligible after averaging the available spectral windows and the dual polarization pairs. Note that the corresponding excess path length rms is expressed in the second vertical axis in microns at the right side.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: R Lep Band 10 continuum image. Left: B2B phase referencing alone (before phase self-cal). Middle: after phase self-cal. Right: calibrated using the phase and amplitude self-cal solutions of the HCN maser channel at v LSRK = 9.4 km s−1. The solid contours start from the 3σ level, increased by a factor of a power of 2, and the dashed line contour denotes the −3σ level. The contour levels are shown on the upper side of each panel. The image peak value and rms noise are listed at the top and bottom of each panel, respectively. The ellipse in the lower left represents the synthesized beam. Note that the synthesized beam size of the middle, continuum phase self-cal image becomes broader compared to that of the original image (left panel) because the phase self-cal solutions were not obtained for some of the more distant antennas and the data for these were flagged in applying the solutions.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: HCN maser cube in Band 10 (yellow contours) at 890.8 GHz, from the J = 10−9 transition between the (1110) and (0400) vibrationally excited states, averaging every four velocity channels of the synthesized image cube with the velocity width of 0.3 km s−1. The continuum emission in Band 10 is shown as a background grayscale gradation. The image cube was created after applying the amplitude and phase self-cal solutions derived using the HCN maser emission at ﹩{v}_{{}_{\mathrm{LSRK}}}=9.4﹩ km s−1. The image rms noise was calculated at each velocity channel from emission-free portions in the image. The minimum image rms noise is 45 mJy beam−1 in the channels with little maser emission at ﹩{v}_{{}_{\mathrm{LSRK}}}=19.9﹩ km s−1, and the maximum image rms noise is 1787 mJy beam−1 at ﹩{v}_{{}_{\mathrm{LSRK}}}=9.4﹩ km s−1. The solid line contours start from the 5σ level per channel at ﹩{v}_{{}_{\mathrm{LSRK}}}=9.4﹩ km s−1 (=8.9 Jy beam−1), increased by a factor of a power of 2. The dashed line contours start from the −5σ level, increased by a factor of a power of 2. The contour levels are −17.8, −8.9, 8.9, 17.8, 35.6, 71.2, 142.4, 284.8, and 569.6 mJy beam−1. The radial LSRK velocity is given at the bottom of each panel, and the synthesized beam size is shown on the lower left and right corners for the HCN maser (5.6 × 5.0 mas) and continuum (5.3 × 4.8 mas), respectively.