adsabs/AstroCLIMB huggingface dataset:
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Quantitative comparison of the five methods by consistent metrics. (a1): The variation of Indicator a obtained by the five methods under different thresholds for a X2.2 WLF. Except for Method 1, all the other methods use intrinsic threshold ﹩{\delta }_{\max 2}﹩. (a2): The variation of Indicator b obtained by the five methods under different thresholds for a X2.2 WLF. (b1)–(c2): Similar to (a1)–(a2), but for the M3.0 and C5.5 WLFs, respectively. The left-hand side of the horizontal axis ticker represents the fixed thresholds used by Method 1, while the right-hand side represents the intrinsic threshold used by other methods. (d): Quantitative assessment of Indicator a for the five methods based on 10 WLFs. The total score for each method is displayed in the legend. (e): Similar to (d), but for Indicator b.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Variation in the E(B − V) with the observed FUV flux when the intrinsic continuum flux is fixed as obtained in obs4.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Variation of intrinsic neutral absorbing column density with the observed NUV − FUV color.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Variation in the X-ray photon index with intrinsic disk flux (DISKBB) for all five observations.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: All-sky orbital poles density distribution for DM particles of the host (gray color map) between 50 and 150 kpc; note that the DM particles of the massive satellite are excluded in all cases. Orbital poles of subhalos and satellite galaxies are shown with open and solid yellow circles respectively. Each row corresponds to a different time in the evolution of the halo at the satellite’s infall (top row), first pericentric passage (middle row), and second pericentric passage (bottom row). MW–LMC idealized simulation (right panels), MW–LMC analog m12b (left panels), and the low-mass analog m12i (middle panels). The orbital poles of the particles were computed after rotating the disk into the x–y plane. The density of orbital poles was computed using HEALPIX with HEALPY (K. M. Górski et al. 2005). In m12i the orbital poles' distribution evolves smoothly from the overdensities of poles close to the equator (upper middle panel) to a colatitudinal distribution of poles (middle and bottom panel). In m12b the distribution of orbital poles changes rapidly after the first pericentric passage (middle left panel), and afterward, clustering of poles is seen around the satellite’s orbital pole (pink marker) at b = 15°, l ≈ 270°). Similarly, in the MW–LMC idealized simulations the clustering occurs at the pericentric passage around the satellite’s pole at l = 0°, b = 0°.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Temporal evolution of the two-point angular correlation function, ﹩\tilde{\omega }(\theta )﹩, of the distribution of orbital poles for the MW–LMC analog (m12b), low-mass satellite (m12i), and idealized MW–LMC halos. In the top (bottom) panels the correlation function was computed on 106 DM (star) particles randomly selected within 50–150 kpc. The distribution of orbital poles is roughly constant in time until a satellite approaches its pericenter (vertical dashed lines). Even minor mergers, such as the one experienced by m12i at t = 8 Gyr, change the orbital poles' distribution. Note that for the idealized MW–LMC halo (top right panel) the relative changes are 2 orders of magnitude lower than both m12i and m12b (see the text for further discussion on this). The correlation function computed in the star particles (bottom panels) varies more due to the presence of large stellar streams and substructures. Changes close to pericentric passages are present, but there are also many more changes that occur through the evolution of the halos.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Magnitude of the host’s velocity in the box reference frame and relative to the host’s velocity at t = 6 Gyr is plotted as a function of time (upper panels) for the MW–LMC analog (left panel), the low-mass satellite analog (middle panel), and the idealized MW–LMC simulations (right panel). The host’s velocity increases by 80 km s−1 between infall time (8 ∼ Gyr) and its pericenter. Finally, the velocity settles after the merger at ≈−40 km s−1 relative to the velocity at t = 6 Gyr. Such rapid motions happen in less than 2 Gyr, which is comparable to the dynamical times of the MW halo at ≈100 kpc. The lower panels show the outer halo COM velocity is relative to the inner halo velocity reported by the halo finder. The outer halo velocity is measured using the subhalos (black) and DM particles (dashed lines) that are beyond 50 kpc. In the MW–LMC analog halo (m12b) the outer halo already has a net motion in the satellites of 30 km s−1 before the satellite’s infall, but not in DM, and reaches its peak velocity (60–80 km s−1) at the first pericenter. In the low-mass satellite analog (m12i) the outer halo does move with respect to the inner halo but only up to 20 km s−1. In the MW–LMC idealized simulations the magnitudes of both the v com,outer and v host are similar to those found in the MW–LMC analog (m12b).
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Orbital properties of the most massive satellites in the Latte suite. For comparison, the MW–LMC idealized simulations are shown with star markers. The color bar shows the satellite–host mass ratio at infall. Overall the majority of the satellites in Latte are on more eccentric orbits and have shorter pericentric passages. In terms of eccentricity, pericenter distance, and satellite–host mass ratios m12b is the closest analog to the MW–LMC.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: 2D density projection of the DM (left panel) and star (right panel) particles of our fiducial MW–LMC analog system in the Latte suite, m12b, at the first pericenter passage (cosmic time of 8.8 Gyr). Here, we use a reference oriented such that the disk of the host galaxy is in the x–y plane through the simulation. All the coordinates (positions and velocities) are computed with respect to the center of the disk of the host galaxy. The orbital history of the LMC-like satellite is shown with dashed lines. This figure was rendered using the PYNBODY visualization module.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Each satellite’s galactocentric position (top panels) and velocity (bottom panels) as a function of time. Gray-shaded regions illustrate the virial radius of the host’s halo. The satellite in MW–LMC analog (left panels) is on an eccentric orbit that after two pericentric passages merges with the host. A similar behavior is seen in the MW–LMC idealized simulations (right panels) for the most massive LMC models (LMC3 and LMC4). In the middle panel, the low-mass satellite exhibits a more circular orbit that merges with the host at the third pericentric passage.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: The successful imaging and detection of three stellar distance indicators in NGC 4536. Left: DECaLS gri image. Footprints of the JWST/NIRCam (pair of white squares), NIRISS (singular white square), and archival HST/Advanced Camera for Surveys (ACS; red square) imaging are plotted, with the overlap of the JWST and HST imaging marked (white hatched). North is up, east is left. The outer region of the galaxy adopted for TRGB analysis lies outside the indicated elliptical radius (white ellipse) of the galaxy’s disk (b/a = 0.36, θ = 120.°7), which is adopted from HyperLEDA (D. Makarov et al. 2014) (http://leda.univ-lyon1.fr/) and corresponds to a distance along its semimajor axis (SMA) equal to ﹩7.^{\prime} 5﹩. Middle column: JWST/NIRCAM color image (Red: F444W, green: (F115W + F444W)/2, and blue: F115W). NIRCam module A is aimed at the spiral arm where H II regions are apparent and the locations of Cepheid variables from A. G. Riess et al. (2016, 2022) are overplotted (white dots with black outline). In the other NIRCam module, plentiful, highly reddened galaxies are seen in the background. Two regions are highlighted (white rectangles) to emphasize where each of the JAGB and TRGB stars are well measured, respectively. Right: zoomed views of the two rectangular regions. The carbon-enhanced JAGB stars (top rectangle) appear red and are clearly distinguished from the RGB stars, which appear blue (relative to 4.4 μm). The JAGB stellar density also falls off more quickly in radial distance than that of the RGB’s due to the galaxy’s outer disk profile being steeper than that of its stellar halo.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: The simultaneous identification of three stellar distance indicators in NGC 4536 is demonstrated by overlaying three distinct stellar populations on the CMD. Black points are all stars contained in the halo selection (see Figure 2), with the green lines outlining the TRGB feature (explored in detail later). Orange points are the JAGB stars selected in the outer disk region via their colors (F115W – F444W > 2.2 mag). Blue points are Cepheids, which predominantly occupy the inner disk region.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: Sources brighter than the approximately identified TRGB magnitude (see Figure 3) are plotted as dots. The spiral arm is clearly revealed in the upper module and contained in the inner disk selection (black dots). The dearth of sources in the outermost region of the imaging (green dots) is the hallmark of an old stellar population, i.e., a spatial manifestation of the TRGB. The intermediate region is identified as the “outer disk” (orange dots). The interplay between this diagnostic and Figure 3 was used to converge on spatial selections for the JAGB and TRGB measurements.
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Pulse profiles for the stars in Figures 1 (left) and 2 (right) with total mass M  T  = 1.4 M ⊙. All stars have a rotation frequency of ν = 200 Hz in the observer’s frame and θ  c  = ζ = π/4.
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Relative changes in gravitational self-lensing due to DM halos for DANSs with ﹩{M}_{T}\left({R}_{B}\right)=2.00{M}_{\odot }﹩ and f  χ  = 0.05. Changes are relative to the no-halo counterpart of each DANS with equal R  B  and mass ﹩{M}_{T}={M}_{T}\left({R}_{B}\right)=2.00{M}_{\odot }﹩. Spin frequency and spot and observer geometries are the same as in Figure 6.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: Cepheid PLR constructed directly from the measured F115W magnitudes and periods from the latest SH0ES sample of 28 Cepheids (R22). No correction has been applied for local scene crowding (see, e.g., A. G. Riess et al. 2016, for a description) nor for extinction. The value of the best-fit slope is −3.15 ± 0.21 mag mag−1, and the dispersion about that slope is 0.240 ± 0.024 mag. The typical F115W photometric uncertainties are 0.015 mag and smaller than the plotted markers.
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Relative changes in gravitational self-lensing due to DM halos for DANSs with ﹩{M}_{T}\left({R}_{B}\right)=1.33{M}_{\odot }﹩ and f  χ  = 0.05. Changes are relative to the no-halo counterpart of each DANS with equal R  B  and mass ﹩{M}_{T}={M}_{T}\left({R}_{B}\right)=1.33{M}_{\odot }﹩. Spin frequency and spot and observer geometries are the same as in Figure 6.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: JAGB carbon star F115W LF, i.e., marginalizing over color for the orange points in Figure 3. The black curve is a kernel density estimate (KDE) of the distribution with modal value equal to 25.036 ± 0.056 mag.
Paper: Forecasts for Helium Reionization Detection with Fast Radio Bursts in the Era of Square Kilometre Array
Authors: Jun-Jie Wei, Chong-Yu Gao
Figure caption: The fractional uncertainty on a measured DMIGM, contributed by the IGM scatter (σ IGM) and the uncertainty of the DM contributions from both the Milky Way halo and the FRB host galaxy (σ halo, host) as a function of redshift. Curves show the quadrature sums of the two contributions for three cases with different σ halo, host values: 0 (blue solid line), 50 (yellow dashed line), and 100 pc cm−3 (green dotted line).
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: (a) Initial magnetic field. (b) Side view of the initial simulation grid blocks (each block contains 8 × 8 × 8 grid cells). (c) Surface driving profile. The PIL is shown in gray in each panel.
Paper: Forecasts for Helium Reionization Detection with Fast Radio Bursts in the Era of Square Kilometre Array
Authors: Jun-Jie Wei, Chong-Yu Gao
Figure caption: PDFs of redshifts derived from the SFH model and three compact star merger models with different merger delay time distributions (Gaussian, lognormal, and power law).
Paper: Forecasts for Helium Reionization Detection with Fast Radio Bursts in the Era of Square Kilometre Array
Authors: Jun-Jie Wei, Chong-Yu Gao
Figure caption: One-dimensional marginalized probability distributions and 1–2σ constraint contours for the reionization parameters A He and ﹩{z}_{\mathrm{re}}﹩ using 104 simulated FRB events. The solid and dashed contours correspond to the cases of z distribution tracing the SFH model and the compact star merger model with power-law merger delay time distribution, respectively. The vertical dotted lines mark the input parameter values used to generate the FRB mocks.
Paper: Forecasts for Helium Reionization Detection with Fast Radio Bursts in the Era of Square Kilometre Array
Authors: Jun-Jie Wei, Chong-Yu Gao
Figure caption: Sensitivity of the S/N = A He/σ(A He) for the detection of He II reionization and the uncertainty on the reionization redshift ﹩\sigma ({z}_{\mathrm{re}})﹩ to the fiducial value of ﹩{z}_{\mathrm{re}}﹩. All the constraints are derived from 104 simulated FRBs for the cases of z distribution following the SFH model (left panel) and the power-law delay model (right panel).
Paper: Forecasts for Helium Reionization Detection with Fast Radio Bursts in the Era of Square Kilometre Array
Authors: Jun-Jie Wei, Chong-Yu Gao
Figure caption: Best-fit reionization parameters (A He and ﹩{z}_{\mathrm{re}}﹩) and their corresponding 1σ uncertainties as a function of the number of simulated FRB data. The star and circle symbols correspond to the cases of z distribution tracing the SFH and power-law delay models, respectively. The horizontal dashed lines stand for the fiducial values.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: (a), (b) Two views of the flux rope (yellow field lines) formed within the sheared filament channel at the end of the driving period (t = 6 hr 57 minutes). Magenta field lines show short flare loop field lines. (c) ∣v∣ showing the pre-eruption plasma jet (analyzed by P. F. Wyper et al. 2022). (d) Synthetic white-light base-difference image (7 hr 30 minutes–6 hr 32 minutes) showing the pre-eruption dimming.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: LASCO C2 running difference images (G. E. Brueckner et al. 1995) showing the different morphologies of CMEs originating from pseudostreamers. (a), (b) Two narrow jet-like events. (c), (d) Fan-shaped CME and its precursor jet. (e), (f) Broad bubble-like CME and its precursor jet. Adapted from P. Kumar et al. (2021).
Paper: The Role of Magnetic Skeleton in Solar Flare Filaments Activity
Authors: Juan Guo, Huaning Wang, Jingxiu Wang, Xiaoshuai Zhu, Jing Huang, Shanqiang Chen, Bingxian Luo, Siqing Liu, Yuanyong Deng, Jiaben Lin
Figure caption: 3D magnetic topology-based NLFFF extrapolation and the activity features. Top panels: magnetic topology over HMI line-of-sight magnetogram. The yellow field lines demonstrate the 3D magnetic skeleton related to the inferred coronal null point (the red star), with the right closed fan spreading out download into some main negative sunspot and the left semiopen fan spreading out of the extrapolation box. The small purple lines beneath the closed fan outline a sheared arcade over the magnetic neutral line, which exhibits similar features and location as the small filament before the eruption. The magnetic pressure is imaged on an inclined cross section crossing the coronal null point and near the sheared arcade (panel (b)) and on a horizontal cross section just over the sheared arcade (panel (d)–(e)). The magnetic pressure at the coronal null point is about 7.5 × 10−6 G2. Bottom panels: AIA 131 Å image showing a hot channel expanding showing a projected ejection region in the ejection region of the magnetic skeleton (panel (c) and (e)).
Paper: Efficient Stochastic Template Bank Using Inner Product Inequalities
Authors: Keisi Kacanja, Alexander H. Nitz, Shichao Wu, Marco Cusinato, Rahul Dhurkunde, Ian Harry, Tito Dal Canton, Francesco Pannarale
Figure caption: Stochastic Bank algorithm diagram. Points are randomly sampled from the prior distribution and within distinct bins defined by chirp time τ 0. Waveforms are then generated with a reduced frequency model. When a template is proposed, we assess if including the proposal in the template bank will improve the coverage of the desired parameter space. This assessment is outlined in the blue box and involves comparing the proposed template with the nearest neighboring templates in chirp time. Templates are added to the bank if the match between the proposed template and the accepted templates falls below the minimal match condition. If the match exceeds the minimal match condition, the bank is deemed adequately covered in that region. Match calculations are stored to streamline the process and avoid redundant computations for new proposed templates, utilizing a triangle inequality for efficient comparisons. Upon completing comparisons and reaching the minimal match threshold, tolerance checks, outlined in red, ensure the bank’s coverage adequacy. If the tolerance condition is unmet, additional samples are drawn, either stochastically from the prior distribution or with a Gaussian Kernel Density Estimation method. The methods are swapped if one technique performs better than the other, as depicted in the beige box. Proposals are once again compared with the accepted templates. Once the tolerance condition is satisfied, accepted templates are saved and the process iterates for subsequent bins until the entire bank is sufficiently covered. The red arrows represent the checks and repetition in method required to fulfill either tolerance or minimal match conditions.
Paper: Efficient Stochastic Template Bank Using Inner Product Inequalities
Authors: Keisi Kacanja, Alexander H. Nitz, Shichao Wu, Marco Cusinato, Rahul Dhurkunde, Ian Harry, Tito Dal Canton, Francesco Pannarale
Figure caption: Cumulative distribution of FFs achieved by the template banks with varying minimal match (top) and varying tolerance (bottom). The minimal matches are fixed to be 0.8, 0.9, and 0.95 in the colored vertical lines and a fixed tolerance of 0.01 in the red horizontal. The tolerances for the bottom plot vary from 0.05, 0.01, and 0.005 in colored vertical dashed lines and a fixed minimal match of 0.95 in a red horizontal line. All plots achieve tolerance at the minimal match condition or before minimal match. We compare how our method performs with an existing stochastic method (P. Ajith et al. 2014; C. Capano et al. 2016) by choosing the same parameter space, minimal match of 0.95, and a convergence criteria of 1000. This bank is comparable to our method generated with a tolerance of 0.01.