adsabs/AstroCLIMB huggingface dataset:
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: Element number ratios in the star at the end of Si burning. The masses used to calculate the ratios at a mass coordinate are cumulative, from the stellar atmosphere on the right to the depth corresponding to the given mass loss on the left.
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: The multiwavelength light curves of Ansky showing a double-peaked structure with long rise and decline timescales in the optical bands. The black vertical line marks the date of our HST/STIS observation, while the gray dashed line indicates the first epoch of detected QPE. The blue and red dashed lines represent the fitted Gaussian rises in the g and r bands, respectively. The dotted line shows the power-law decline. The optical light curves are binned in 10 day intervals, with the original unbinned data overplotted in the background with reduced opacity. The shaded region highlights the rebrightening phase.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: Top panel: the HST STIS spectrum of Ansky observed on 2025 May 24 UT. The red and green dashed lines represent our best-fit blackbody and power-law models, respectively. Bottom panel: the residual spectrum after subtracting the power-law fitting component. The blue dashed line indicates the location of C IV λ1549.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: The fit to the UV-optical photometric SED of Ansky and comparison with the UV-optical spectra. The green and red dashed lines represent the power-law and blackbody fitting of the SED, respectively. The black and gray lines show the UV (HST/STIS on 2025 May 24) and optical spectra (LRIS/Keck on 2025 June 1), respectively. The blue solid dots denote the photometric measurements of Ansky at the epoch quasi-simultaneously with the UV spectroscopic observation. The far-UV spectrum provides the strongest evidence for the deviation from a lower-temperature blackbody model. The excess of optical spectra over photometry at λ > 4000 Å is due to the strong host contamination.
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: Left panel: the HST ACQ image taken on 2025 May 24 UT in the clear filter. Middle panel: the fitted model of SDSSJ1335+0728. Right panel: the residual image from our fit. The center of the galaxy SDSS J1335+0728 is marked with a red circle of radius ﹩0\mathop{.}\limits{^{\prime\prime} }2﹩.
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: Rest-frame optical spectra of Ansky. Each spectrum is labeled by the instrument employed and the date of observation.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: The evolution of blackbody temperature, radius, and luminosity of Ansky from top to bottom, respectively. Note that black circles denote fits constrained by UV photometry, while blue circles indicate fits without real UV constraints. The red line represents a power-law decay fit with an index of −0.51.
Paper: Ion-scale Solitary Structures in the Solar Wind Observed by Solar Orbiter and Parker Solar Probe
Authors: Yufei Yang, 宇菲 杨, Timothy S. Horbury, Domenico Trotta, Lorenzo Matteini, Joseph H. Wang, Andrey Fedorov, Philippe Louarn, Stuart D. Bale, Marc Pulupa, Davin E. Larson, Roberto Livi, Michael L. Stevens, Milan Maksimovic, Yuri V. Khotyaintsev, Andrea Larosa
Figure caption: Statistical analysis results of the ion-scale solitary structures data set. (a) Normalized occurrence rate (events per day), representing the aggregated occurrence rate across data sets adjusted for data availability and scaled to address methodological differences and (b) fractional magnetic field enhancement (δ∣B∣/〈∣B∣〉), both presented as functions of radial distance. Error bars in (a) represent standard errors, assuming occurrences are Poisson random variables. (c) Distributions of convected event radial widths, Δr, normalized by proton inertial length (dp) and proton Larmor radius (ρp), with separate frequency plots for events from Solar Orbiter (SO) and Parker Solar Probe (PSP). (d) δ∣B∣/〈∣B∣〉 plotted against proton beta (βp) for each event. The blue dashed line represents the theoretical upper bound ﹩\sqrt{1+{\beta }_{{\rm{p}}}}-1﹩ on δ∣B∣/〈∣B∣〉, restricted by βp under pressure-balance conditions. Legends label data sources by method: manually identified events (SO manual: blue circles; PSP manual: orange crosses) and ML-detected events (PSP ML: green triangles).
Paper: Ion-scale Solitary Structures in the Solar Wind Observed by Solar Orbiter and Parker Solar Probe
Authors: Yufei Yang, 宇菲 杨, Timothy S. Horbury, Domenico Trotta, Lorenzo Matteini, Joseph H. Wang, Andrey Fedorov, Philippe Louarn, Stuart D. Bale, Marc Pulupa, Davin E. Larson, Roberto Livi, Michael L. Stevens, Milan Maksimovic, Yuri V. Khotyaintsev, Andrea Larosa
Figure caption: Examples of ion-scale solitary structures observed by SO (a), (b) and PSP (c), showing magnetic field profiles and plasma density in the RTN frame. Each panel presents BR, BT, BN, ∣B∣, and high-resolution electron number density NE during the event. The legend specifies the heliocentric distance to the Sun in astronomical units, the proton beta (βp), and the event width normalized by the proton inertial length (dp) for each event. Note: NE is not available for event (b).
Paper: Ion-scale Solitary Structures in the Solar Wind Observed by Solar Orbiter and Parker Solar Probe
Authors: Yufei Yang, 宇菲 杨, Timothy S. Horbury, Domenico Trotta, Lorenzo Matteini, Joseph H. Wang, Andrey Fedorov, Philippe Louarn, Stuart D. Bale, Marc Pulupa, Davin E. Larson, Roberto Livi, Michael L. Stevens, Milan Maksimovic, Yuri V. Khotyaintsev, Andrea Larosa
Figure caption: An example of a multiple-event period observed by SO. Panels show (a) BR and VR, (b) BT and BN; (c) ∣B∣, Np (proton number density), and NE (electron number density); (d) magnetic, plasma (evaluated using high-resolution electron number density and proton temperature), and total pressures; and (e) plasma β, calculated using the magnetic and plasma pressures. Triangles across the panel grid lines indicate the occurrence of each event.
Paper: Magnetars in Binaries as the Engine of Actively Repeating Fast Radio Bursts
Authors: Bing Zhang, Rui-Chong Hu
Figure caption: Various magnetar formation channels through single and binary evolution. Magnetars with a black-colored magnetic field background are isolated, while those with a light-colored background are in binary systems. The figure also shows the magnetar’s spin axis (white) and magnetic axis (orange; when misaligned from the spin axis), with the curved orange arrow indicating the flip evolution of the magnetic axis. The dashed lines indicate that, in some cases, the spin and magnetic axes of magnetars differ from what the flowchart shows.
Paper: Ion-scale Solitary Structures in the Solar Wind Observed by Solar Orbiter and Parker Solar Probe
Authors: Yufei Yang, 宇菲 杨, Timothy S. Horbury, Domenico Trotta, Lorenzo Matteini, Joseph H. Wang, Andrey Fedorov, Philippe Louarn, Stuart D. Bale, Marc Pulupa, Davin E. Larson, Roberto Livi, Michael L. Stevens, Milan Maksimovic, Yuri V. Khotyaintsev, Andrea Larosa
Figure caption: Normalized distributions of angle θ between the background magnetic field (B0) and (a) the radial direction, (b) the minimum-variance direction (﹩{{\boldsymbol{e}}}_{{\rm{\min }}}﹩), and (c) the maximum variance direction (﹩{{\boldsymbol{e}}}_{{\rm{\max }}}﹩). Legends are shared across all panels and represent events from Solar Orbiter (SO events) and randomly sampled intervals without events (SO nonevents).
Paper: Magnetars in Binaries as the Engine of Actively Repeating Fast Radio Bursts
Authors: Bing Zhang, Rui-Chong Hu
Figure caption: Fractions of magnetars from different formation channels based on the fiducial model. Different bars represent different magnetar formation fractions among all NSs.
Paper: Global Compressive Oscillations in the Outer Solar Corona Driven by an Extreme Coronal Mass Ejection
Authors: Suzana S. A. Silva, J. J. González-Avilés, Pete Riley, Michal Ben-Nun, Erico L. Rempel, Leonardo F. G. Batista, Gary Verth, Istvan Ballai, Chia-Hsien Lin, Luiz A. C. A. Schiavo, Viktor Fedun
Figure caption: Top-left panel: 3D view of the simulation domain, 12 hr after CME onset. This panel shows the proton number density, volume-rendered and saturated at 500 particles cm–3, highlighting the propagating CME structure. The blue line indicates the direction of CME propagation. Top-right and bottom panels: time–distance diagrams of the perturbation reconstructions for the variables ﹩{\mathrm{log}}_{10}(p)﹩, ﹩{\mathrm{log}}_{10}({N}_{p})﹩, ﹩{\mathrm{log}}_{10}({T}_{p})﹩, vx, vy, and vz, using modes 1–2, 3–4, and 5–6. The symbol ﹩^{\prime} ﹩ denotes perturbed variables, and the time–distance profiles were computed along the blue line shown in the top-left panel. The red dashed line marks the onset of the CME in the simulation.
Paper: Early Evidence for Polar Orbits of Sub-Saturns around Hot Stars
Authors: Emma Dugan, Xian-Yu Wang, Agustin Heron, Hareesh Gautham Bhaskar, Malena Rice, Cristobal Petrovich, Songhu Wang
Figure caption: Top left: local CCFs (out-of-transit to in-transit) in the stellar rest frame behind TOI-1135b. The solid orange lines represent local CCFs at disk positions with 〈μ〉 ≥ 0.4, dashed orange lines correspond to 0 < 〈μ〉 < 0.4, and gray lines indicate out-of-transit regions. Bottom left: a two-dimensional map of the local CCFs, color-coded by local flux. Top right: local RVs derived from local CCFs where 〈μ〉 ≥ 0.4, with the two best-fit models (orange: differential rotation + center-to-limb quadric model with i⋆ < 90°; gray: solid body + center-to-limb quadric model) shown as dashed lines. Bottom right: residuals corresponding to the two models shown above.
Paper: Early Evidence for Polar Orbits of Sub-Saturns around Hot Stars
Authors: Emma Dugan, Xian-Yu Wang, Agustin Heron, Hareesh Gautham Bhaskar, Malena Rice, Cristobal Petrovich, Songhu Wang
Figure caption: Projected spin–orbit angle as a function of stellar effective temperature for transiting exoplanets. The top panel shows sub-Saturns, while the bottom panel displays hot Jupiters. The vertical dashed line indicates the Kraft break at 6100 K, separating stars with convective envelopes (cooler) from those with radiative envelopes (hotter). TOI-1135b is marked with a red star and labeled for reference. The predicted relationship between Teff  and λ from secular resonance crossing (C. Petrovich et al. 2020) is shown as the shaded gray region.
Paper: Global Compressive Oscillations in the Outer Solar Corona Driven by an Extreme Coronal Mass Ejection
Authors: Suzana S. A. Silva, J. J. González-Avilés, Pete Riley, Michal Ben-Nun, Erico L. Rempel, Leonardo F. G. Batista, Gary Verth, Istvan Ballai, Chia-Hsien Lin, Luiz A. C. A. Schiavo, Viktor Fedun
Figure caption: Time–distance diagrams along the blue line shown in Figure 2, reconstructed from the simulated white-light perturbations using modes (a) 1–2, (b) 3–4, (c) 5–6, and (d) 7–8. For each mode pair, the left panel shows the temporal evolution of the reconstructed perturbation as a function of heliocentric distance, while the right panel displays the corresponding FFT of the signal extracted at R = 0.50 au, with the dominant oscillation period (T) indicated in each plot. The onset of the CME is marked by the dashed dark-cyan line.
Paper: Global Compressive Oscillations in the Outer Solar Corona Driven by an Extreme Coronal Mass Ejection
Authors: Suzana S. A. Silva, J. J. González-Avilés, Pete Riley, Michal Ben-Nun, Erico L. Rempel, Leonardo F. G. Batista, Gary Verth, Istvan Ballai, Chia-Hsien Lin, Luiz A. C. A. Schiavo, Viktor Fedun
Figure caption: Analysis of LASCO C3 white image perturbations using selected modes of SPOD. The top panel shows a polar representation of the corona with concentric circles. The right panels display the corresponding time–distance diagrams for each circle, where the vertical axis represents the angle along the curve, and the horizontal axis indicates the time in hours. The CME onset is marked by the dark-cyan dashed line. Red and blue hues denote positive and negative fluctuations in the SPOD intensity modes.
Paper: Global Compressive Oscillations in the Outer Solar Corona Driven by an Extreme Coronal Mass Ejection
Authors: Suzana S. A. Silva, J. J. González-Avilés, Pete Riley, Michal Ben-Nun, Erico L. Rempel, Leonardo F. G. Batista, Gary Verth, Istvan Ballai, Chia-Hsien Lin, Luiz A. C. A. Schiavo, Viktor Fedun
Figure caption: Analysis of LASCO C3 white-light perturbations using selected modes of SPOD. Top row: LASCO C3 image a few hours after the CME onset, showing the three analyzed radial directions (lines 1–3). Middle panels: time–distance maps along each line. The first column shows intensity perturbations, while the second and third columns show reconstructions of perturbations using SPOD modes 4–5 and 7–8, respectively. The CME onset is marked by a dashed dark-cyan line. Red and blue hues represent positive and negative fluctuations in the perturbations or SPOD intensity modes. Bottom row: FFT power spectra of the reconstructed intensity fluctuations at 10 R⊙. The dashed red line marks the 99% confidence level derived from a Monte Carlo permutation test; spectral peaks above this line are statistically significant.
Paper: Global Compressive Oscillations in the Outer Solar Corona Driven by an Extreme Coronal Mass Ejection
Authors: Suzana S. A. Silva, J. J. González-Avilés, Pete Riley, Michal Ben-Nun, Erico L. Rempel, Leonardo F. G. Batista, Gary Verth, Istvan Ballai, Chia-Hsien Lin, Luiz A. C. A. Schiavo, Viktor Fedun
Figure caption: Running-difference LASCO C3 images of the 2012 July 23 CME at two representative times (03:54:06 UT, top row; 05:54:06 UT, bottom row). Left: original data. Right: filtered data after applying a Savitzky–Golay filter along the radial direction (window length 5, polynomial order 2) and a 10 × 10 median filter in the image plane.
Paper: Global Compressive Oscillations in the Outer Solar Corona Driven by an Extreme Coronal Mass Ejection
Authors: Suzana S. A. Silva, J. J. González-Avilés, Pete Riley, Michal Ben-Nun, Erico L. Rempel, Leonardo F. G. Batista, Gary Verth, Istvan Ballai, Chia-Hsien Lin, Luiz A. C. A. Schiavo, Viktor Fedun
Figure caption: Equatorial slice of the CME simulation 20 hr after launch. Panels show (a) radial velocity Vr (km s−1), (b) log of proton density Np (cm−3), (c) log of proton temperature Tp (K), and (d) radial magnetic field Br (nT). Red, black, and yellow arrows indicate, respectively, the forward shock and compression region, the reverse shock and magnetic distortions of the Parker spiral, and the shock heating at the forward front.
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption: pn images (0.2–12 keV) of the On-Pulse (left) and Off-Pulse (right) phase intervals for the region containing X−8 and X−2. The circles indicate the 95% positional uncertainty for each source.
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption: Allowed acceleration and acceleration derivative along the line of sight (alos and ﹩{\dot{a}}_{{\rm{los}}}﹩, respectively) for different values of the orbital period, mass of the donor star, and for two representative inclination angles of the orbital plane.
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption: pn lightcurves of X−8 in three energy bands, binned at 2 ks. The top three panels show the light curves in the 0.2–12 keV (total), 0.2–3 keV (soft), and 3–12 keV (hard) bands. The bottom panel shows the hardness ratio between the soft and hard bands. Time zero corresponds to 60864.794 MJD.
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption: pn spectra of X−8 fitted with an absorbed disk-blackbody. The left panel shows the Off-pulse spectrum, the right panel the On-pulse. Bottom panels show the residuals.
Paper: Discovery of a 9.67 s Pulsar in an Ultraluminous X-Ray Source in NGC 4631 with XMM-Newton
Authors: Lorenzo Ducci, Sandro Mereghetti, Fabio Pintore, Sinan Allak, Andrea Santangelo, Manami Sasaki, Patrick Kavanagh
Figure caption: Pulse profile of X−8 obtained from pn data in the energy band 0.2−12 keV. The profile is background-subtracted and corrected for the spin-up. The inset shows the pulsed fractions in two sub-bands.
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: Top panel: rising timescale (t1/2,rise) versus black hole mass (MBH). Bottom panel: peak blackbody luminosity (LBB) versus black hole mass (MBH). We compare Ansky (red dot) and AT2022gri (gold dot) with other optical TDEs (blue dots) from Y. Yao et al. (2023), with the featureless subclass indicated by black dots.
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: Comparison of the UV spectra of Ansky with those of other featureless TDEs (AT2022gri and AT2021ehb; Y. Yao et al. 2022). Also shown for comparison are the UV spectra of the prototype QPE source GSN069 (G. Miniutti et al. 2019; Z. Sheng et al. 2021), which is also likely a TDE; the SDSS quasar composite spectrum (T. W. Jensen et al. 2016); and a representative weak-emission-line quasar (SDSSJ090843.25+285229.8; J. D. Paul et al. 2022). The fluxes of AT2021ehb and GSN069 are scaled by the coefficients of 0.4 and 0.3, respectively.
Paper: Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
Authors: Jiazheng Zhu, Ning Jiang, Yibo Wang, Tinggui Wang, Luming Sun, Shiyan Zhong, Yuhan Yao, Ryan Chornock, Lixin Dai, Jianwei Lyu, Xinwen Shu, Christoffer Fremling, Erica Hammerstein, Shifeng Huang, Wenkai Li, Bei You
Figure caption: Schematic illustration of a featureless TDE occurring in the special environment of SDSSJ1335+0728.
Paper: Magnetars in Binaries as the Engine of Actively Repeating Fast Radio Bursts
Authors: Bing Zhang, Rui-Chong Hu
Figure caption: Illustration of three possible scenarios explaining the observed RM evolution in different FRBs. In each case, the left panel presents a cartoon showing different phases of a binary system and the surrounding environment of magnetars, with blue solid lines representing the orbits, white solid lines representing magnetic field lines, and white dashed lines representing the LOS. The right panel shows the corresponding RM evolution over time (case I, irregular RM evolution of FRB 20201124A, H. Xu et al. 2022; case II, RM reversals of FRB 20190520B, R. Anna-Thomas et al. 2023; case III, RM flare and RM reversals in FRB 20220529, Y. Li et al. 2025b).
Paper: Magnetars in Binaries as the Engine of Actively Repeating Fast Radio Bursts
Authors: Bing Zhang, Rui-Chong Hu
Figure caption: A schematic illustration of the physical configuration surrounding an accreting magnetar. The central sphere represents the magnetar, surrounded by an orange accretion disk. Three unit vectors are shown to indicate key orientations: the m vector (light blue) represents the magnetic axis (z-axis), the s vector (dark blue) denotes the magnetar’s spin axis, and the d vector (orange) is normal to the accretion disk plane (accretion disk axis).
Paper: Magnetars in Binaries as the Engine of Actively Repeating Fast Radio Bursts
Authors: Bing Zhang, Rui-Chong Hu
Figure caption: Fractions of different magnetar companion types, including MS star subtypes.
Paper: Cosmological Constraints on Nonphantom Dynamical Dark Energy with DESI Data Release 2 Baryon Acoustic Oscillations: A 3σ+ Lensing Anomaly
Authors: Shouvik Roy Choudhury, Teppei Okumura, Keiichi Umetsu
Figure caption: The CMB lensing-potential power spectrum for different values of the constant DE EoS w. The angular scale of sound horizon at recombination, ﹩{\theta }_{s}^{* }﹩, is kept fixed by adjusting H0.
Paper: Cosmological Constraints on Nonphantom Dynamical Dark Energy with DESI Data Release 2 Baryon Acoustic Oscillations: A 3σ+ Lensing Anomaly
Authors: Shouvik Roy Choudhury, Teppei Okumura, Keiichi Umetsu
Figure caption: The 68% and 95% marginalised contours in the w0,DE–wa,DE plane for different data combinations. The area to the right of the vertical dashed blue line and above the slanted dashed blue line represents the parameter space corresponding to quintessence-like or nonphantom dark energy.