adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Bars Form Dark Matter Counterparts in TNG50
Authors: Neil Ash, Monica Valluri, Yingtian Chen, Eric F. Bell
Figure caption: Evolution of the bar pattern speed for subhaloID 574286 over the last 8 Gyr. The bar pattern speed was measured using both the Wigner ﹩{ \mathcal D }﹩-matrix method using the star particles (cyan line) and by a CWT using the stellar and DM particles at ∼2.1 comoving kpc averaged over all five quadrupolar BFE terms. The pattern speeds of the DM and stellar bars evolve synchronously throughout the last 8 Gyr, and slow down for most of the evolution until they are spun up by a merger beginning around ∼2 Gyr ago. This merger is evident in the power in aspherical terms (l > 0) of the density BFE in DM (see Figure 4), along with several others. Approximate pericenter passages are marked by the magenta dashed lines.
Paper: Stellar Bars Form Dark Matter Counterparts in TNG50
Authors: Neil Ash, Monica Valluri, Yingtian Chen, Eric F. Bell
Figure caption: Cumulative power in the aspherical terms of the DM density BFE. The presence of several massive satellites is evident. Approximate pericenter passages are marked by the magenta dashed lines.
Paper: Luminosity Function of Collapsar Gamma-Ray Bursts: The Progenitor of Long Gamma-Ray Bursts Is Not Singular
Authors: Yan-Kun Qu, 艳坤 屈, Zhong-Xiao Man, Shuang-Xi Yi, 双喜 仪, Yu-Peng Yang, 玉鹏 杨
Figure caption: The green data points represent the luminosity distribution of 301 long GRBs with P ≥ 1 photon cm−2 s−1. The solid lines depict the luminosity distribution of collapsar GRBs as predicted by different models. For comparison, we also plot the luminosity distribution of long GRBs predicted by different models from G.-X. Lan et al. (2021; gray dashed lines). From left to right, the models are the no evolution model, luminosity evolution model, and density evolution model.
Paper: Luminosity Function of Collapsar Gamma-Ray Bursts: The Progenitor of Long Gamma-Ray Bursts Is Not Singular
Authors: Yan-Kun Qu, 艳坤 屈, Zhong-Xiao Man, Shuang-Xi Yi, 双喜 仪, Yu-Peng Yang, 玉鹏 杨
Figure caption: The luminosity distribution of 134 long GRBs with z ≥ 2 and P ≥ 1 photons cm2 s−1. The three curves represent the best-fit expected luminosity distributions of three different models. The shaded areas indicate the 1σ errors.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: The metallicity radial gradient from both the N2 (left) and the O3N2 (right) indices. The right-side y-axis in both panels shows the corresponding gas-phase metallicity calculated from the calibration equations derived in M. Curti et al. (2020). The black solid line shows the best linear fit to all of the data, and the red and dark red shaded regions signify the 3σ and 5σ, respectively, confidence intervals of the fit. For y = 12 + log(O/H), the slopes of the fit are −0.017 and −0.020 dex kpc−1, respectively. The color bar shows the absolute difference between the Hα emission line velocity offset and the mass-weighted H I 21 cm velocity of the ISM in the region. Regions 15 and 19, which are labeled and are at 6.1 and 7.2 kpc, show both anomalously low metallicity and a high velocity difference. The blue line shows the fit without the two ALM regions. The fits (slopes and intercepts) are presented in Table A2.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: (Left) The metallicity radial metallicity profiles found from our 26 H II regions in dex/R 25 in comparison to the four CHAOS galaxies from D. A. Berg et al. (2020). NGC 99 (green and pink solid lines) has a shallower slope than all of the CHAOS galaxies. The shaded regions indicate the 1σ error. (Right) A histogram of metallicity gradients in 504 galaxies found by L. S. Pilyugin et al. (2023). The green arrow indicates where NGC 99 fits in this distribution. The black arrow indicates the metallicity gradient observed in the Milky Way.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: (Left) The gas-phase metallicity of the 26 H II regions is shown as a function of gas fraction with the points color coded by effective yield, y eff. A closed-box model is assumed to calculate effective yield. The lines show the true yield, y O, found by C. Leitherer et al. (2014; dash) and F. Vincenzo et al. (2016b; solid and dashed–dotted, respectively). (Right) For the same H II regions, the effective yield is now shown as a function of galactocentric radius color coded by gas fraction. All of the H II regions have an effective yield lower than the true yield found by F. Vincenzo et al. (2016b). The effective yield is constant across the disk of the galaxy. The two ALM H II regions, numbers 15 and 19, are marked.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: The Balmer decrement of each H II region as a function of its galactocentric radius (left) and star formation rate (right). The associated error bars are overplotted in red. The observed H II regions within 10 kpc of the center of NGC 99 show a flat radial distribution. H II regions outside of 10 kpc show wide scatter.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: COS spectra of the Lyα transition plotted at the rest frame of NGC 99 (z = 0.0177). The best combined profile is plotted in red, and the resulting column density estimate is shown in the upper right. The dominant absorption component (A) is −44 km s−1 offset from the systemic velocity of the galaxy, with three weaker components (B–D) located at 34 km s−1, 99 km s−1, and 366 km s−1. Lyα is the only detected species associated with the galaxy’s CGM. Measurements for Lyα and upper limits for the metal lines are presented in Table 2.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: Optical image (left) of NGC 99 (top left of image) and its companion J002353.17+154356.8 (bottom right of image) from the DESI Legacy Survey (A. Dey et al. 2019). The projected distance between the objects is 57 kpc. (right) The optical spectrum showing the Hα and [N II]λ6583 emission lines of J002353.17+154356.8 obtained with the MMT using the Binospec instrument. The redshift was measured to be 0.01747.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: Distribution of 26 H II regions (filled gold circles) on a background of hexagon bins from SDSS-DR8 galaxies (left) and from CALIFA H II regions (right). The color bar shows the number of galaxies or H II regions in each bin. The data points show a 0.5–1.0 dex offset in [S II] from the majority of SDSS galaxies and CALIFA H II regions.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption:  r-band images of the NGC 99 with the locations H II regions indicated by the circles, which are color coded based on their gas-phase metallicity (left) and velocity offset of the Hα emission line (right). Regions 15 and 19 show abnormally low metallicities and high velocities relative to their surrounding regions.
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: A typical MMT/Binospec spectrum of an H II region in NGC 99. The flux is shown in log scale to show the level of the underlying stellar continuum. The three insets highlight the emission lines of interest in this study.
Paper: Interaction of the Prominence Plasma within the Magnetic Cloud of an Interplanetary Coronal Mass Ejection with the Earth’s Bow Shock
Authors: Hadi Madanian, Li-Jen Chen, Jonathan Ng, Michael J. Starkey, Stephen A. Fuselier, Naoki Bessho, Daniel J. Gershman, Terry Z. Liu
Figure caption: An overview of the upstream density structure and its interaction with the bow shock on 2023 April 24. Panels (a) and (b) show the magnetic field and proton and alpha particle densities in the pristine solar wind. Magnetic field measurements (c), ion energy flux spectra (d), electron density (red), temperature (black), and ion density (blue; (e)) across the bow shock are also shown. Density peaks of the double-peak structure are annotated on panel (b). Data in panels (a) and (b) are from the Wind spacecraft time shifted by ∼42 minutes, while panels (c)–(e) show MMS1 spacecraft measurements. The regular magnetosheath (“Msheath”), enhanced magnetosheath (“En Msheath”), and solar wind (SW) regions in MMS data are identified above panel (c). The bow shock is marked with a dashed vertical line. The instance of initial plasma compression is identified by the dashed box on panel (e).
Paper: Interaction of the Prominence Plasma within the Magnetic Cloud of an Interplanetary Coronal Mass Ejection with the Earth’s Bow Shock
Authors: Hadi Madanian, Li-Jen Chen, Jonathan Ng, Michael J. Starkey, Stephen A. Fuselier, Naoki Bessho, Daniel J. Gershman, Terry Z. Liu
Figure caption: Two-dimensional phase-space ion distributions in the V ∣∣−V ⊥1 plane downstream (first and second columns) and upstream (third column) of the bow shock. Data in the first row are from the FPI instrument, while the second and third rows show data from the HPCA instrument. Distributions in panels (a)–(c) include all ions. Panels (d)–(f) show alpha particles, and panels (g)–(i) show He+ distributions. V ⊥1 is along the component of the population flow velocity perpendicular to the local magnetic field.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The Voigt profile fit for the M3 sight line (NGC 5272-ZNG1). The black dashed line shows the joint fit including all the absorption components. We separate two intermediate-velocity gas clouds, IVa and IVb (blue solid lines), from the Milky Way ISM (green shaded) and star (gray shaded). The component labeled IVa is well detected in highly ionized metal species, but is severely blended with saturated absorption from the Milky Way in a few low-ionization metal species (red labels), which makes it impossible to constrain gas column densities from those absorption lines. We mark IVC nondetections in a given ion species with a purple label.
Paper: Interaction of the Prominence Plasma within the Magnetic Cloud of an Interplanetary Coronal Mass Ejection with the Earth’s Bow Shock
Authors: Hadi Madanian, Li-Jen Chen, Jonathan Ng, Michael J. Starkey, Stephen A. Fuselier, Naoki Bessho, Daniel J. Gershman, Terry Z. Liu
Figure caption: Counts of simulated particles for (a) protons, (b) He+, and (c) alpha particles.
Paper: Interaction of the Prominence Plasma within the Magnetic Cloud of an Interplanetary Coronal Mass Ejection with the Earth’s Bow Shock
Authors: Hadi Madanian, Li-Jen Chen, Jonathan Ng, Michael J. Starkey, Stephen A. Fuselier, Naoki Bessho, Daniel J. Gershman, Terry Z. Liu
Figure caption: (a)–(c) Downstream temperatures for protons, He+, and alpha particles, respectively. Parallel (red) and perpendicular (blue) temperatures are shown. (d)–(e) Downstream ion velocities for protons, He+, and alpha particles, respectively.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: 3D distribution of the targeted GCs in the Galactocentric system where the Galactic center lies at (0, 0, 0) kpc and the Sun is at (−8.122, 0, 0) kpc. We mark the GC sight lines where IVCs or/and HVCs are detected in the UV spectrum as “DHI detection” (blue star). A “DHI nondetection” (gray star) indicates that gas kinematically distinct from the Milky Way ISM was not present in the spectrum.
Paper: Interaction of the Prominence Plasma within the Magnetic Cloud of an Interplanetary Coronal Mass Ejection with the Earth’s Bow Shock
Authors: Hadi Madanian, Li-Jen Chen, Jonathan Ng, Michael J. Starkey, Stephen A. Fuselier, Naoki Bessho, Daniel J. Gershman, Terry Z. Liu
Figure caption: Wind spacecraft observations of the ICME. Panel (a) shows magnetic field strength measurements over 2 days starting on 2023 April 23. Different components of the ICME, namely, the interplanetary shock, sheath, and the magnetic cloud are annotated on this panel. Proton (cyan) and alpha particle (yellow) densities in panel (b) are shown during the period of the double-peak density structure within the magnetic cloud associated with the prominence plasma.
Paper: Double-edged Sword: The Influence of Tidal Interaction on Stellar Activity in Binaries
Authors: Yuedan Ding, Shidi Zhang, Henggeng Han, Wenyuan Cui, Song Wang, Min Fang, Yawei Gao
Figure caption:  S indices vs. rotation periods for single stars (red dots) and orbital periods for binaries. The pluses represent the median S-index value in each period bin, and the uncertainties are calculated using the 16th and 84th percentiles. The shaded region indicates the 16th and 84th percentiles of S indices for binaries with periods ranging from 0.7 to 7 days.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption:  Redback modeling results for SN 2021ywf, with the arnett + tophat model above and the Radio SSA model below.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption:  Redback modeling results for SN 2020tkx, with the arnett + tophat model above and the Radio SSA model below.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2020wgz, SN 2020abxl, and SN 2020abxc.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2020adow, SN 2021bmf, and SN 2021epp.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2021ncn, SN 2021too, and SN 2021ywf.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2020jqm, SN 2020lao, and SN 2021qjv.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2021fop, SN 2021hyz, and SN 2021ktv.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2020dgd, SN 2020hes, and SN 2020hyj.
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2020rfr, SN 2020rph, and SN 2020tkx.
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: Illustration of two coordinate systems. (a) One is a Cartesian coordinate system (x, y, z) with the z-axis along the magnetic axis (unit vector ﹩\hat{{\boldsymbol{m}}}﹩), sharing the same origin  O  with its corresponding spherical coordinate system (r, θ, ϕ). In the latter, r is the radius, and θ and ϕ are the magnetic colatitude and azimuth, respectively. (b) The other is a system (X, Y, Z) whose Z-axis is in the direction of the LOS (unit vector ﹩\hat{{\boldsymbol{n}}}﹩), and the X-axis in the plane of ﹩\hat{{\boldsymbol{n}}}﹩ and the star spin axis (unit vector ﹩\hat{{\boldsymbol{\Omega }}}﹩). Correspondingly, its spherical coordinate system (r, Θ, Φ) has inclination Θ and azimuth Φ with respect to the LOS. Thus, ﹩\hat{{\boldsymbol{m}}}﹩ has a coordinate (Θ m , Φ m ) in this system. The angles that the spin axis makes with the LOS and the magnetic axis are denoted as χ and ς, respectively.
Paper: Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Shu-Qing Zhong, Long Li, Biao Zhang, Zi-Gao Dai
Figure caption: The picture illustrates three commonly discussed models that generate an FXRB: (a) the emission from a trapped fireball modified by RCS; (b) an outflow from a trapped-expanding fireball along open magnetic field lines; and (c) the far-away synchrotron radiation in a forward shock due to the interaction of relativistic ejecta and an ion shell.