adsabs/AstroCLIMB huggingface dataset:
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: A plot of midradio continuum star formation rate, SFRMRC vs. H α  estimated star formation rate in the context of that for FRB 20121102A (cyan), FRB 20190520B (magenta), and FRB 20201124A (dark green) with the SFRMRC of the first two estimated from their 1.5 GHz PRS luminosity. The SFRMRC plotted for FRB 20201124A is from the 6 GHz flux density and represents the lowest possible SFRMRC as indicated by the gray upward arrow. The location of the orange circle (20190417A-S1) indicates that there is an additional cause of radio emission responsible for the observed emission.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: VLA images—FRB 20180916B and FRB 20200120E. There is no radio source at the location of these FRBs. The red crosshairs indicate the subarcsecond position of the FRBs but are much larger than the representative of the positional uncertainties.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Optical images showing associations of the two potential radio sources from our sample. Left: DESI r-band field of FRB 20181030A showing the host galaxy of the FRB and the radio source—20181030A-S1. Right: Gemini North deep image of the field of FRB 20190417A. The yellow crosshair shows the location of the likely host of the radio source 20190417A-S1, which is the faint optical source near a bright star. The red “+” sign indicates the location of the radio source for both fields.
Paper: Slope of Magnetic Field–Density Relation as an Indicator of Magnetic Dominance
Authors: Mengke Zhao, Guang-Xing Li, Keping Qiu
Figure caption: The B–ρ slope k  B−ρ  and Alfvén Mach number ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ relation. The crosses in the left panel show the positions of three rescaled simulations with β 0 as 0.2, 2, and 20 in the k  B−ρ  and ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ plane, in which k  B−ρ  is the B–ρ slope of the mean density in various simulations. The red dashed line shows the fitted B–ρ slope k  B−ρ  and Alfvén Mach number ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ relation. The blue and orange columns show the k  B−ρ  positions of the previous observation, Taurus, and the NGC 6334 center region, respectively. The right panels depict the spatial distribution of the magnetic field (B-field) in a two-dimensional x–y slice, which comes from simulations with different β 0 and Alfvén Mach number ﹩{{ \mathcal M }}_{{\rm{A}}}﹩. The color-coded maps represent these simulations as follows: the blue map corresponds to β = 0.2 with Alfvén Mach number ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ = 0.31, the green map to β = 2 with ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ = 0.49, and the red map to β 0 = 20 with ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ = 2.36. The blue vector arrows illustrate the local magnetic field orientations. The background contours illustrate the density distribution, ranging from 10−21 to 10−18 g cm−3.
Paper: Slope of Magnetic Field–Density Relation as an Indicator of Magnetic Dominance
Authors: Mengke Zhao, Guang-Xing Li, Keping Qiu
Figure caption:  B–ρ relation in multiregions. This panel displays the relation between magnetic field (B) and density (ρ) following the exponential function. The red line presents the exponential B–ρ relation derived by the ﹩{{ \mathcal M }}_{{\rm{A}}}﹩–k  B–ρ  relation and ﹩{{ \mathcal M }}_{{\rm{A}}}-\rho ﹩ relation. Within this panel, the blue scatter points represent the distribution of sources measured with the Zeeman effect in the B–ρ space, as detailed in R. M. Crutcher et al. (2010). The black dashed line shows the old version (power-law) B–ρ relation fitted by the Zeeman source (blue scatters). The blue, green, and red clouds display the distribution of rescaling simulations with various ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ as 0.31, 0.49, and 1.29, respectively. The blue, green, and red columns show the ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ and mean density of rescaling simulations with various ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ as 0.31, 0.49, and 1.29, respectively.
Paper: Model-independent Calibration for Sound Horizon: Combining Observations of Supernovae and Baryon Acoustic Oscillation Measurements
Authors: Tonghua Liu, Xinyi Zhong, Marek Biesiada, Jieci Wang
Figure caption: The ﹩{r}_{s}^{h}﹩ calibration results using 15 independent 2D and 4 DESI BAO measurements combined with SN Ia data sets.
Paper: Slope of Magnetic Field–Density Relation as an Indicator of Magnetic Dominance
Authors: Mengke Zhao, Guang-Xing Li, Keping Qiu
Figure caption:  B-field and slope of B–ρ relation in the Taurus outer and NGC 6334 center regions. The panels show the magnetic field morphology and slope of the B–ρ relation in the Taurus outer region and NGC 6334 center region. The B–ρ distribution is derived from Zeeman observations in the Taurus outer region (R. M. Crutcher et al. 2010; T. C. Ching et al. 2022) and that of NGC 6334 from H.-B. Li et al. (2015). The magnetic field morphology is derived by Planck 353 GHz dust polarization (Planck Collaboration et al. 2020) and James Clerk Maxwell Telescope 850 μm dust polarization (D. Arzoumanian et al. 2021).
Paper: Model-independent Calibration for Sound Horizon: Combining Observations of Supernovae and Baryon Acoustic Oscillation Measurements
Authors: Tonghua Liu, Xinyi Zhong, Marek Biesiada, Jieci Wang
Figure caption: The probability density function of ﹩{r}_{s}^{h}﹩ using all 2D BAO and BAO DESI measurements and two SN Ia data sets. Comparison with previous works is also provided.
Paper: Slope of Magnetic Field–Density Relation as an Indicator of Magnetic Dominance
Authors: Mengke Zhao, Guang-Xing Li, Keping Qiu
Figure caption: Fitting the slope of the B–ρ relation in log–log space. Panels (a), (b), and (c) display the B–ρ distribution of simulations with β 0 = 0.2, 2, and 20, respectively. The red solid lines show the average B–ρ relation, and the blue lines show the dispersion region of the average B–ρ relation. The red dashed lines are linear equations fitting the average B–ρ relation. The blue perpendicular lines present the mean density ﹩\bar{\rho }﹩. The slope of the B–ρ relation is fitted around the mean density of the simulation as 0.15, 0.21, and 0.35, respectively.
Paper: Model-independent Calibration for Sound Horizon: Combining Observations of Supernovae and Baryon Acoustic Oscillation Measurements
Authors: Tonghua Liu, Xinyi Zhong, Marek Biesiada, Jieci Wang
Figure caption: Left panel: the PDFs for the relative standard ruler ﹩{r}_{s}^{h}﹩ using 2D BAO plus Pantheon data sets. Right panel: Similar to left figure but for Pantheon+ data set.
Paper: Model-independent Calibration for Sound Horizon: Combining Observations of Supernovae and Baryon Acoustic Oscillation Measurements
Authors: Tonghua Liu, Xinyi Zhong, Marek Biesiada, Jieci Wang
Figure caption: The probability density function of ﹩{r}_{s}^{h}﹩ using recent BAO DESI measurements with the Pantheon data set.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: A time–distance plot of temperature (left), linear particle density (center), and ﹩{\rm{log}}_{10}﹩ of the normalized particle density (right) for an interval of ﹩{10}^{5}\rm{\unicode{x000A0}s\unicode{x000A0}}\left(\unicode{x0007E}27\rm{\unicode{x000A0}hr}\right)﹩ following an increase in the heating ratio to ﹩\alpha ={{ \mathcal H }}_{b}{{\ell }}_{b}/{{ \mathcal H }}_{g}{{\ell }}_{g}=6﹩. Outward-propagating density fluctuations occur in phase with the condensation cycles at regular intervals of ﹩\unicode{x0007E}3.5\rm{\unicode{x000A0}hr}﹩. The striped pattern in the center and right panels closely matches the average characteristic speed of acoustic waves ﹩\left(u+{c}_{s}\right)﹩, which ranges from ﹩250﹩ to ﹩450{\rm{\unicode{x000A0}km\unicode{x000A0}s}}^{-1}﹩, with an average value of ﹩\unicode{x0007E}350{\rm{\unicode{x000A0}km\unicode{x000A0}s}}^{-1}﹩ (dashed line). The electron thermal speed is much higher than the acoustic speed ﹩({v}_{e}\sim 20\times {c}_{s})﹩, as reflected in the slope of the bright horizontal streaks in the left panel.
Paper: X-Ray Spectra of Black Hole X-Ray Binaries with Returning Radiation
Authors: Temurbek Mirzaev, Cosimo Bambi, Askar B. Abdikamalov, Jiachen Jiang, Honghui Liu, Shafqat Riaz, Swarnim Shashank
Figure caption: Synthetic reflection spectra in the rest frame of the material in the disk at different radial coordinates (r = 1.3, 3, and 10 r g) when the Eddington-scaled luminosity of the source is λ = 0.01. Yellow solid curves describe the direct incident spectra from the corona, black solid curves describe the incident spectra of the returning radiation of the thermal component, blue dashed curves are the reflection spectra produced by the direct radiation from the corona and the returning radiation of the thermal component, and red dashed curves are for the final reflection spectra including the returning radiation of the reflection radiation. In the top panels, the spectrum of the source is dominated by the spectrum from the corona (ρ = L corona/L disk = 100). In the central panels, the luminosity of the corona and of the disk are equivalent (ρ = 1). In the bottom panels, there is no corona, and the reflection spectrum is entirely generated by the returning radiation of the thermal component (ρ = 0). See the text for more details.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: The charge-state distributions (left) at ﹩r=21\,{R}_{\odot }﹩                   ﹩(s\sim 1.5\times {10}^{4}\,{\rm{Mm}})﹩ and average charge state (right) of oxygen ﹩\left(Z=8\right)﹩ and iron ﹩\left(Z=26\right)﹩ as functions of height for three characteristic values of the heating, indicated in blue, red, and black. On the right, the dashed blue and dashed–dotted red curves are steady-state solutions, while the solid black curves are successive snapshots separated by ﹩\unicode{x0007E}30﹩ minutes during the ablation and relaxation phases of a typical TNE cycle.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: The time evolution of ﹩n﹩, ﹩T﹩, and ﹩nuA﹩ depicted during the condensation phase, which lasts approximately ﹩1.5\,\mathrm{hr}﹩ for the case of marginal nonequilibrium, beginning with the development of a convergent flow near ﹩{s}_{n}﹩ and ending when the temperature near ﹩{s}_{n}﹩ drops to chromospheric values and the trajectory of the condensate begins to accelerate rapidly downward under the influence of gravity.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: The time evolution of ﹩n﹩, ﹩T﹩, and                          ﹩nuA﹩                       depicted during the ablation phase, which lasts approximately ﹩2.2\,\rm{hr}﹩ for the case of marginal nonequilibrium, beginning with the upwelling of material at the base of the TR and ending when all of the precipitated condensate material is expelled back into the corona and the outward mass near                          ﹩{s}_{p}﹩                       begins to slow.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: The time evolution of ﹩n﹩, ﹩T﹩, and ﹩nuA﹩ depicted during the relaxation phase, which lasts approximately ﹩17\,\rm{hr}﹩ for the case of marginal nonequilibrium, beginning with the deceleration of the outward mass flux near ﹩{s}_{p}﹩ and ending when the mass flux develops a local convergence at ﹩{s}_{n}﹩.
Paper: X-Ray Spectra of Black Hole X-Ray Binaries with Returning Radiation
Authors: Temurbek Mirzaev, Cosimo Bambi, Askar B. Abdikamalov, Jiachen Jiang, Honghui Liu, Shafqat Riaz, Swarnim Shashank
Figure caption: Disk–corona model. Figure from C. Bambi (2022) under the terms of the Creative Commons Attribution 4.0 International License.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: Dependence of TNE-induced cycle duration (and frequency) on the heating ratio ﹩\alpha ﹩. These values represent the average cycle duration over a ﹩56\,\rm{hr}﹩ simulation interval for each value of ﹩\alpha ﹩, measured from the moment of condensation.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: IBEX 2012A 1.1 keV map, with Compton–Getting effects and survival probability corrections. Red orbit arcs 1 and 1′ show the first two half-orbits of pixels taken by IBEX within this half-year (see that the change from orbits to half-orbits was made after orbit 129, 2011 June, as described by D. J. McComas et al. 2011; see also Section 2 of D. J. McComas et al. 2024). Orange orbit arcs 2 and 2′ show the second two half-orbit of pixels taken by IBEX. Purple orbit arcs 3 and 3′ show the third two half-orbit of pixels taken by IBEX. For illustration purposes, orbit arcs might be slightly off from their true location. In this figure, new orbits appear right from the current orbit until the full sky map data is taken in the half-year period (for the detailed data intervals and orbit/arc numbers used for IBEX maps, see Table 1 of D. J. McComas et al. 2024).
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: Histograms of the explosion properties derived for the Ic-BL sample. The mean values and 1σ dispersions for the properties are shown with solid and dashed lines, respectively. Top panel: the M Ni distribution for the SNe Ic-BL sample. Middle panel: the M ej distribution for the SNe Ic-BL sample. Lower panel: the E K distribution for the SNe Ic-BL sample.
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: Explosion properties (M Ni, M ej, and E K) plotted against each other. Top panel: M Ni plotted against M ej. We do not find any correlations between the two, with a p-value of 0.86. The dashed line indicates the boundary of M Ni = M ej/2. Events above that boundary are likely not solely powered by radioactive decay (D. Kasen & L. Bildsten 2010). Middle panel: E K plotted against M Ni. We do not find any correlation between the two, with a p-value of 0.75. Bottom panel: E K plotted against M ej. We find a significant correlation between the two, with a p-value of 0.007.
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: Best-fit Linmix linear regression model fitting between the peak radio luminosities and the explosion properties and photospheric velocities shown in red. Black points indicate limits, while green points indicate detections. We find no statistically significant correlations between the peak radio luminosities and any of the parameters. The parameters for SN 1998bw (J. Sollerman et al. 2000; K. W. Weiler et al. 2001) and SN 2002ap (E. Berger et al. 2002; P. A. Mazzali et al. 2002) are shown as reference.
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: Histograms showing the distribution of explosion properties and v ph for the population of events with radio observations. We distinguish events that have radio detections in orange and events that have radio nondetections in blue. We find no statistical differences between the populations for any of the properties.
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 2018ell, SN 2018hsf, and SN 2018keq. The phases next to each spectrum are the rest-frame days since the maximum r-band flux from the GP processing. The spectra for the rest of the events except for those presented in single-object works (SN 2018bvw, SN 2018gep, and SN 2020bvc) are presented in a similar format 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: The best-fit magnetar powered model fit to SN 2020wgz in the r band on the left, and g band on the right.
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 2019hsx, SN 2019gwc, and SN 2019lci.
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 2019qfi, SN 2020zg, and SN 2020ayz.