adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Illustration of our shadow morphology depicted by normalized temperature in disks with σ  ϕ  = 0.236 and 0.079 for fast (β = 0.001) and slow (β = 1) cooling processes. With fast cooling, the low-temperature regions caused by shadows largely reflect the equilibrium temperature we prescribe at the shadow location. With longer cooling timescale, these regions deviate from the prescribed shadow positions toward the leading side, and exhibit significantly weaker amplitude.
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 TRGB’s metallicity-dependent slope determined from [Fe/H] = −1.90 to +0.06 in the F115W vs. (F115W – F444W) CMD as predicted by the BaSTI stellar evolution models for a range of ages that can be expected in galaxy stellar halos. The predicted metallicity-dependent slope decreases and the trend flattens for older populations t age ≳ 6 Gyr, suggesting that targeting pristine stellar halo populations will be key to reducing population-dependent systematic errors in the measurement of TRGB distances in the IR with JWST.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: The observed Stokes parameters from HONIR and Bok in the Q–U plane for SN 2023ixf. The color map on the right represents the SN phase. The Stokes Q–U from S. S. Vasylyev et al. (2023) for SN 2023ixf is overplotted. The shaded regions depict the dominant axis of the CSM-outer ejecta (in blue) and the inner ejecta-core (in red) inferred from the temporal evolution of SN 2023ixf.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Evolution of Hα 6563 Å, [O I] 6300, 6364 Å, and [Ca II] 7291, 7324 Å during the early-nebular phase of SN 2023ixf. The vertical lines represent the rest-wavelength of the features labeled in each subplot. The zero-velocity corresponds to 6563 Å, 6300 Å, and 7308 Å in the three subplots, respectively. The blueshifted offset of 1500 km s−1 in O I doublet is distinctly visible. The redshifted excess in H α and [Ca II] λ λ 7291, 7324 is labeled at +5000 km s−1. The insets show a zoomed view of the peak of the Hα and [Ca II], showing redward attenuation as the SN progressed onto the nebular phase.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Temporal evolution of polarization and its PA in the R-band for SN 2023ixf in comparison to SN 1987A (P. Barrett 1988), SN 2004dj (D. C. Leonard et al. 2006), and SN 2013ej (B. Kumar et al. 2016). Estimates of continuum polarization from S. S. Vasylyev et al. (2023) for SN 2023ixf are overplotted. The observed and ISP-corrected polarization is shown with empty and filled markers, respectively. The r-band light curve of SN 2023ixf is plotted in the top panel for reference.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption:  Left-hand Panel: Photospheric phase evolution of SN 2023ixf. Prominent spectral features are labeled and depicted using colored shaded areas. Right-hand Panel: Comparison of the early- and late-plateau phase spectrum of SN 2023ixf with other SNe II from the literature with signatures of CSM interaction in the top and bottom panels, respectively. References: SN 2013by (S. Valenti et al. 2015); SN 2014G (G. Terreran et al. 2016); SN 2018gj (R. S. Teja et al. 2023b); SN 2020jfo (R. S. Teja et al. 2022); SN 2020pni (G. Terreran et al. 2022); SN 2020tlf (W. V. Jacobson-Galán et al. 2022).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Left-hand Panel: Hydrodynamical modeling of the light curves of SN 2023ixf with only a compact CSM (dashed line) and including an extended CSM (solid line). The shaded region shows the UV excess from the interaction due to the extended CSM. Top right-hand panel: The density structure of the RSG progenitor, the inner-compact CSM, and the extended CSM. The inner-compact CSM extended to 5 × 1014 cm and the extended CSM extends to 1 × 1016 cm. Bottom right-hand panel: The photospheric velocity estimates from both the hydrodynamic models are compared with the observed evolution of photospheric velocity.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Spectropolarimetric observation of SN 2023ixf averaged out over (a) 27.9 days (June 14–16) and (b) 30.9 days (June 18, 19). The five panels from the top represent the flux spectrum (F  λ ), the fractional Stokes parameters q and u, polarization (p), and PA, respectively, and binned to 25 Å for clarity. The panels show the observed and the ISP-corrected polarization along with the estimated ISP. The prominent emission features of Hα and Hβ, chosen for ISP estimation, are indicated by the vertical shaded region. The polarization uncertainty is shown via a shaded region around the solid line. (The continuum polarization data are available as data behind the figure.)
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Temporal evolution of Hβ and Hα profile of SN 2023ixf from the decline of the flash-ionization phase until the late-plateau phase. The rest-frame zero-velocity is marked with a gray line. The red lines mark the absorption minima of the P-Cygni absorption (8500 km s−1) and the HV absorption (13,500 km s−1) when they first appear simultaneously in the spectra on ∼16 days. The blue edge of the HV feature (20,000 km s−1) is shown with a blue line. The clumpy features that appear over several epochs are indicated in green boxes.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption:  Left-hand Panel: Nebular spectroscopic evolution of SN 2023ixf from HCT. The marked vertical lines indicate the rest-wavelength of the labeled spectral features. Right-hand Panel: Comparison of the early- and late-plateau phase spectrum of SN 2023ixf with other SNe II from the literature with signatures of CSM interaction in the top and bottom panels, respectively. References: SN 2013 (S. Valenti et al. 2015); SN 2014G (G. Terreran et al. 2016); SN 2018gj (R. S. Teja et al. 2023b); SN 2020jfo (R. S. Teja et al. 2022); and SN 2020tlf (W. V. Jacobson-Galán et al. 2022).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Comparison of Fe II λ 5169 line velocity evolution of SN 2023ixf in comparison with SNe II from the literature and the mean photospheric velocity evolution for SNe II computed by C. P. Gutiérrez et al. (2017a).
Paper: A Search for Collisions and Planet–Disk Interactions in the Beta Pictoris Disk with 26 Years of High-precision HST/STIS Imaging
Authors: Arin M. Avsar, Kevin Wagner, Dániel Apai, Christopher C. Stark, Mark C. Wyatt
Figure caption: 5σ 2D collisional sensitivity maps for the β Pic disk. Each map shows the mass of a single collisional progenitor necessary to have a 5σ detection in our ratio maps. The epochs used in the ratio maps are given in parentheses in the title of each panel. The gray regions indicate regions in the disk blocked out by our coronagraphic wedge. The radial labels are shown in units of au. The maps are shown from a face-on perspective of the disk, and the black arrows indicate the direction to the observer. We can see a large increase in progenitor mass over the 6 years modeled, pointing to continual monitoring being essential to finding collisional remnants in scattered light observations and observing multi-wavelength evolution of the remnants.
Paper: A Search for Collisions and Planet–Disk Interactions in the Beta Pictoris Disk with 26 Years of High-precision HST/STIS Imaging
Authors: Arin M. Avsar, Kevin Wagner, Dániel Apai, Christopher C. Stark, Mark C. Wyatt
Figure caption: Ratio grid maps showing the percentage change in surface brightness between epochs and associated 1σ uncertainties in each 10 au × 10 au grid cell. The asterisks indicate cells where the SNR of the change in surface brightness is ≥5. The area within the gray region is blocked out because the disk surface brightness is dominated by PSF subtraction residuals. The top image should be used as a reference to where in the disk each grid cell is probing. We can see in the 2023/2012 and 2021/2012 ratio grid maps a significant, consistent brightening of the disk below the western midplane. This region is shown in the black boxed area.
Paper: A Search for Collisions and Planet–Disk Interactions in the Beta Pictoris Disk with 26 Years of High-precision HST/STIS Imaging
Authors: Arin M. Avsar, Kevin Wagner, Dániel Apai, Christopher C. Stark, Mark C. Wyatt
Figure caption: Midplane radial surface brightness measurement and epoch comparison. The top three panels show individual radial surface brightness measurements along the disk midplane of each epoch in units of mJy arcsec−2. The bottom two panels show the percentage change in midplane radial surface brightness profiles between epochs (2021/2012 and 2023/2012), with the shaded region around the lines indicating the 1σ uncertainty. Aperture photometry along the disk midplane shows observed variation to be consistent with noise in the data to 3σ.
Paper: A Search for Collisions and Planet–Disk Interactions in the Beta Pictoris Disk with 26 Years of High-precision HST/STIS Imaging
Authors: Arin M. Avsar, Kevin Wagner, Dániel Apai, Christopher C. Stark, Mark C. Wyatt
Figure caption: Simulation of two planetesimals of 15 Ceres masses colliding at 100 au in the β Pic disk. The collision was simulated as if it occurred right after our 2021 epoch of data was taken and is then injected in the 2023 epoch of data. The collision is very difficult to see in the 2023 epoch alone due to the high surface brightness of the disk. However, taking a ratio between the two epochs allows the excess surface brightness from the collision to stand out as a clear detection. No such signals are seen in any of the ratio maps, allowing us to rule out any new major collisions in the disk.
Paper: A Search for Collisions and Planet–Disk Interactions in the Beta Pictoris Disk with 26 Years of High-precision HST/STIS Imaging
Authors: Arin M. Avsar, Kevin Wagner, Dániel Apai, Christopher C. Stark, Mark C. Wyatt
Figure caption: Visual comparison of four epochs of the β Pic disk. The top left panels show two archival images. The 1997 image is reproduced from D. Apai et al. (2015), while we re-reduce the 2012 data set. The bottom left panels show two new STIS coronagraphic images of the β Pic disk (2021, 2023). The right panel shows the mean-combined image of the 2012–2023 data sets, along with the orbit of β Pic b relative to the disk and the orientation of the inclined inner disk (D. A. Golimowski et al. 2006; D. Apai et al. 2015). The images are shown on a logarithmic stretch ranging from 0.01 to 100 counts s−1. All images are rotated to the common north up, east left orientation.
Paper: A Search for Collisions and Planet–Disk Interactions in the Beta Pictoris Disk with 26 Years of High-precision HST/STIS Imaging
Authors: Arin M. Avsar, Kevin Wagner, Dániel Apai, Christopher C. Stark, Mark C. Wyatt
Figure caption: An example of PSF subtraction regions for our automated pipeline. Before the grid search, the inner 30 × 30 pixels of the disk are masked so that we are only minimizing diffraction spike light that is not contaminated by disk light. Our grid search, described in Section 3, iterates through all parameters until it finds the combination that minimizes the squared sum of the diffraction spike residuals pictured.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The waterfalls of the far sidelobe events, including one from PSR B0329+54, another from PSR B0531+21, and the others from FRBs. Each panel represents one far sidelobe event. The sub-panel, the timing, and frequency resolutions are described in Figure 1. For events 20190202B, 20191202A, and 201912E, only three of four W–E beams in the same N–S row are above the detection threshold. For events 20190125B, 20191104B, and 20210810A, there are lower-S/N detections in adjacent beam rows, which are not shown.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The localization offset comparisons of three methods. We note that Method 1 has the smallest systematic errors and Method 3 has the largest ones.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The SVD decomposition of the holography data B f,ρ(f) of CygA. We show the first eight modes in the panels. Left: the eigenfunction of frequency (U fn ). Middle: the eigenvalues (S n ). Right: the eigenfunction of ρ(f) (V  n ρ(f)).
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: Spectra (solid black) and fitted model (solid red) for the Method 1 intensity localizations of example pulses from PSRs B0329+51 and B0531+21 and the 10 sidelobe events. The underlying fitted power-law model FRB spectrum is plotted as gray dashed lines.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The localization offset comparisons of Method 1 and Method 2. We did not understand the origin of the systematic errors of Method 2, and the localization with voltage data in the future could further improve the localization precision.