adsabs/AstroCLIMB huggingface dataset:
Paper: A Repeating Fast Radio Burst Source in a Low-luminosity Dwarf Galaxy
Authors: Danté M. Hewitt, Mohit Bhardwaj, Alexa C. Gordon, Aida Kirichenko, Kenzie Nimmo, Shivani Bhandari, Ismaël Cognard, Wen-fai Fong, Armando Gil de Paz, Akshatha Gopinath, Jason W. T. Hessels, Franz Kirsten, Benito Marcote, Vladislavs Bezrukovs, Richard Blaauw, Justin D. Bray, Salvatore Buttaccio, Tomas Cassanelli, Pragya Chawla, Alessandro Corongiu, William Deng, Hannah N. Didehbani, Yuxin Dong, Marcin P. Gawroński, Marcello Giroletti, Lucas Guillemot, Jeff Huang, Dmitriy V. Ivanov, Ronniy C. Joseph, Victoria M. Kaspi, Mikhail A. Kharinov, Mattias Lazda, Michael Lindqvist, Giuseppe Maccaferri, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Alexey Melnikov, Daniele Michilli, Andrey G. Mikhailov, Anya E. Nugent, Omar S. Ould-Boukattine, Zsolt Paragi, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, Ketan R. Sand, Vishwangi Shah, Kaitlyn Shin, Mark P. Snelders, Tiziana Venturi, Na Wang, David R. A. Williams-Baldwin, Jun Yang, Jianping P. Yuan
Figure caption: The left and right panels show bursts B1 and B2, detected in the PRECISE and ÉCLAT projects, respectively. In each subfigure, a dynamic spectrum of the burst is shown in panel (c). Bursts B1 and B2 have been dedispersed using DMs of 580.1 and 579.9 pc cm−3, respectively. The horizontal white lines indicate channels contaminated by RFI that have been masked. A frequency-averaged (over the entire observing band) total intensity profile of the burst is shown in black in panel (b). The unbiased linear polarization is shown in red and the circular polarization in blue. In panel (a), the probability density function of the PPA, at each time step, is shown. The bursts have been derotated according to their respective RMs (46.5 rad m−2 for B1 and −5.2 rad m−2 for B2), and the PPA is referenced to infinite frequency. In panel (d), the time-averaged frequency spectrum (integrated over the burst duration indicated by the horizontal purple bar in panel (b)) is shown in purple. Note that the observing bandwidths differ between the two instruments.
Paper: A Repeating Fast Radio Burst Source in a Low-luminosity Dwarf Galaxy
Authors: Danté M. Hewitt, Mohit Bhardwaj, Alexa C. Gordon, Aida Kirichenko, Kenzie Nimmo, Shivani Bhandari, Ismaël Cognard, Wen-fai Fong, Armando Gil de Paz, Akshatha Gopinath, Jason W. T. Hessels, Franz Kirsten, Benito Marcote, Vladislavs Bezrukovs, Richard Blaauw, Justin D. Bray, Salvatore Buttaccio, Tomas Cassanelli, Pragya Chawla, Alessandro Corongiu, William Deng, Hannah N. Didehbani, Yuxin Dong, Marcin P. Gawroński, Marcello Giroletti, Lucas Guillemot, Jeff Huang, Dmitriy V. Ivanov, Ronniy C. Joseph, Victoria M. Kaspi, Mikhail A. Kharinov, Mattias Lazda, Michael Lindqvist, Giuseppe Maccaferri, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Alexey Melnikov, Daniele Michilli, Andrey G. Mikhailov, Anya E. Nugent, Omar S. Ould-Boukattine, Zsolt Paragi, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, Ketan R. Sand, Vishwangi Shah, Kaitlyn Shin, Mark P. Snelders, Tiziana Venturi, Na Wang, David R. A. Williams-Baldwin, Jun Yang, Jianping P. Yuan
Figure caption: The r-band AB magnitude vs. inferred redshift for the host of FRB 20190208A against a background of published FRB host galaxies (references in the main text). We show the placement of L* field galaxies and scale them in orders of magnitude down to 0.001L*. The true magnitude of O4 is indicated by the horizontal dashed line. Overplotted on this line are two probability density functions (PDFs) for the redshift, described in detail in Section 3.3. The orange redshift PDF indicates a conservative estimate, where DMhost = 0 pc cm−3, using the framework from J. P. Macquart et al. (2020). The pink redshift PDF uses an upper limit on scattering to constrain DMhost, using the framework from J. M. Cordes et al. (2022). The most probable inferred redshift range for FRB 20190208A indicates that the host is consistent with a <0.01L* galaxy.
Paper: A Repeating Fast Radio Burst Source in a Low-luminosity Dwarf Galaxy
Authors: Danté M. Hewitt, Mohit Bhardwaj, Alexa C. Gordon, Aida Kirichenko, Kenzie Nimmo, Shivani Bhandari, Ismaël Cognard, Wen-fai Fong, Armando Gil de Paz, Akshatha Gopinath, Jason W. T. Hessels, Franz Kirsten, Benito Marcote, Vladislavs Bezrukovs, Richard Blaauw, Justin D. Bray, Salvatore Buttaccio, Tomas Cassanelli, Pragya Chawla, Alessandro Corongiu, William Deng, Hannah N. Didehbani, Yuxin Dong, Marcin P. Gawroński, Marcello Giroletti, Lucas Guillemot, Jeff Huang, Dmitriy V. Ivanov, Ronniy C. Joseph, Victoria M. Kaspi, Mikhail A. Kharinov, Mattias Lazda, Michael Lindqvist, Giuseppe Maccaferri, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Alexey Melnikov, Daniele Michilli, Andrey G. Mikhailov, Anya E. Nugent, Omar S. Ould-Boukattine, Zsolt Paragi, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, Ketan R. Sand, Vishwangi Shah, Kaitlyn Shin, Mark P. Snelders, Tiziana Venturi, Na Wang, David R. A. Williams-Baldwin, Jun Yang, Jianping P. Yuan
Figure caption: PATH posteriors, P(O∣x), for the FRB 20190208A field as a function of increasing assumed localization uncertainty (radius-equivalent). The actual 1-σ  x  localization precision of the source is shown by the dashed vertical line. The P(O∣x) for objects O1 to O9 are represented by solid curves and their priors, P(O), by horizontal dotted lines with corresponding colors (see legend). Shaded gray regions illustrate reasonable and robust host associations (defined as P(O∣x) > 0.8 and >0.9, respectively).
Paper: A Repeating Fast Radio Burst Source in a Low-luminosity Dwarf Galaxy
Authors: Danté M. Hewitt, Mohit Bhardwaj, Alexa C. Gordon, Aida Kirichenko, Kenzie Nimmo, Shivani Bhandari, Ismaël Cognard, Wen-fai Fong, Armando Gil de Paz, Akshatha Gopinath, Jason W. T. Hessels, Franz Kirsten, Benito Marcote, Vladislavs Bezrukovs, Richard Blaauw, Justin D. Bray, Salvatore Buttaccio, Tomas Cassanelli, Pragya Chawla, Alessandro Corongiu, William Deng, Hannah N. Didehbani, Yuxin Dong, Marcin P. Gawroński, Marcello Giroletti, Lucas Guillemot, Jeff Huang, Dmitriy V. Ivanov, Ronniy C. Joseph, Victoria M. Kaspi, Mikhail A. Kharinov, Mattias Lazda, Michael Lindqvist, Giuseppe Maccaferri, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Alexey Melnikov, Daniele Michilli, Andrey G. Mikhailov, Anya E. Nugent, Omar S. Ould-Boukattine, Zsolt Paragi, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, Ketan R. Sand, Vishwangi Shah, Kaitlyn Shin, Mark P. Snelders, Tiziana Venturi, Na Wang, David R. A. Williams-Baldwin, Jun Yang, Jianping P. Yuan
Figure caption: Radio continuum maps from our 1.4 GHz EVN observations (uncleaned; left) and the VLA observations in C configuration at 6 GHz (cleaned; right) to search for persistent radio emission. The rms is 31 and 4 μJy beam−1 for the EVN and VLA images, respectively. The ellipses in the EVN image are centered on the VLBI position of FRB 20190208A and are described in Section 2.5. The white circle in the VLA image also indicates the FRB position but is much larger than the aforementioned ellipses. We find no PRSs associated with FRB 20190208A.
Paper: A Repeating Fast Radio Burst Source in a Low-luminosity Dwarf Galaxy
Authors: Danté M. Hewitt, Mohit Bhardwaj, Alexa C. Gordon, Aida Kirichenko, Kenzie Nimmo, Shivani Bhandari, Ismaël Cognard, Wen-fai Fong, Armando Gil de Paz, Akshatha Gopinath, Jason W. T. Hessels, Franz Kirsten, Benito Marcote, Vladislavs Bezrukovs, Richard Blaauw, Justin D. Bray, Salvatore Buttaccio, Tomas Cassanelli, Pragya Chawla, Alessandro Corongiu, William Deng, Hannah N. Didehbani, Yuxin Dong, Marcin P. Gawroński, Marcello Giroletti, Lucas Guillemot, Jeff Huang, Dmitriy V. Ivanov, Ronniy C. Joseph, Victoria M. Kaspi, Mikhail A. Kharinov, Mattias Lazda, Michael Lindqvist, Giuseppe Maccaferri, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Alexey Melnikov, Daniele Michilli, Andrey G. Mikhailov, Anya E. Nugent, Omar S. Ould-Boukattine, Zsolt Paragi, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, Ketan R. Sand, Vishwangi Shah, Kaitlyn Shin, Mark P. Snelders, Tiziana Venturi, Na Wang, David R. A. Williams-Baldwin, Jun Yang, Jianping P. Yuan
Figure caption: All known bursts. detected from FRB 20190208A are indicated by dashed vertical lines. Bursts detected by CHIME/FRB are indicated in gray, while the bursts detected by PRECISE (B1) and ÉCLAT (B2) are in orange and purple, respectively. The MJD is shown on the bottom axis and the corresponding calendar date on the top axis. The solid orange curve shows the cumulative time (in hours) that FRB 20190208A has been observed by PRECISE, while the solid purple shows the same but for the ÉCLAT project on the NRT.
Paper: A Repeating Fast Radio Burst Source in a Low-luminosity Dwarf Galaxy
Authors: Danté M. Hewitt, Mohit Bhardwaj, Alexa C. Gordon, Aida Kirichenko, Kenzie Nimmo, Shivani Bhandari, Ismaël Cognard, Wen-fai Fong, Armando Gil de Paz, Akshatha Gopinath, Jason W. T. Hessels, Franz Kirsten, Benito Marcote, Vladislavs Bezrukovs, Richard Blaauw, Justin D. Bray, Salvatore Buttaccio, Tomas Cassanelli, Pragya Chawla, Alessandro Corongiu, William Deng, Hannah N. Didehbani, Yuxin Dong, Marcin P. Gawroński, Marcello Giroletti, Lucas Guillemot, Jeff Huang, Dmitriy V. Ivanov, Ronniy C. Joseph, Victoria M. Kaspi, Mikhail A. Kharinov, Mattias Lazda, Michael Lindqvist, Giuseppe Maccaferri, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Alexey Melnikov, Daniele Michilli, Andrey G. Mikhailov, Anya E. Nugent, Omar S. Ould-Boukattine, Zsolt Paragi, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, Ketan R. Sand, Vishwangi Shah, Kaitlyn Shin, Mark P. Snelders, Tiziana Venturi, Na Wang, David R. A. Williams-Baldwin, Jun Yang, Jianping P. Yuan
Figure caption: Dirty map of B1, the burst from FRB 20190208A detected in PRECISE observations. The cyan plus sign indicates the position of the phase center, the green star shows the position of the pixel with the peak brightness, and the white cross marks the center of the Gaussian ellipse.
Paper: A Repeating Fast Radio Burst Source in a Low-luminosity Dwarf Galaxy
Authors: Danté M. Hewitt, Mohit Bhardwaj, Alexa C. Gordon, Aida Kirichenko, Kenzie Nimmo, Shivani Bhandari, Ismaël Cognard, Wen-fai Fong, Armando Gil de Paz, Akshatha Gopinath, Jason W. T. Hessels, Franz Kirsten, Benito Marcote, Vladislavs Bezrukovs, Richard Blaauw, Justin D. Bray, Salvatore Buttaccio, Tomas Cassanelli, Pragya Chawla, Alessandro Corongiu, William Deng, Hannah N. Didehbani, Yuxin Dong, Marcin P. Gawroński, Marcello Giroletti, Lucas Guillemot, Jeff Huang, Dmitriy V. Ivanov, Ronniy C. Joseph, Victoria M. Kaspi, Mikhail A. Kharinov, Mattias Lazda, Michael Lindqvist, Giuseppe Maccaferri, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Alexey Melnikov, Daniele Michilli, Andrey G. Mikhailov, Anya E. Nugent, Omar S. Ould-Boukattine, Zsolt Paragi, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, Ketan R. Sand, Vishwangi Shah, Kaitlyn Shin, Mark P. Snelders, Tiziana Venturi, Na Wang, David R. A. Williams-Baldwin, Jun Yang, Jianping P. Yuan
Figure caption: The frequency coverage for different antennas in our PRECISE observations are shown here by horizontal purple bars. The edges of subbands are indicated by dashed black vertical lines. The shaded orange region indicates the spectral extent of burst B1.