adsabs/AstroCLIMB huggingface dataset:
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Isochrones computed with Z = 0.014 GENEC tracks without rotation from 1 to 4 Myr. The tracks in red are produced with STARBURST99 and the tracks in black are produced with pySTARBURST99, showing good agreement between the two code versions.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Example of grid coverage for SED predictions with extension for VMS at Z = 0.014. GENEC evolutionary tracks are overplotted at regular intervals from 9 to 500 M⊙. This coverage is available for all metallicities. A similar level of coverage is available at zero metallicity, where the tracks are much hotter than any others.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Synthetic FUV SEDs from STARBURST99  compared to those produced with pySTARBURST99 in both cases, utilizing the S. Ekström et al. (2012) stellar evolutionary models at Z = 0.014 and WM-BASIC  spectra at Z = 0.02. The evolution with time is shown from 1 to 10 Myr at intervals of 1 Myr.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: H I ionizing fluxes with metallicity from solar to zero metallicity. The solid lines show H I ionizing fluxes made with FASTWIND models and an upper mass limit of 120 M⊙, without rotation. The dashed lines are as the solid lines but with an upper mass limit of 300 M⊙.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Synthetic FUV SEDs from pySTARBURST99, utilizing the S. Ekström et al. (2012) stellar evolutionary models at Z = 0.014 and FASTWIND spectra at Z = 0.014. This is compared with the addition of VMS evolutionary tracks up to 300 M⊙ from S. Martinet et al. (2023) and FASTWIND models tailored to match the extended parameter space coverage from VMS evolutionary tracks. The evolution with time is shown from 1 Myr to 10 Myr at intervals of 1 Myr.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Synthetic FUV SEDs, utilizing the S. Ekström et al. (2012) stellar evolutionary models at Z = 0.014 for both, with WM-BASIC  spectra at Z = 0.02 compared with FASTWIND  spectra at Z = 0.014. The evolution with time is shown from 1 to 10 Myr at intervals of 1 Myr.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Low-resolution synthetic SEDs with metallicities representative of populations in the Galactic center to zero metallicity. These are produced at 2 Myr using pySTARBURST99 with the GENEC tracks, new FASTWIND model grid, an upper mass limit of 120 M⊙ and no rotation.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: He II ionizing fluxes as in Figure 7.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: He I ionizing fluxes as in Figure 7.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: As described in Figure 7, but showing bolometric luminosity.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Hα EWs as in Figure 7.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: Waterfall plots of bursts whose hosts have measured spectroscopic redshifts, ordered by specific peak luminosity (Jy Gpc2) from lowest to highest. We note no obvious trends with increasing isotropic-equivalent burst luminosity but reserve a detailed analysis for future work. FRB 20231204A and FRB 20231128A are repeating sources; both show downward-drifting burst morphology characteristic of CHIME/FRB-detected repeating sources. Each plot is labeled with the time resolution to which we downsampled the dynamic spectrum. Masked channels are plotted at the zero-point of the color scale.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: The sky distribution in R.A. (top) and decl. (bottom) of host galaxy candidates as a function of PATH posterior probability P(O∣x), which have a low false-positive fraction (see Section 3). The uniformity of the gold-sample hosts in R.A. and decl., relative to the full sample of bursts, indicates the absence of strong modifications to the survey footprint of the telescope induced by host association.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: As described in Figure 7, but showing wind momentum.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: Wind-momentum fluxes over time for a typical single stellar population with an upper mass limit of 120 M⊙, no rotation comparing STARBURST99 with pySTARBURST99 and a few other mass-loss and terminal wind speed recipes on the MS.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: UV slopes computed from synthetic FUV SEDs, within the range of 1250–1750 Å, including the contribution from the nebular continuum.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: As described in Figure 7, but showing wind power.
Paper: pySTARBURST99: The Next Generation of STARBURST99
Authors: Calum Hawcroft, Claus Leitherer, Oskar Aranguré, John Chisholm, Sylvia Ekström, Sébastien Martinet, Lucimara P. Martins, Georges Meynet, Christophe Morisset, Andreas A. C. Sander, Aida Wofford
Figure caption: As described in Figure 7, but showing MV.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: The offset distribution of the pulsar localizations in our sample of test pulsars, plotted here including low-decl. sources. At the 1σ level, the distribution has rms values of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5, 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩6, and 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩54 for the “Closest,” “max-S/N,” and “Closest and good” strategies, respectively. On the basis of these statistics and the overall false-positive fraction of the host associations in our sample, we choose a 1σ astrometric error of 2″. At higher decl., if the localizations of B0919+06 are omitted, they are 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩919, 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩936, and 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩943, respectively, further establishing that this is a conservative choice.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: Validation of decl. uncertainties outputted by the CHIME/FRB baseband localization pipeline (D. Michilli et al. 2021). Left panel: decl. offsets as a function of detection S/N for a sample of 100 pulses from 18 unique pulsars covering a decl. range +6∘ ≤ δ ≤ +80∘. Offsets and their associated uncertainties are represented by open-face, black markers, and error bars, respectively. For reference, the measured S/N and decl. uncertainties associated with FRBs presented in this work are indicated by the blue error bars at a fiducial decl. offset of −2﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5. Theoretical uncertainty for a burst detected at zenith by CHIME/FRB as a function of S/N is depicted by the two red curves (K. W. Masui et al. 2019; D. Michilli et al. 2021). Right: histogram of measured decl. offsets normalized by their outputted uncertainties. As expected, the normalized values are well described by a Gaussian distribution with a mean of 0.1 and a standard deviation of 1.0 (overplotted dashed, red line).
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: For each sight line, we plot the probability that the galaxy candidate with the highest P(O∣x) is the true host as a function of its r-band magnitude. We also plot the false-positive rate of claimed associations calculated within a bin in mr, determined from simulations (B. Andersen et al. 2025, in preparation). Points and traces are colored according to their respective optical survey (blue for DECaLS, and orange for Pan-STARRS); high-extinction sight lines are denoted as E(B − V) > 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩3 and indicated with x’s. The circles highlighted in yellow and gray refer to the host candidates in our gold and silver samples, respectively. We observe that the highest PATH probability achieved by any host candidate in our sample tends to drop below 0.9 at ∼22 mag. This suggests that our archival imaging, which goes as deep as 23–23.5 mag, is sufficiently deep for making confident host galaxy associations.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: Offsets between measured and true pulsar positions, along the CHIME–KKO baseline direction, for a sample of pulsars. Each point is the offset of the measured position from the true position using a different in-beam calibrator. Each column shows offsets for a given baseband acquisition, grouped by target pulsar. The color of the point indicates which calibrator would be selected by each selection strategy—red for maximum S/N, blue for the closest in decl., and green for our chosen strategy of selecting the closest calibrator that is within 2 ns from the median. Gray points indicate calibrators that do not qualify under any of these strategies.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: The observed distribution of the extragalactic DM, defined as DMtot –DMMW,ISM–DMMW,halo, for FRBs in our sample. Different colors refer to our “gold” and “silver” samples (see text), which have lower mean extragalactic DMs than that of the full sample.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: Each FRB field with a host galaxy for which the PATH algorithm yields P(O∣x) > 0.9 (i.e., the gold sample of FRBs in Table 1). Bright stars are visible in many fields; these are excluded automatically or during manual vetting of each host association (see text). The 1σ and 3σ localization contours are displayed as solid and dashed white ellipses, respectively. The top host candidate for each burst in our gold sample is denoted by a red square. Additionally, we have included the field of FRB 20230311A (see text). The images of some fields (FRB 20230222B, 20231123A, and 20231223C) lacked one or more color channels in publicly available images, resulting in their tinted appearance.
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: The Macquart relation for a selection of host galaxies in the literature shows the complementary redshift coverage of various FRB surveys at the time of this writing. Galaxy redshifts and FRB DM measurements are taken from S. P. Tendulkar et al. (2017), B. Marcote et al. (2020), S. Bhandari et al. (2022), A. C. Gordon et al. (2023), D. Michilli et al. (2023), M. Bhardwaj et al. (2024), A. L. Ibik et al. (2024a), C. J. Law et al. (2024), and K. Sharma et al. (2024).