adsabs/AstroCLIMB huggingface dataset:
Paper: A Glimpse of the New Redshift Frontier through AS1063
Authors: Vasily Kokorev, Hakim Atek, John Chisholm, Ryan Endsley, Iryna Chemerynska, Julian B. Muñoz, Lukas J. Furtak, Richard Pan, Danielle Berg, Seiji Fujimoto, Pascal A. Oesch, Andrea Weibel, Angela Adamo, Jeremy Blaizot, Rychard Bouwens, Miroslava Dessauges-Zavadsky, Gourav Khullar, Damien Korber, Ilias Goovaerts, Michelle Jecmen, Ivo Labbé, Floriane Leclercq, Rui Marques-Chaves, Charlotte Mason, Kristen B. W. McQuinn, Rohan Naidu, Priyamvada Natarajan, Erica Nelson, Joki Rosdahl, Alberto Saldana-Lopez, Daniel Schaerer, Maxime Trebitsch, Marta Volonteri, Adi Zitrin
Figure caption: UV continuum slope and delensed luminosity. The black dashed line shows the best-fitting β−MUV relation from F. Cullen et al. (2023) for star-forming galaxies at z = 8–16. The gray shaded area corresponds to the 68% confidence interval. Our secure (>5σ) sources at z ∼ 16, shown with red diamonds, appear to be consistent with the predicted trend within 1σ, although systematically shifted to bluer slopes.
Paper: A Glimpse of the New Redshift Frontier through AS1063
Authors: Vasily Kokorev, Hakim Atek, John Chisholm, Ryan Endsley, Iryna Chemerynska, Julian B. Muñoz, Lukas J. Furtak, Richard Pan, Danielle Berg, Seiji Fujimoto, Pascal A. Oesch, Andrea Weibel, Angela Adamo, Jeremy Blaizot, Rychard Bouwens, Miroslava Dessauges-Zavadsky, Gourav Khullar, Damien Korber, Ilias Goovaerts, Michelle Jecmen, Ivo Labbé, Floriane Leclercq, Rui Marques-Chaves, Charlotte Mason, Kristen B. W. McQuinn, Rohan Naidu, Priyamvada Natarajan, Erica Nelson, Joki Rosdahl, Alberto Saldana-Lopez, Daniel Schaerer, Maxime Trebitsch, Marta Volonteri, Adi Zitrin
Figure caption: Theoretical comoving number densities of z > 16 galaxies in the literature. Our completeness-corrected densities are shown in red. Black lines are median values; shaded areas show 68th percentiles. Values have been homogenized in terms of redshift interval (16 < z < 20) and delensed. While high, our predictions generally align with the upper edge of the theoretical predictions (P. Dayal et al. 2014, 2019; C. A. Mason et al. 2015; P. Behroozi et al. 2019; V. Mauerhofer & P. Dayal 2023; J. B. Muñoz et al. 2023; R. Feldmann et al. 2025; Z. Li et al. 2024).
Paper: The Extreme Faraday Effect in Fast Radio Bursts
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Theoretical prediction of (a) the burst profile and (b) the dynamic spectrum of a microsecond-duration radio burst after passing through a dense magnetized electron–ion plasma. The gray thick curve, the red curve, and the blue curve represent the frequency-averaged intensity I, linearly polarized intensity ﹩L\equiv \sqrt{{Q}^{2}+{U}^{2}}﹩, and circularly polarized intensity V, respectively. The only varying parameter in these panels is RM, with adopted values 2 × 104, 4 × 104, and 2 × 105 rad m−2 from left to right. The dynamic spectra of the L-mode subpulse and the R-mode subpulse are symmetric about the arrival time, both showing conspicuous frequency drifting with t ∝ ν−3 profiles, which are outlined by white dashed curves. The original radio burst is assumed to be fully linearly polarized and has no intrinsic frequency drifting.
Paper: The Extreme Faraday Effect in Fast Radio Bursts
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Theoretical prediction of (a) the burst profile and (b) the dynamic spectrum of a microsecond-duration radio burst after passing through a dense magnetized electron–positron pair plasma. The gray thick curve, the blue curve, and the red curve represent the frequency-averaged intensity I, Stokes parameter Q, and parameter ﹩H\equiv \sqrt{{U}^{2}+{V}^{2}}﹩, respectively. The only varying parameter in these panels is DMpair, with adopted values 10−4, 2 × 10−4, and 10−3 pc cm−3 from left to right. An abrupt orthogonal jump in the PA appears when the two subpulses are well separated. Only the O-mode branch shows frequency drifting, which can be characterized by t ∝ ν−2. The original pulse is assumed to be fully linearly polarized and has equal X-mode and O-mode components. The intrinsic frequency drifting of the original pulse is omitted.
Paper: The Extreme Faraday Effect in Fast Radio Bursts
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Frequency–width diagram of a few selected short-duration FRBs. Bursts from different papers are distinguished by different colors and shapes. Lines of different colors represent the cases in which the observed RM values of these bursts equal their critical values given by Equation (3). The gray dashed line represents RMc = 107 rad m−2. In the selected CHIME sample (brown triangles), the component with the minimum width in each burst is adopted. The brown dashed line represents RMc = 103 rad m−2, which is almost the maximum RM within the CHIME sample. The central frequency is adopted for these bursts. All bursts lie above their corresponding colored lines, which suggests that the conditions for the extreme Faraday effect are not met in these observations.
Paper: The Extreme Faraday Effect in Fast Radio Bursts
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Various pulse profiles with different relative scattering broadening ﹩{\widetilde{\tau }}_{\,{\rm sc}\,}﹩ and relative intrinsic width ﹩{\widetilde{\sigma }}_{t}﹩. The gray thick curve and the blue curve represent the total intensity and the circularly polarized intensity, respectively. Scattering begins to smear one of the circularly polarized modes when ﹩{\widetilde{\tau }}_{\,{\rm sc}\,}\gtrsim 1﹩. For an extremely large relative scattering broadening, the curve of circular polarization exhibits a dip structure, which is consistent with the case discussed by A. Suresh & J. M. Cordes (2019). The linear polarization component may be depolarized and thus is not considered here.
Paper: The Extreme Faraday Effect in Fast Radio Bursts
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Schematic illustration of the extreme Faraday effect in an electron–positron pair plasma. The propagation direction (gray arrow) of the original linearly polarized pulse (magenta) is assumed to be perpendicular to the background magnetic field (green arrows). The pulse ultimately splits into two linearly polarized subpulses (red and blue) with orthogonal polarization directions.
Paper: The Extreme Faraday Effect in Fast Radio Bursts
Authors: Yu-Chen Huang, Zi-Gao Dai
Figure caption: Schematic illustration of the extreme Faraday effect. An incident electromagnetic pulse (magenta) is linearly polarized and propagates along a background magnetic field (green arrow). When the RM exceeds the critical value given by Equation (3), the pulse splits into two circularly polarized subpulses (red and blue) due to different group velocities between the two subpulses.