adsabs/AstroCLIMB huggingface dataset:
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Logarithm of the production factors of the 15 M ⊙ stars of Set Z (top panels), Set F (central panels), and Set E (bottom panels) as a function of the atomic number A. The color scale on the right marks the different initial equatorial velocity of the star, from nonrotating (dark blue) up to 800 km s−1 (yellow).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: The variation of the parameter χ (Equation (3)) between central He ignition and exhaustion, as a function of the initial equatorial velocity for the 15 (filled diamonds) and the 25 M ⊙ (filled dots) in Set Z (red), Set F (green), and Set E (blue).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Same as Figure 27, but for the 25 M ⊙ models.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Total net yield of elements from Ga up to Bi (S3083; see text) as a function of the initial velocity for all the explored metallicity.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Trend of the yields of Sr, Ba, and Pb as a function of the initial rotation velocity (left panels) and of the Δχ parameter (right panels; see text): 15 M ⊙ (green diamonds), 25 M ⊙ (green dots) Set F, 15 M ⊙ (blue diamonds), and 25 M ⊙ (blue dots) Set E.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: [X/O] distribution for the 15 M ⊙ stellar models for Set F (top panel) and Set E (bottom panel) as a function of the atomic number Z. The two vertical dashed–dotted lines correspond to the atomic number of Sr (Z = 38) and Ba (Z = 56).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: [X/Mg] distribution for the 15 M ⊙ stellar models for Set F (top panel) and Set E (bottom panel) as a function of the atomic number Z. The two vertical dashed–dotted lines correspond to the atomic number of Sr (Z = 38) and Ba (Z = 56).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Nitrogen yields as a function of the initial rotation velocity.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Same as Figure 28 but for the 25 M ⊙ models.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Flourine yields as a function of the initial rotation velocity.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Internal structure of the nonrotating 25 M ⊙ star of Set Z (top panels) and Set F (bottom panels) before (left panels) and after (right panels) the convective H–He shell merging. The black, red, green, magenta, and blue solid lines represent the abundance in mass fraction of the principal nuclear species (H, 4He, 12C, 20Ne, and 16O) as a function of the internal mass coordinate, and they refer to the secondary y-axis. The other solid lines show the internal distribution of the most produced nuclei during the merger between the H and the He convective shells (in particular, 14N is the violet solid line), and they refer to the principal y-axis.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Top panel: presupernova (dashed lines) and postexplosive (solid lines) structure of a 25 M ⊙ star at [Fe/H] = −5, rotating at 600 km s−1. In this case, the abundances are presented as a function of the internal mass of the star, from the center up to the base of the H shell. The gray bands in the plot mark each explosive burning stage in the corresponding internal mass coordinate, as discussed in the text. The dashed lines represent the abundances of the isotopes at the presupernova stage, while the solid lines represent the isotopic abundances after the explosive nucleosynthesis. Bottom panel: pre-explosive (black dots) and explosive (red dots) yields of the model 025f600.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Kippenhahn diagrams of the rotating 15 M ⊙ models of [Fe/H] = −4. The color coding is the same as in Figure 2.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Kippenhahn diagrams of the rotating 15 M ⊙ models of [Fe/H] = −5. The color coding is the same as in Figure 2.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Internal structure after the C–O shell merger in two 15 M ⊙ rotating stars, i.e., 015f600 (left panel) and 015e300 (right panel). The dashed lines (right y-axis) represent the main nuclear species (H, 4He, 12C, 16O, 20Ne, and 28Si), while the solid lines (left y-axis) show the internal profile of selected s-process isotopes: 88Sr (weak component), 138Ba (main component), 208Pb (heavy component), and one isotope between the neutron magic nuclei N = 50, and N = 82, ﹩{}^{120}\mathrm{Sn}﹩. Finally, the gray solid line represents the 19F abundance.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Internal structure at core He exhaustion of four representative models 015f600, 025f600, 015e300, and 025e700. The dashed lines (right y-axis) represent the main nuclear species (H, 4He, 12C, 16O, and 20Ne), while the solid lines (left y-axis) show the internal profile of selected s-process isotopes: 88Sr (weak component), 138Ba (main component), 208Pb (heavy component), and one isotope between the neutron magic nuclei N = 50, and N = 82, ﹩{}^{120}\mathrm{Sn}﹩. At last, the gray solid line represents the 19F abundance.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: The compactness ξ of the star evaluated at 2.5 M ⊙ (filled dots) and at the border of the CO core (filled triangles) at the presupernova stage in 15 M ⊙ (red points) and 25 M ⊙ (blue points) in Set Z (top panel), Set F (central panel), and Set E (bottom panel).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Comparison of the entropy profile (per nucleon in units of Boltzmann constant k B, green lines) as a function of the internal pressure P between the nonrotating 015e000 model (dashed lines) and the rotating 015e300 one (solid lines). Blue and magenta lines show the abundances in mass fraction of 16O and 20Ne, respectively, in the two cases. The yellow and the gray zones show the O and Ne convective regions in the nonrotating and in the rotating models, respectively.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Same as Figure 17, but after the full development of the C convective shell.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Same as Figure 17, but after the formation of the He convective shell.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: The normalized particle spectra of test particles as obtained at different simulation times t = 120R0/c, t = 400R0/c, and t = 1000R0/c for the simulation runs FR Ia, Ib (left panel), Ic and FR II (right panel). The normalization factors are chosen differently for the purpose of visualization. To avoid overlapping lines, we only show the particle spectrum above the injection energy.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: The velocity (left panel) and magnetic field (right panel) profiles in the radial direction are averaged over the axial and azimuthal directions for the simulated jets at the frozen time t = tfrozen.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: An example of simulation run FR II at t = tfrozen. The box size is 6R0 × 3R0 × 6R0. The distribution of the axial velocity βy is shown in order to illustrate the spine-sheath jet and cocoon structure. Magnetic field lines are shown with color coding of their magnitude. The black arrows represent test particles with larger arrow sizes for higher-energy particles.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: The time evolution of mean energy (left panel) and mean radial position (right panel) for the FR I simulations. The right panel has the same figure legend as the left panel. The solid lines, labeled with “all” are for the all-particle sample. The dashed–dotted lines, labeled with “HE” are for the high-energy component.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: The spectra are integrated over time to mimic continuous particle injections for our simulation runs. The vertical lines denote the Hillas reference limit for the jet. The spectra are normalized such that the first data points are equal to unity. The spikes in the spectra are an artifact of the monoenergetic injection (see γinj in Table 1).
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: Exemplary trajectories of four test particles are shown with different colors for the FR Ib simulation run. The trajectories are projected in the radial direction of the jet. The left y-axis is the Lorentz factor (γ) of test particles. The blue lines are the velocity profiles of the jet at different simulation times, with the values shown at the right y-axis.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: The spectral energy distributions (left panel) and spatial distributions (right panel) are shown for particles injected at different radii at the frozen time tfrozen = 120R0/c. The particle energy spectra are normalized to unity at the peak value, while the spatial distribution is normalized so that the sum of dthe istribution equals to unity.
Paper: Observed Fluctuation Enhancement and Departure from WKB Theory in Sub-Alfvénic Solar Wind
Authors: David Ruffolo, Panisara Thepthong, Peera Pongkitiwanichakul, Sohom Roy, Francesco Pecora, Riddhi Bandyopadhyay, Rohit Chhiber, Arcadi V. Usmanov, Michael Stevens, Samuel Badman, Orlando Romeo, Jiaming Wang, 嘉明 王, Joshua Goodwill, Melvyn L. Goldstein, William H. Matthaeus
Figure caption: Solar wind fluctuation energy per unit volume vs. Alfvén Mach number MA and radial distance r for PSP data during orbits 8–17. Each blue point shows a 1 minute averaged value. Red circles indicate the mean value in each bin, where bins are combined until they have at least 100 data points, and each error bar indicates the standard error of the mean of data in that bin. Magnetic fluctuation energy per volume: (a) δB2/μ0 vs. MA and (b) vs. r/R⊙. Velocity fluctuation energy per volume: (c) ρδV2 vs. MA and (d) vs. r/R⊙. MA is computed using the density data set described in the text. Velocity fluctuation is computed only when SPAN-i data satisfy quality conditions described in the text. The evolutionary trend predicted from WKB theory for “fossil” Alfvénic fluctuations that propagate outward without interaction, ﹩{ \mathcal E }\propto {[{M}_{{\rm{A}}}{({M}_{{\rm{A}}}+1)}^{2}]}^{-1}﹩ (dashed curves in panels (a) and (c)), fails to explain the PSP data for sub-Alfvénic solar wind, i.e., for MA < 1. The discrepancy implies that most solar wind fluctuation energy does not originate near the solar surface but rather is strongly enhanced in situ at 0.5 ≲ MA ≲ 1.
Paper: Observed Fluctuation Enhancement and Departure from WKB Theory in Sub-Alfvénic Solar Wind
Authors: David Ruffolo, Panisara Thepthong, Peera Pongkitiwanichakul, Sohom Roy, Francesco Pecora, Riddhi Bandyopadhyay, Rohit Chhiber, Arcadi V. Usmanov, Michael Stevens, Samuel Badman, Orlando Romeo, Jiaming Wang, 嘉明 王, Joshua Goodwill, Melvyn L. Goldstein, William H. Matthaeus
Figure caption: Quantities related to Alfvén wave action vs. Alfvén Mach number MA, expected to be conserved in WKB theory. (a) ﹩{r}^{2}{(V+{V}_{{\rm{A}}})}^{2}\delta {B}^{2}/({\mu }_{0}{V}_{{\rm{A}}})﹩ vs. MA and (b) ﹩{r}^{2}{(V+{V}_{{\rm{A}}})}^{2}\rho \delta {V}^{2}/{V}_{{\rm{A}}}﹩ vs. MA, evaluated here from PSP data, are not constant as a function of MA, except possibly for 1 < MA < 2. The solid (red) line is bin-averaged data. Vertical axes are normalized to the value at MA = 1 (horizontal dark blue line). As a guide, the vertical black dashed line at MA = 1 indicates the Alfvén transition zone. In the sub-Alfvénic region (MA < 1), these quantities are increasing, violating conservation of wave action, and suggesting in situ fluctuation energy enhancement.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: The turbulence spectra for the velocity (Pv) and magnetic field (PB) are shown for the different simulation runs. The vertical dotted lines correspond to the average Larmor radii of the injected energy for different simulations (see Section 3 and Appendix C for details).
Paper: Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM
Authors: Yuto Mochizuki, Masahiro Tsujimoto, Richard L. Kelley, Bert Vander Meulen, Teruaki Enoto, Yutaro Nagai, Chris Done, Pragati Pradhan, Natalie Hell, Katja Pottschmidt, Ken Ebisawa, Ehud Behar
Figure caption: (a) FW positions, (b) 2–12 keV count rate binned at 100 s, (c) the fraction of Hp events, and (d) orbital phase (M. Falanga et al. 2015). The observation was interrupted by South Atlantic Anomaly passages (blue) and ADR recycles (red). The FW 55Fe was illuminated several times as shown in (a) during on-source integration time, leading to an additional count rate of 20 s−1.
Paper: Observed Fluctuation Enhancement and Departure from WKB Theory in Sub-Alfvénic Solar Wind
Authors: David Ruffolo, Panisara Thepthong, Peera Pongkitiwanichakul, Sohom Roy, Francesco Pecora, Riddhi Bandyopadhyay, Rohit Chhiber, Arcadi V. Usmanov, Michael Stevens, Samuel Badman, Orlando Romeo, Jiaming Wang, 嘉明 王, Joshua Goodwill, Melvyn L. Goldstein, William H. Matthaeus
Figure caption: Alfvén ratio rA = μ0ρδV2/δB2 of solar wind fluctuation energies vs. Alfvén Mach number MA. WKB theory for noninteracting fossil Alfvén waves predicts equipartition, i.e., rA = 1. This PSP observation near the Sun is consistent with observations at greater distances that typically indicate rA < 1. This can be understood in terms of turbulence effects (see, e.g., W. H. Matthaeus & M. L. Goldstein 1982; W. H. Matthaeus & S. L. Lamkin 1986; P. Thepthong et al. 2024). Orange dashed line marks 0.5 on vertical axis.
Paper: Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM
Authors: Yuto Mochizuki, Masahiro Tsujimoto, Richard L. Kelley, Bert Vander Meulen, Teruaki Enoto, Yutaro Nagai, Chris Done, Pragati Pradhan, Natalie Hell, Katja Pottschmidt, Ken Ebisawa, Ehud Behar
Figure caption: (a) Resolve spectra out of the eclipse in the 2–12 keV band. A close-up view of the Fe K band is given in the inset. (b) Fe Kα spectra and their best-fit models and (c) residuals to the fit at ϕorb = 0.25 (blue) and 0.75 (orange). Compare to Figure 4 (a) in P. S. Wojdowski et al. (2003) for previously the best spectra with the Chandra grating spectrometer.
Paper: Acceleration of Ultra-high-energy Cosmic Rays in the Kiloparsec-scale Jets of Nearby Radio Galaxies
Authors: Jie-Shuang Wang, 界双 王, Brian Reville, Frank M. Rieger, Felix A. Aharonian
Figure caption: The time evolution of the mean particle energy (left panel) and the spectra (right panel) of the FR Ib and FR Ib-hi simulations. The definition of the all-particle sample and HE component in the left panel are the same as in Figure 5. In the right-hand panel, the normalization and particle energy range are selected for visualization purposes, similar to Figure 4.
Paper: Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM
Authors: Yuto Mochizuki, Masahiro Tsujimoto, Richard L. Kelley, Bert Vander Meulen, Teruaki Enoto, Yutaro Nagai, Chris Done, Pragati Pradhan, Natalie Hell, Katja Pottschmidt, Ken Ebisawa, Ehud Behar
Figure caption: Best-fit values of (a) Fe Kα line center, (b) flux, and (c) width as well as (d) fEW as a function of ϕorb. Shaded areas indicate eclipses. In (a), the data are compared to the RV curve of the NS (red), O star (green), and the best fit to the data outside the eclipse (blue). Positive RVs are in the approaching direction. Results of the radiative transfer calculation are compared in (c) and (d) for the O star surface (blue) and stellar wind (orange) as the site of Fe Kα production.
Paper: Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM
Authors: Yuto Mochizuki, Masahiro Tsujimoto, Richard L. Kelley, Bert Vander Meulen, Teruaki Enoto, Yutaro Nagai, Chris Done, Pragati Pradhan, Natalie Hell, Katja Pottschmidt, Ken Ebisawa, Ehud Behar
Figure caption: Schematic view and the radiative transfer calculation setup at ϕorb = 0.75. The CoM is placed at the origin, and the orbit is projected on its plane. The line of sight is toward +y-axis direction. The locations of the NS (red), O star (black), and an O star surface closest to the NS (blue) are shown with filled circles of their colors. The NS and O star orbits are shown with dotted circles. For the NS orbit, the eclipsed part is shown in transparency, and ϕorb is shown in text. The Roche potential is shown with the turquoise contours. The scale length of Pspinc is shown at the bottom left. For the modeling, the O star surface is approximated by a sphere with a radius of RO in blue, which subtends an angle θ0 seen from the NS. A reflection path is shown with black arrows.
Paper: Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM
Authors: Yuto Mochizuki, Masahiro Tsujimoto, Richard L. Kelley, Bert Vander Meulen, Teruaki Enoto, Yutaro Nagai, Chris Done, Pragati Pradhan, Natalie Hell, Katja Pottschmidt, Ken Ebisawa, Ehud Behar
Figure caption: (a) Pulse shape folded by Pspin, (b) phase delay relative to the lowest energy band as a function of energy, and (c) pulse fraction as a function of energy. The Fe Kα count rate is from 6.35 to 6.45 keV.
Paper: Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM
Authors: Yuto Mochizuki, Masahiro Tsujimoto, Richard L. Kelley, Bert Vander Meulen, Teruaki Enoto, Yutaro Nagai, Chris Done, Pragati Pradhan, Natalie Hell, Katja Pottschmidt, Ken Ebisawa, Ehud Behar
Figure caption: Relation between τFe and fEW. The observed results at different ϕorb are shown with plus symbols, while the simulated results are shown with dotted lines of different colors for different f ∈ {0, 0.15, 0.9}.
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: Left: MMT i-band image of the field surrounding the FRB 20190208A localization. No host is visible, with a 3σ limit of i ≳ 25.7 mag (AB) at the position of FRB 20190208A. Right: GTC r-band image showing the same field but achieving about 2 mag greater depth (see Section 3). The dashed black box indicates the region that was considered in host association, and the nine sources that were identified as potential candidate hosts are marked by black circles (see Section 3.3). The green crosshair indicates the FRB position—note that the EVN burst localization region is much smaller, roughly the pixel scale in this image. In the GTC image, the FRB position is spatially coincident with source O4 (also see Table 2), which is not visible in the MMT image. The gray disk in the bottom right of the inset indicates the effective point-spread function of the GTC image. The seeing varied in the range 0.″6–0.″9 during the GTC observations.