adsabs/AstroCLIMB huggingface dataset:
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Mass completeness vs. redshift at different magnitudes for our galaxy sample. The left panel shows the MIRI/F770W magnitudes while the right panel shows the NIRCam/F444W magnitudes. The green dashed lines show detection limits (7σ for F444W, 2σ for MIRI/F770W). The purple solid lines indicate the corresponding magnitudes for an old galaxy template formed at z = 15 at M⋆ = 109M⊙. The same mass limits are shown with the blue solid line for a 300 Myr star-forming galaxies (SFG) template with constant star formation (CSF) history and E(B − V) = 0.1. The black and red data points denote, respectively, the galaxies with M⋆ > 109M⊙ and M⋆ > 1010M⊙.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Comparison with previous SMF studies based on mainly NIRCam data. The filled red circles denote the observed values based on our primary sample (i.e., excluding LRDs) with MIRI constraints. The red solid lines indicate the best-fit Schechter function (before convolution) of this work, while the other lines show the SMFs from other recent works based on mainly JWST/NIRCam data (T. Harvey et al. 2024; A. Weibel et al. 2024; M. Shuntov et al. 2025).
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Comparison of MIRI images reduced with default and our modified pipelines in PRIMER-COSMOS. Left: MIRI F770W and F1800W images reduced with default JWST calibration pipeline (level 3 science images from the MAST archive). Right: MIRI F770W and F1800W images reduced with modified pipelines.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: M⋆ vs. absolute UV magnitude (M1600) for our primary galaxy sample. The red solid lines show best-fit linear relations per redshift bin, while previous estimates from A. Grazian et al. (2015) are shown by the blue dashed lines. The best-fit parameters for the linear M⋆–M1600 relations (logM⋆ = a × M1600 + b) are indicated at the bottom-left corner of each panel.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Example SEDs and photo-z pdfs for galaxies with underestimated z without MIRI. The top two panels show the best-fit SEDs and pdfs of their photo-z values when fitted without MIRI, while the bottom two panels show results when MIRI is included. The spec-z of each source is indicated by the red vertical line, with their values shown in the top-right corner of the p(z) plots.
Paper: The Intracluster Light Analysis of the Most Evolved Systems of Galaxies: Fossil Groups
Authors: Nícolas O. L. de Oliveira, Yolanda Jiménez-Teja, Renato A. Dupke, Eleazar R. Carrasco, Anton M. Koekemoer, Yuanyuan Su, Jose Manuel Vilchez, Jimmy A. Irwin, Eric D. Miller, Lucas E. Johnson
Figure caption: ICL fractions measured for the three FGs added to a sample of galaxy clusters and groups analyzed by Y. Jiménez-Teja et al. (2018, 2021) and N. O. L. de Oliveira et al. (2022) at rest-frame wavelength. Merging systems are represented in red, and relaxed systems are represented in blue. FG systems are represented in black symbols with corresponding error bars. We also include the bona fide FG (RXJ1007, black triangle) analyzed by R. A. Dupke et al. (2022).
Paper: The Intracluster Light Analysis of the Most Evolved Systems of Galaxies: Fossil Groups
Authors: Nícolas O. L. de Oliveira, Yolanda Jiménez-Teja, Renato A. Dupke, Eleazar R. Carrasco, Anton M. Koekemoer, Yuanyuan Su, Jose Manuel Vilchez, Jimmy A. Irwin, Eric D. Miller, Lucas E. Johnson
Figure caption: Original images of RXJ0856 (left), RXJ1136 (center), and RXJ1410 (right) in the F606W filter and their corresponding galaxy members in green circles. Saturated stars are masked in white circles. North is up, east is left.
Paper: The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse
Authors: Steve B. Howell, David R. Ciardi, Catherine A. Clark, Douglas A. Hope, Colin Littlefield, Elise Furlan
Figure caption: The AAVSO photometric observations of Betelgeuse. The V and B band measurements cover the past 8 years including the deep fading of Betelgeuse in late 2019 to early 2020 known as the Great Dimming event. The dates of our two speckle observations are marked.
Paper: The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse
Authors: Steve B. Howell, David R. Ciardi, Catherine A. Clark, Douglas A. Hope, Colin Littlefield, Elise Furlan
Figure caption: The magnitude contrast sensitivity of the 2020 February (dashed red) and 2024 December (solid blue) data plotted as a function of the radial distance from the primary star. The curves represent the sensitivity to a companion at 1σ. The overplotted point represents the detected companion with 1σ uncertainties on its magnitude. The uncertainty on the separation is represented by the size of the plotting symbol. The companion was detected at a significance of ∼1.5σ.
Paper: The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse
Authors: Steve B. Howell, David R. Ciardi, Catherine A. Clark, Douglas A. Hope, Colin Littlefield, Elise Furlan
Figure caption: The reconstructed images from the 2020 February 17 observations at 562 nm (left) and for the 2024 December 9 observations at 466 nm (right). The images are oriented such that north is up and east is left, and the color bar shows the relative scaling applied to both images. The inset image shows a diffraction-limited PSF standard star observed near in time to Betelgeuse. Note the probable direct-imaging detection of the companion to Betelgeuse in the 2024 image (arrow) that is absent in the 2020 observations.
Paper: The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse
Authors: Steve B. Howell, David R. Ciardi, Catherine A. Clark, Douglas A. Hope, Colin Littlefield, Elise Furlan
Figure caption: Example cuts through the stellar disk 2D profile of Betelgeuse during the 2020 February and 2025 December observations. The vertical dotted lines show the locations of the first derivative inflection points in each profile (see text). The angular diameters measured in this manner are listed in Table 1.
Paper: First Detection of Circular Polarization in Radio Continuum Toward a Massive Protostar
Authors: A. G. Cheriyan, S. Vig, Nirupam Roy, Samir Mandal, C. Carrasco-González, A. Rodríguez-Kamenetzky, A. Pasetto
Figure caption: (a) Stokes I emission of the polarization calibrator J2355+4950. (b) Stokes ﹩\sqrt{{Q}^{2}+{U}^{2}}﹩ image of J2355+4950. (c) Stokes V image of J2355+4950. The cyan ellipse represents the beam.
Paper: The Kangaroo’s First Hop: The Early Fast Cooling Phase of EP250108a/SN 2025kg
Authors: Rob A. J. Eyles-Ferris, Peter G. Jonker, Andrew J. Levan, Daniele Bjørn Malesani, Nikhil Sarin, Christopher L. Fryer, Jillian C. Rastinejad, Eric Burns, Nial R. Tanvir, Paul T. O'Brien, Wen-fai Fong, Ilya Mandel, Benjamin P. Gompertz, Charles D. Kilpatrick, Steven Bloemen, Joe S. Bright, Francesco Carotenuto, Gregory Corcoran, Laura Cotter, Paul J. Groot, Luca Izzo, Tanmoy Laskar, Antonio Martin-Carrillo, Jesse Palmerio, Maria E. Ravasio, Jan van Roestel, Andrea Saccardi, Rhaana L. C. Starling, Aishwarya Linesh Thakur, Susanna D. Vergani, Paul M. Vreeswijk, Franz E. Bauer, Sergio Campana, Jennifer A. Chacón, Ashley A. Chrimes, Stefano Covino, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Nusrin Habeeb, Dieter H. Hartmann, Agnes P. C. van Hoof, Páll Jakobsson, Yashaswi Julakanti, Giorgos Leloudas, Daniel Mata Sánchez, Christopher J. Nixon, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan Quirola-Vásquez, Ben C. Rayson, Ruben Salvaterra, Ben Schneider, Manuel A. P. Torres, Tayyaba Zafar
Figure caption: The spectral sequence of SN 2025kg’s fast cooling phase with times given in the observer frame. Emission and absorption lines typically detected in galaxy spectra are marked in solid and dashed gray lines, respectively. In addition, blackbody fits to each continuum (see text) are plotted in black.
Paper: The Kangaroo’s First Hop: The Early Fast Cooling Phase of EP250108a/SN 2025kg
Authors: Rob A. J. Eyles-Ferris, Peter G. Jonker, Andrew J. Levan, Daniele Bjørn Malesani, Nikhil Sarin, Christopher L. Fryer, Jillian C. Rastinejad, Eric Burns, Nial R. Tanvir, Paul T. O'Brien, Wen-fai Fong, Ilya Mandel, Benjamin P. Gompertz, Charles D. Kilpatrick, Steven Bloemen, Joe S. Bright, Francesco Carotenuto, Gregory Corcoran, Laura Cotter, Paul J. Groot, Luca Izzo, Tanmoy Laskar, Antonio Martin-Carrillo, Jesse Palmerio, Maria E. Ravasio, Jan van Roestel, Andrea Saccardi, Rhaana L. C. Starling, Aishwarya Linesh Thakur, Susanna D. Vergani, Paul M. Vreeswijk, Franz E. Bauer, Sergio Campana, Jennifer A. Chacón, Ashley A. Chrimes, Stefano Covino, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Nusrin Habeeb, Dieter H. Hartmann, Agnes P. C. van Hoof, Páll Jakobsson, Yashaswi Julakanti, Giorgos Leloudas, Daniel Mata Sánchez, Christopher J. Nixon, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan Quirola-Vásquez, Ben C. Rayson, Ruben Salvaterra, Ben Schneider, Manuel A. P. Torres, Tayyaba Zafar
Figure caption: The discovery image of SN 2025kg. The stacked LT IO:O g-band image is shown on the left, the Pan-STARRS template is shown in the center, and the subtraction is shown on the right. The images are oriented with north to the top and east to the left and the position of SN 2025kg is marked with the cross hairs.
Paper: The Kangaroo’s First Hop: The Early Fast Cooling Phase of EP250108a/SN 2025kg
Authors: Rob A. J. Eyles-Ferris, Peter G. Jonker, Andrew J. Levan, Daniele Bjørn Malesani, Nikhil Sarin, Christopher L. Fryer, Jillian C. Rastinejad, Eric Burns, Nial R. Tanvir, Paul T. O'Brien, Wen-fai Fong, Ilya Mandel, Benjamin P. Gompertz, Charles D. Kilpatrick, Steven Bloemen, Joe S. Bright, Francesco Carotenuto, Gregory Corcoran, Laura Cotter, Paul J. Groot, Luca Izzo, Tanmoy Laskar, Antonio Martin-Carrillo, Jesse Palmerio, Maria E. Ravasio, Jan van Roestel, Andrea Saccardi, Rhaana L. C. Starling, Aishwarya Linesh Thakur, Susanna D. Vergani, Paul M. Vreeswijk, Franz E. Bauer, Sergio Campana, Jennifer A. Chacón, Ashley A. Chrimes, Stefano Covino, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Nusrin Habeeb, Dieter H. Hartmann, Agnes P. C. van Hoof, Páll Jakobsson, Yashaswi Julakanti, Giorgos Leloudas, Daniel Mata Sánchez, Christopher J. Nixon, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan Quirola-Vásquez, Ben C. Rayson, Ruben Salvaterra, Ben Schneider, Manuel A. P. Torres, Tayyaba Zafar
Figure caption: The UVOIR light curve of SN 2025kg’s fast cooling phase. The photometry has been corrected for Galactic extinction of AV = 0.049 (E. F. Schlafly & D. P. Finkbeiner 2011) using the K. D. Gordon et al. (2023) Milky Way model. The vertical lines indicate the times of our spectroscopic observations (with colors corresponding to Figure 4).
Paper: The Kangaroo’s First Hop: The Early Fast Cooling Phase of EP250108a/SN 2025kg
Authors: Rob A. J. Eyles-Ferris, Peter G. Jonker, Andrew J. Levan, Daniele Bjørn Malesani, Nikhil Sarin, Christopher L. Fryer, Jillian C. Rastinejad, Eric Burns, Nial R. Tanvir, Paul T. O'Brien, Wen-fai Fong, Ilya Mandel, Benjamin P. Gompertz, Charles D. Kilpatrick, Steven Bloemen, Joe S. Bright, Francesco Carotenuto, Gregory Corcoran, Laura Cotter, Paul J. Groot, Luca Izzo, Tanmoy Laskar, Antonio Martin-Carrillo, Jesse Palmerio, Maria E. Ravasio, Jan van Roestel, Andrea Saccardi, Rhaana L. C. Starling, Aishwarya Linesh Thakur, Susanna D. Vergani, Paul M. Vreeswijk, Franz E. Bauer, Sergio Campana, Jennifer A. Chacón, Ashley A. Chrimes, Stefano Covino, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Nusrin Habeeb, Dieter H. Hartmann, Agnes P. C. van Hoof, Páll Jakobsson, Yashaswi Julakanti, Giorgos Leloudas, Daniel Mata Sánchez, Christopher J. Nixon, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan Quirola-Vásquez, Ben C. Rayson, Ruben Salvaterra, Ben Schneider, Manuel A. P. Torres, Tayyaba Zafar
Figure caption: The photometric SEDs of SN 2025kg at various epochs (given in the observer frame) fitted with sampled blackbody models.
Paper: A Transiting Giant on a 7.7 yr Orbit Revealed by Transit Timing Variations in the TOI-201 System
Authors: Gracjan Maciejewski, Weronika Łoboda
Figure caption: Transit observables for TOI-201 b from the dynamical model. (a) Transit timing residuals relative to the refined linear ephemeris, derived using midtransit times from TESS Sectors 2–39 (blue dots). The thick blue line represents the linear ephemeris propagated to later epochs, where deviations caused by TOI-201 c become apparent. A set of 50 posterior realizations is overplotted to illustrate the uncertainty in this ephemeris. Midtransit times of TOI-201 b that deviate significantly from the linear prediction are highlighted in green. The best-fitting two-planet dynamical model is shown as a thick red line, with 100 posterior samples overplotted to illustrate model uncertainty. The shaded gray region indicates the window of upcoming TESS observations. The vertical dashed line marks the transit of TOI-201 c. (b) Transit timing residuals relative to the best-fitting dynamical model. (c) and (d) Evolution of the impact parameter bb and transit duration τb, respectively, as predicted by the model. Uncertainties are indicated by the ensemble of posterior realizations. (e) HARPS RV measurements with the best-fitting two-planet dynamical model overplotted. The RV modulation induced by TOI-201 b is superimposed on a long-term trend caused by TOI-201 c. The residuals are shown in panel (f). (g) Schematic diagram showing the astrocentric architecture of the TOI-201 system. The orbits of planets b and c are shown in red and blue, respectively. Uncertainties are illustrated using 100 posterior samples. Planet positions at the epoch of Tmid,c are marked with dots, and the host star is shown as an orange dot. Sizes of all bodies are not to scale. The pale green region indicates the circumstellar habitable zone, using conservative inner and outer boundaries (runaway and maximum greenhouse) computed via Equations (2) and (3) from R. K. Kopparapu et al. (2013).
Paper: A Transiting Giant on a 7.7 yr Orbit Revealed by Transit Timing Variations in the TOI-201 System
Authors: Gracjan Maciejewski, Weronika Łoboda
Figure caption: Transit light curves of TOI-201 b observed with TESS. Transits consistent with a linear ephemeris are shown in blue, with predicted midtransit times marked by the dashed gray line. Transits exhibiting significant timing offsets, particularly those from Sectors 65–88, are plotted in green. Best-fitting models are overlaid in red, with residuals shown below.
Paper: A Transiting Giant on a 7.7 yr Orbit Revealed by Transit Timing Variations in the TOI-201 System
Authors: Gracjan Maciejewski, Weronika Łoboda
Figure caption: Transit light curve of TOI-201 c detected in TESS Sector 64. The best-fitting model is shown in red, with residuals plotted below.
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: Left panel: the mass and radius diagram of all confirmed transiting brown dwarfs and low-mass stars. The colored dashed lines are the theoretical isochrones of cool brown dwarfs with different ages at solar metallicity from I. Baraffe et al. (2003). The vertical solid line marks the mass of 80 MJ. Right panel: the eccentricity vs. orbital periods of known transiting brown dwarfs (orange) and low-mass stars (red). The vertical dashed line marks the 10 day period boundary that we used to select long-period objects for statistics. The blue dots are the selected transiting warm Jupiters, while the transiting hot Jupiters are shown as gray dots for reference. In both panels, TOI-5575 b is shown as a black star.
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: Left panel: the TESS and ASP light curves folded in phase with the transit ephemeris from the joint analysis along with the best-fit transit models. Right panel: the full SPIRou RV time series and the phase-folded RVs. The error bars presented here are the quadrature sum of the original RV uncertainties and the instrument jitter. The black solid line is the best-fit Keplerian model. The residuals are shown below each subplot.
Paper: Cosmic Clues from Amaterasu: Blazar-driven Ultrahigh-energy Cosmic Rays?
Authors: Saikat Das, Srijita Hazra, Nayantara Gupta
Figure caption: Multiwavelength SED of PKS 1717+177 showing the synchrotron (orange solid), external Compton (green dotted), the external photon field (brown dashed), the hadronic cascade (blue solid), and the ﹩{\nu }_{\mu }+{\overline{\nu }}_{\mu }﹩ spectrum (magenta) in the observer frame. Black data points show the spectral data from radio to VHE γ-rays, and upper limits are shown in gray. The black and gray error bars correspond to the neutrino flux from TXS 0506+056, which is shown for reference, assuming a 7.5 and 0.5 yr limit. The SSC spectrum shown in cyan color is negligible in the EC model. The orange dashed and blue dashed lines show the sensitivity of CTA-North and LHAASO detectors, respectively.
Paper: Cosmic Clues from Amaterasu: Blazar-driven Ultrahigh-energy Cosmic Rays?
Authors: Saikat Das, Srijita Hazra, Nayantara Gupta
Figure caption: UHECR particles placed randomly on the surface of the Galactic horizon (red) for M. Unger & G. R. Farrar (2024b) magnetic field with momentum vector given by von Mises–Fisher distribution concentrated around the angular uncertainty region, centered on the best-fit direction at Earth. The black and blue dots correspond to the Galactic center and Earth. A backtracking simulation of protons from Earth to these directions shows negligible deflections in the GMF, illustrating the requirement for a high magnitude of EGMF.
Paper: First Detection of Circular Polarization in Radio Continuum Toward a Massive Protostar
Authors: A. G. Cheriyan, S. Vig, Nirupam Roy, Samir Mandal, C. Carrasco-González, A. Rodríguez-Kamenetzky, A. Pasetto
Figure caption: (a) Total intensity radio map of the I18162 region at the VLA C band. The contour levels in cyan are marked in the color bar, where the beam size is 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 × 5﹩\mathop{.}\limits^{\unicode{x02033}}﹩0. (b) Linearly polarized emission observed toward the near jet lobes of I18162. The cyan contours overlaid on the image are the Stokes I contours, which are the same as in panel (a). The green ellipse at the bottom-left corner shows the beam size. The color bar is shown on the right side of the image.
Paper: First Detection of Circular Polarization in Radio Continuum Toward a Massive Protostar
Authors: A. G. Cheriyan, S. Vig, Nirupam Roy, Samir Mandal, C. Carrasco-González, A. Rodríguez-Kamenetzky, A. Pasetto
Figure caption: Plot of fractional circular polarization (solid black circles) and Stokes I flux densities (histogram in green) as a function of frequency. The data depict the fractional circular polarization at the central frequencies of spectral windows used in the analysis. The red dashed line represents the nominal fractional CP of 4% assumed in our estimations; see Section 3 for details.
Paper: First Detection of Circular Polarization in Radio Continuum Toward a Massive Protostar
Authors: A. G. Cheriyan, S. Vig, Nirupam Roy, Samir Mandal, C. Carrasco-González, A. Rodríguez-Kamenetzky, A. Pasetto
Figure caption: Variation of the number of turbulent cells (KoutR) with respect to the change in the Lorentz factor (﹩{\gamma }_{\min }﹩). The color bar represents the ratio of the total magnetic field and magnetic field toward the line of sight (B0/Bz). The pale magenta-colored region represents the feasible values of ﹩{\gamma }_{\min }﹩ and KoutR considering B0 > Bz, Faraday conversion, and Faraday depolarization.
Paper: Cosmic Clues from Amaterasu: Blazar-driven Ultrahigh-energy Cosmic Rays?
Authors: Saikat Das, Srijita Hazra, Nayantara Gupta
Figure caption: Proton luminosity in the 0.1 TeV to 10 EeV energy range constrained by the detection of 1 UHE proton event in the Telescope Array energy bin 148–340 EeV. The different curves correspond to various values of rigidity cutoff ﹩{R}_{{\rm{\max }}}﹩ in the injection spectrum.
Paper: First Detection of Circular Polarization in Radio Continuum Toward a Massive Protostar
Authors: A. G. Cheriyan, S. Vig, Nirupam Roy, Samir Mandal, C. Carrasco-González, A. Rodríguez-Kamenetzky, A. Pasetto
Figure caption: (a) Circularly polarized Stokes V emission observed toward the central source I18162. The white contours overlaid on the image are the Stokes I contours, which are the same as in Figure 1. The color bar is shown on the right side of the image. (b) Zoomed-in view of the central region exhibiting the circularly polarized emission. The green ellipse at the bottom-left corner shows the beam size.
Paper: First Detection of Circular Polarization in Radio Continuum Toward a Massive Protostar
Authors: A. G. Cheriyan, S. Vig, Nirupam Roy, Samir Mandal, C. Carrasco-González, A. Rodríguez-Kamenetzky, A. Pasetto
Figure caption: (a) Stokes I emission of the flux calibrator 3C286. (b) Stokes ﹩\sqrt{{Q}^{2}+{U}^{2}}﹩ emission of the flux calibrator 3C286. (c) Stokes V image of the flux calibrator 3C286. The cyan ellipse represents the beam.