adsabs/AstroCLIMB huggingface dataset:
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Comparison of velocity and length scale for filament/prominence eruptions on the Sun and EK Dra. Blue circles and orange crosses show solar filament eruptions with and without associated CMEs, respectively (D. Seki et al. 2021). The dark green symbols (circle and downward-pointing triangles) and red/blue squares show stellar prominence and filament eruptions on EK Dra, respectively. Stellar velocities are maximum LoS values, while solar velocities are maximum radial values. The solid black line indicates an empirical solar threshold that roughly separates CME-associated and non-CME filament eruptions (D. Seki et al. 2021).
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Cumulative flare frequency as a function of flare energy for EK Dra and V889 Her. Data from all TESS sectors are shown in black, while individual sectors are shown with colored lines.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: (Left) Size–stellar mass relation of our quasar host galaxies compared with the control sample of star-forming galaxies (SFGs) and from COSMOS-Web (see L. Yang et al. 2025) at redshift 6 < z < 7. The two gray stars with arrows are the host measurements with size or stellar mass as upper limits. We also include seven quiescent galaxies (QGs) at 4 < z < 5 for comparison. In addition, the best-fit relations for the COSMOS-Web sample, derived assuming the power-law model, are also shown. We measure the sizes of our sample host galaxies using the F356W filter, while the COSMOS-Web sample adopts the F444W filter (see Section 4.4 for methodological details). The results show that the sizes of our quasar hosts appear to be similar to the SFGs for a given stellar mass, while the two post-starbursts are consistent with the QGs at lower redshifts within the 1σ level. The dashed horizontal line indicates the PSF size at redshift 6. (Right) Projected 2D stellar mass surface density within Reff as a function of redshift, compared with those of quiescent galaxies from the literature (R. E. Skelton et al. 2014; A. C. Carnall et al. 2023; E. Vanzella et al. 2023; D. J. Setton et al. 2024; A. Weibel et al. 2025; A. de Graaff et al. 2025) as well as with 1 < z < 2.5 AGN-host galaxies revealed by COSMOS-Web (T. S. Tanaka et al. 2025). Most of our quasar hosts fall below the typical quiescent threshold (dashed line of 1010 M⊙/kpc2 as introduced in A. Weibel et al. 2025). The two post-starburst targets are in the top region of our sample. The typical uncertainty associated with the density measurements of the hosts in our sample is 0.5 dex.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Statistics of the flare rise phase duration (GOES start to peak time difference) for the five flare categories. (a) Distribution of durations for all flares observed by EIS in the catalog. (b) Distribution of the number of individual EIS time steps (y-axis) captured between 400 and 5000 s preceding the GOES flare peak, representing the data subset used for the preflare analysis in this study. The mean (dashed purple line) and median (solid red line) durations are indicated in each panel. The comparison shows that the preflare subset analyzed is slightly biased toward atypical rise durations compared to the overall sample.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: This figure presents the results of our simulations assessing the recovery of host galaxy properties for all 12 quasar targets in F356W. The top panel shows the recovered host magnitudes minus the truth, while the bottom panel displays the recovered effective radii minus the truth, both plotted as a function of input host magnitude and host-to-total flux ratio. Our results demonstrate that the dispersion in inferred host magnitude increases for fainter hosts (those with magnitudes >25) and for systems with host-to-total flux ratios below 10%. Nevertheless, the systematic biases in both magnitude and size remain small (<0.5 mag, or 0.2 dex), even in cases of nonsignificant detection such as J1146−0005. Additionally, our simulations reproduce the overestimation of host size observed for J0911+0152. Overall, these results validate the robustness of our image decomposition approach and confirm that our methodology yields reliable host property measurements.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: This figure illustrates how the inferred host properties in NIRCam/F356W vary with changes in the fixed Sérsic index n values, ranging from 1 to 4. Since the Sérsic index controls the central flux concentration, increasing n results in a brighter inferred host. However, the response of the inferred effective radius (Reff) to changes in n is not uniform. Generally, our results indicate a negative trend when the host is bright (mag ≲ 24.5) and compact (log Reff(″) ≲ −0.7), while a positive trend emerges when the host is faint and extended. In this work, we adopt the combined results obtained by fixing the Sérsic index to n = 1, 2, 3, and 4.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Illustration of the steps taken to identify flare footpoints for EIS analysis detailed in Section 2, using a M2.8 flare on 2024 June 3, with peak time at 12:27:00 UT. Left to right: AIA 94 Å difference image between GOES peak and start time showing the flare location, AIA 1700 Å flare footpoint image at GOES peak time, AIA 1700 Å with intensity threshold contours (blue), filtered footpoint regions >50 AIA pixels, expanded by 3 AIA pixels and reprojected 1700 Å mask to EIS WCS at 15:08:12 UT, and corresponding EIS Fe XVI 262.98 Å nonthermal velocity map with the footpoint mask overlaid (white contour).
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: Example of a simulation for a challenging case: J0844−0132. (Top) The mock image is generated by injecting the best-fit quasar, a host galaxy model, and a nearby galaxy model into a realistic JWST background, incorporating observational noise and PSF mismatch. In this realization, the recovered host magnitude differs from the input by −0.2 mag. The label “2 galaxy(s)” indicates that we applied two galaxies in the fitting, i.e., the host galaxy and the nearby galaxy. (Bottom) Same as above, but without injecting a host galaxy component. In this scenario, the host signal in the third panel is no longer present.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: Size evolution of our quasar hosts with redshift, comparing them to the rest-frame optical sizes of star-forming and quiescent galaxies at a fixed stellar mass of 5 × 1010 M⊙ at 0 < z < 10; the comparative observational measurements and evolution trends are provided by A. van der Wel et al. (2014), L. Yang et al. (2025). We also incorporate recent quasar host size measurements from the COSMOS-Web survey, as reported by T. S. Tanaka et al. (2025). The result suggests that most massive hosts (log M*/M⊙ > 10.5) have systematically smaller effective radii, approaching the compact sizes characteristic of quiescent galaxies.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Flare class distribution analyzed in this study. We categorize the flares into 5 categories, C1, C2−3, C > 4, M- and X-class.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Normalized nonthermal velocities for different Fe emission lines and He II 256.32 Å intensity (top row) plotted against flare class and spectral line. Black vertical line at t = 0 s indicates GOES flare peak time, shaded-gray vertical areas indicates GOES flare start time to peak time. Red- and blue-dashed lines indicate the nonthermal velocity primary onset time with smoothing window = 8, and precursor onset time identified mostly in M-class, respectively. Gray-varying lines above and below the black curves indicate the vnt evolution with different smoothing windows as part of our sensitivity analysis. The red- and blue-shaded areas around the dashed lines represent the standard deviation of the onset times.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Nonthermal velocity evolution for M-class flares from 12,000 s before to 12,000 s (i.e., 200 minutes) after GOES X-ray peak. Solid varying line indicates the vnt median, dotted line indicates the mean, and the shaded area indicates the 25 and 75 percentile. The vertical shaded area indicates time between GOES X-ray start to peak for this flare category (Figure 2). The faint gray-varying line above the vnt line indicates He II 256.32 Å intensity. The horizontal bar at the bottom of each subplot indicate how many vertical EIS columns or EIS time steps went into the calculation of the respective temporal bin, with yellow indicating more time steps, purple indicating fewer. Emissions from Fe XII, XIV, XV and XVI are the better sampled ions across different flare classes. Data used to create this figure and similar plots for all flare classes are available at doi:10.5281/zenodo.15613861.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: EUV nonthermal velocity onset time of the spectral lines in Figure 6 (purple to yellow squares) compared to median GOES start time (black squares). Diamond shapes at M-class indicates precursor onset times illustrated as blue lines in Figure 6. GOES peak time is at t = 0 s. Gray horizontal lines and shades indicate the He II 256.32 Å intensity onset time. The evolution of onset times show a moderate dependence in C1 and C2–3 flares, but less so in C > 4 and M-class flares.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Similar plot to Figure 4. Nonthermal velocity results for C1 flares. Solid line indicates the median, dotted line indicate the mean, and the shaded area indicates the 25 and 75 percentile. The vertical shaded area indicates the SXR start to peak time for this flare category. The horizontal bar at the bottom of each subplot indicate how vertical EIS columns went into the calculation of the respective bin.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Demonstration of the piecewise linear fit to determine nonthermal velocity onset times. Top panel shows the Fe XII 195.12 Å vnt (green line), smoothed vnt using a smoothing window = 8 (purple line). Bottom panel shows the linear fits determined through the PWLF algorithm (light green line). First breakpoint (purple dot) indicates the precursor onset, second breakpoint indicates the primary onset (green dot).
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Nonthermal velocity analysis done on a subset of flares associated with CME from J. Hernandez Camero et al. (2025) between 2011 and 2018. M-class flares associated with CME shows much earlier precursor onset time (blue line).
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: EUV nonthermal primary and precursor onset time (minutes) before GOES SXR start between flare categories and spectral line from Fe VIII to Fe XVI. Top row shows He II 256.32 Å intensity onset times. M** indicates the precursor onset time.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Example of GOES background removal algorithm illustrated in Section 2.2. The purple line indicates the original GOES flux, light green indicates the rolling background, dark green at the bottom row indicates the background removed GOES flux. This figure shows a example of M1.4 flare being reclassified to M1.3 after background removal.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Similar to Figure 11 but on C2–3 flares.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: ALMA 1.3 mm (Band 6) dust continuum around the IRAS 04125+2902 system. (a) CLEAN image with Briggs weighting (robust = 0.5). The white ellipse indicates the synthesized beam. (b) SpM image with a color scale following a linear law with a scaling exponent of 1.0. The white ellipse represents the effective spatial resolution estimated using the point-injection method. The white contours show the continuum emission at 0.03, 0.05, and 0.08 Jy arcsec−2. (c) Same as panel (b), but with the color scale given by a power law with a scaling exponent of 0.5.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: (Left) Radial intensity profile averaged over the full azimuthal angle, shown on a linear scale in the top panel and a logarithmic scale in the bottom one. The profile is linearly interpolated onto radial grid points spaced by 0.1 au using interpolate.interpld from the SciPy module. The light colored ribbon represents the error of the mean at each radius. (Right) Peak intensity profile in the azimuthal direction after their brightness distributions were deprojected using idisk and PA. The dotted violet lines show the profiles of the SpM image smoothed with the CLEAN beam by the CASA task imsmooth.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: Velocity-channel maps of 12CO J = 2–1 emission toward IRAS 04125+2902 with a velocity resolution of 0.6 km s−1. The central velocity vcent is to be 7.7 km s−1. The white cross represents the position of IRAS 04125+2902. The white contours show the 12CO J = 2–1 emission for 8.0, 16.0, and 24.0 mJy beam−1. The white ellipse in the lower left corner of each panel represents the synthesized beam of ﹩0\mathop{.}\limits^{^{\prime\prime} }155\times 0\mathop{.}\limits^{^{\prime\prime} }106﹩ (27 au×17 au) with a PA of 27﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4.
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Differential energy spectra of the all-flavor neutrino flux from a population of spiders, all RBs (red lines), half RBs and half BWs (blue lines), half RBs and half BWs with pair multiplicity k = 104 (cyan lines) in the sky region ∣l∣ ≤ 180° and ∣b∣ ≤ 5°. Solid lines are obtained by extracting ﹩{\mathrm{log}}_{10}\,\dot{E}﹩ from a Gaussian distribution with mean μ = 34.5 and variance σ = 0.5. Dashed lines are obtained by extracting ﹩{\mathrm{log}}_{10}\,\dot{E}﹩ from a uniform distribution in the interval [33, 35]. The magenta region corresponds to the superposition of the three IceCube best-fits for the galactic component with their 1σ uncertainty (R. Abbasi et al. 2023).
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Scenario 2: IBS→CS(ν) Same as in Figure 6 but for the all-flavor neutrino flux. The 90% confidence-level median sensitivities of the IceCube (blue band) (M. G. Aartsen et al. 2020), KM3Net-ARCA (orange band) (S. Aiello et al. 2019), and TRIDENT (green band) (Z. P. Ye et al. 2023) detectors, based on 10, 6, and 10 yr of data-taking, respectively, are shown assuming a power-law source spectrum with an index of 2.
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: (a) Gamma-ray flux from known RBs (red thin lines) and BWs (black thin lines), listed in Tables 2 and 3, respectively. The flux is calculated assuming a companion magnetic field fixed at Bc = 10 G. We also display the LHAASO 1 yr sensitivity threshold (blue line) and the 50 hr CTA sensitivity threshold (orange lines). (b) Same as (a) but with companion magnetic field fixed at Bc = 103 G. All the curves are calculated assuming scenario 1 with k calculated from Equation (18).
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: All-flavor neutrino flux from known RBs (red thin lines) and BWs (black thin lines). We also display the 10 yr IceCube (blue line) and KM3Net (dashed orange line) sensitivity threshold. All the curves are calculated assuming scenario 1 with k calculated from Equation (18).