adsabs/AstroCLIMB huggingface dataset:
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: The muted morning and clear evening limbs can mimic a higher metallicity and/or cooler uniform limb. Based on Equation (10) from (M. R. Line & V. Parmentier 2016), we calculated the biased metallicity and temperature as functions of their respective true values in five cases. In the limit where the morning limb is completely featureless and the evening limb is clear (f = 1/2), metallicity can be biased upward by ∼2 dex, or temperature can be biased downward by half.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: We fitted a power law function to the measured δAH error and calculated LSM values based on the nine planets in this work. Then we defined LSMempirical so it scales inversely to δAH error.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: All known transiting exoplanets (gray) to date and the 105 planets (color) with LSMempirical > 1.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Segment of a mock J1342 spectrum centered on the z = 7.443 and z = 7.476 absorbers. The blue curve shows the assumed intrinsic model of the spectrum with the two absorbers using the physical parameters from Section 2. The orange curve shows our reduction of the JWST/NIRSpec G235H spectrum first presented in C23. The black curve shows a mock 1 hr observation with ELT/MICADO at R = 20,000.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Similar to Figure 5 but assuming the absorption system properties from C23’s analysis of the J1342 NIRSpec spectrum.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Similar to Figure 3 but assuming the absorption system properties from C23’s analysis of the J1342 NIRSpec spectrum.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Comparison between our EW measurements of Mg IIλλ2796,2803 (squares) and O Iλ1302 (circles) and those from C23 for the three z > 7.3 absorption systems. The dashed curve shows the one-to-one line corresponding to equal measurements.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Similar to Figure 2 but instead using the original absorber EW measurements from C23.
Paper: Detailed Radial Scale Height Profile of Dust Grains as Probed by Dust Self-scattering in HL Tau
Authors: Haifeng Yang, 海峰 杨, Ian W. Stephens, Zhe-Yu Daniel Lin, Manuel Fernández-López, Zhi-Yun Li, Leslie W. Looney, Rachel Harrison
Figure caption: The ﹩{Q}^{{\prime} }﹩ profiles along the minor axes for the near- and farsides of the inner disk, shown as red and blue curves, respectively. The solid lines represent the data, with darker and lighter shades representing σ and 3σ errors, respectively. The dashed curves represent the models. The vertical dashed and dotted lines represent the characteristic radius of the inner disk, Rc, and the location of the first gap, respectively. From the top row to the bottom row, we present models with H/R = 0.05,  0.1,  0.15,  and 0.2. The left column shows the results from our models. The right column adds a Gaussian profile with negative values at the location of the first gap and a width corresponding to the deprojected beam size along the minor axis. This extra Gaussian component is introduced to mimic the influence of the azimuthal polarization patterns in the gap. See the main text for more details.
Paper: Detailed Radial Scale Height Profile of Dust Grains as Probed by Dust Self-scattering in HL Tau
Authors: Haifeng Yang, 海峰 杨, Ian W. Stephens, Zhe-Yu Daniel Lin, Manuel Fernández-López, Zhi-Yun Li, Leslie W. Looney, Rachel Harrison
Figure caption: Upper panels: the transformed Stokes parameters ﹩{Q}^{{\prime} }﹩ and ﹩{U}^{{\prime} }﹩. The units are mJy beam−1 for all panels. Lower panels: the masked Stokes ﹩{Q}^{{\prime} }﹩ and ﹩{U}^{{\prime} }﹩, which only show data on the rings and the inner disk. The masked ﹩{Q}^{{\prime} }﹩ is mostly positive and larger than ﹩{U}^{{\prime} }﹩ in the masked regions. The polarization orientation is mostly uniform along the minor axis of the disk, coming from inclination-induced polarization. This is the target of the modeling in this work.
Paper: Detailed Radial Scale Height Profile of Dust Grains as Probed by Dust Self-scattering in HL Tau
Authors: Haifeng Yang, 海峰 杨, Ian W. Stephens, Zhe-Yu Daniel Lin, Manuel Fernández-López, Zhi-Yun Li, Leslie W. Looney, Rachel Harrison
Figure caption: Visualization of how inclination-induced polarization and radiation-anisotropy-induced polarization contribute jointly to the observed polarization pattern.
Paper: Spectral Hardening Reveals Afterglow Emergence in Long-duration Fast X-Ray Transients: A Case Study of GRB 250404A/EP250404a
Authors: Yi-Han Iris Yin, Yuan Fang, Bin-Bin Zhang, Chen Deng, Jun Yang, Run-Chao Chen, Yuan Liu, Yehao Cheng, Dong Xu, Xiaofeng Wang, Rongfeng Shen, Rui-Zhi Li, Jirong Mao, Wen-Xiong Li, Alberto Javier Castro-Tirado, Weihua Lei, Shao-Yu Fu, Yuan-Pei Yang, Shuai-Qing Jiang, Jie An, Chun Chen, Zhong-Nan Dong, Guowang Du, Ali Esamdin, Zhou Fan, Haicheng Feng, Lu Feng, Emilio Fernández-García, Xing Gao, Maria Gritsevich, Wei-Jian Guo, Jingwei Hu, You-Dong Hu, Yanlong Hua, Abdusamatjan Iskandar, Junjie Jin, Niu Li, Xia Li, Ziwei Li, Jia-Qi Lin, Dezi Liu, Jinzhong Liu, Qichun Liu, Xiaowei Liu, Xing Liu, Daniele B. Malesani, Ignacio Pérez-García, Hui Sun, Xue-Feng Wu, Yun-Ao Xiao, Ding-Rong Xiong, Shengyu Yan, Beibei Zhang, Jinghua Zhang, Haichang Zhu, Zipei Zhu, Hu Zou, Weimin Yuan, Bing Zhang
Figure caption: The optical spectrum observed by the GMG-2.4 m telescope. The wavelength-calibrated 2D spectrum and the corresponding flux-calibrated 1D spectrum are shown. The 1D raw, smoothed, and error spectra are shown in sky blue, red, and gray lines, respectively. Multiple metal absorption lines at a redshift of z = 1.88 are marked with vertical dashed lines. Note that the flux calibration should be treated with caution due to the absence of a standard star observation on the same night. Instead, a previously obtained standard star spectrum was used for the flux calibration.
Paper: Spectral Hardening Reveals Afterglow Emergence in Long-duration Fast X-Ray Transients: A Case Study of GRB 250404A/EP250404a
Authors: Yi-Han Iris Yin, Yuan Fang, Bin-Bin Zhang, Chen Deng, Jun Yang, Run-Chao Chen, Yuan Liu, Yehao Cheng, Dong Xu, Xiaofeng Wang, Rongfeng Shen, Rui-Zhi Li, Jirong Mao, Wen-Xiong Li, Alberto Javier Castro-Tirado, Weihua Lei, Shao-Yu Fu, Yuan-Pei Yang, Shuai-Qing Jiang, Jie An, Chun Chen, Zhong-Nan Dong, Guowang Du, Ali Esamdin, Zhou Fan, Haicheng Feng, Lu Feng, Emilio Fernández-García, Xing Gao, Maria Gritsevich, Wei-Jian Guo, Jingwei Hu, You-Dong Hu, Yanlong Hua, Abdusamatjan Iskandar, Junjie Jin, Niu Li, Xia Li, Ziwei Li, Jia-Qi Lin, Dezi Liu, Jinzhong Liu, Qichun Liu, Xiaowei Liu, Xing Liu, Daniele B. Malesani, Ignacio Pérez-García, Hui Sun, Xue-Feng Wu, Yun-Ao Xiao, Ding-Rong Xiong, Shengyu Yan, Beibei Zhang, Jinghua Zhang, Haichang Zhu, Zipei Zhu, Hu Zou, Weimin Yuan, Bing Zhang
Figure caption: The spectral index evolutions and light curves for four scenarios of the transition from the prompt emission to the afterglow in the long-duration fast X-ray transients. The purple, blue, and yellow dots represent the spectral indices of the total, prompt, and afterglow emission spectra. The colored curves demonstrate the flux evolution in linear and logarithmic scale. From top to bottom: case I, case II, case III, and case IV.
Paper: Spectral Hardening Reveals Afterglow Emergence in Long-duration Fast X-Ray Transients: A Case Study of GRB 250404A/EP250404a
Authors: Yi-Han Iris Yin, Yuan Fang, Bin-Bin Zhang, Chen Deng, Jun Yang, Run-Chao Chen, Yuan Liu, Yehao Cheng, Dong Xu, Xiaofeng Wang, Rongfeng Shen, Rui-Zhi Li, Jirong Mao, Wen-Xiong Li, Alberto Javier Castro-Tirado, Weihua Lei, Shao-Yu Fu, Yuan-Pei Yang, Shuai-Qing Jiang, Jie An, Chun Chen, Zhong-Nan Dong, Guowang Du, Ali Esamdin, Zhou Fan, Haicheng Feng, Lu Feng, Emilio Fernández-García, Xing Gao, Maria Gritsevich, Wei-Jian Guo, Jingwei Hu, You-Dong Hu, Yanlong Hua, Abdusamatjan Iskandar, Junjie Jin, Niu Li, Xia Li, Ziwei Li, Jia-Qi Lin, Dezi Liu, Jinzhong Liu, Qichun Liu, Xiaowei Liu, Xing Liu, Daniele B. Malesani, Ignacio Pérez-García, Hui Sun, Xue-Feng Wu, Yun-Ao Xiao, Ding-Rong Xiong, Shengyu Yan, Beibei Zhang, Jinghua Zhang, Haichang Zhu, Zipei Zhu, Hu Zou, Weimin Yuan, Bing Zhang
Figure caption: Corner plot of the posterior probability distributions of the parameters for afterglow fitting using the FS+RS model with u-, v-, and g-band correction factors. The red error bars represent 1σ uncertainties.
Paper: Evidence of a Fraction of LIGO/Virgo/KAGRA Events Coming from Active Galactic Nuclei
Authors: Liang-Gui Zhu, 良贵 朱, Xian Chen, 弦 陈
Figure caption: AGN density distributions and completeness analysis. Top left: on-sky surface density distribution of SDSS AGNs, showing cumulative area vs. density. The sky area element for statistics is ΔΩ ≈ 1.56 deg2. Bottom left: redshift-dependent spatial density of AGNs in low- (dotted line), high- (dashed line), and extreme high-density (solid line) regions. Right panels: survey-depth completeness (ci/fcover,i) vs. localization error volume (ΔVc) for candidate AGN hosts of individual GW events, color-coded by AGN subcatalogs: black represents the full AGN catalog; cyan, blue, and red, respectively, represent the lower, moderate, and higher Lbol subcatalogs (top); and corresponding λEdd divisions (bottom).
Paper: Evidence of a Fraction of LIGO/Virgo/KAGRA Events Coming from Active Galactic Nuclei
Authors: Liang-Gui Zhu, 良贵 朱, Xian Chen, 弦 陈
Figure caption: Comparison between real and mock constraints on fagn based on all O1–O4a GW events. Top panels: constraints using the lower Lbol subcatalog with injected values ﹩{f}_{{\rm{agn}}}^{{\rm{inj}}}=0﹩ and ﹩{f}_{{\rm{agn}}}^{{\rm{inj}}}=0.4﹩, respectively. Bottom panels: constraints using the lower λEdd subcatalog with injected values ﹩{f}_{{\rm{agn}}}^{{\rm{inj}}}=0﹩ and ﹩{f}_{{\rm{agn}}}^{{\rm{inj}}}=0.3﹩. In each panel, the cyan solid lines correspond to the result derived from real observation, while the gray curves correspond to mock simulation. The black dashed curve denotes the median of the simulated results, and the gray shaded areas indicate the 50% and 90% distribution intervals.
Paper: Evidence of a Fraction of LIGO/Virgo/KAGRA Events Coming from Active Galactic Nuclei
Authors: Liang-Gui Zhu, 良贵 朱, Xian Chen, 弦 陈
Figure caption: Skymaps of three precisely localized O4 GW candidates and scatter plots of their neighboring AGNs. The two white contours in each panel represent the 50% and 90% CLs of the skymap. The blue/gray stars represent the AGNs inside/outside the localization error volume of 90% CL.
Paper: Evidence of a Fraction of LIGO/Virgo/KAGRA Events Coming from Active Galactic Nuclei
Authors: Liang-Gui Zhu, 良贵 朱, Xian Chen, 弦 陈
Figure caption: Probability distributions of fagn derived from O1 to O4a (top) and O1 to O3 (bottom) after excluding the four best localized LVK events. The line styles are the same as in Figure 3. The vertical dotted lines show the upper limits of fagn according to the 90% CL.
Paper: Evidence of a Fraction of LIGO/Virgo/KAGRA Events Coming from Active Galactic Nuclei
Authors: Liang-Gui Zhu, 良贵 朱, Xian Chen, 弦 陈
Figure caption: Probability distributions of fagn derived for all O1–O4a GW events. Different curves correspond to lower (cyan), moderate (blue), and higher (red) Lbol (left panel) or λEdd (right) subcatalogs. Results for the full catalog are shown with black curves. Vertical dotted lines mark the 90% CL upper limits.
Paper: Evidence of a Fraction of LIGO/Virgo/KAGRA Events Coming from Active Galactic Nuclei
Authors: Liang-Gui Zhu, 良贵 朱, Xian Chen, 弦 陈
Figure caption: Distributions of AGNs in the Lbol–λEdd plane. The two white contours represent the 50% and 90% CLs of the AGN distribution. The cyan, blue, and red regions (dots) correspond to the lower, moderate, and higher Lbol (λEdd) AGN subcatalogs, respectively.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: Distribution of special star associations in the x–y and l–b spaces, with different colors indicating member stars of different star associations. Arrows indicate the peculiar velocities (hollow arrows) and velocities in the LCF (solid arrows) of the star associations. The orange circle represents the Sun, and the white arrow points toward the direction of the Galactic center. The background of the left figure is the x–y plane of the 3D (x, y, z) dust image in the solar neighborhood and the background of the right figure is the l–b plane of the 3D (l, b, d) interstellar dust spatial distribution map drawn by G. Edenhofer et al. (2024).
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: An illustration of our hypothesis that different subassociations within the star associations have been affected by multiple SN explosions. The hexagonal points in different colors represent the various star associations, the gray and black stars denote two SN explosions, and the dashed lines indicate the reduction in molecular cloud velocity after SN explosions and the process of star association formation affected by the SN explosions.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: Histogram of the LSR radial velocities of the star association member stars calculated using parameter ﹩{U}_{\odot }^{{\rm{std}}}=10.0﹩ km s−1, ﹩{V}_{\odot }^{{\rm{std}}}=15.4﹩ km s−1, and ﹩{W}_{\odot }^{{\rm{std}}}=7.8﹩ km s−1 (F. J. Kerr & D. Lynden-Bell 1986), with the vertical line (with a dot at the top) indicating the LSR radial velocity of the star association obtained through KDE fitting.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: This figure illustrates the assumptions we made during the estimation of the energy released by combined massive star action (including SN explosions). The dashed circles represent the combined massive star action. We infer that the second SN explosion should have occurred between the blue dashed circle and the Bubble-edge.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: The spatial distribution of the member stars of the parent association and the subassociations, as well as the PMS stars in the region defined by −90° < l < 30°, −60° < b < 60°, and 80 pc < d < 220 pc.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: This figure illustrates the process of velocity transformation in different reference frames for these unique star associations, including the dynamical LSR frame, local corotating frame (LCF), and peculiar velocities.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Phase portraits for ψ⋆0 = 70° at ϵ⋆d = 0.5 (a), 0.9 (b), 2.0 (c), and 3.0 (d). Portraits are plotted in the (Δh, ψ⋆0 − ψ1⋆) plane, where Δh denotes the difference between the longitudes of the planet’s orbit and the disk, and ψ⋆0 − ψ1⋆ denotes the angle between l1 and ﹩{\hat{{\boldsymbol{l}}}}_{{\rm{d}}}﹩. In each panel, equilibria are marked by colored points. Note due to the symmetry, if (Δh, ψ⋆0 − ψ1⋆) is an equilibrium, (Δh − π,  π − ψ⋆0 + ψ1⋆) is also an equilibrium. Trajectories passing through saddle points (bold curves) partition the phase space into distinct libration zones. Red curves show the numerical solution for a fiducial one-planet system at the specified ϵ⋆d, by using the secular model based on Laplace–Lagrange theory (Appendix A). The fiducial system parameters are m⋆ = 1 M⊙, R⋆ = 1.5 R⊙, P⋆ = 5 days, m1 = 5 M⊕, a1 = 0.05 au, mdk0 = 0.02 M⊙, rin = 0.03 au, rc = 2 au, rout = 50 au, τv,in = 1 × 104 yr, and ψ⋆0 = 70°. (Definitions of these parameters can be found in Appendix A)
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Coplanar equilibrium solutions as a function of ϵ⋆d for ψ⋆0 = 35°, ﹩44\mathop{.}\limits^{^\circ }6﹩, and 75° (top to bottom panels, respectively), derived from Equation (10). The vertical dashed lines in the bottom panel denote bifurcation points B1 and B2: at B1, new equilibria P4 and P5 emerge, while at B2, equilibria P3 and P4 merge and annihilate.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Bifurcation curves presented in the (ψ⋆0, ϵ⋆d) parameter space by using the bifurcation condition (Equation (11)). The curves for B1 and B2 are distinguished by different colors. The critical primordial obliquity for triggering the bifurcation is indicated.
Paper: Delayed Launch of Ultrafast Outflows in the Tidal Disruption Event AT2020afhd
Authors: Zikun Lin, Yanan Wang, De-Fu Bu, Junjie Mao, Jifeng Liu
Figure caption: The long-term unabsorbed X-ray (0.3–2 keV) light curve of AT2020afhd, starting from the discovery date (MJD 60310). Gray circles, squares, and stars represent observations from NICER, Swift, and XMM-Newton/PN, respectively. Data points in red indicate observations where an absorption feature was detected in the spectrum. The orange, green, blue, and purple shaded regions correspond to the four epochs used to combine the Swift spectra, as described in Section 3.
Paper: Delayed Launch of Ultrafast Outflows in the Tidal Disruption Event AT2020afhd
Authors: Zikun Lin, Yanan Wang, De-Fu Bu, Junjie Mao, Jifeng Liu
Figure caption: The continuum residuals of the selected NICER (top five panels) and XMM-Newton/PN (bottom three panels) spectrum. Red curves indicate detections of absorption lines. For comparison, two additional XMM-Newton/PN observations without detected absorption features are shown in gray. The dashed line marks the absorption feature at 0.95 keV.
Paper: Puzzling Variation of Gamma Rays from the Sun over the Solar Cycle Revealed with Fermi-LAT
Authors: A. Acharyya, A. Adelfio, M. Ajello, L. Baldini, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, S. Buson, R. A. Cameron, P. A. Caraveo, F. Casaburo, F. Casini, E. Cavazzuti, D. Cerasole, N. Cibrario, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, F. Cuna, A. Cuoco, S. Cutini, F. D'Ammando, D. Depalo, S. W. Digel, N. Di Lalla, L. Di Venere, A. Domínguez, A. Fiori, Y. Fukazawa, P. Fusco, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, M. Giliberti, F. Giordano, M. Giroletti, S. Guiriec, R. Gupta, M. Hashizume, E. Hays, J. W. Hewitt, A. Holzmann Airasca, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, A. Laviron, J. Li, A. Liguori, I. Liodakis, P. Loizzo, F. Longo, F. Loparco, S. López Pérez, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, R. Martinelli, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Michailidis, P. F. Michelson, N. Mirabal, T. Mizuno, P. Monti-Guarnieri, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, A. Reimer, O. Reimer, M. Sánchez-Conde, P. M. Saz Parkinson, D. Serini, C. Sgrò, E. J. Siskind, P. Spinelli, D. Tak, L. Tibaldo, D. F. Torres, J. Valverde, Z. Wadiasingh, W. Zhang
Figure caption: Panel (a): percentage of the flux variation of the solar disk component above 25 MeV, 500 MeV, and 1 GeV vs. time in years. For normalization, the average flux values used are 9.15, 4.69, and 2.23 (× 10−8 cm−2 s−1), respectively. The gray regions define systematic uncertainties. Panel (b): flux variation in time of the solar disk component above 1 GeV compared with the SSN. Panel (c): flux variation in time of the solar disk component above 1 GeV compared with the CR proton flux at 2.14–2.4 GV (M. Aguilar et al. 2021). Panel (d): flux variation in time of the solar disk component above 1 GeV compared with the Moon’s flux above 56 MeV (M. Ackermann et al. 2016).