adsabs/AstroCLIMB huggingface dataset:
Paper: Predicting the Energy Spectra of Solar Energetic Particles with a Machine Learning Regression Algorithm
Authors: Jiajun Liu, Zhendi Huang, Jingnan Guo, Yubao Wang, Jiajia Liu
Figure caption: Left: correlation heat map of all events used in this study between the peak flux of each of the 11 energy channels and various event-associated parameters including the first seven rows—solar wind speed at 1 au (V sw), longitude of solar flare (﹩{\mathrm{Lon}}_{\mathrm{flare}}﹩), latitude of solar flare (﹩{\mathrm{Lat}}_{\mathrm{flare}}﹩), width of CME (W cme), speed of CME (V cme), and peak and integral flux of the flare soft X-ray (﹩{F}_{{\mathrm{SXR}}_{\mathrm{peak}}}﹩ and ﹩{F}_{{\mathrm{SXR}}_{\mathrm{int}}}﹩). Right: correlation heat map between the integral fluence of each energy channel and the same event features as shown in the left panel. The labels f1 to f11 denote the SEP flux for 11 different energy channels (5.00–7.23, 7.23–10.46, 10.46–15.12, 15.12–21.87, 21.87–31.62, 31.62–45.73, 45.73–66.13, 66.13–95.64, 95.64–138.3, 138.3–200.0, and 200.0–289.2 MeV).
Paper: The Discovery of Polarized Water Vapor Megamaser Emission in a Molecular Accretion Disk
Authors: Jack F. Gallimore, C. M. Violette Impellizzeri, Samaneh Aghelpasand, Feng Gao, Virginia Hostetter, Boy Lankhaar
Figure caption: An overlay of H2O maser spot positions and the 21.9 GHz continuum image of the radio component S1 of NGC 1068. Coordinate offsets are relative to R.A. (J2000) = 02h42m40.ˢ70907, decl. (J2000) = −00°00′47.″9444. Maser spots are plotted as filled circles color coded to the recessional velocity relative to V (LSRK) = 1130 km s−1. The size of the maser spots scales with the square root of the integrated flux density (i.e., larger circles are brighter maser spots). The brightest maser groups (R1, R2, etc.) are labeled using the naming convention of GI23. The radio continuum is plotted as filled contours. The contour levels are −34 (dashed), 34, 57, 97, 164, and 276 μJy beam−1. The equivalent brightness temperatures are (−0.11, 0.11, 0.18, 0.31, 0.53, 0.88) × 106 K. The peak surface brightness is 451.5 ± 0.1 μJy beam−1, equivalent to brightness temperature (1.45 ± 0.05) × 106 K. The locations of the central compact continuum source, NGC 1068*, and the northern continuum plume, S1-North, are annotated. The continuum restoring beam (FWHM) is the magenta ellipse at the lower right.
Paper: The Discovery of Polarized Water Vapor Megamaser Emission in a Molecular Accretion Disk
Authors: Jack F. Gallimore, C. M. Violette Impellizzeri, Samaneh Aghelpasand, Feng Gao, Virginia Hostetter, Boy Lankhaar
Figure caption: Linear polarization map of the H2O megamasers of NGC 1068. The maser spots are plotted as in Figure 1, except the spots are now plotted with uniform size. Electric polarization vectors are plotted as cyan lines centered at the position of the peak in the linear polarization maps. The line lengths are proportional to the fractional linear polarization; a 5% linear polarization scale bar is provided at the upper left. Polarization vectors are plotted only for those maser spots where the linear polarization fraction is greater than 5σ. The best-fit disk kinematic PA (GI23), an approximation to the major axis of the edge-on disk, is plotted as a black dashed line. The plot has been modified to help the reader follow the geometry.
Paper: The Discovery of Polarized Water Vapor Megamaser Emission in a Molecular Accretion Disk
Authors: Jack F. Gallimore, C. M. Violette Impellizzeri, Samaneh Aghelpasand, Feng Gao, Virginia Hostetter, Boy Lankhaar
Figure caption: Restored and naturally weighted Stokes I, Q, and U images of the five brightest H2O maser sources in NGC 1068. The rightmost column shows images of the linearly polarized flux density. Each row is a different spectral channel with recessional velocity, V (LSRK), labeled in the first column. All images are 10 mas and centered on the brightest maser in that channel. The images are displayed with a positive linear stretch in the viridis (blue–green–yellow–white) color map. The display stretches are Stokes I, (−1, 300) mJy beam−1; Stokes Q and U, (−3, 3) mJy beam−1; and polarized flux, (0, 4) mJy beam−1. The synthetic beam size (FWHM) is 1.34 × 0.52 mas, PA 4.°2.
Paper: The Cosmological Optical Convergence: Extragalactic Background Light from TeV Gamma Rays
Authors: Lucas Gréaux, Jonathan Biteau, Mireia Nievas Rosillo
Figure caption: EBL intensity at z = 0 as a function of wavelength. Indirect γ-ray measurements from this work are shown as red circles. IGL measurements from S. P. Driver et al. (2016) and S. Koushan et al. (2021) are shown as upward-pointing triangles, as labeled in the figure. The direct measurement from M. Postman et al. (2024) in the optical band is shown as downward-pointing triangle. The EBL models from R. C. Gilmore et al. (2012), S. K. Andrews et al. (2017b), and A. Saldana-Lopez et al. (2021) are shown as dashed–dotted, solid, and dashed lines, respectively. These data sets are collected in J. Biteau (2023).
Paper: The Cosmological Optical Convergence: Extragalactic Background Light from TeV Gamma Rays
Authors: Lucas Gréaux, Jonathan Biteau, Mireia Nievas Rosillo
Figure caption: Residual EBL intensity at z = 0 as a function of wavelength with respect to the IGL measurements from S. P. Driver et al. (2016) and S. Koushan et al. (2021). Results derived in this work are shown with circles for each wavelength bin. The horizontal band is the result of a constant fit to the residuals over the full wavelength range. The measurements from T. R. Lauer et al. (2022) and M. Postman et al. (2024) are shown with downward-pointing triangles, as labeled in the figure.
Paper: Direct Observations of a Shock Traversing Preceding Two Coronal Mass Ejections: Insights from Solar Orbiter, Wind, and STEREO Observations
Authors: Yutian Chi, Chenglong Shen, Zhiyong Zhang, Mengjiao Xu, Dongwei Mao, Junyan Liu, Can Wang, Bingkun Yu, Jingyu Luo, Zhihui Zhong, Yuming Wang
Figure caption: Panel (a): the positions of three separated spacecraft (Wind, Solar Orbiter, and STEREO-A) at 00:00 UT on 2023 November 28, in the inner heliosphere. The purple, green, and yellow arrows represent the reconstructed propagation direction of the three CMEs from the GCS model, respectively. The circles represent the half angular width of the CMEs derived from the GCS model. Panels (b)–(d): solar wind plasma and magnetic field parameters detected at Solar Orbiter, Wind, and STEREO-A spacecraft. From top to bottom, the panels show the magnetic field strength, the r, t, and n magnetic field components in RTN coordinate, the elevation θ and azimuth ϕ of field direction in RTN coordinate, bulk speed, proton density, proton temperature, proton β, total pressure (only in panel (c)), and Dst index (only in panel (c)), respectively. The purple, green, and yellow shade regions show the intervals of ICME-1, ICME-2, and ICME-3, respectively. The purple vertical line indicates the arrival time of shock-1, which is associated with ICME-1. The yellow dashed vertical line indicates the arrival time of shock-3, which is associated with ICME-3.
Paper: Direct Observations of a Shock Traversing Preceding Two Coronal Mass Ejections: Insights from Solar Orbiter, Wind, and STEREO Observations
Authors: Yutian Chi, Chenglong Shen, Zhiyong Zhang, Mengjiao Xu, Dongwei Mao, Junyan Liu, Can Wang, Bingkun Yu, Jingyu Luo, Zhihui Zhong, Yuming Wang
Figure caption: Panel (a) the full-Sun images at Hα line center (6562.8 Å) from CHASE spectroscopic observations at 23:49:15 UT on 2023 November 27. Panel (b) eruption of CME-2 in the inner corona detected by Lyα Solar Telescope (LST) on board the ASO-S. Panel (c) full-Sun images at Hα line center (6562.8 Å) from CHASE spectroscopic observations at 20:42:03 UT on 2023 November 28. Panel (d) STEREO-A radio dynamic spectrum associated with the interaction between CME-1 and CME-2. Panels (e)–(h) the running difference images of the three CMEs detected by STEREO-A/SECCHI and SOHO/LASCO on 2023 November 28. Panels (i)–(l) are the best-fitting results for the three CMEs. The purple, green, and yellow meshes display the results of the GCS fitting for CME-1, CME-2, and CME-3, respectively. Panel (m) shows the time-elongation map derived from the COR2, HI1, and HI2 cameras on board STEREO-A. The purple, green, and yellow arrows indicate the tracks of CME-1, CME-2, and CME-3, respectively. The black arrows show the potential interaction region based on the merged track.
Paper: Direct Observations of a Shock Traversing Preceding Two Coronal Mass Ejections: Insights from Solar Orbiter, Wind, and STEREO Observations
Authors: Yutian Chi, Chenglong Shen, Zhiyong Zhang, Mengjiao Xu, Dongwei Mao, Junyan Liu, Can Wang, Bingkun Yu, Jingyu Luo, Zhihui Zhong, Yuming Wang
Figure caption: In situ observations for ICME-1 (left panels), flux rope (middle panels), and ICME-2 (right panels). From top to bottom, the panels display the magnetic field strength, the r, t, and n magnetic field components in RTN coordinate, the elevation θ, and the azimuth ϕ of field direction in RTN coordinate. The black, red, and blue lines in the field data panels correspond to the observations from Wind, STEREO-A, and Solar Orbiter, respectively. The STEREO-A and Solar Orbiter observations are time-shifted to align with the start times of the structures. The black, red, and blue vertical dotted–dashed lines indicate the end time of the ICMEs detected by Wind, STEREO-A, and Solar Orbiter, respectively. The observations from Solar Orbiter in panel (c) are scaled to match the interval of ICME-2 detected at WIND.
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: Location of the X-ray shell. (a) ROSAT PSPC X-ray image (see Appendix A) of the nebula W50 overlapped by the intensity contour of the 1.4 GHz VLA observation (G. M. Dubner et al. 1998). (b) Zoom-in dual-band XMM-Newton image in the region marked in yellow in 0.4–1.2 keV (red) and 2.0–5.0 keV (cyan) with pointlike sources subtracted. Each bin shares an average signal-to-noise ratio of 10. The softer and harder energy bands highlight the thermal and nonthermal emission of the nebula, respectively. The green region labels the shell-like structure.
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: Evolution of a bubble powered by isotropic disk winds with a power of 3 × 1037 erg s−1 within a uniform medium and a dense cloud in the north. From top to bottom, the rows show the evolution of the density, temperature, and X-ray surface brightness in 0.4–2.5 keV. The bottom panels give the surface brightness evolution for the case where the cloud is rotated 41.°4 toward us (so that it is projected 30 pc north of SS 433). From left to right, the age of the wind bubble is 20, 95, and 150 kyr, respectively, corresponding to the age of the SNR, the beginning of the collision with the dense cloud, and the later evolution of the wind bubble.
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: Zoom-in multiband images of our region of interest. (a) XMM-Newton EPIC 0.4–1.2 keV mosaic in units of counts deg−2 s−1. Each bin has a signal-to-noise ratio of ∼10. The X-ray shell and clump are labeled in white and cyan, respectively. The green solid and dashed lines mark the jet axis and cone of the jet precession and nod, respectively (S. Fabrika 2004). (b) VLA 1.4 GHz intensity map in units of mJy beam−1 (G. M. Dubner et al. 1998). (c) Sino-German 6 cm polarized fraction map in units of percentage (X. Y. Gao et al. 2011). (d) Arecibo H I intensity in 68–75 km s−1 in units of K (J. E. G. Peek et al. 2018; Y. Su et al. 2018).
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: Left panel: mass “budget” of the compact object. The blue solid line represents the mass of the He core (T. Sukhbold et al. 2016). Yellow diamonds and green triangles correspond to models with a given explosion energy (W. Zhang et al. 2008). Gray upper limits label the maximum compact remnant mass among different explosion parameters with a given progenitor mass (C. L. Fryer et al. 2018). The other scatter points are adopted from four different central engines (T. Sukhbold et al. 2016), and only cases with a compact object mass over 2 M ⊙ are shown here. Right panel: mass of black holes with successful SN explosion as a function of the explosion energy. Blue stars are given by T. Sukhbold et al. (2016), while orange triangles (20 M ⊙) and green diamonds (25 M ⊙) are from C. L. Fryer et al. (2018). Only cases where the black hole mass exceeds 2 M ⊙ are reserved.
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: Spectra with folded models of the regions Shell (left column) and Clump (right column). From top to bottom are the null hypothesis and the vnei, vpshock, vapec, and vapec* models. Different components of the MOS2 spectra are labeled with dashed lines. The null hypothesis spectra mark the astrophysical background from the local hot bubble, galactic halo, and background in yellow, cyan, and blue, respectively. For the others, the astrophysical background is labeled in yellow, while the extra thermal component is marked in cyan. Gray lines represent the Al K fluorescence lines of the instrument background.
Paper: Predicting the Energy Spectra of Solar Energetic Particles with a Machine Learning Regression Algorithm
Authors: Jiajun Liu, Zhendi Huang, Jingnan Guo, Yubao Wang, Jiajia Liu
Figure caption: (a) A diagram of the cost-complexity pruning (CCP) algorithm. x 1 and x 2 are the features, while θ 1 and θ 2 are the thresholds. value1 to value4 represent the decisions at each terminal node. (b) Model framework. ﹩\hat{f}({E}_{i})﹩ represents the predicted flux of SEP in the ith energy channel, where i ranges from 2 to 10. ﹩{\hat{f}}_{\mathrm{peak}}(E)﹩ and ﹩{\hat{f}}_{\mathrm{int}}(E)﹩ represent the predicted peak flux and integral fluence of SEP across all energy channels.
Paper: Predicting the Energy Spectra of Solar Energetic Particles with a Machine Learning Regression Algorithm
Authors: Jiajun Liu, Zhendi Huang, Jingnan Guo, Yubao Wang, Jiajia Liu
Figure caption: Comparison between actual energy spectra and predictions for an SEP event (from the SEPEM data set, Section 2), which occurred on 2005 September 13 (top panels) and a the recent GLE event (outside the data set), which occurred on 2024 May 13 (bottom panels). The error bar in energy represents the measured (or calibrated or predicted) energy range of each channel. More details can be found in the text.
Paper: Predicting the Energy Spectra of Solar Energetic Particles with a Machine Learning Regression Algorithm
Authors: Jiajun Liu, Zhendi Huang, Jingnan Guo, Yubao Wang, Jiajia Liu
Figure caption: Correlation between the model predictions and observations for proton peak flux and integral fluence in different energy ranges. (a) and (b) show the peak flux for 5–7.23 MeV and 7.23–10.46 MeV, respectively; (c) and (d) show the integral fluence for 5–7.23 MeV and 7.23–10.46 MeV, respectively. The yellow shaded area in the testing set represents the 95% confidence interval.
Paper: No Thick Atmosphere on the Terrestrial Exoplanet Gl 486b
Authors: Megan Weiner Mansfield, Qiao Xue, Michael Zhang, Alexandra S. Mahajan, Jegug Ih, Daniel Koll, Jacob L. Bean, Brandon Park Coy, Jason D. Eastman, Eliza M.-R. Kempton, Edwin S. Kite
Figure caption: Contour plot showing the planetary dayside temperature of Gl 486b as a function of Bond albedo (A B) and heat-redistribution factor (ε). Note that T s, a/R s, and R p/R s are identical. They are drawn from each sample in the EXOFASTv2 MCMC fitting. The solid line shows a contour of the median planetary temperature inferred for Gl 486b, and the surrounding dotted lines show 1σ, 2σ, and 3σ intervals. The yellow arrow on the color bar shows the maximum dayside temperature predicted for Gl 486b if it had zero Bond albedo and no heat redistribution. Gray, light blue, red, green, and orange dots show approximate values for the solar system bodies Moon, Mercury, Mars, Earth, and Venus, respectively. Our observations of Gl 486b are most consistent with airless bodies like the Moon and Mercury that have slight nonzero albedos, and they are highly inconsistent with a thick Earth-like or Venus-like atmosphere.
Paper: No Thick Atmosphere on the Terrestrial Exoplanet Gl 486b
Authors: Megan Weiner Mansfield, Qiao Xue, Michael Zhang, Alexandra S. Mahajan, Jegug Ih, Daniel Koll, Jacob L. Bean, Brandon Park Coy, Jason D. Eastman, Eliza M.-R. Kempton, Edwin S. Kite
Figure caption: The cosmic shoreline (dashed blue line; K. J. Zahnle & D. C. Catling 2017), compared to select rocky bodies in the solar system (blue) and in M Dwarf systems (black, orange). The plotted cosmic shoreline is a relationship between escape velocity and normalized cumulative XUV irradiation that is empirically observed in the solar system. For exoplanets, crosses indicate planets whose observations rule out thick atmospheres and are consistent with no atmosphere. For solar system bodies, crosses, open circles, and filled circles indicate bodies with no atmosphere, thin (P < 1 bar) atmospheres, and thick (P ≥ 1 bar) atmospheres, respectively. Gl 486b is the second closest exoplanet to the shoreline probed for an atmosphere so far, after TRAPPIST-1c.
Paper: No Thick Atmosphere on the Terrestrial Exoplanet Gl 486b
Authors: Megan Weiner Mansfield, Qiao Xue, Michael Zhang, Alexandra S. Mahajan, Jegug Ih, Daniel Koll, Jacob L. Bean, Brandon Park Coy, Jason D. Eastman, Eliza M.-R. Kempton, Edwin S. Kite
Figure caption: Comparison of the eclipse spectrum of Gl 486b (black points) with a variety of atmosphere and bare rock forward models. Top and middle panels show all bare rock and atmosphere models that have a reduced χ 2 of ≤1.5, respectively, assuming the number of degrees of freedom equals the number of data points. The bottom panel shows a selection of bare rock and atmosphere models that give worse fits to the data. The only atmospheres as consistent with our data as the bare rock models have relatively low surface pressures and/or small concentrations of the infrared absorbers H2O and CO2.
Paper: No Thick Atmosphere on the Terrestrial Exoplanet Gl 486b
Authors: Megan Weiner Mansfield, Qiao Xue, Michael Zhang, Alexandra S. Mahajan, Jegug Ih, Daniel Koll, Jacob L. Bean, Brandon Park Coy, Jason D. Eastman, Eliza M.-R. Kempton, Edwin S. Kite
Figure caption: MIRI/LRS eclipse spectra of Gl 486b from the reductions with SPARTA (black) and Eureka! (red). Thin points show results from the two individual eclipses, and thick points show weighted averages of both eclipses combined. The two data reductions are offset slightly in wavelength for clarity. Both independent reductions of both eclipses are in good agreement with each other.
Paper: No Thick Atmosphere on the Terrestrial Exoplanet Gl 486b
Authors: Megan Weiner Mansfield, Qiao Xue, Michael Zhang, Alexandra S. Mahajan, Jegug Ih, Daniel Koll, Jacob L. Bean, Brandon Park Coy, Jason D. Eastman, Eliza M.-R. Kempton, Edwin S. Kite
Figure caption: Pairs plot for the best-fit parameters from the joint stellar and planetary fit described in Section 2.3, as well as the derived temperature ratio (﹩{ \mathcal R }﹩) described in Section 3. Black and blue plots show results using a PHOENIX (F. Allard et al. 2012) and SPHINX (A. R. Iyer et al. 2023) stellar model, respectively. Off-diagonal plots show 2D posterior probabilities for pairs of parameters, with dark, medium, and light shading showing 1σ, 2σ, and 3σ confidence intervals. On-diagonal plots show marginalized posterior probability distributions for each individual parameter.
Paper: No Thick Atmosphere on the Terrestrial Exoplanet Gl 486b
Authors: Megan Weiner Mansfield, Qiao Xue, Michael Zhang, Alexandra S. Mahajan, Jegug Ih, Daniel Koll, Jacob L. Bean, Brandon Park Coy, Jason D. Eastman, Eliza M.-R. Kempton, Edwin S. Kite
Figure caption: White light curves for both the SPARTA (black) and Eureka! (red) reductions of observations of Gl 486b. The dashed gray line shows the best-fit eclipse depth from the SPARTA reduction.
Paper: On the Contribution of Unresolved Pulsars to the Ultra-high-energy Galactic Diffuse Gamma-Ray Emission
Authors: Samy Kaci, Gwenael Giacinti, Dmitri Semikoz
Figure caption: Summary of the source-generation procedure. Panel (a) shows the ATNF pulsars with age from 0 to 10 Myr in the region (between the two dashed lines) used to extract their statistical properties. Panel (b) shows the ATNF and the synthetic pulsars generated with the same statistical properties and the field of view of LHAASO starting from the orange dashed line and ending at the red dashed line (counterclockwise). Histogram (panel (c)) shows the age distribution of the ATNF pulsars in the sampling region shown in panel (a). Panel (d) shows the relationship between the age of pulsars and their spin-down power. Panels (e) and (f) respectively show the relationship between the spin-down power and the reference flux and the spin-down power and the spectral index reported by KM2A in Z. Cao et al. (2024). The red lines and the yellow shaded areas in panels (d), (e), and (f), respectively, show the linear regression fit to the data and the 68% containment region of the data or the 1σ deviation from the fit.
Paper: On the Contribution of Unresolved Pulsars to the Ultra-high-energy Galactic Diffuse Gamma-Ray Emission
Authors: Samy Kaci, Gwenael Giacinti, Dmitri Semikoz
Figure caption: Contribution of unresolved pulsars to the diffuse gamma-ray background measured by LHAASO. The upper left (right) panel shows the diffuse flux measured by KM2A and the flux of unresolved pulsars in the inner (outer) Galaxy. The lower left (right) panel shows the relative contribution of unresolved pulsars to the diffuse flux measured by LHAASO in the inner (outer) Galaxy.
Paper: On the Contribution of Unresolved Pulsars to the Ultra-high-energy Galactic Diffuse Gamma-Ray Emission
Authors: Samy Kaci, Gwenael Giacinti, Dmitri Semikoz
Figure caption: Flux of unresolved pulsars together with that of resolved pulsars without masks in the inner (left panel) and outer (right panel) Galaxy. The same cuts in spin-down power have been used in Figure 3.
Paper: On the Contribution of Unresolved Pulsars to the Ultra-high-energy Galactic Diffuse Gamma-Ray Emission
Authors: Samy Kaci, Gwenael Giacinti, Dmitri Semikoz
Figure caption: Expected gamma-ray flux of unresolved pulsars (without cut in spin-down power) above 10 TeV in the ﹩\left(l,b\right)﹩ plane for the inner Galaxy (upper panel) and outer Galaxy (lower panel). The white regions represent the masks of LHAASO from Z. Cao et al. (2023). The upper bound of the color bar represents the sensitivity of LHAASO to a point source located at a decl. of −10°, and the lower bound of the color bar represents 0.1% of its upper bound.