# The LHAASO PeVatron Bright Sky: What We Learned
## 3 Overview of the 12 LHAASO Sources  
The Large High altitude Air Shower Observatory (LHAASO), located in Sichuan (province of China) at 4410 m altitude, is a complex of EAS detectors, with the aim of studying both CRs and \(\gamma\)-rays in the sub-PeV to 1000 PeV energy range [129]. It is composed of three arrays: a kilometer square array (KM2A, 10 TeV-100 PeV, UHE \(\gamma\)-ray detector with an energy resolution \(\leq 20\%\), angular resolution of \(0.25^{\circ}\), and sensitivity (at 50 TeV) of \(10^{-14}\) erg cm\({}^{-2}\) s\({}^{-1}\)), a water Cherenkov detector array (WCDA, down to 0.1 TeV, angular resolution of \(0.2^{\circ}\), and sensitivity (\(E>2\) TeV) of \(10^{-12}\) erg cm\({}^{-2}\) s\({}^{-1}\)), and a wide field-of-view Cherenkov telescope array (WFCTA, 0.1-1000 PeV) [130].  
The 12 Galactic PeVatrons were detected by the half-completed LHAASO-KM2A, with an angular resolution of \(0.4^{\circ}\) and an energy resolution of 28% at 30 TeV [43] (see Figure 6). The indicated \(E_{max}\) in the table represents the maximum energy detected for each source (for the Crab Nebula, there is an updated value, see the dedicated Section 3.1). Among them, the UHE emissions in the regions of LHAASO J1825-1326, LHAASO J1908+0621, and LHAASO J2018+3651 had already been detected by HAWC ([21], eHWC J1825-134, eHWC J1907+063, eHWC [2019+368], and LHAASO J0534+2202 (Crab Nebula) was de tected at \(E>150\) TeV by HAWC and Tibet AS\(\gamma\)[20; 23]. LHAASO J0534+2202 is the only candidate PeVatron detected by LHAASO with a firm association. The low angular resolution of the LHAASO instruments implies that for every candidate there are at least two candidate TeV counterparts.  
In addition to the 12 well-known PeVatrons published in [43], the LHAASO collaboration published two papers on two other sources detected at VHE: LHAASO J0341+5258 [44] and LHAASO J0621+3755 [45]. LHAASO J0341+5258 is a unidentified source associated with GMCs [131] but without any detected PWN or SNR in the surroundings. LHAASO J0621+3755 is one of the four TeV halos of our galaxy (see Section 2.4) detected and identified to date [119; 132]. It is a new source in the TeV domain [131] and is spatially coincident with the Fermi-LAT PSR J0622+3749 that has a spin-down sufficient to explain the halo luminosity. Moreover, its spectrum can be explained using super-diffusion models [133]; all the criteria to be a TeV halo are respected [119].  
These two sources are not in the main paper [43] nor in the PeVatron Table in Figure 6 because they have a significance at \(100\) TeV \(<5\sigma\), and for this reason we do not take them into account in this work, where we summarize what has been done from a theoretical and experimental point of view on every LHAASO PeVatron source in [43]. Our aim is to clarify what we know and what we have learned about every LHAASO source and their origin, both from a \(\gamma\)-ray and neutrino point of views. A theoretical interpretation and/or analysis of the existent models is beyond the scope of this work.  
In the Figure 19, we summarize the main conclusions about the origin of \(\gamma\)-ray emissions from the LHAASO sources, together with their coordinates, detected maximum energies, and detection significance.