# The LHAASO PeVatron Bright Sky: What We Learned
## 4 The Future  
Our space and \"on-Earth\" facilities have allowed us to know a lot about CRs and their sources. However, this is not sufficient to have a definitive answer to the question \"What is the origin of CRs?\"  
After the review of all the LHAASO candidate PeVatrons, it is quite clear what ingredients are required to have a better understanding of galactic CRs:  
* Higher angular resolution of the future VHE/UHE \(\gamma\)-ray instruments;
* Higher sensitivity of the future neutrino experiments;
* Multiwavelength and multi-messenger analysis of the same source;
* Improvements in the comprehension of the micro-physics of different kinds of source. According to the observational evidence, a very high angular resolution is the most important feature in an instrument for looking into these sources. This would allow a much better source association of detected \(\gamma\)-ray emissions, a deeper understanding of a possible energy dependent morphology, and to strengthen multiwavelength correlations. The highest possible energy sensitivity is also fundamental, but LHAASO has proven that this is sufficient to identify the presence of PeVatrons in our Galaxy but not to make a firm association with a parent source and to discern hadronic from leptonic emissions. Morphological information will also be crucial for understanding certain specific parameters of candidate PeVatrons. For example, compact sub-degree regions in PWNe indicate a high magnetic field and fast synchrotron losses, and the detection of extended X-ray nebula should mean that LHAASO \(\gamma\)-ray detection originates from the up-scattering of the 2.7 K CMB radiation in PWNe [26]. Such a detection is challenging for the current X-ray instruments (XMM-Newton, Chandra), but will be possible for the eROSITA satellite, which will have a larger FoV [26]. Even if the LACTs have some evident disadvantages with respect to the EAS arrays (e.g., limited duty cycle (10-15%) or limited FoV), their low-energy threshold and high angular resolution (\(<\)0.1\({}^{\circ}\) at 1 TeV) make IACTs ideal for detailed morphological studies. For this reason, instruments such as the ASTRI Mini-Array and CTA will make a difference (see Figure 17, right). In addition, the higher sensitivity of the ASTRI Mini-Array, and in particular of CTA South, will allow enhancing the number of VHE sources detected in the TeV band, up to a factor of several hundred [70] (see Figure 17, left). Figure 17: (**Left**): Angular resolution of the current and future instruments from [207] with the addition of the ASTRI Mini-Array updated curve with optimized cuts from [208] and the LHAASO curve from [77]. (**Right**): Differential sensitivity curves of the current and future VHE/UHE instruments from [209], expanded with the addition of the ASTRI Mini-Array curves for 50 h and 500 h and other instrument curves [208]. The ASTRI Mini-Array will have its first three telescopes operative at the beginning of 2024 and the whole array in the first half of 2025. This means that its first results will be parallel or just before the full operation of IceCube-Gen2 (2030s), KM3 NeT-ARCA, and P-ONE (after 2030) in the next 5-10 years, preparing the ground for a future \(\gamma\)-ray-neutrino combined analysis. In [35], the authors estimated the observational time it takes for a \(5\sigma\) detection using the so-called Planetary Neutrino Monitoring System (PLE\(\
u\)M) [210], a global repository of HE neutrino observations by current and future neutrino telescopes. According to their computations (and relative assumptions on the threshold energy and models), they found that in the next 20 years the PLE\(\
u\)M could discover neutrino emissions from the Crab Nebula, LHAASO J1825-1326, LHAASO J1839-0545, LHAASO J1908+0621, LHAASO J2018+3651, and LHAASOJ2226+6057.