THE 1st LHAASO SYMPOSIUM

28 May 2023, 09:00 → 2 Jun 2023, 22:00 Asia/Shanghai

Tianfu Cosmic Ray Research Centre

Zhen Cao (高能所)

LHAASO (Large High Altitude Air Shower Observatory) has provided crucial insights into the origin and nature of cosmic rays, particularly in the ultra-high-energy regime. Its results also have implications for multi-messenger astronomy, as LHAASO can detect gamma rays in coincidence with other messengers, such as neutrinos and gravitational waves.

This international symposium aims to bring together experts and scholars from around the world to discuss the latest research findings of LHAASO and their corresponding implications in various aspects of astrophysics, including cosmic ray physics and multi-messenger astronomy. We hope that this symposium will foster academic exchange and collaboration, and deepen our understanding of the significance and importance of the LHAASO experiment in advancing our knowledge of  the universe.

The conference participants are welcomed to register for a  visit to LHAASO site on Mt. Haizi (4410 m a.s.l), Daocheng, Sichuan Province after the conference in Chengdu. The cost is covered by the participants themselves. 

Important Dates

1. Call for abstracts of posters : the beginning of March 2023  (If you need an indico account for abstract submitting, please contact liaosy@ihep.ac.cn), oral presentations are invited. 

2. Opening of the registration and reservation of hotel rooms:   March 10, 2023

3. Deadline for abstract submission: May 19, 2023

4. Deadline for registration:  May 15, 2023

6. Onsite conference reception: May 28, 2023

7. The conference starts: May 29, 2023

application_form_for_registration_fee_waiver.doc

poster of the 1st LHAASO symposium

Sunday, 28 May

Registration & Reception

18:00 Dinner

Monday, 29 May

Registration & Reception: Registration all day

Welcome

Convener: Zhen Cao (高能所)

Morning Session I: GALACTIC CR

Convener: Felix Aharonian (MPIK/DIAS)

1 LHAASO Experiment (General+ first catalog)

Speakers: Zhen Cao (Insitute of High Energy Physics, CAS) , songzhan Chen (Insitute of High Energy Physics, CAS)

2 Galactic Cosmic Rays - Accelearion and propagation

online

Speaker: Mikhail Malkov (University of California, San Diego)

3 CTA and complementarity of techniques

Speaker: Prof. Werner Hofmann (MPIK)

10:45 Coffee break & Group Picture

Moring Session II: GALACTIC CR

Convener: Songzhan Chen (IHEP, CAS)

4 about Stellar Clusters/SNR and Cosmic Rays

Speaker: Stefano Gabici (Université Paris Cité, CNRS, Astroparticule et Cosmologie)

gabici.pdf

5 LHAASO – SNRs

Speaker: Siming Liu (Southwest Jiaotong University)

6 LHAASO - Stellar Clusters

Speaker: Ruizhi Yang (University of Science and Technology of China)

13:00 Lunch

Afternoon session I: GALACTIC CR

Convener: Ruizhi Yang (University of Science and Technology of China)

7 Turbulent magnetic fields: detections, and implications on CRs

Speaker: Huirong Yan (D)

8 To be confirmed

Speaker: Gwenael Giacinti (MPIK Heidelberg)

9 First-principle simulations of cosmic-ray transport in the self-confinement regime

Cosmic-rays (CRs) have been recognized to play an important role in the galactic ecosystem through CR feedback. The key underlying microphysics lie in the CR gyro-resonant instabilities, which trigger the growth of Alfv’en waves that lead to energy and momentum exchange between the CRs and the background plasmas, as well as CR self-confinement. I will present simulations of the CR gyro-resonant instabilities using the magnetohydrodynamic-particle-in-cell (MHD-PIC) method in a variety of simulation settings. By designing a streaming box and an expanding box framework, our simulations achieve the steady-state balance between wave growth and damping, as well as between driving CR streaming/anisotropy and isotropization via wave scattering. It allows us to measure the CR transport coefficients from first principles as a function of background environment, which will offer reliable subgrid prescriptions for macroscopic studies of CR feedback and transport.

Speaker: Xuening Bai (Tsinghua University)

10 Start Clusters as gamma-ray sources

In the last decade several Young Star Clusters have been associated to diffuse gamma-ray sources both in the GeV and TeV energy ranges. The origin of such emission is still debated, however hadronic processes due to interaction between gas and locally accelerated cosmic rays seems to be favored at least in some cases. The acceleration mechanism is probably related to powerful stellar winds emitted by the most massive stars in the clusters. I will present a model based on acceleration at the termination shock of those winds, showing how the predicted gamma-ray emission agrees with the one observed from the Cygnus OB association. Moreover, using the same model I will present the total contribution to the diffuse Galactic gamma-sky due to clusters which are too dim to be resolved as single sources by present gamma-ray telescopes.

Speaker: Giovanni Morlino (INAF-Astronomical Observatory of Arcetri)

11 Particles and radiation from supernova remnants

Unveiling the origin of the cosmic-ray (CR) flux observed at Earth remains among the main challenges in the field of astroparcle physics. The Galactic CR component is believed to be produced bysupernova remnants (SNRs) as a result of diffusive shock acceleration, though the acvity of this class of sources in the knee region is yet to be proven. In this context, the process through which accelerated particles escape from their sources affects both the spectral and morphological radiave signatures from these sources as well as the formation of the CR spectrum. As a result, the gammaray emission strongly depends on the level of diffusion experienced by the parcles at the accelerator, that can hence be constrained observationally together with the maximum energy of particles achieved, as I will discuss in this contribution.

Speaker: Silvia Celli (La Sapienza University of Rome)

17:10 Coffee Break

Afternnon Session II: MULTIWAVELENGTH

Convener: Hao Zhou (Shanghai Jiao Tong University)

12 The Milky Way Imaging Scroll Painting (MWISP) Survey Project: New Molecular Line Data along the Northern Galactic Plane

Molecular clouds are the cold and dense part (n ≥ 10^2 cm-3) of hierarchical interstellar medium concentrated toward the Galactic disk. A number of wide-field surveys in molecular lines have been made to investigate the gas distribution and physical processes. Significant progresses have been made over the last 50 years. However, further improvement of our understanding of interstellar molecular gas was hampered by sensitivity, sky coverage, spatial resolution, velocity coverage, spectral or velocity resolution, and line tracers. The Milky Way Imaging Scroll Painting (MWISP) project was initiated to map the northern galactic plane in 12CO/13CO/C18O J=1-0 lines using the Superconducting Spectroscopic Array Receiver (SSAR), a sideband-separation superconducting SIS focal plane array receiver system at the 13.7m millimeter-wave radio telescope of Purple Mountain Observatory Qinghai Station. An area of 2400 deg^2 within L=10~250 deg, B=+/-5 deg was fully covered in its first phase by 11 observing seasons over the period of 2011-2021. MWISP survey is characteristic of high sensitivity, wide sky coverage, and most importantly, multi-line tracers for the first time of its kind. In this talk, I will introduce the general features of the survey, presenting the large-scale CO data and images of molecular emission, examples of discoveries and statistics, followed by illustration of Galactic targets or areas which may be of potential interests to the study of high-energy gamma-rays and cosmic-ray phenomena.

Speaker: Prof. Ji Yang (speaker: Yang Su) (Purple Mountain Observatory, Chinese Academy of Sciences)

13 The Einstein Probe Mission

Einstein Probe (EP) is an upcoming space mission dedicated to the detection and characterization of high-energy transients. It will carry one wide-field lobster-eye X-ray telescope to monitor the soft X-ray sky in 0.5-4 keV with a 3600 square-degree FoV, and a narrow-field X-ray telescope in 0.3-10 keV for deep follow-up observations and precise source locating. Transient alerts can be issued quickly to trigger follow-up observations at multi-wavelengths. Aiming for launch by the end of 2023, EP is a mission of the Chinese Academy of Sciences with the participation of ESA and MPE. This talk will introduce the latest status of the EP mission, and present the prospects of EP in the high-energy transient and multi-messenger astrophysics. Recent results from the EP-WXT pathfinder (also known as LEIA) launched in July 2022 will also be presented.

Speaker: Chichuan Jin (National Astronomical Observatories (NAOC), CAS)

14 Update on ASTRI: Technology and science using wide-field aplanatic IACT telescopes

The ASTRI program was launched 10 years ago with the goal of developing small-sized dual-mirror aplanatic wide-field IACT telescopes as a precursor to the array of small-sized telescopes (SSTs) for the Cherenkov Telescope Array (CTA) observatory's southern site. The program initially received support from INAF and MUR (the Italian Ministry for Universities and Research), but it later gained support from other international partners such as the University of Sao Paulo/FAPESP, Nort-West University/South Africa, IAC, FGG, and Université de Geneve at different stages of the project. The program's first significant achievement was the development of the end-to-end ASTRI-Horn prototype and its installation at the INAF site of Serra La Nave. The prototype featured an innovative compact camera based on SiPM sensors and proved the dual-mirror Schwarzschild-Couder optical configuration as an aplanatic system while detecting the Crab Nebula in gamma rays. The telescope underwent major refurbishment and is now used to observe the volcano's bright gamma-ray sources, cosmic rays, and muon radiography studies. Meanwhile, the ASTRI mini-array is being implemented in Tenerife to study the gamma-ray sky in the 1-100 TeV energy band with unprecedented angular resolution (3 arcmin), which complements LHAAZO perfectly. This talk discusses the project's current status, scientific goals, and expectations.

Speaker: Prof. Giovanni Pareschi (INAF-Astronomical Observatory of Brera)

15 ASTRI Optical design

ASTRI is a 4 m class Imaging Atmospheric Cherenkov Telescope (IACT) devoted to the observation of gamma sources in the TeV emission band. The telescope implements an innovative optical design based on the dual-mirror Schwartzchild –Couder (SC) configuration. The SC configuration was proposed at the beginning of 1900 as an aplanatic configuration capable of reducing off-axis angular resolution degradation and hence enhancing the field of view. ASTRI was inaugurated in 2014 and is the first telescope realized in SC configuration. The optical performance of ASTRI is perfectly matching the TeV band IACT requirements with an angular resolution <0.2° across the field of view of about ~10°.

ASTRI was then adopted as a baseline for the Cherenkov Telescope Array Small Size telescopes and is going to be implemented in 9 replicas at the ASTRI Mini Array, a TeV band Cherenkov Observatory realized by the Italian Institute for Astrophysics at the Tenerife site.

Speaker: Giorgia Sironi (INAF)

19:00 Dinner

Tuesday, 30 May

Morning Session I: PWN

Convener: Siming Liu (Southwest Jiaotong University)

16 about Pulsar Wind Nebulae

Speaker: Dmitry Khangulyan (Rikkyo University)

17 LHAASO results on PWNe and Pulsar Halos

Speaker: Ruoyu Liu (Nanjing University)

18 Binaries seen in Gamma ray

Speaker: Jian Li (USTC)

10:45 Coffee break & Poster time

Moring Session II: CRs

Convener: Huihai He (Institute of High Energy Physics, CAS)

19 Galactic Cosmic Rays- general review

Speaker: author: Samuel Ting, speaker: Zuhao Li (IHEP)

20 CR Spectra below knees-DAMPE

Speaker: Xiang Li (Purple Mountain Observatory， CAS)

21 CR Spectra in the knee region

Speaker: Paolo Lipari (INFN Roma 1)

13:00 Lunch

Poster time

Afternoon session I: PWN

Convener: Ruoyu Liu (Nanjing University)

22 LHAASO PWN tail: PSR J1740+1000

Speaker: Renfeng Xu (IHEP)

23 LHAASO Millisecond pulsar PWN: J0218+4232

Speaker: Zhe LI (IHEP)

24 LHAASO Geminga spectrum and morphology

Speaker: Yingying Guo (PMO)

25 How do pulsars generate extended VHE sources? A PWN tale

Currently, the bulk of Galactic VHE sources are associated with isolated, rotation powered neutron stars (i.e. pulsars). However, how pulsars produce such sources is poorly understood. Answering this question requires understanding the evolution of the pulsar wind nebulae (PWN) produced by the neutron star -- where particles are believed to be accelerated to the required PeV energies and then injected into their surroundings. In this presentation, I will discuss a simple one-zone model for such sources, and how the application of this model to PWNe in different stages of their evolution can be used to understand the origin of the highest energy sources in the Milky Way.

Speaker: Josepf Gelfand (New York University)

26 Spatially resolved TeV emission from the jets of the microquasar SS 433

The microquasar system SS 433 provides a unique opportunity to study mildly relativistic collimated jets in our own Galaxy. From its core, a binary system hosting a stellar-mass black hole, two persistent, semi-relativistic jets are launched, almost perpendicular to the line of sight. X-ray observations reveal that these jets extend out to around 100 pc on either side of the central system, terminating at the radio structure W50. The jets of SS 433 were recently reported to be a source of TeV gamma-rays by the HAWC collaboration. I will report the results of deep observations of this system with the H.E.S.S. array of telescopes, resulting in the first detection of the system by an Imaging Atmospheric Cherenkov Telescope array.
To fully exploit the capabilities of the H.E.S.S. observations, a new approach to background rejection was deployed, which I will briefly describe. It is based on the detection of Cherenkov light from muons by large Imaging Atmospheric Cherenkov Telescopes (IACTs), such as the telescope located at the center of the H.E.S.S. array. The application of this technique leads to a factor four reduction in background above several tens of TeV in the H.E.S.S. stereoscopic analysis.
The superior energy and angular resolution of the H.E.S.S. array compared to HAWC allow for a detailed study of the morphology and spectral energy distribution of the gamma-ray emission in the jets, including a measurement of the physical extension of the emission and of the spectra of the jets out to tens of TeV. This measurements are put in the context of the multi-wavelength emission from the jets to constrain the properties of the high energy particle population responsible for the emission.

Speaker: Laura OLIVERA NIETO (MPIK)

16:10 Coffee Break

Afternnon Session II: DIFFUSE AND CR

Convener: Qiang Yuan (Purple Mountain Observatory)

27 Diffuse gamma-ray and neutrino background from Milky Way Galaxy

Recently LHAASO measured diffuse gamma-ray background from Milky Way in inner and outer Galaxy. In this talk I’ll discuss how combining this information with Fermi LAT gamma-ray,
IceCube neutrino and cosmic ray data we can constrain models
of cosmic ray propagation in Galaxy.

Speaker: Dmitri Semikoz (APC, Paris)

28 multi-messenger approach of searching for PeVatrons and UHECR sources

Speaker: Zhuo Li (Peking University)

29 Particle acceleration and multi-messenger radiation from extragalactic outflows

Winds and outflows are ubiquitous at several scales throughout the Cosmos.They often develop a bubble structure characterized by strong shocks and turbulence where high-energy particles can be efficiently produced.
I will present a model in which diffusive shock acceleration is a
key process to energize particles in such astrophysical winds.
I will show some model applications in the context of starburst galaxies and active galactic nuclei and I will discuss the associated multi-messenger implications in terms of high-energy photons, neutrinos and escaping cosmic rays.

Speaker: Enrico Perreti (University of Copenhagen, Niels Bohr Institute)

30 Cosmic rays and diffuse gamma-ray emission from the Milky Way

Speaker: Susumu Inoue (Bunkyo University)

18:30 Dinner

Wednesday, 31 May

Morning Session I: CR direct

Convener: Shoushan Zhang (Institute of High Energy Physics)

31 LHAASO - Cosmic Rays

Speaker: Shoushan Zhang (Institute of High Energy Physics)

32 LHAASO Diffuse: Qiang Yuan

Speaker: Qiang Yuan (Purple Mountain Observatory)

33 Extragalactic Cosmic Rays

Online

Speaker: Pierre Sokolsky

LHAASO talk.pdf

10:45 Coffee break

Moring Session II: extragalactic

Convener: Min Zha (IHEP, CAS)

34 GRBs and their Afterglows

Speaker: Prof. Bing Zhang (University of Nevada, Las Vegas)

35 LHAASO - Extragalactic (GRB afterglows and AGN)

Speaker: Xiangyu Wang (Nanjing University)

36 Gamma Ray Emitting AGN

Speaker: Prof. Paolo Coppi (Yale University )

13:00 Lunch

Afternoon session I: CR and extragalactic

Convener: Xiangyu Wang (Nanjing University)

37 measurements of mean logarithmic mass of cosmic rays near the knee region by LHAASO

Speaker: Hengying Zhang (IHEP)

38 LHAASO AGN: NGC 1275 and Mrk 421

Speaker: Min Zha (Institute of High Energy Physics, CAS)

39 Galactic black holes as PeVatrons

Speaker: Shigeo Kimura (Tohoku University )

15:30 Coffee break

Afternnon Session II: GRB/neutrino/DM

Convener: Xiaojun Bi (IHEP)

40 Jitter Mechanism as a Kind of Coherent Radiation: GRB 221009A beyond 10 TeV

The emission of GRB 221009A beyond 10 TeV has been detected by LHAASO. We suggest jitter radiation as a possible explanation for the TeV emission of this energetic GRB. We first present a short review on both synchrotron mechanism and jitter mechanism. We then present the kinetic turbulence that can work on the small length scale. In our scenario, the jitter radiation field is linked to the perturbation field, and the perturbation field is dominated by the kinetic turbulence. The jitter radiation can reach the TeV energy band when we consider either electron cooling or Landau damping. We further suggest that the jitter radiation in the very high-energy band is coherent, and the observational flux of GRB 221009A in the TeV energy band can be reproduced by the the coherent jitter mechanism. In addition, the coherent jitter radiation is expected to have wide applications in the high-energy astrophysical research field.

Speaker: Jirong Mao (Yunnan Observatory, CAS)

41 Early TeV Gamma-Ray Afterglow of GRBs

LHAASO and/or CTA will increase the detected samples of TeV afterglows of GRBs in the near future, which is essential to revealing jet magnetization, particle acceleration, and magnetic field amplification. The emission from the reverse shock largely depends on the magnetization of the jets.
On the other hand, X-ray afterglows frequently show a shallow decaying emission in their first few thousand seconds. Possible models for the shallow decay phase are continuous energy injection, late catch-up of lately launched ejecta, the evolution of microscopic parameters, thin wind profile of the circumstellar medium, and so on.
Depending on the models, the TeV emission of the early afterglow will show different behaviors. We show model calculations of multi-wavelength lightcurves based on our time-dependent simulation code. The detection of early TeV afterglows will provide a clue to distinguishing the models of the shallow decay phase.

Speaker: Katsuaki Asano

42 Probing the Glashow resonance and beyond with ultrahigh energy neutrino telescopes

The standard model (SM) of particle physics predicts the resonant scattering of electron anti-neutrinos off the electron target, as first pointed out by Sheldon Glashow. The Glashow resonance is the only feasible way now to distinguish between neutrinos and antineutrinos at ultrahigh energies. Recently, a candidate event with an energy deposition of around 6.05 PeV has been confirmed by the IceCube Observatory. Such an event arises very likely from the Glashow resonance and can provide us valuable information about the source of cosmic rays and ultrahigh energy neutrinos. I will first talk about the implications of this Glashow resonance candidate to cosmic neutrino sources, incorporating both the atomic Doppler broadening effect and initial state radiation while calculating the cross section. Then, I move on to discussing the prospect of upcoming neutrino telescopes. In particular, the potential of mountain-valley telescopes for the Glashow resonance will be emphasized. Finally, I will discuss exotic resonances arising from new physics beyond the SM.

Speaker: Dr Guoyuan Huang (Max-Planck-Institut für Kernphysik)

Glashow.pdf

43 Nuclear and electron cascades induced by UHECRs

Speaker: Dr Bing T. Zhang (Kyoto Univeristy)

44 LHAASO Dark matter: Dwarf Spheroidal Galaxies

Speaker: Xiaoyuan Huang (Purple Mountain Observatory, CAS)

45 LHAASO Updating with WCDA for LHAASO J2108+5157 or LHAASO J0341+5258

Speaker: Shicong HU (IHEP)

18:30 Reception Dinner

Thursday, 1 June

Morning Session I: Multimessenger and Multiwavelength

Convener: Zhiguo Yao (IHEP, Beijing, China)

46 LHAASO - Fundamental Physics (DM, LIV, etc.)

Speaker: Xiao-Jun Bi (IHEP)

47 Gravitaion waves and GRBs

Speaker: Barbara Patricelli (University of Pisa)

10:10 Coffee break

Moring Session II: Multimessenger and Multiwavelength

Convener: Zhen Cao (高能所)

48 Fermi - summary of the Fermi Results

Speaker: Donggeun Tak (Seoul National University)

49 Low Energy Neutrinos

Speaker: Wei Wang (Sun Yat-sen University)

50 about High Energy Neutrinos

Speaker: Dr Ke Fang (University of Wisconsin-Madison )

Concluding Remark

Convener: Felix Aharonian (MPIK/DIAS)

self-arrangement (shuttle bus from hotel to metro station)

Friday, 2 June

visit to LHAASO Observatory site in Daocheng: the flights are recommended: 1. from Chengdu Tianfu International Airport to Daocheng Yading Airport, Jun. 2nd, CA2561 , 07:40（TFU， T2）-09：00 （DCY） 2. from Daocheng Yading Airport to Chengdu Tianfu International Airport, Jun 3rd, CA2562 , 09:50(DCY) -11:15(TFU, T2) . There will be bus to take visitors from Daocheng Yading airport to LHAASO site on June 2, and from the hotel in Daocheng to Yading airport on June 3.

the flights are recommended: 1. from Chengdu Tianfu International Airport to Daocheng Yading Airport,
Jun. 2nd, CA2561 , 07:40（TFU， T2）-09：00 （DCY）
2. from Daocheng Yading Airport to Chengdu Tianfu International Airport,
Jun 3rd, CA2562 , 09:50(DCY) -11:15(TFU, T2)

There will be bus to take visitors from There will be bus to take visitors from Xinglong Lake hotel to Tianfu airport, from Daocheng Yading airport to LHAASO site on June 2, and from the hotel in Daocheng to Yading airport on June 3.