KMI/NITEP School 2026: Dark Matter — from Ultra Light to Super Massive
from
Monday 9 March 2026 (09:00)
to
Wednesday 11 March 2026 (17:40)
Monday 9 March 2026
09:00
Opening
Opening
09:00 - 09:15
Room: ES635
09:15
Lecture1-1
-
John Ellis
Lecture1-1
John Ellis
09:15 - 10:45
Room: ES635
10:45
Coffee Break
Coffee Break
10:45 - 11:15
Room: ES635
11:15
Lecture2-1
-
Alejandro Ibarra
Lecture2-1
Alejandro Ibarra
11:15 - 12:45
Room: ES635
12:45
Lunch
Lunch
12:45 - 14:15
Room: ES635
14:15
Lecture3-1
-
Hidetoshi Otono
Lecture3-1
Hidetoshi Otono
14:15 - 15:45
Room: ES635
15:45
Coffee break
Coffee break
15:45 - 16:15
Room: ES635
16:15
Lecture4-1
-
Masaki Yamashita
Lecture4-1
Masaki Yamashita
16:15 - 17:45
Room: ES635
18:00
Reception / Poster Session
Reception / Poster Session
18:00 - 20:00
Room: ITbM 1F Hall
Tuesday 10 March 2026
09:00
Lecture4-2
-
Masaki Yamashita
Lecture4-2
Masaki Yamashita
09:00 - 10:30
Room: ES635
10:30
Coffee Break
Coffee Break
10:30 - 11:00
Room: ES635
11:00
Lecture1-2
-
John Ellis
Lecture1-2
John Ellis
11:00 - 12:30
Room: ES635
12:30
Lunch
Lunch
12:30 - 14:00
Room: ES635
14:00
Lecture5-1: Detection of dark matter axions -- from classical microwaves to quantised photons --
-
Akira Miyazaki
Lecture5-1: Detection of dark matter axions -- from classical microwaves to quantised photons --
Akira Miyazaki
14:00 - 15:30
Room: ES635
Axions were originally proposed to solve the strong CP problem and are among the leading candidates for ultralight dark matter in cosmology. In contrast to particle-like dark matter candidates such as Weakly Interacting Massive Particles (WIMPs) and Freeze-In Massive Particles (FIMPs), axions and axion-like particles can be described as a classical field. This behavior arises from their large occupation number and macroscopic de Broglie wavelength, which lead to coherent, wave-like dynamics on laboratory scales. In the presence of a static magnetic field, non-relativistic dark matter axions can be converted into microwave photons via the inverse Primakoff effect. The resulting signal is semi-classical and forms the basis of resonant and broadband detection strategies. Particular emphasis in this lecture course will be placed on the wake-like behavior of axion dark matter and its phenomenological differences from conventional particle-like dark matter candidates. The course covers the theoretical foundations and experimental techniques of axion detection, progressing from basic principles to current state-of-the-art approaches and future directions. The structure is as follows: ## 5-1) Overview of axion searches General introduction, theoretical framework, and a survey of ongoing and planned experiments worldwide. ## 5-2) Classical detection schemes Microwave cavities and materials, resonator design, signal readout, and analog and digital signal processing. ## 5-3) Quantum detection schemes Coherent states and Roy J. Glauber’s theorem, quantum noise and the standard quantum limit, squeezing techniques, and photon counting. Because some of the required quantum optical concepts may be less familiar to particle physicists, Part 5-3 includes hands-on exercises on basic quantum optics. Participants are encouraged to bring pen and paper to work through operator manipulations in bra–ket notation.
15:30
Coffee Break
Coffee Break
15:30 - 16:00
Room: ES635
16:00
Lecture3-2
-
Hidetoshi Otono
Lecture3-2
Hidetoshi Otono
16:00 - 17:30
Room: ES635
17:30
Seminar1
-
Kohei Hayashi
Seminar1
Kohei Hayashi
17:30 - 18:15
Room: ES635
Wednesday 11 March 2026
09:00
Lecture2-2
-
Alejandro Ibarra
Lecture2-2
Alejandro Ibarra
09:00 - 10:30
Room: ES635
10:30
Coffee Break
Coffee Break
10:30 - 11:00
Room: ES635
11:00
Lecture5-2: Detection of dark matter axions -- from classical microwaves to quantised photons --
-
Akira Miyazaki
Lecture5-2: Detection of dark matter axions -- from classical microwaves to quantised photons --
Akira Miyazaki
11:00 - 12:30
Room: ES635
Axions were originally proposed to solve the strong CP problem and are among the leading candidates for ultralight dark matter in cosmology. In contrast to particle-like dark matter candidates such as Weakly Interacting Massive Particles (WIMPs) and Freeze-In Massive Particles (FIMPs), axions and axion-like particles can be described as a classical field. This behavior arises from their large occupation number and macroscopic de Broglie wavelength, which lead to coherent, wave-like dynamics on laboratory scales. In the presence of a static magnetic field, non-relativistic dark matter axions can be converted into microwave photons via the inverse Primakoff effect. The resulting signal is semi-classical and forms the basis of resonant and broadband detection strategies. Particular emphasis in this lecture course will be placed on the wake-like behavior of axion dark matter and its phenomenological differences from conventional particle-like dark matter candidates. The course covers the theoretical foundations and experimental techniques of axion detection, progressing from basic principles to current state-of-the-art approaches and future directions. The structure is as follows: ## 5-1) Overview of axion searches General introduction, theoretical framework, and a survey of ongoing and planned experiments worldwide. ## 5-2) Classical detection schemes Microwave cavities and materials, resonator design, signal readout, and analog and digital signal processing. ## 5-3) Quantum detection schemes Coherent states and Roy J. Glauber’s theorem, quantum noise and the standard quantum limit, squeezing techniques, and photon counting. Because some of the required quantum optical concepts may be less familiar to particle physicists, Part 5-3 includes hands-on exercises on basic quantum optics. Participants are encouraged to bring pen and paper to work through operator manipulations in bra–ket notation.
12:30
Lunch
Lunch
12:30 - 14:00
Room: ES635
14:00
Lecture5-3: Detection of dark matter axions -- from classical microwaves to quantised photons --
-
Akira Miyazaki
Lecture5-3: Detection of dark matter axions -- from classical microwaves to quantised photons --
Akira Miyazaki
14:00 - 15:30
Room: ES635
Axions were originally proposed to solve the strong CP problem and are among the leading candidates for ultralight dark matter in cosmology. In contrast to particle-like dark matter candidates such as Weakly Interacting Massive Particles (WIMPs) and Freeze-In Massive Particles (FIMPs), axions and axion-like particles can be described as a classical field. This behavior arises from their large occupation number and macroscopic de Broglie wavelength, which lead to coherent, wave-like dynamics on laboratory scales. In the presence of a static magnetic field, non-relativistic dark matter axions can be converted into microwave photons via the inverse Primakoff effect. The resulting signal is semi-classical and forms the basis of resonant and broadband detection strategies. Particular emphasis in this lecture course will be placed on the wake-like behavior of axion dark matter and its phenomenological differences from conventional particle-like dark matter candidates. The course covers the theoretical foundations and experimental techniques of axion detection, progressing from basic principles to current state-of-the-art approaches and future directions. The structure is as follows: ## 5-1) Overview of axion searches General introduction, theoretical framework, and a survey of ongoing and planned experiments worldwide. ## 5-2) Classical detection schemes Microwave cavities and materials, resonator design, signal readout, and analog and digital signal processing. ## 5-3) Quantum detection schemes Coherent states and Roy J. Glauber’s theorem, quantum noise and the standard quantum limit, squeezing techniques, and photon counting. Because some of the required quantum optical concepts may be less familiar to particle physicists, Part 5-3 includes hands-on exercises on basic quantum optics. Participants are encouraged to bring pen and paper to work through operator manipulations in bra–ket notation.
15:30
Coffee Break
Coffee Break
15:30 - 16:00
Room: ES635
16:00
Seminar2
-
Elisa Ferreira
Seminar2
Elisa Ferreira
16:00 - 16:45
Room: ES635
16:45
Seminar3
-
Kazunori Kohri
Seminar3
Kazunori Kohri
16:45 - 17:30
Room: ES635
17:30
Closing
Closing
17:30 - 17:40
Room: ES635