Opening Room: ES635

Lecture1-1: Introduction to Dark Matter

• John Ellis

Room: ES635

Lecture2-1: Particle Dark Matter

• Alejandro Ibarra

Room: ES635

Lecture3-1

• Hidetoshi Otono

Room: ES635

Lecture4-1: Physics of Dark Matter Direct Detection

• Masaki Yamashita

Room: ES635 1. Motivation/Evidence of Dark Matter 2. Dark Matter Candidates and WIMPs 3. Why WIMP? 4. Experimental Search for WIMPs

Reception / Poster Session Room: ITbM 1F Hall

Lecture4-2: Physics of Dark Matter Direct Detection

• Masaki Yamashita

Room: ES635 1. WIMP Direct Detection 2. Background Sources 3. Detection Technologies 4. Liquid Xenon Time Projection Chamber 5. Current Experiments 6. Future Experiments 7. Summary and Outlook

Lecture3-2

• Hidetoshi Otono

Room: ES635

Lecture1-2: Introduction to Dark Matter

• John Ellis

Room: ES635

Lecture5-1: Detection of dark matter axions -- from classical microwaves to quantised photons --

• Akira Miyazaki

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.

Seminar1: Dark Matter in the Milky Way

• Kohei Hayashi

Room: ES635

Lecture2-2: Particle Dark Matter

• Alejandro Ibarra

Room: ES635

Lecture5-2: Detection of dark matter axions -- from classical microwaves to quantised photons --

• Akira Miyazaki

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.

Lecture5-3: Detection of dark matter axions -- from classical microwaves to quantised photons --

• Akira Miyazaki

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.

Seminar2: Narrowing down the mass range of ultra-light dark matter

• Elisa Ferreira

Room: ES635

Seminar3: Primordial Black Hole Darke Matter

• Kazunori Kohri (NAOJ / KEK / SOKENDAI / Kavli IPMU)

Room: ES635

Closing Room: ES635