Workshop on Cosmic Indicators of Dark Matter 2024

15 Oct 2024, 10:00 → 17 Oct 2024, 12:20 Asia/Tokyo

Tohoku University

Workshop on Cosmic Indicators of Dark Matter 2024

Date: October 15-17, 2024

Venue: Aoba Science Hall, Tohoku University
(in-person event, but will broadcast via Zoom for registered participants)

Overview:

Dark matter is prevalent in the present universe. Although its composition remains unknown, dark matter plays a crucial role in the formation of the hierarchical structures of the universe. They are visible as galaxies or galaxy clusters, which are embedded in or co-exist with invisible dark matter halo structures.

The progress of dark matter study over the past decade pushes us to consider much wider possibilities for particle dark matter, ranging from extremely low to extremely high mass regimes. They can leave characteristic signatures corresponding to their production processes in the early universe, influence on halo and galaxy structure formations, or interaction around the current solar system.

Building on the success of VLDM2021 and VLDM2023, this workshop will discuss recent experimental results, future prospects, and theoretical advancements in the study of focusing on their cosmological signatures.  Especially, the scope of the workshop is expanded to include dark matter heavier than the TeV scale. The workshop will feature invited talks by experts in relevant fields, as well as contributed talks. One of the key aims of this workshop is to deepen our understanding of recent developments and invoke discussions towards the next decade. The following is a list of representative topics:

• Axion and axion like particles
• Dark photon and other light/heavy dark matter
• Dark matter search experiments
• Multi-messenger observations of dark matter and halo properties
• Black hole superradiance
• Cosmic birefringence
• Structure formation

Invited Speakers:

• Kohei Hayashi (National Institute of Technology, Sendai College)
• Joerg Jaeckel (Universität Heidelberg)
• Qiuyue Liang (Kavli IPMU)
• Nils Nilsson (IBS)
• Tatsumi Nitta (ICEPP, UTokyo)
• Masamune Oguri (Chiba University)
• Yuki Sakakihara (Yamagata University)
• Yikun Wang (Caltech)

Code of Conduct:
It is the policy of the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU) that all members and visitors will conduct themselves in a professional manner that is welcoming and free from any form of discrimination, harassment, or retaliation. Members and visitors will avoid any inappropriate actions or statements based on individual characteristics such as age, race, ethnicity, gender, sexual orientation, marital status, nationality, or political affiliation. Disruptive or harassing behavior of any kind will not be tolerated. Harassment includes but is not limited to inappropriate or intimidating behavior and language, unwelcome jokes or comments, unwanted touching or attention, offensive images, photography without permission, and stalking. Members and visitors will treat each other with respect to create a collegial, inclusive, and professional environment at the Kavli IPMU.

 

Organizers:
Elisa Ferreira (Kavli IPMU)
Tomohiro Fujita (Ochanomizu)
Motoko Fujiwara (TUM)
Nagisa Hiroshima (YNU)
Naoya Kitajima (Tohoku)
Eiichiro Komatsu (MPA / Kavli IPMU)
Yuta Michimura (RESCEU)
Kohta Murase (PSU)
Atsushi Naruko (YITP)
Ippei Obata (Kavli IPMU)
Tatsuya Ogawa (Tohoku)
Maresuke Shiraishi (SUS)
Fuminobu Takahashi (Tohoku)
Fujii Toshihiro (OMU)
Yuko Urakawa (KEK)
Masaki Yamada (Tohoku)
Masato Yamanaka (Hosei)
Wen Yin (TMU)

Supported by:
JSPS KAKENHI No. JP20H05851 (PI: Fuminobu Takahashi)
JSPS KAKENHI No. JP20H05852 (PI: Kohta Murase)
JSPS KAKENHI No. JP20H05854 (PI: Yuta Michimura)
JSPS KAKENHI No. JP20H05859 (PI: Eiichiro Komatsu)
JSPS KAKENHI No. JP22K14035 (PI: Nagisa Hiroshima)

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Tuesday 15 October

13:20 Registration and welcome remarks (Ippei Obata)

1 Cosmic Birefringence and Spacetime-Symmetry Breaking

Recently, a CMB signal of parity violation in the form of isotropic cosmic birefringence has been claimed, a signal consistent with being produced through an axion-photon coupling. In this talk, I will introduce a generic EFT constructed for studies of spacetime-symmetry breaking. Focusing on the photon sector, I will show that a CPT-odd EFT term in fact takes the same form as an axion-photon coupling and that the non-zero cosmic-birefringence angle produces the strongest constraint on this EFT coefficient to date.

Speaker: Nils A. Nilsson

14:30 Break (Next session chaired by Tomohiro Fujita)

2 String-wall composites from torus knot vacuum of an axionlike model and the cosmological simulations

We study a simple axionlike model with two complex scalar fields under global U (1) symmetry. The charge of one scalar field is double the other one. A particular feature of our model is that a vacuum manifold is a torus knot, resulting in the formation of a string-wall network. We numerically show that the network becomes a network of narrow strips of string-wall composites (a “kishimen” network.) We find some of strip loops cut off from the network have the shape of a Moebius strip. The fact that the walls are confined in narrow strips implies that our model is free from the domain wall problem.

Speaker: Yuki Sakakihara

202410_Cosmic_Indicators_sakakihara.pdf

3 Simulations of Ellipsoidal PBH Formation and the impact of Non-Spherical effects on the PBH mass function

Numerical simulations have been instrumental in advancing our understanding of Primordial Black Hole (PBH) formation and in providing precise estimates of their abundance in the Universe. Traditionally, these simulations have assumed spherical collapse, but indeed, the most realistic initial configuration is an ellipsoid. In this presentation, I will discuss recent findings on non-spherical PBH formation, focusing on its dynamics and the effect of non-sphericities on the threshold of formation. Our results indicate, for the cases tested, that non-spherical effects are crucial when the fluctuation amplitude is near the collapse threshold (critical regime), preventing a significant number of configurations from forming black holes. However, when considering these effects in the statistical estimation of the PBH mass function, their overall impact is minimal.

Speaker: Albert Escrivà

cosmic indicators dark matter.pdf

16:00 Break (Next session chaired by Tomohiro Fujita)

4 Caustic crossings as a new probe of dark matter

Caustic crossings are highly magnified individual stars observed in high magnification regions of massive galaxy clusters. The first discovery was reported in 2018, and the number of detections is rapidly increasing thanks to James Webb Space Telescope. In this talk I will discuss how we can use caustic crossings for probing nature of dark matter.

Speaker: Masamune Oguri

tohoku2024_public.pdf

Wednesday 16 October

09:20 Break (Next session chaired by Toshihiro Fujii)

5 Interferometric searches for dark matter

Speaker: Yikun Wang

CIDM2024_YikunWang.pdf

6 A dark photon search with a gravitational wave detector and the effect of the relative motion of detectors

The search for dark matter using gravitational wave detectors is attracting significant attention. These detectors have extremely high sensitivity to small displacements, which could be used to detect interactions with ultralight dark matter. Different models predict that dark matter interacts with gravitational wave detectors through various mechanisms. This sensitivity to displacement could allow the detection of dark matter signals. In this study, we discuss methods to detect dark matter signals in data from gravitational wave detectors and how to set upper limits when no candidate signals are found. When estimating these limits, it is essential to account for the relative velocity between the detectors and dark matter. We propose an upper limit estimation method that incorporates this factor.

Speaker: Takumi Fujimori

CIDM_talk_202410_final.pdf

10:30 Break (Next session chaired by Wen Yin)

7 Bubble misalignment mechanism for axions

We study the dynamics of axions at first-order phase transitions in non-Abelian gauge theories. When the duration of the phase transition is short compared to the timescale of the axion oscillations, the axion dynamics is similar to the trapped misalignment mechanism. On the other hand, if this is not the case, the axions are initially expelled from the inside of the bubbles, generating axion waves on the outside. Analogous to the Fermi acceleration, these axions gain energy by repeatedly scattering off the bubble walls. Once they acquire enough energy, they can enter the bubbles. If the axion oscillations are relevant only inside the bubbles during the phase transition, the axion abundance is significantly enhanced compared to models where the axion mass is either constant or varies continuously as a function of temperature. The increase in axion abundance depends on the axion mass, the duration of the phase transition, and the bubble wall velocity. This mechanism results in a spatially inhomogeneous distribution of axions, which could lead to the formation of axion miniclusters. It has potential implications for the formation of oscillons/I-balls, axion warm dark matter, cosmic birefringence, and the production of dark photons.

Speaker: Junseok Lee

CIDM_Lee.pdf

8 nπ ambiguity of cosmic birefringence and its effect on ALP search

Recently, several papers have reported so-called 'Cosmic birefringence', which is a rotation of the direction of linear polarization of CMB. This might be a hint of new physics beyond standard models because the signal means large scale parity violation of this universe. The reported angles of the rotation are ~0.3 deg. However, we point out there is a nπ phase ambiguity for the angle. This ambiguity is trivial from the observational method to determine the angle, but has not been discussed seriously so far though it can impact on the origin of cosmic birefringence. We also discuss how to constrain the ambiguity.

Speaker: Fumihiro Naokawa

9 Multi-Field Oscillons in Real-FLS model

Oscillons are soliton-like localized configurations formed by real scalar fields. In the context of cosmology, it is predicted that oscillons are formed in inflationary models or axion models, and they are suggested to be the origin of gravitational waves or the seeds of primordial black holes. Typically, oscillons are studied in the context of a single real scalar field. However, the existence and nature of oscillons in systems with two or more interacting real scalar fields present an intriguing problem. Recently, such multi-field oscillons have been constructed using two-timing analysis. In this talk, we will apply the two-timing analysis and construct multi-field oscillons within our real-FLS model.

Speaker: Tasuya Ogawa

12:00 Photo session

12:10 Lunch

13:50 Break (Next session chaired by Masato Yamanaka)

10 Searches for wavelike dark matter utilizing superconducting qubits

A DFSZ axion search needs a detector that has an extreme sensitivity to photons. Due to its huge electric dipole moment and intrinsic low noise feature, superconducting qubits are an excellent candidate for the searches. In this talk, we introduce ways to utilize superconducting qubits in dark matter searches and these experimental statuses. Also, we mention a strategy for axion searches by applying magnetic field to superconducting qubits.

Speaker: Tatsumi Nitta

CIDM2024_TatsumiNitta.pdf

11 Current status of sensitivity improvement of Dark matter Axion search with riNg Cavity Experiment (DANCE)

Axion and Axion-Like Particles (ALPs) are one of the candidates of dark matter. Axion weakly interacts with photon, electron, proton and so on. Many experiments have been proposed by using the axion-photon conversion under magnetic fields. However, axion has not been observed yet. Our research group has proposed Dark matter Axion search with riNg Cavity Experiment (DANCE). DANCE aims to detect axion without using magnetic fields. The axion-photon interaction induces a rotation of linearly polarized light. We aim to detect the amplified rotation angle with a bow-tie optical ring cavity. In the prototype experiment with a bow-tie optical ring cavity with a round-trip of 1 m (DANCE Act-1), the reflection phase difference between s-polarization and p-polarization on the mirrors of the cavity was observed. This was due to oblique incidence on the mirrors, and we were not able to achieve simultaneous resonance, which is necessary to conduct a sensitive broadband axion search. Recently, we achieved simultaneous resonance by adding an auxiliary cavity to compensate for the reflection phase difference. However, the optical loss on the polarization beam splitter between a bow-tie optical ring cavity and an auxiliary cavity degrades the sensitivity to axion. Also, the measurement results of DANCE Act-1 revealed the time drift of the reflection phase difference between polarizations on the mirrors of the cavity. This makes it challenging to conduct an accurately sensitive axion search. An alternative approach to address these issues is to tune the reflection phase difference between polarizations by tuning laser wavelength. This approach achieves simultaneous resonance by canceling the reflection phase difference between polarizations when light is reflected on the mirrors. In this talk, I will report the detail of simultaneous resonance for DANCE.

Speaker: Hinata Takidera

20241016_CIDM2024_Takidera_v2.pdf

12 Visualizing high energy particles of extensive air showers with Subaru Hyper Supreme-Cam

Extensive air showers induced from high‐energy cosmic rays provide a window into understanding the most energetic phenomena in the universe. We report on visualizing high energy particles of these showers with the silicon imaging detector Subaru Hyper Suprime‐Cam. This method has the advantage of being able to measure individual secondary particles with unprecedented resolution and might be applicable for dark matter search. I will share an interdisciplinary project for combining the Subaru telescope and cosmic ray detectors to decipher details of extensive air showers, dubbed Air-shower Lensing Observatory at High Altitude (ALOHA).

Speaker: Toshihiro Fujii

241016_VisualizingEAS_CIDM_Fujii.pdf

15:20 Break (Next session chaired by Naoya Kitajima)

13 Isotropic cosmic birefringence from an oscillating axion-like field

We propose a new mechanism for isotropic cosmic birefringence with an axion-like field that rapidly oscillates during the recombination epoch. In conventional models, the field oscillation during the recombination epoch leads to a cancellation of the birefringence effect and significantly suppresses the EB spectrum of the cosmic microwave background (CMB) polarization. By introducing an asymmetric potential to the axion, this cancellation becomes incomplete, and a substantial EB spectrum can be produced. This mechanism also results in a washout of the EE spectrum, which can be probed in future CMB observations. Our findings suggest the possibility that an axion-like field responsible for isotropic cosmic birefringence can also account for a significant fraction of dark matter.

Speaker: Kai Murai

CIDM_Murai_OscBiref.pdf

14 Thermal productions of axion in DFSZ-type axion models

Axion is a strong candidate for dark matter and has several types of production mechanisms. While the misalignment mechanism has been well-known since long ago and is usually assumed, thermal productions are another attractive possibility. In this talk, we will discuss thermal productions of the axion in DFSZ-type axion models, which involve heavy additional Higgs bosons. Interestingly, in this setup, axion is predominantly produced from the heavy Higgs boson decays, assuming that the reheating temperature of the Universe is larger than the mass of the heavy Higgs bosons. This is a characteristic feature of the DFSZ-type models in the sense that this does not happen in KSVZ-type axion models. Focusing on the axion with a mass of keV to sub-GeV scale, we will discuss how cosmological observations such as X-ray and CMB constrain the model parameter space.

Speaker: Kodai Sakurai

Sakurai_0ct.16.pdf

15 ALP Dark Matter and Measuring its Abundance

Speaker: Joerg Jaeckel

Tohoku-JJ.pdf

17:10 Discussion

18:00 Banquet

Thursday 17 October

09:20 Break (Next session chaired by Yuta Michimura)

16 Axion Detection Experiments Meet the Majoron

The majoron is a well-motivated light (pseudo-Nambu-Goldstone) boson associated with the spon- taneous breaking of a global lepton-number symmetry. In this letter, we relate the spontaneous breaking scale and its soft-breaking mass by requiring that the majoron is the main component of the dark matter. An electromagnetic-anomalous coupling can be induced by minimally modi- fying the original majoron model, surprisingly, predicting a parameter region that largely overlaps with the QCD-axion dark matter band. Thus, we expect that axion search experiments meet the ma joron.

Speaker: Qiuyue Liang

CIDM_QiuyueLiang.pdf

10:10 Break (Next session chaired by Nagisa Hiroshima)

17 Recent updates on the morphology of the Galactic Center excess

The Galactic Center Excess (GCE) detected by Fermi-LAT resembles a signal of WIMP dark matter annihilation, although it may also be attributed to a population of millisecond pulsars in the inner Milky Way. I will discuss recent updates in studying the morphology of the GCE. I will show that the bulge model based on the latest VVV survey is consistently favored by data. I will also show that millisecond pulsars contribute to the gamma-ray sky in various region.

Speaker: Deheng Song

song.pdf

18 Dark matter on small scales

Dark matter is now known to be the vital ingredient for the growth of structure in the Universe, but its nature remains a mystery. Dark matter on the small mass scales, such as within galactic and sub-galactic structures, may well be the key to shedding light on fundamental properties of dark matter and new physics. In particular, revealing dark matter distributions in less massive galaxies is of crucial for testing dark matter models and constraining particle candidate of dark matter. In this talk, I will discuss the current efforts to constrain dark matter distributions in the Milky Way, dwarf spheroidals, and nearby galaxies through dynamical analysis of their currently available data. I will then discuss the future prospects for these dark matter studies.

Speaker: Kohei Hayashi

CosmicIndicators_20241017_Hayashi.pdf

11:30 Closing remarks and discussion (Fuminobu Takahashi)