CETUP* 2025

Jun 9, 2025, 2:00 AM → Jul 12, 2025, 5:00 PM US/Mountain

Lead/Deadwood Middle School

Barbara Szczerbinska (Texas A&M University - Corpus Christi), Bhaskar Dutta (Texas A&M University), Jaret Heise (SDSTA/SURF), K.S Babu (Oklahoma State University), Louie Strigari (Texas A&M University)

CETUP* 2025

Special Note to CETUP* Participants:  If you are interested in attending the Particle Physics and Cosmology Conference (PPC) this summer please register soon to take advantage of the lower registration fee. The registration fee will go up by 100 USD after the deadline. CLICK HERE FOR INFORMATION ABOUT PPC 2025.

 

SEE "WORKSHOP ANNOUNCEMENTS" IN THE LEFT NAVIGATION FOR WORKSHOP UPDATES. 

 

The Institute for Underground Science at SURF hosts the Center for Theoretical Underground Physics and Related Areas workshop, located in the beautiful Black Hills of South Dakota. 

 

CETUP* Mission:

To promote organized research in physics, cosmology and astrophysics, geoscience, and other fields related to science done in underground laboratories worldwide via individual and collaborative research in a dynamic atmosphere of intense scientific interactions.

 

Why CETUP*: 

With over 20 underground laboratories around the world hosting experiments in nuclear and particle physics, astrophysics, cosmology, and geosciences, there is a growing global interest in underground science. The Center for Theoretical Underground Physics and Related Areas (CETUP*) responds to this need by bringing together scientists from various disciplines, both theoretical and experimental, at its annual workshop.

 

CETUP* creates an inclusive, stimulating environment that promotes creative thinking and open discussions. Researchers from different backgrounds, experience levels, and countries collaborate to address critical questions in fundamental research. This collaborative spirit helps to nurture the next generation of scientists while driving progress in multiple fields.

 

Since 2011, CETUP* has taken place in the breathtaking Black Hills of South Dakota, nestled in the historic towns of Lead and Deadwood, near the Sanford Underground Research Facility (SURF)—the deepest underground lab in the U.S. This stunning location, enriched by deep Native American cultural and historical roots, offers a truly unique and inspiring backdrop for our workshop.

 

NOTE:  Up to two weeks of lodging and a modest per diem will be provided. There is no registration fee for CETUP* participants, however, registration is required.  

Previous Workshops:

• CETUP* 2024: Dark Matter, Neutrino Physics
• CETUP* 2023: Dark Matter, Neutrino Physics
• CETUP* 2016: Physics and Instrumentation of the Near Detector for the Long-Baseline Neutrino Experiment, From Grand Unification to String Theory and Back, Dark Matter
• CETUP* 2015: Dark Matter, Neutrino Physics (nuclear and particle physics), Particle Physics and Cosmology
• CETUP* 2014: Neutrino Interactions, Systematic Uncertainties, Near Detector Physics
• CETUP* 2013: Dark Matter, Neutrino Physics, Astrophysics, Particle Physics and Cosmology
• CETUP* 2012: Dark Matter, Neutrino Physics, Grand Unification
• CETUP* 2011: Geo-neutrinos, Neutrino Physics, Grand Unification

 

PLEASE NOTE: 

The Particle Physics and Cosmology 2025 Conference (PPC) is also happening consecutively with CETUP* and being held in Deadwood, South Dakota this year, from June 23 - 27. Registration is separate from CETUP*. For more information, please go to the Indico event page.

 

1. Video About The Institute at SURF

2. The Institute at SURF website

3. Video About SURF

4. Video of things to do in the Black Hills area

5. Neutrino Day 2024 recap video

SURF website

Mon, June 9 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary School (Via SURF Shuttle)

9:00 AM → 9:30 AM Dark Matter Workshop Welcome, Important Updates, Helpful Resources, and Group Photo¶

Speaker: Stacie Granum (SDSTA/The Institute)

9:30 AM → 9:45 AM SURF and The Institute for Underground Science Overview and Update¶

9:45 AM → 10:00 AM Break

10:00 AM → 10:45 AM TALK: Scalars Relics From the Hot Big Bang¶

Author and Speaker: David Cyncynates
Abstract: Motivated by the unexplained origins of dark matter and the cosmological constant, fifth-force experiments provide an important avenue to address major open questions in physics. These experiments take place at low energies, probing interactions among atoms, nucleons, or electrons in atomic energy levels, and are agnostic to the UV origin of any new force. However, such interactions, if present, lead to dynamics in the early Universe that can have cosmological implications. In this talk, I will compute the effect of the early Universe plasma on the scalar field, accounting for the full structure of the Standard Model—spontaneous symmetry breaking, dimensional transmutation, and the running of gauge couplings. We will see that the resulting relic abundance of the fifth-force-carrying scalar field is largely independent of how it couples to the Standard Model, ultimately pointing to a cosmologically preferred region of experimental parameter space.

10:45 AM → 2:00 PM Discussion, Collaborations, and Lunch¶

Lunch provided at the Middle School.

2:00 PM → 2:45 PM TALK: Shedding Infrared Light on QCD Axion and ALP Dark Matter with JWST¶

Author and Speaker: Ranjan Laha
Abstract: James Webb Space Telescope (JWST) has opened up a new chapter in infrared astronomy. Besides the discovery and a deeper understanding of various astrophysical sources, JWST can also uncover the non-gravitational nature of dark matter (DM). If DM is QCD axion or an eV-scale Axion-like particle (ALP), it can decay into two photons in the infrared band. This will produce a distinct line signature in the spectroscopic observations made by JWST. Using the latest NIRSpec IFU spectroscopic observations from JWST, we put the strongest bound on the photon coupling for QCD axion/ ALP DM in the mass range between 0.47 and 2.55 eV. In particular, we are able to probe a new mass range for ALP DM between ∼ 0.47 eV to 0.78 eV beyond what can be probed by globular cluster observations. We constrain well-motivated and UV complete models of QCD axion and ALP DM, including predictions from some models derived from string theory and/ or various Grand Unification scenarios. Future JWST observations of DM-rich systems with a better understanding of the astrophysical and instrumental backgrounds can thus enable us to potentially discover QCD axion and ALP DM.

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Tue, June 10 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary School (Via SURF Shuttle)

9:00 AM → 9:45 AM TALK: The MAGIS-100 Experiment and a Future Kilometer-scale Atom Interferometer¶

Author and Presenter: Dylan Temples
Abstract: The dearth of signals unambiguously attributable to WIMP dark matter motivates exploring new parameter space, particularly the ultra-light dark matter (ULDM) regime, where the signal is not scattering events but wave phenomena. The proliferation of quantum technologies has enabled searches for ULDM at previously inaccessible sensitivity. One such technology is atom interfer- ometry which can measure time-dependent fluctuations in the energy spacing of atoms as well as in the light-travel time across the apparatus, enabling searches for ULDM and gravitational waves, respectively. In this talk, I will review the science case for long baseline atom interferometers, such as MAGIS-100 at Fermilab, provide an update on the experiment’s status, and discuss the need for a future, kilometer-scale atom interferometer which would achieve unprecedented sensitivity to ULDM and gravitational waves in the “Mid-Band”region between LIGO and LISA.

9:45 AM → 10:00 AM Break

10:00 AM → 10:45 AM TALK: Terahertz-Radiometer for Axions (T-RAX)¶

Author and Presenter: Tao Xu
Abstract: Axions, originally proposed to solve the strong CP problem, are a well-motivated dark matter candidate. While many experiments have searched for axion dark matter across a broad mass range, the meV mass region remains less explored. In this talk, I will introduce the Terahertz- Radiometer for AXions (T-RAX)—a proposed experiment designed to search for meV axion dark matter through its coupling to photons. T-RAX aims to detect surface radiation signals via the Primakoff effect from novel epsilon-near-zero metamaterials operating at THz frequencies. Lever- aging recent developments in semiconductor quantum structures, the detector features a compact design and electromagnetically tunable plasma frequencies. I will present the current status of the T-RAX proposal and show simulation results demonstrating its potential to probe previously unconstrained regions of axion dark matter parameter space.

10:45 AM → 2:30 PM Discussion, Collaboration, and Lunch¶

Lunch provided at the Middle School.

2:30 PM → 3:15 PM TALK: Inelastic Dark Matter Freeze-In and Indirect Detection¶

Author and Presenter: Douglas Tuckler
Abstract: Inelastic dark matter is a well-motivated benchmark for freeze-out and freeze-in production. In the freeze-in regime, if the mass splitting between the two dark matter states is small enough, the heavy dark matter state can be cosmologically long-lived and makes up half of the DM abundance at present time. If the mass splitting is lower than an MeV, the heavier dark matter state can only decay to photons and generates an indirect detection signal that can be observed with X-ray telescopes. In this talk, we consider inelastic dark matter with a dark photon mediator such that the heavier state decays to three photons. This photon spectrum can be detected by X-ray telescopes such as INTEGRAL/SPI, and we will show that indirect detection can access parameter space of dark photons that is currently unconstrained by other experiments.

3:15 PM → 4:30 PM Discussions and Collaborations¶

4:30 PM → 5:00 PM Travel to SLHVC (Via SURF Shuttle)

5:00 PM → 6:30 PM CETUP* Social - workshop participants, families and staff invited!

Wed, June 11 ¶

8:30 AM → 9:00 AM Travel to SLHVC (Via SURF Shuttle)

9:00 AM → 10:00 AM Deeper Talks: SURF Seminar Series (CETUP* speaker)¶

The Institute for Underground Science and SURF is proud of its researcher community and this series aims to strengthen the sense of intellectual community. It provides a platform for researchers to discuss their work, share insights, and foster interdisciplinary connections.

Topic and Speaker(s) to be determined

10:00 AM → 10:30 AM Travel Back to School (Via SURF Shuttle)

The SURF shuttle will pick participants up at the Visitor Center (front entrance) and travel back to the Lead-Deadwood Elementary school.

10:30 AM → 12:45 PM Discussion, Collaboration, and Lunch¶

12:45 PM → 1:30 PM TALK: Dark Matter Catalyzed Baryon Destruction¶

Authors: Yohei Ema, Robert McGehee, Maxim Pospelov
Presenter: Robert McGehee
Abstract: WIMP-type dark matter may have additional interactions that break baryon number, leading to induced nucleon decays which are subject to direct experimental constraints from proton decay experiments. In this talk, we analyze a possibility of continuous baryon destruction, deriving strong limits from the dark matter accumulating inside old neutron stars, as such a process leads to excess heat generation. We construct the simplest particle dark matter model that breaks baryon and lepton numbers separately but conserves B − L. Virtual exchange by DM particles in this model results in di-nucleon decay via nn → nν¯ and np → ne+ processes.

1:30 PM → 1:45 PM Break

1:45 PM → 2:30 PM TALK: Exploring Low-Energy Microphysics Relevant to Particle Sensing with Quantum Devices¶

Author and Presenter: Ryan Linehan
Abstract: The search for low-mass dark matter and coherent neutrino scattering has placed an emphasis on developing particle detectors with energy thresholds below 1 eV. As this energy scale is below the electronic bandgap for common detector materials, low-threshold detection largely relies on the ability to sense phononic excitations in cryogenic devices, often using superconducting thin film sensor architectures. To confidently use these phonon-sensing architectures for detection, it is imperative to understand the low-energy microphysical response of both the substrate and superconductor to particle impacts. This challenge is compounded by the increasing adoption of ultra-sensitive superconducting quantum sensor architectures, whose susceptibility to on-chip en- vironmental noise motivates dedicated exploration of the microphysical systems producing this noise. In this talk, we discuss aspects of this low-energy response that are relevant to operation of superconducting quantum sensors in a detection mode, and the HEP-inspired tools being devel- oped to model and characterize them.

2:30 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel Back to Hampton Inn (Via SURF Shuttle)

Thu, June 12 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary School (Via SURF Shuttle)

9:00 AM → 9:45 AM TALK: Can the LHC be Sensitive to Light Dark Mediators?¶

Author: Deepak Sathyan
Co-Authors: Bhaskar Dutta, Aparajitha Karthikeyan, Doojin Kim, Hyunyong Kim
Presenter: Deepak Sathyan
Abstract: We propose a novel method to obtain sensitivity to dark mediators and dark sectors at the LHC with masses of ∼ 10 MeV − 10 GeV, providing complementarity with short baseline beam dump experiments. For this talk, we consider dark photons, which can be produced at the LHC from neutral meson decays, bremsstrahlung off baryons, or directly produced in correlation with a jet. We then consider visible decays to muon pairs as the signal channel and provide methods to control backgrounds. We show a range of sensitivities dependent on various estimates of backgrounds and different signal threshold requirements.

9:45 AM → 10:00 AM BREAK

10:00 AM → 10:45 AM TALK: Loosely Bound Composite Dark Matter¶

Author and Presenter: Joe Bramante
Abstract: It has long been appreciated that dark matter may reside in composite states. However, there are a number of simple composite dark matter models still being uncovered. I will some detection prospects and model considerations for loosely bound composite dark matter, where the binding energy of constituent particles is small relative to the constituent mass.

10:45 AM → 1:00 PM Discussion, Collaboration, and Lunch¶

Lunch will be provided at the Middle School

1:00 PM → 2:30 PM Communicating with Media 2.0¶

SURF Communications Team: Ann Metli and Mike Ray

2:30 PM → 3:15 PM TALK: Primordial Gravitational Waves from Phase Transitions During Reheating¶

Author and Presenter: Fazlollah Hajkarim
Abstract: We study primordial gravitational waves (GWs) generated from first-order phase transitions (PTs) during cosmic reheating. Using a minimal particle physics model, with a general parametrization of the inflaton energy density and the evolution of the Standard Model temperature, we explore the conditions under which PTs occur and determine the corresponding PT parameters. We find that, in certain cosmological scenarios, PTs can be delayed and prolonged compared to the standard post-inflationary evolution. Finally, incorporating these PT parameters, we compute the resulting GW spectrum while accounting for the uncertainties related to cosmic reheating.

3:15 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

8:00 PM → 10:00 PM Pub Talk + Trivia (prizes awarded)¶

CETUP* participant talk and physics trivia related to Dark Matter (prizes awarded)

Fri, June 13 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary School (Via SURF Shuttle)

9:00 AM → 9:45 AM TALK: Dark Matter Phase Space Distributions: Simulations, Observations and Calculations¶

Author and Presenter: Jason Kumar
Abstract: We consider three broad approaches to determining the phase space distribution of dark matter in a halo: numerical simulations, Jeans modeling using stellar kinematic data, and analytic analysis. We investigate the advantages and limitations of these approaches, and the extent to which they provide complementary information. We discuss the impact of these results on dark matter indirect detection searches.

9:45 AM → 10:00 AM BREAK

10:00 AM → 11:00 AM Bridging the Gap: Communicating Cutting-Edge Science to Students¶

Speaker: Nicol Reiner (SURF E&O)

11:00 AM → 2:00 PM Discussion, Collaboration, Lunch¶

Lunch not provided. Please use per diem cards.

2:00 PM → 2:45 PM TALK: Nonlinear Dynamics and Dark Matter Abundance of a Light QCD Axion¶

Author and Presenter: Raymond Co
Abstract: We investigate the field dynamics of the ZN QCD axion, a variant of the QCD axion that couples to N copies of the Standard Model. Contributions from N − 1 dark sectors and the visible sec- tor QCD lead to an exponentially suppressed axion mass and a time-dependent periodic potential. The potential minimum is at θ = π before the QCD phase transition. After the phase transition, this point becomes a hilltop and multiple minima develop with only one of them actually solving the strong CP problem. The resultant non-trivial field dynamics, such as rotations over potential barriers and oscillations from the hilltop, give rise to parametric resonance production of axions. We perform the first lattice simulations of the axion field evolving through the QCD phase transi- tion in an expanding universe. We find that nonlinear effects significantly impact the axion’s relic abundance and final settling point. We show the viable parameter space in which this light QCD axion can simultaneously constitute all of dark matter and solve the strong CP problem.

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Mon, June 16 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary School (Via SURF Shuttle)

9:00 AM → 9:30 AM Dark Matter Workshop Welcome, Important Updates, Helpful Resources, and Group Photo¶

Speaker: Stacie Granum (SDSTA/The Institute)

9:30 AM → 9:45 AM SURF and The Institute for Underground Science Overview and Update¶

9:45 AM → 10:00 AM Break

10:00 AM → 10:45 AM TALK: Enhanced Dark Matter Abundance from First-Order Phase Transitions¶

Author and Speaker: Rouzbeh Allaverdi
Abstract: I discuss a novel scenario to obtain the correct relic abundance for thermally under-produced dark matter. This scenario utilizes a strongly first-order phase transition that gives rise to dark matter mas. Freeze-out in the broken phase can yield the desired abundance in the entire region currently allowed by observational bounds and theoretical constraints. The accompanying gravitational waves are strong enough to be detected by many upcoming and proposed experiments. This, in tandem with dark matter indirect searches, provides a multi-messenger probe of such models. Positive signals in the future can help reconstruct the potential governing the phase transition and shed light on an underlying particle physics realization.

10:45 AM → 2:00 PM Discussion, Collaboration, and Lunch¶

Lunch provided at the Middle School.

2:00 PM → 2:45 PM TALK: Ab Initio Nuclear Calculations for Dark Matter-Nucleus and neutrino-Nucleus Scattering¶

Author and Speaker: Baishan Hu
Abstract: Over the past decades, ab initio nuclear calculations have made dramatic progress, especially reaching heavy mass nuclei such as 208Pb [1]. This means that it becomes possible to obtain first-principles computation (with quantified uncertainties) of quantities that even reside in the heavy-mass region. The quantities include these relevant for astrophysics and searches for physics beyond the Standard Model. In this talk, I will present a conceptual introduction to modern ab initio nuclear theory. Then, I will focus on recent advances in ab initio calculations of nuclear re- sponses for dark matter-nucleus [2] and neutrino-nucleus elastic and inelastic scattering. Finally, I will present our recent investigation of the ATOMKI anomaly using ongoing proton beam dump neutrino experiments [3].
[1]. Ab initio predictions link the neutron skin of 208Pb to nuclear forces. B.S. Hu, et al. Nat. Phys. 18, 1196 (2022). arXiv:2112.01125v1 (2021).
[2]. Ab initio structure factors for spin-dependent dark matter direct detection. B.S. Hu, et al. Phys. Rev. Lett. 128, 072502 (2022). arXiv:2109.00193.
[3]. A novel investigation of the ATOMKI anomaly. B. Dutta, W.C. Huang, B.S. Hu, R.G. Van de Water. arXiv:2410.17968.

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Tue, June 17 ¶

8:00 AM → 8:15 AM REMINDER: SURF UNDERGROUND TOUR DAY - pick at 8:30 a.m. MT¶

Participants going on the underground tour will follow this schedule. Participants not going on the tour will have other activities to participate in at the Middle School. More information will follow.

Those not going on the underground tour will have the option to attend a Hoist Room tour.

8:30 AM → 9:00 AM Pickup at Hampton Inn and Travel to SURF for Underground Tour (via SURF shuttle)¶

Underground Tour participants (please read below)

If you are a foreign national, you will be required to show your passport before going underground and complete a SURF Access Request Form.

Anyone entering the underground must be 18 years or older, must complete safety training, and sign an Acknowledgement of Risk and Release, Agreement Not to Sue and Waiver.

Temperatures are in the low- to mid-70s on the 4,850-foot level.

SURF will provide personal protective equipment (coveralls, hardhats, cap lamps, safety glasses, etc.). For safety purposes, we require tour guests to wear clothing that is appropriate at a construction site: full-length pants or jeans, shirt with sleeves (at least ¼ length) and sturdy, closed-toe shoes, and socks. Restrooms are available underground. Cameras are welcome.

Your underground visit may require walking up to one mile, sometimes over uneven ground. All those who are going underground must be able to perform the following activities:

Don and wear the required PPE.
Don and use a self-rescuer.
Walk in both warm/hot and humid conditions.
Walk across uneven or slippery surfaces for distances in excess of one mile.
Tolerate standing in very close proximity to others while riding in the personnel cage.
Tolerate changes in elevation.
Recognize and respond to emergency signals and signs (visual, auditory, and olfactory).
Travel to egress points unassisted, and under their own power.
Ascend and descend three flights of stairs.

9:00 AM → 9:30 AM SURF Overview¶

9:30 AM → 10:15 AM Safety Training and Waivers (Passports as required)¶

10:15 AM → 11:00 AM SURF Underground Tour Lunch¶

11:00 AM → 11:45 AM SURF Underground Tour PPE, Cage down Yates at 11:30AM¶

11:45 AM → 3:30 PM SURF Underground Tour¶

3:30 PM → 4:00 PM Return to Surface and Return PPE¶

4:00 PM → 4:30 PM Travel to Hampton Inn Hotel (via SURF shuttle)¶

Wed, June 18 ¶

9:30 AM → 10:00 AM Travel to Sanford Lab Homestake Visitors Center¶

10:00 AM → 11:00 AM Deep Roots: Tawney Brunsch with Lakota Funds, a Native CDFI on Pine Ridge¶

11:00 AM → 11:15 AM Travel to Ethnobotanical Garden¶

11:15 AM → 11:45 AM Explore/Walk the Garden¶

11:45 AM → 12:00 PM Travel Back to Lead/Deadwood Elementary School¶

12:00 PM → 1:00 PM Lunch¶

1:00 PM → 1:45 PM TALK: The Radio Synchrotron Background - New Particle Processes?¶

Author and Speaker: Jack Singal
Abstract: It has become apparent that the background brightness level of diffuse radio emission on the sky and its level of anisotropy is significantly higher than those which can result from known classes of astrophysical radio sources. In contrast to the more well-known photon backgrounds at microwave, infrared, optical/UV, X-ray, and gamma-ray wavelengths, where the levels of brightness and anisotropy at least roughly match those expected from known cosmological and astrophysical sources, the "radio synchrotron background" at radio wavelengths provides clear motivation for considering new sources and new particle-based emission mechanisms, including those from the dark sector. This talk will summarize the current understanding of the radio synchrotron background and some of the proposed particle-based emission mechanisms.

1:45 PM → 2:00 PM Break

2:00 PM → 2:45 PM TALK: A Dark Inferno Melting Earth's Core¶

Authors: Christopher Cappiello and Tansu Daylan
Presenter: Christopher Cappiello
Abstract: The search for dark matter is one of the crucial open problems in both particle physics and cosmol- ogy. If dark matter scatters with Standard Model particles, it could accumulate inside the Earth and begin to annihilate, producing heat within the Earth’s core. While past work has been done on the effect that this heat would have once it reached the surface, we model the flow of heat through the Earth’s core by numerically solving the heat equation to model dark matter’s effect on the interior of the planet. We compute how long it takes for the core to come into thermal equilibrium and show that for a wide range of dark matter parameters, a substantial fraction of the inner core would be melted by dark matter annihilation. Our analysis produces new limits on dark matter annihilating in the Earth, points out important new effects that must be considered when studying planetary heating by dark matter, and suggests new dark matter observables that could be searched for in exoplanet populations.

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn

Thu, June 19 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:45 AM TALK: Indirect Detection of Hot Dark Matter¶

Author and Presenter: Pearl Sandick
Abstract: Cosmologically stable, light particles that came into thermal contact with the Standard Model in the early universe may persist today as a form of hot dark matter. For relics with masses in the eV range, their role in structure formation depends critically on their mass. We trace the evolution of such hot relics and derive their density profiles around cold dark matter halos, introducing a framework for their indirect detection. Applying this framework to axions — a natural candidate for a particle that can reach thermal equilibrium with the Standard Model in the early universe and capable of decaying into two photons — we establish stringent limits on the axion-photon coupling using current observations of dwarf galaxies, the Milky Way halo, and galaxy clusters.

9:45 AM → 10:00 AM BREAK

10:00 AM → 10:45 AM TALK: Primordial Black Holes as Dark Sector Factories¶

Author and Presenter: Jae Hyeok
Abstract: In this talk, I present the potential use of primordial black holes (PBHs) as probes of the dark sector. Through Hawking radiation, black holes emit all particle species with masses below their Hawking temperature, providing a unique and gravitationally universal production mechanism. PBHs can reach Hawking temperatures of up to tens of MeV, enabling the emission of dark sector particles with masses up to this energy scale. By analyzing the gamma-ray spectrum from PBHs, we can probe dark sector particles that produce observable photon signals. Moreover, by studying the mass distribution of evaporating PBHs, it may be possible to access even heavier dark sector particles, including those without any direct couplings to the visible sector.

10:45 AM → 2:00 PM Discussion, Collaboration, and Lunch¶

Lunch provided at Middle School.

2:00 PM → 2:45 PM TALK: Multi-Messenger Probes of Leptophilic Dark Matter¶

Author and Presenter: Debasish Borah
Abstract: We propose a multi-messenger frontier probe of leptophilic dark matter (DM) by considering an effective field theory (EFT) setup. Adopting an EFT approach, we write down dimension six op- erators connecting the standard model lepton (SM) fields and DM. Considering DM relic to be generated via either thermal freeze-out or UV freeze-in, we check the discovery prospects at fu- ture lepton colliders as well as direct and indirect detection frontiers. While non-thermal produc- tion of DM during an extensive reheating phase after inflation has interesting gravitational wave signatures, such leptophilic DM scenario can also lead to observable dark radiation at cosmic mi- crowave background (CMB) experiments if light neutrinos in the standard model are of Dirac type. The interplay of existing bounds and future sensitivities from cosmological observations related to DM relic, direct and indirect detection of DM, astrophysics, gravitational waves, CMB and lepton colliders leave promising discovery prospects of such leptophilic DM at multi-messenger frontiers.

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

8:00 PM → 10:00 PM Pub Talk + Trivia (prizes awarded)¶

CETUP* participant talk and physics trivia related to Dark Matter (prizes awarded)

Fri, June 20 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:30 AM Student Day: Introductions¶

9:30 AM → 10:30 AM Career Panel¶

10:30 AM → 10:45 AM BREAK

10:45 AM → 12:00 PM Scientist Mentor/Student Speed Match Up and Shadow¶

12:00 PM → 1:30 PM Lunch with Students¶

Lunch provided at Middle School.

1:30 PM → 2:15 PM TALK New Ideas for Leptogenesis¶

Authors: Peisi Huang, Tao Xu, Kairui Zhang
Presenter: Peisi Huang
Abstract: In this talk, I will discuss two new mechanisms for leptogenesis. In the first scenario, we introduce a temperature-dependent coupling between the right-handed neutrino and Standard Model parti- cles. This coupling experiences suppression at high temperatures and becomes sizable when the lepton asymmetry washout processes are Boltzmann-suppressed. Such a feature ensures that the washout rates remain consistently below the Hubble expansion rate, preserving all lepton asymme- try generated in the decay of right-handed neutrinos. In the second scenario, We explore flavored resonant leptogenesis embedded in a neutrinophilic 2HDM. Successful leptogenesis is achieved by the very mildly degenerate two heavier right-handed neutrinos~(RHNs) N2 and N3 with a level of only ΔM32/M2∼(0.1%−1%). The lightest RHN, with a MeV-GeV mass, lies below the sphaleron freeze-out temperature and is stable, serving as a dark matter candidate. The model enables TeV- scale leptogenesis while avoiding the extreme mass degeneracy typically plagued conventional resonant leptogenesis. Baryon asymmetry, neutrino masses, and potentially dark matter relic den- sity can be addressed within a unified, experimentally testable framework.

2:15 PM → 4:00 PM Discussion and Collaboration - Students Shadow¶

4:00 PM → 4:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Mon, June 23 ¶

8:00 AM → 5:00 PM Particle Physics and Cosmology Conference (separate registration)

Tue, June 24 ¶

8:00 AM → 5:00 PM Particle Physics and Cosmology Conference (separate registration)

Wed, June 25 ¶

8:00 AM → 5:00 PM Particle Physics and Cosmology Conference (separate registration)

Thu, June 26 ¶

8:00 AM → 5:00 PM Particle Physics and Cosmology Conference (separate registration)

Fri, June 27 ¶

8:00 AM → 5:00 PM Particle Physics and Cosmology Conference (separate registration)

Sat, June 28 ¶

8:00 AM → 12:00 PM Particle Physics and Cosmology Conference (separate registration)

Mon, June 30 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:30 AM Neutrino Workshop Welcome, Important Updates, Helpful Resources, and Group Photo¶

Speaker: Stacie Granum (SDSTA/The Institute)

9:30 AM → 9:45 AM SURF and The Institute for Underground Science Overview and Update¶

9:45 AM → 10:00 AM Break

10:00 AM → 10:45 AM TALK: Effective Field Theory for Radiative Corrections to Charged-Current Processes: Neutron Decay and VUD¶

Author and Presenter: Oleksandr Tomalak
Abstract: We study radiative corrections to low-energy charged-current processes involving nucleons, such as neutron beta decay and (anti)neutrino-nucleon scattering within a top-down effective-field- theory approach. First, we match the Standard Model to the low-energy effective theory valid below the weak scale, specifying the scheme dependence of the Wilson coefficients. We evolve the resulting effective coupling down to the hadronic scale using renormalization group equations. To evaluate radiative corrections at scales of the neutron decay, we perform matching to heavy- baryon chiral perturbation theory and subsequently, below the pion-mass scale, to a pionless ef- fective theory, evolving the effective couplings all the way down to the scale of the electron mass, relevant for beta decay. We provide a representation for hadronic corrections in terms of infrared finite convolutions of simple kernels with the single-nucleon matrix elements of time-ordered prod- ucts of two and three quark bilinears (vector, axial-vector, and pseudoscalar). Using our new result for the radiative corrections, we update the extraction of the largest Cabibbo-Kobayashi-Maskawa matrix element Vud from the neutron decay.

10:45 AM → 2:00 PM Discussion, Collaborations, and Lunch¶

2:00 PM → 2:45 PM TALK: TBD¶

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Tue, July 1 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:45 AM TALK: Standard Model and Beyond the Standard Model Perspectives on Coherent Elastic Neutrino-Nucleus Scattering¶

Author and Presenter: Valentina De Romeri
Abstract: In this talk, I will discuss the physics potential of coherent elastic neutrino-nucleus scattering (CEvNS), a neutral-current process in which a neutrino scatters off an entire nucleus. I will first briefly review the main features of CEvNS and the status of current observations. Then, I will examine how these measurements have enabled a broad range of physics applications, from preci- sion tests of the Standard Model to probes of new physics, with particular relevance to dark matter direct detection experiments.

9:45 AM → 10:00 AM BREAK

10:00 AM → 10:45 AM TALK: TBD¶

10:45 AM → 2:00 PM Discussion, Collaboration, and Lunch¶

2:00 PM → 2:45 PM TALK: TBD¶

2:45 PM → 4:30 PM Discussion and Collaboration¶

4:30 PM → 5:00 PM Travel to SLHVC (Via SURF Shuttle)

5:00 PM → 7:00 PM CETUP* Social - workshop participants, families and staff invited!

Wed, July 2 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:45 AM TALK: TBD¶

9:45 AM → 10:00 AM BREAK

10:00 AM → 10:45 AM TALK: TBD¶

10:45 AM → 1:00 PM Discussion, Collaboration, and Lunch¶

1:00 PM → 2:30 PM Communicating with Media 2.0¶

SURF Communications Team: Ann Metli and Mike Ray

2:30 PM → 3:15 PM TALK: TBD¶

3:15 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Thu, July 3 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:45 AM TALK: TBD¶

9:45 AM → 10:00 AM BREAK

10:00 AM → 10:45 AM TALK: TBD¶

10:45 AM → 2:00 PM Discussion, Collaboration, and Lunch¶

2:00 PM → 2:45 PM TALK: TBD¶

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

8:00 PM → 10:00 PM Pub Talk + Trivia (prizes awarded)¶

CETUP Participant Talk and Physics Trivia (Related to Neutrinos)

Fri, July 4 ¶

8:00 AM → 4:00 PM Enjoy Holiday Festivities! U.S. Independence Day!

Mon, July 7 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:30 AM Neutrino Workshop Welcome, Important Updates, Helpful Resources, and Group Photo¶

Speaker: Stacie Granum (SDSTA/The Institute)

9:30 AM → 9:45 AM The Institute for Underground Science at SURF Update and Overview¶

9:45 AM → 10:00 AM Break

10:00 AM → 10:45 AM TALK: What's the Wave Packet Size of Neutrinos?¶

Author and Presenter: Shirley Lie
Abstract: Standard calculations of neutrino oscillation are predicated on the assumption that neutrinos’ wave packets maintain coherence throughout their propagation. Effects associated with neutrino wave packet decoherence—specifically, damping of the oscillation probabilities—were previously con- sidered unobservable in terrestrial experiments. However, recent claims suggest that if sterile neu- trinos exist, we could observe decoherence effects in terrestrial experiments. To test these claims, one must compute the neutrino wave packet size for a given source. In this talk, I will discuss our efforts to determine the wave packet size for neutrinos produced in accelerator-based experi- ments. We demonstrate that it is feasible to compute this value through a well-defined framework accompanied by precise input parameters.

10:45 AM → 2:00 PM Discussion, Collaboration, and Lunch¶

2:00 PM → 2:45 PM TALK: TBD¶

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel Back to Hampton Inn (Via SURF Shuttle)

Tue, July 8 ¶

8:00 AM → 8:15 AM REMINDER: SURF UNDERGROUND TOUR DAY - pick up at 8:30AM MT¶

8:30 AM → 9:00 AM Pickup at Hampton Inn and Travel to SURF for Underground Tour (via SURF shuttle)¶

Underground Tour participants (please read below)

If you are a foreign national, you will be required to show your passport before going underground and complete a SURF Access Request Form.

Anyone entering the underground must be 18 years or older, must complete safety training, and sign an Acknowledgement of Risk and Release, Agreement Not to Sue and Waiver.

Temperatures are in the low- to mid-70s on the 4,850-foot level.

SURF will provide personal protective equipment (coveralls, hardhats, cap lamps, safety glasses, etc.). For safety purposes, we require tour guests to wear clothing that is appropriate at a construction site: full-length pants or jeans, shirt with sleeves (at least ¼ length) and sturdy, closed-toe shoes, and socks. Restrooms are available underground. Cameras are welcome.

Your underground visit may require walking up to one mile, sometimes over uneven ground. All those who are going underground must be able to perform the following activities:

Don and wear the required PPE.
Don and use a self-rescuer.
Walk in both warm/hot and humid conditions.
Walk across uneven or slippery surfaces for distances in excess of one mile.
Tolerate standing in very close proximity to others while riding in the personnel cage.
Tolerate changes in elevation.
Recognize and respond to emergency signals and signs (visual, auditory, and olfactory).
Travel to egress points unassisted, and under their own power.
Ascend and descend three flights of stairs.

9:00 AM → 9:30 AM SURF Overview¶

9:30 AM → 10:15 AM Safety Training and Waivers (Passports as required)¶

10:15 AM → 11:00 AM SURF Underground Tour Lunch¶

11:00 AM → 11:45 AM SURF Underground Tour PPE, Cage down Yates at 11:30AM¶

11:45 AM → 3:30 PM SURF Underground Tour¶

3:30 PM → 4:00 PM Return to Surface and Return PPE¶

4:00 PM → 4:30 PM Travel to Hampton Inn Hotel (via SURF Shuttle)¶

Wed, July 9 ¶

8:30 AM → 9:00 AM Travel to Sanford Lab Homestake Visitors Center¶

9:00 AM → 10:00 AM Deeper Talks: SURF Seminar Series (CETUP speaker)¶

10:00 AM → 10:30 AM Travel to Ethnobotanical Garden¶

10:30 AM → 11:30 AM Guest Speaker at Ethnobotanical Garden¶

Speaker: Rylan Sprague (Mount Rushmore National Memorial)

11:30 AM → 12:00 PM Travel to Lead/Deadwood Elementary School (via SURF Shuttle)¶

12:00 PM → 1:00 PM Lunch at Middle School¶

Lunch provided at Middle School.

1:00 PM → 1:45 PM TALK: TBD¶

1:45 PM → 2:00 PM Break

2:00 PM → 2:45 PM TALK: TBD¶

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Thu, July 10 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:45 AM Talk: TBD¶

9:45 AM → 10:00 AM Break

10:00 AM → 11:00 AM Bridging the Gap: Communicating Cutting-Edge Science to Students¶

education research focus.

Speakers: Ashley Armstrong, Julie Dahl

11:00 AM → 2:00 PM Discussion, Collaboration, Lunch¶

2:00 PM → 2:45 PM Talk: TBD¶

2:45 PM → 5:00 PM Discussion and Collaboration¶

5:00 PM → 5:30 PM Travel to Hampton Inn (Via SURF Shuttle)

8:00 PM → 10:00 PM Pub Talk + Trivia (prizes awarded)¶

CETUP* participant talk and physics trivia related to Dark Matter (prizes awarded)

Fri, July 11 ¶

8:30 AM → 9:00 AM Travel to Lead-Deadwood Elementary (Via SURF Shuttle)

9:00 AM → 9:30 AM Student Day: Introductions¶

9:30 AM → 10:30 AM Career Panel¶

10:30 AM → 10:45 AM Break

10:45 AM → 12:30 PM Scientist Mentor/Student Speed Match Up and Show¶

12:30 PM → 2:00 PM Lunch with Students¶

2:00 PM → 2:45 PM TALK: TBD¶

2:45 PM → 4:00 PM Discussion and Collaboration - Students Shadow¶

4:00 PM → 4:30 PM Break (SURF Shuttle will pick up at Hotel for Kick-Off Reception)

4:30 PM → 5:00 PM Travel to Sanford Lab Homestake Visitor Center (via SURF Shuttle)¶

Pick up at Hampton Inn Hotel. Participants and accompanying family and friends welcome to take the SURF shuttle to the visitor center.

5:00 PM → 7:00 PM Neutrino Day Kick-Off Reception¶

private reception to kick-off the annual Neutrino Day Community-wide Science Festival (participants and accompanying family and friends are welcome)

Sat, July 12 ¶

8:30 AM → 4:30 PM Neutrino Day (CETUP participants are welcome and encouraged to volunteer for science panel and other activities!)