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

                                                       Week 3

 

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

CETUP Menu 2nd Session Week One.docx

CETUP Menu 2nd Session Week Two.docx

SURF website

Mon, June 9 ¶

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

1 Dark Matter Workshop Welcome, Important Updates, Helpful Resources¶

Speaker: Stacie Granum (SDSTA/The Institute)

CETUP Welcome PPT 2025.pptx

2 Welcome and Updates from 9:00 - 9:30 a.m.¶

9:45 AM Break

3 TALK: A 6D Jeans Analysis of the Sagittarius Dwarf Spheroidal Core¶

Author and Speaker: Isabelle Goldstein
Abstract: The stellar kinematics in dwarf galaxies can provide a wealth of information about its underlying dark matter distribution. Line of sight velocity dispersion measurements from six classical dwarf galaxies can be used to show that axion-like particles with masses of order m ~ 10−22 eV are inconsistent with the potential distribution in classical dwarf galaxies unless the hierarchical assembly of the Milky Way did not trace the mean evolution of Milky Way size halos. However, line of sight velocity constraints alone are subject to degeneracies between central dark matter density and stellar velocity anisotropy.
Using Gaia DR3 data, we examine the kinematics of the central core of the Sagittarius (Sgr) dwarf spheroidal galaxy which includes proper motions and line-of-sight velocities for member stars in addition to their projected positions. We extract a sample of bright stars that are high-probability members of Sgr. We obtain a velocity anisotropy of βa=−2.24±1.99, which implies a system with tangentially-biased orbits. Proper motions and complete position information could be used to break the existing velocity anisotropy and central density degeneracy; however without accurate distances to these stars, a 6D Jeans analysis cannot be performed. We use new observations obtained with the Magellan/MIKE spectrograph to measure distances and line-of-sight velocities for RR Lyrae and red clump stars with the Sgr core to perform a full 6D Jeans analysis.

Goldstein_CETUP2025.pdf

4 Discussion, Collaborations, and Lunch at 12:00 p.m. in room 131¶

Lunch provided at the Elementary School

5 TALK: Phenomenology of forbidden dark matter decay¶

Author and Speaker: Debasish Borah
Abstract: The visible part of the present Universe is composed of matter or baryons only with negligible trace of antimatter. As the Universe is expected to start out with as much antimatter as matter, the present observation has led to the longstanding puzzle of baryon asymmetry of Universe. Another intriguing puzzle is the presence of non-luminous or dark matter in the present Universe contributing more than five times the visible matter to the total energy budget. This talk will discuss the impact of forbidden decays of particles in the early Universe enabled by finite-temperature effects on simultaneous generation of dark matter and baryon asymmetry. It will also touch upon additional phenomenological implications like gravitational waves, primordial black holes, large neutrino asymmetry etc. depending upon the particular model implementation.

dborah presentation.pdf

6 Discussion and Collaboration¶

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

Tue, June 10 ¶

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

7 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 Break

8 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 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

10 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.

11 Discussions and Collaborations¶

4:00 PM Travel to Hampton Inn or SLHVC (Via SURF Shuttle)

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

Wed, June 11 ¶

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

12 Deeper Talks: SURF Seminar Series (Robert McGehee)¶

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

Speaker: Robert McGehee (University of Minnesota)

10:00 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.

13 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

14 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.

2:00 PM Break

15 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.

16 Discussion and Collaboration¶

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

Thu, June 12 ¶

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

17 TALK: Probing Primordial Perturbations via CMB B-mode Polarization¶

Author: Tao Xu
Presenter: Tao Xu
Abstract: Primordial perturbations are a central target of cosmological observations, providing critical insights into the early universe and the theory of inflation. We propose using CMB B-mode polarization as a novel probe of curvature perturbations on scales $k\sim 1-100{\mathrm{M}\mathrm{p}\mathrm{c}}^{-1}$, a regime beyond the reach of traditional measurements. I will discuss the gravitational waves induced by primordial perturbations that affect CMB polarization, and the sensitivity of future CMB experiments to this signal.

TaoXu_CETUP2025.pdf

9:45 AM BREAK

18 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.

19 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

20 Communicating with Media 2.0¶

SURF Communications Team: Ann Metli and Mike Ray

21 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.

22 Discussion and Collaboration¶

4:15 PM Travel to Hampton Inn (Via SURF Shuttle)

23 Pub Talk + Trivia (prizes awarded)¶

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

Fri, June 13 ¶

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

24 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.

Speaker: Jason Kumar (University of Hawaii)

CETUP2025a Kumar updated.pdf

9:45 AM BREAK

25 Bridging the Gap: Communicating Cutting-Edge Science to Students¶

Speaker: Nicol Reiner (SURF E&O)

26 Discussion, Collaboration, Lunch (Lunch is at 12:00PM)¶

27 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.

Speaker: Raymond Co (Indiana University)

Nonlinear Dynamics and Dark Matter Abundance of a Light QCD Axion.pdf

1:45 PM BREAK

28 Deadwood Alive! Gunslinger Show at 2:00 p.m. (optional)¶

located across the street from the elementary school and one block down at Outlaw Square outdoor event space.

2:30 PM BREAK

3:30 PM Travel to Hampton Inn (Via SURF Shuttle)

Mon, June 16 ¶

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

29 Dark Matter Workshop Welcome and Updates¶

Speaker: Stacie Granum (SDSTA/The Institute)

CETUP Welcome PPT 2025.pptx

9:30 AM Break

30 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.

31 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

32 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 BREAK

33 TALK: A 'Dark' Matter Perspective on KM3-230213A¶

Authors: Bhupal Dev (Washington University in St. Louis)
Bhaskar Dutta (Texas A&M University), Aparajitha Karthikeyan, Writasree Maitra (Washington University in St. Louis), Louie Strigari (Texas A&M University), Ankur Verma (Texas A&M University)
Presenter: Aparajitha Karthikeyan
Abstract: The recent KM3NeT observation of the O(100 PeV) event KM3-230213A is puzzling because IceCube, with a much larger effective area and exposure, has not found any such events. In this talk, we will present a novel solution to this conundrum in terms of dark matter (DM) scattering in the Earth's crust. We show that intermediate dark-sector particles that decay into muons are copiously produced when high-energy (∼100 PeV) DM propagates through a sufficient amount of Earth overburden. To address the non-observation of similar events at IceCube, we will demonstrate via two examples of weakly coupled long-lived dark sector scenarios that are sourced from a high-luminosity blazar. We calculate the corresponding dark sector cross sections, lifetimes, and blazar luminosities required to yield one event at KM3NeT, satisfy all the lab-based constraints, and also predict the number of IceCube events for these parameters that can be tested very soon.

CETUP2025_AKarthikeyan_builds.pdf

34 Discussion and Collaboration¶

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

Tue, June 17 ¶

35 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 underground will have a free day to explore the area or continue collaborations at their leisure.

36 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.

37 SURF Overview¶

SURF Overview-CETUP-2025_06_17-Rev3.pdf

38 Safety Training and Waivers (Passports as required)¶

39 SURF Underground Tour Lunch¶

40 SURF Underground Tour PPE, Cage down Yates at 11:30AM¶

41 SURF Underground Tour¶

42 Return to Surface and Return PPE¶

43 Travel to Hampton Inn Hotel (via SURF shuttle)¶

Wed, June 18 ¶

44 Travel to Sanford Lab Homestake Visitors Center¶

45 Deep Roots: Tawney Brunsch with Lakota Funds, a Native CDFI on Pine Ridge¶

46 Travel to Ethnobotanical Garden¶

47 Explore/Walk the Garden¶

48 Travel Back to Lead/Deadwood Elementary School¶

49 Lunch¶

50 TALK: Ab Initio Nuclear Calculations for Dark Matter-Nucleus and Neutrino-Nucleus Scattering¶

Author and Speaker: Baishan Hu
Abstract: Ab Initio Nuclear Calculations for Dark Matter-Nucleus and Neutrino-Nucleus Scattering
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.

1:45 PM Break

51 TALK: Observational Signatures of Cosmological Stasis¶

Authors: Brooks Thomas, Keith R. Dienes, Lucien Heurtier, Daniel Hoover, Fei Huang, Anna Paulsen, Tim M. P. Tait
Presenter: Brooks Thomas
Abstract: Cosmological stasis is a phenomenon wherein the abundances of multiple cosmological energy components with different equations of state remain constant for an extended period despite the expansion of the universe. In this talk, I discuss the possible observational implications of this phenomenon. These include characteristic imprints in the stochastic gravitational-wave background and an enhanced growth of perturbations in the density of matter on small scales.

CETUP-2025-40-min.pdf

2:45 PM Break

52 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.

3:45 PM Break

4:00 PM Travel to Hampton Inn

Thu, June 19 ¶

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

53 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 BREAK

54 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.

55 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

Lunch provided at Middle School.

56 TALK: Scalar Relics from the Big Bang¶

Author and Presenter: 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 ex- periments 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 interac- tions, 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 trans- mutation, 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.

1:45 PM BREAK

57 TALK: Shedding Infrared Light on QCD Axion and ALP Dark Matter with JWST¶

Author and Presenter: Ranjan Laha
Abstract: James Webb Space Telescope (JWST) has opened up a new chapter in infrared astronomy. Be- sides 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.

58 Discussion and Collaboration¶

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

59 Pub Talk + Trivia (prizes awarded)¶

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

CETUP-science-funding-outreach-2025-30-min.pdf

Fri, June 20 ¶

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

60 Student Day: Introductions¶

61 Career Panel (Brooks, Pearl, Ryan, Christopher, Dylan, Baishan)¶

Speakers: Baishan Hu (Texas A&M University), Prof. Brooks Thomas (Lafayette College), Christopher Capiello, Dylan Temples (Fermilab), Pearl Sandick (University of Utah), Ryan Linehan (Fermi National Accelerator Laboratory)

10:30 AM BREAK

62 Scientist Mentor/Student Speed Match Up and Shadow¶

63 Lunch with Students¶

Lunch provided at Middle School.

64 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.

Leptogenesis.pdf

65 Discussion and Collaboration - Students Shadow¶

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

Mon, June 23 ¶

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

Tue, June 24 ¶

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

Wed, June 25 ¶

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

Thu, June 26 ¶

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

Fri, June 27 ¶

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

Mon, June 30 ¶

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

66 Registration in Lobby, Welcome in Room 132¶

67 Neutrino Workshop Welcome, Important Updates, Helpful Resources¶

Speaker: Stacie Granum (SDSTA/The Institute)

9:45 AM Break

68 TALK: Effective field theory for radiative corrections to charged-current processes: neutron decay, Vud, and gA. Hadronic uncertainty in neutral currents¶

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 effective 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 products 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.
I also refine the treatment of hadronic uncertainties in low-energy neutral-current processes, significantly reducing the current error estimate. These improvements have direct implications for all neutral-current interactions at low energies, including parity-violating electron scattering, elastic (anti)neutrino-electron scattering, coherent elastic (anti)neutrino-nucleus scattering, and atomic parity violation.

Speaker: Dr Oleksandr Tomalak

Tomalak_talk_CETUP_2025.pdf

69 TALK: Revisiting Reactor Anti-Neutrino 5 MeV Bump with 13C Neutral-Current Interaction¶

Speaker: Seodong Shin
Abstract: For the first time, we comprehensively examine the potential of a neutral current interaction of reactor neutrino with
C
emitting a 3.685 MeV photon to identify the origin of the 5 MeV bump in reactor antineutrino spectra observed through the inverse beta decay (IBD) process. This anomaly may be due to new physics, reactor antineutrino flux inaccuracies, or IBD systematics.
The 3.685 MeV photon released during the de-excitation of
C to its ground state is observable in
liquid scintillator detectors. Remarkably, we confirm the powerfulness of our proposal by completely ruling out a new physics scenario explaining the bump from the existing NEOS data. We also explore the potential of current and forthcoming experiments, including solar neutrino studies at JUNO, pion and muon decay-at-rest experiments at OscSNS, and isotope decay-at-rest studies at Yemilab, to measure the cross section precisely enough to distinguish the expected bump and the theoretical flux models via our channel.

Speaker: Seodong Shin (Jeonbuk National University)

CETUP25.pdf

70 Discussion, Collaborations, and Lunch (Lunch is at 12:00PM)¶

71 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.

Speaker: Valentina De Romeri (IFIC (CSIC/UV))

De_Romeri_CETUP.pdf

72 TALK: Mass from Angular Scanning¶

Speaker Jong-Chul Park

Speaker: Jong-Chul Park (Chungnam National University)

AngularScanning_CETUP2025_pdf.pdf

73 Discussion and Collaboration¶

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

Tue, July 1 ¶

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

74 TALK: Minimal Non-Abelian Flavor Symmetry and Neutrino Oscillations¶

Author: Zurab Tavartkiladze
Abstract: Aiming to explore an extension of the Standard Model, that incorporates non-Abelian flavor symmetry, we will examine the potential for a framework that does not require flavon states. Our proposed model leads to a highly economical and predictive lepton sector. The neutrino oscillations and other implications will be also discussed.

Speaker: Zurab Tavartkiladze (Ilia State University)

2025.07.01-Tavartkiladze-CETUP-talk-1.pdf

2025.07.01-Tavartkiladze-CETUP-talk-1.pptx

9:45 AM BREAK

75 TALK: Hyper-K¶

Volodymyr Takhistov

Speaker: Voloymyr Takhistov (QUP, KEK)

CETUP2025_HK_Takhistov.pdf

76 Talk: Addressing Short-Baseline Neutrino Excesses via Photon Signatures¶

Author: Doojin Kim
Abstract: The MiniBooNE low-energy excess remains one of the most prominent anomalies in neutrino experiments, with recent MicroBooNE results reporting a mild excess in the single-photon channel. We propose new scenarios involving light dark matter and/or neutrinos that can simultaneously explain both the MiniBooNE and MicroBooNE excesses. Our framework introduces photons produced via 2-to-3 scattering processes between neutrinos or dark matter and nuclei, mediated by light particles. We identify viable regions in parameter space consistent with current constraints and highlight that these scenarios can be probed by upcoming experimental data.

Speaker: Doojin Kim (University of South Dakota)

Presentation_CETUP2025_DoojinKim.pdf

77 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

78 TALK: High-quality axions from vertical and horizontal symmetries¶

Speaker: Vasja Susič (LNF, INFN)

cetup2025_susic_v2.pdf

79 TALK: Ab Initio Nuclear Calculations for Neutrino-Nucleus Scattering¶

Speaker: Baishan Hu

Speaker: Baishan Hu (Texas A&M University)

CETUP_neutrino_BaishanHu.pdf

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

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

Wed, July 2 ¶

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

80 TALK: Neutrino-Dark Matter Connection¶

Author and Presenter: Bhupal Dev
Abstract: Do neutrinos interact with Dark Matter (or dark sector, in general)? We study various cosmological, astrophysical and laboratory observables that can address this question. We show that neutrino-dark sector interactions can also resolve some tensions in cosmology and astrophysics.

Speaker: Bhupal Dev (Washington University in St. Louis)

Dev_CETUP_070225.pptx

9:45 AM BREAK

81 TALK: Status and Plan for DAMSA, a Novel Dark Messenger Search Experiment¶

Speaker: Jaehoon Yu

Speaker: Jaehoon Yu (University of Texas at Arlington)

damsa-net-cetup-070225.pptx

82 TALK: Decoupling Neutrino Magnetic Moment from Mass with SU(2)L Invariance¶

Author: Anil Thapa
Abstract: Standard Model extensions that yield observable neutrino magnetic moments typically also induce large neutrino masses, incompatible with experimental limits. This tension motivates the search for mechanisms that naturally decouple magnetic moments from mass generation without requiring fine-tuning. In this talk, I will propose a novel mechanism for generating Dirac and Majorana neutrino magnetic moments, in which the associated mass contributions are forbidden by $SU(2{)}_L$ invariance. By carefully selecting the $SU(2{)}_L$ representations connecting to the loop diagram, we ensure that only the effective dipole operator involving the non-Abelian part of the photon -- the neutral gauge boson -- is generated. Crucially, the corresponding mass diagram, obtained by removing the external gauge boson leg, vanishes. We provide explicit UV completions that implement this mechanism and yield neutrino magnetic moments as large as from TeV-scale new physics.

Speaker: Anil Thapa (Colorado State University)

NMM_anil.pdf

83 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

84 Communicating with Media 2.0¶

SURF Communications Team: Ann Metli and Mike Ray

SURF Media Training-CETUP-2025 .pdf

85 Discussion and Collaboration¶

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

Thu, July 3 ¶

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

86 TALK: Gravitational waves and neutrino masses in conformal models¶

Danny Marfatia

Speaker: Danny Marfatia

MajoronNanoGrav.pdf

9:45 AM BREAK

87 TALK: Measuring the Cosmic Ray Spectrum with Next-Generation Neutrino Detectors¶

Author: Stephan Meighen-Berger
Abstract: In this talk, we will discuss how upcoming kiloton-scale neutrino detectors, like Hyper-Kamiokande, can be used to measure the primary cosmic ray spectrum. Unlike traditional balloon or satellite missions that offer limited spatial and temporal coverage, large neutrino detectors provide full-sky monitoring over extended periods. By analyzing the atmospheric neutrinos produced in cosmic ray interactions, we show that these detectors can distinguish between competing models of the cosmic ray spectrum, even in the presence of uncertainties in neutrino cross sections and hadronic cascades. This is achieved by using a new method for reconstructing the primary cosmic ray spectrum from neutrino data, reducing flux uncertainties from ~20% to just 7%. This improved precision not only enhances our understanding of cosmic rays but also potentially boosts sensitivities of key neutrino studies, such as oscillation parameters. As an example, I will discuss a hypothetical sin²θ₂₃ measurement and how the reduction of the cosmic ray uncertainty can potentially double Hyper-K's precision. These results demonstrate how neutrino observatories are poised to play a central role in advancing both cosmic ray and neutrino physics.

Speaker: Stephan Meighen-Berger (The University of Melbourne)

CETUP_2025.pdf

88 TALK: THE SUN SHINES ON EVERYTHING: Probing Solar Neutrinos at Dark Matter Detectors¶

Speaker: Nityasa Mishra
Abstract: Solar neutrinos provide a powerful probe of neutrino physics at dark matter detectors. Their low thresholds and large exposures enable precise measurements of neutrino scattering. Future directional detectors will add sensitivity by leveraging the solar origin of the signal to distinguish new physics from backgrounds. Together, these experiments offer a novel path to explore both Standard Model and beyond-Standard Model neutrino properties.

Speaker: Nityasa Mishra (Texas A&M university)

CETUP.pptx

89 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

90 TALK: Neutrino Mass and Parity¶

In this talk, I will discuss how parity relates to neutrino mass. I will discuss two types of models: the left-right symmetric model and mirror symmetric model. In the former, we will look at neutrino mass, the associated low scale phenomenology as well as a new mass bound on right-handed gauge boson. In the latter, we will see how quasi(pseudo)-Dirac neutrinos arise and investigate the connection to baryon asymmetry and dark matter.

Speaker: Chee Sheng Fong (Universidade Federal do ABC)

Fong_CETUP25_sh.pdf

91 Talk: Entanglement of Astrophysical Neutrinos¶

Speaker: Baha Balantekin

CETUP2025.pptx

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

92 Pub Talk + Trivia (prizes awarded)¶

CETUP Participant Talk and Physics Trivia (Related to Neutrinos)

Baha Balantekin - Science Talk

Adrian Thompson - Neutrino Physics Trivia

Speakers: Adrian Thompson (Northwestern University), Baha Balantekin

Fri, July 4 ¶

8:00 AM Enjoy Holiday Festivities! U.S. Independence Day! (No Workshop Programming)

Click the link below for holiday activities:
https://www.blackhillsbadlands.com/events/events/independence-day/4th-of-july-calendar/

Mon, July 7 ¶

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

93 Registration/Sign-In (lobby)¶

94 Neutrino Workshop Welcome, Important Updates, and Helpful Resources¶

Speaker: Stacie Granum (SDSTA/The Institute)

95 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.

Speaker: Shirley Li (UC Irvine)

10:30 AM Break

96 TALK: Low-Scale Quark-Lepton Unification in a Pati-Salam Framework¶

We propose a $E_6$-inspired Pati-Salam (PS) model that naturally accommodates multi-TeV leptoquark gauge bosons, $X_{\mu }$, while incorporating a softly broken $Z_2$ symmetry. Standard Model (SM) fermions are $Z_2$-even in this framework, whereas exotic fermions are $Z_2$-odd. An interesting feature of the model is that the PS gauge bosons are $Z_2$-odd, enabling them to couple exclusively between ordinary and exotic fermions, except in the right-handed down-type sector, where mixing arises due to the soft breaking of $Z_2$. This structure leads to helicity suppression of meson decays at the tree level, with unsuppressed contributions appearing only at the one-loop level, which allows a lower PS breaking scale. Such a scale offers exciting collider prospects, particularly for probing leptoquark gauge bosons, and the distinctive signature of vector-like down-type quark carrying a fractional baryon number of $\pm 2/3$.

Speaker: Sumit Biswas (Oklahoma State University)

97 Discussion, Collaboration, and Lunch (Lunch is at 12:00PM)¶

98 TALK: New Physics Solutions to the LSND and MiniBooNE Anomalies After Recent MicroBooNE Results¶

Author and Presenter: Rajesh Gandhi
Abstract: Recent results from MicroBooNE have significantly constrained the possible new physics solutions to the LSND and MiniBooNE anomalies. I will review the current theoretical and experimental situation vis a vis these anomalies and briefly point to the future possibilities for BSM physics.

Speaker: Rajesh Gandhi (Harish Chandra Research Institute)

99 Talk: TBD¶

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

Tue, July 8 ¶

100 REMINDER: SURF UNDERGROUND TOUR DAY - pick up at 8:30AM MT¶

Participants going on the underground tour will follow this schedule.

Participants not going underground will have a free day to explore the area or continue collaborations at their leisure.

101 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.

102 SURF Overview¶

103 Safety Training and Waivers (Passports as required)¶

104 SURF Underground Tour Lunch¶

105 SURF Underground Tour PPE, Cage down Yates at 11:30AM¶

106 SURF Underground Tour¶

107 Return to Surface and Return PPE¶

108 Travel to Hampton Inn Hotel (via SURF Shuttle)¶

Wed, July 9 ¶

109 Travel to Sanford Lab Homestake Visitors Center¶

110 Deeper Talks: Solar Neutrinos: History and Observations¶

Speaker: Aldo Ianni (Laboratori Nazionali del Gran Sasso)

111 Travel to Ethnobotanical Garden¶

112 Guest Speaker at Ethnobotanical Garden¶

Speaker: Rylan Sprague (Mount Rushmore National Memorial)

113 Travel to Lead/Deadwood Elementary School (via SURF Shuttle)¶

114 Lunch at Elementry School¶

115 TALK: Interplay of Nuclear and New Physics with Low-Energy Neutrino Sources¶

Author: Vishvas Pandey
Abstract: Low-energy neutrino sources, such as those from stopped pion or core-collapse supernova, interact with target nuclei in detectors through either coherent elastic or inelastic scattering processes. These interactions provide valuable insights into various Standard Model and Beyond the Standard Model phenomena, with significant implications for nuclear physics, particle physics, and astrophysics. The precision of coherent elastic scattering, where the nucleus remains in its ground state, depends on the accuracy of the underlying weak form factor of the nucleus. In contrast, inelastic scattering, where neutrinos excite the target nucleus to low-lying nuclear states, involves complex nuclear structures and dynamics and are quite poorly constrained. In this talk, I will present an overview of the field, highlight recent advancements, and outline future directions.

Speaker: Vishvas Pandey (Fermilab)

116 TALK: On the asymmetric distribution of decay products of heavy fermions¶

Speaker: Takuya Okawa
Abstract: The question of whether neutrinos are Dirac or Majorana remains open. This is mainly because almost all of the accessible neutrinos, such as laboratory neutrinos and neutrinos of astrophysical origin, are ultra-relativistic, erasing signatures that distinguish Dirac from Majorana neutrinos. We thus consider heavy neutrinos and discuss the possibility of distinguishing their Dirac versus Majorana nature. In particular, we allow a heavy neutrino to decay into another neutrino and an intermediate particle, which subsequently decays into the Standard Model particles. Then, we analyze the angular distribution of decay products for both Dirac and Majorana heavy neutrinos.

Speaker: Takuya Okawa (Washington University in St. Louis)

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

117 CETUP* Social hosted by Hampton Inn Lead¶

Thu, July 10 ¶

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

118 TALK: Does the 220 PeV Event at KM3NeT Point to New Physics?¶

Speaker Vedran Bridar
Abstract: The KM3NeT collaboration recently reported the observation of KM3-230213A, a neutrino event with an energy of 220 PeV, nearly an order of magnitude more energetic than the highest-energy neutrino in IceCube's catalog. Despite its larger effective area and longer data-taking period, IceCube has not observed events of similar energies which implies a 2–3σ tension, depending on the type of neutrino source. The 220 PeV neutrino detected at KM3NeT traversed approximately 147 km through rock and sea, whereas neutrinos from the same location in the sky would cross only about 14 km of ice to reach IceCube. In this talk, I will show how this difference in propagation distance helps to resolve this tension. Specifically, I will present a scenario where the source emits sterile neutrinos that partially convert to active neutrinos via oscillations. I will discuss two mechanisms: one where a new-physics matter potential induces a resonance in sterile-to-active transitions, and another involving off-diagonal neutrino non-standard interactions. In both cases, oscillations over 100 km enhance the active neutrino flux at KM3NeT with respect to the flux at IceCube.

Speaker: Vedran Brdar (Oklahoma State University)

9:45 AM Break

119 Bridging the Gap: Communicating Cutting-Edge Science to Students¶

education research focus.

Speakers: Ashley Armstrong, Julie Dahl

11:00 AM Break

120 Talk: Supernova Gamma-Ray Constraints from Radiative Particle Decays¶

Author: Garv Chauhan

Speaker: Garv Chauhan (Virginia Tech)

121 Discussion, Collaboration and Lunch at 12:00pm¶

122 Talk: Hints of New Physics from the KM3NeT and ANITA Anomalies¶

Author: Dibya S. Chattopadhyay
Co-author: Vedran Brdar
Abstract: The KM3NeT collaboration recently reported the observation of KM3-230213A, a neutrino event with an energy of 220 PeV. The absence of any
PeV events in IceCube, despite its larger effective area and longer data-taking period, suggests an anomaly, with a tension quantified between approximately ~2 and 3.5, depending on the assumed source model. This implies a possible new physics origin for the event KM3-230213A.
Meanwhile, the anomalous upgoing events detected by the ANITA experiment, with energies near 1 EeV and arrival angles implying traversal through thousands of kilometers of Earth, similarly hint at a possible origin involving new physics in the neutrino sector.
We investigate two mechanisms that could simultaneously account for both anomalies: one in which a new matter potential induces a resonance in sterile-to-active neutrino transitions, and another involving off-diagonal neutrino non-standard interactions. Using the arc lengths traversed by the ANITA events, we identify the relevant parameter space and explore how matter-enhanced oscillations between the sterile and active sectors may help explain both the ANITA and KM3NeT observations. Overall, we examine the possibility that recent ultra-high-energy neutrino observations have already observed physics beyond the Standard Model.

Speaker: Dibya Sankar Chattopadhyay (Oklahoma State University)

123 Talk: Electroweak Precision with Muon Collider Neutrinos¶

Presenter: Adrian Thompson
Abstract: The standard candles of electroweak observables can be studied through the lens of neutrino-electron scattering as a purely weak process. We project the sensitivity of a neutrino detector situated around 100 meters away in the plane of a high energy muon storage ring or muon collider with , 1.5, and 5 TeV muon beam energies, providing a highly energetic and highly intense source of electron and muon (anti)neutrinos. We find world-leading sensitivity to the weak couplings at the sub-percent level is possible, with sensitivity to the Standard Model prediction for the neutrino charge radius. Finally, we show that sensitivity to the momentum transfer dependence of at the level, within a single dataset and configuration of the proposed experiment, is possible.

Speaker: Adrian Thompson (Northwestern University)

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

124 Pub Talk + Trivia (prizes awarded)¶

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

Fri, July 11 ¶

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

125 Student Day: Introductions¶

126 Career Panel¶

10:30 AM Break

127 Scientist Mentor/Student Speed Match Up and Show¶

128 Discussion, Collaboration, and Lunch with Students (Lunch at 12:00pm)¶

students shadow during discussion and collaboration

129 TALK: Signatures of quasi-Dirac neutrinos in diffuse high-energy astrophysical neutrino data¶

Speaker: Yago Porto (ABC Federal University)

130 TALK: Modeling prompt atmospheric lepton fluxes with intrinsic charm contribution¶

Speaker: Diksha Garg
Abstract: The all-sky very-high-energy (–GeV) atmospheric muon flux has been measured by IceCube. The higher end of this energy range is expected to come from the prompt component. IceCube also measures the atmospheric muon neutrino flux at high energies; however, due to the dominant contribution from astrophysical sources, it is only able to place an upper limit on the prompt atmospheric muon neutrino flux. In this work, we present a new evaluation of the prompt atmospheric muon flux, incorporating for the first time an intrinsic charm component in the colliding nucleons. The inclusion of intrinsic charm enhances the forward production of hadrons such as, and, which subsequently decay into muons and muon neutrinos. We demonstrate that the intrinsic charm contribution leads to an increase in both the prompt muon and muon neutrino fluxes. To model intrinsic charm production, we consider the Regge-based ansatz that is implemented within the MCEq framework for lepton flux calculations. Finally, we explore the challenges in reconciling predictions that simultaneously match IceCube’s measured atmospheric muon flux and its upper bound on the prompt muon neutrino flux.

Speaker: DIKSHA GARG (The University of Iowa)

4:00 PM Travel to Hampton Inn, Quick break before Reception

131 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.

132 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 Neutrino Day (CETUP participants are welcome and encouraged to volunteer for science panel and other activities!)