We consider complex, supersymmetric, non-extremal Euclidean black holes that are asymptotically locally AdS , with $\textit{S}$ × $\textit{M}$ conformal boundary. We study field theory backgrounds consisting of various $\textit{M}$ , and explicitly construct Killing spinors that are anti-periodic around the Euclidean time circle. Focussing on elliptically/biaxially squashed three-spheres and Lens spaces, we compute the supersymmetric index of the 𝒩 = 4 SYM in a Cardy-like limit. While such black holes have not been constructed for general $\textit{M}$ , we demonstrate that the supersymmetric indices can be recovered from gravity computations using equivariant localization, by extending the boundary Killing spinors to the bulk. We show that this involves gluing the black hole geometry with a supersymmetric, horizonless AlAdS geometry, chosen such that the Casimir energy is removed from the supersymmetric partition function.

United Kingdom

Jaeha Park

Localizing AlAdS5 black holes and the SUSY index on $\textit{S}$ 1 $\textit{× M}$ 3

<p>Radio pulses generated by cosmic-ray air showers can be used to reconstruct key properties like the energy and depth of the electromagnetic component of cosmic-ray air showers. Radio detection threshold, influenced by natural and anthropogenic radio background, can be reduced through various techniques. In this work, we demonstrate that convolutional neural networks (CNNs) are an effective way to lower the threshold. We developed two CNNs: a classifier to distinguish radio signal waveforms from background noise and a denoiser to clean contaminated radio signals. Following the training and testing phases, we applied the networks to air-shower data triggered by scintillation detectors of the prototype station for the enhancement of IceTop, IceCube’s surface array at the South Pole. Over a four-month period, we identified 554 cosmic-ray events in coincidence with IceTop, approximately five times more compared to a reference method based on a cut on the signal-to-noise ratio. Comparisons with IceTop measurements of the same air showers confirmed that the CNNs reliably identified cosmic-ray radio pulses and outperformed the reference method. Additionally, we find that CNNs reduce the false-positive rate of air-shower candidates and effectively denoise radio waveforms, thereby improving the accuracy of the power and arrival time reconstruction of radio pulses.</p>

United States

R. Abbasi

Germany

M. Ackermann

New Zealand

J. Adams

S.K. Agarwalla

Belgium

J.A. Aguilar

Denmark

M. Ahlers

J.M. Alameddine

S. Ali

N.M. Amin

K. Andeen

C. Argüelles

Y. Ashida

S. Athanasiadou

S.N. Axani

R. Babu

X. Bai

J. Baines-Holmes

A. Balagopal V.

S.W. Barwick

S. Bash

V. Basu

R. Bay

J.J. Beatty

J. Becker Tjus

P. Behrens

Sweden

J. Beise

C. Bellenghi

B. Benkel

S. BenZvi

D. Berley

Italy

E. Bernardini

D.Z. Besson

E. Blaufuss

L. Bloom

S. Blot

I. Bodo

F. Bontempo

J.Y. Book Motzkin

C. Boscolo Meneguolo

S. Böser

O. Botner

J. Böttcher

J. Braun

B. Brinson

Canada

Z. Brisson-Tsavoussis

Australia

R.T. Burley

D. Butterfield

M.A. Campana

K. Carloni

J. Carpio

S. Chattopadhyay

N. Chau

Z. Chen

D. Chirkin

S. Choi

B.A. Clark

A. Coleman

P. Coleman

G.H. Collin

D.A. Coloma Borja

A. Connolly

J.M. Conrad

R. Corley

D.F. Cowen

C. De Clercq

J.J. DeLaunay

D. Delgado

T. Delmeulle

S. Deng

P. Desiati

K.D. de Vries

G. de Wasseige

T. DeYoung

J.C. Díaz-Vélez

S. DiKerby

M. Dittmer

A. Domi

L. Draper

L. Dueser

D. Durnford

K. Dutta

M.A. DuVernois

T. Ehrhardt

L. Eidenschink

A. Eimer

P. Eller

E. Ellinger

D. Elsässer

R. Engel

H. Erpenbeck

W. Esmail

S. Eulig

J. Evans

P.A. Evenson

K.L. Fan

K. Fang

Japan

K. Farrag

A.R. Fazely

Taiwan

A. Fedynitch

N. Feigl

Identification and denoising of radio signals from cosmic-ray air showers using convolutional neural networks

We consider M-theory on the backgrounds $$ {\mathrm{AdS}}_4\times {S}^7/{\mathbb{Z}}_{N_f} $$ and AdS × $\textit{S}$ /ℤ , which have fixed point loci AdS × $\textit{S}$ for $\textit{d}$ = 3, 6. These theories are holographically dual to certain CFTs in $\textit{d}$ = 3, 6 with eight supercharges. We compute the bulk cubic couplings between graviton KK modes and gluon KK modes living on the fixed points of these theories, which are generically extremal. We use these couplings to compute the graviton exchange term that appears in the strong coupling expansion of holographic correlators of gluon KK modes 〈22$\textit{pp}$〉 in these theories, and check that it matches the expected flat space limit. We express the answer in terms of a new reduced correlator solution to the superconformal Ward identities, which we derive for all CFTs with eight supercharges in 3 ≤ $\textit{d}$ ≤ 6.

Shai Chester

Rishi Mouland

Jesse Muiden

Clément Virally

Extremal couplings and gluon scattering in M-theory

The existence of a large extra dimension in which only gravity propagates would have spectacular consequences for cosmology and laboratory experiments. In the strong coupling limit of the $\textit{E}$ × $\textit{E}$ heterotic string theory, the gauge and matter fields live at the end of the eleventh dimension, which becomes a natural candidate for a micron-size $\textit{dark dimension}$. In this work, however, we show that the length of the M-theory interval is severely constrained by proton decay searches. Our results indicate that in such constructions the size of the eleventh dimension is $\textit{R}$ ≲ 𝒪(10 ) meters.

Switzerland

Mario Reig

Ignacio Ruiz

The dark dimension, proton decay, and the length of the M-theory interval

Using data samples collected by the Belle and Belle II experiments at the Υ(4$\textit{S}$) resonance with integrated luminosities of 571 fb and 365 fb , respectively, we measure the pseudoscalar $\textit{B}$-meson mass difference to be $\textit{m}$($\textit{B}$ ) − $\textit{m}$($\textit{B}$ ) = (0$\textit{.}$495 ± 0$\textit{.}$024 ± 0$\textit{.}$005) MeV/$\textit{c}$ . The results are based on a simultaneous fit to the variable $${\overline{M} }_{bc}$$ , which is related to the $\textit{B}$ momentum, for $\textit{B}$ and $\textit{B}$ candidates; and to the energy dependence of $$\mathcal{R}=\sigma ({e}^{+}{e}^{-}\to {B}^{0}{\overline{B} }^{0}) / \sigma ({e}^{+}{e}^{-}\to {B}^{+}{B}^{-})$$ , which is measured using changes in the average center-of-mass energy over the data taking periods. The phase-space hypothesis $$\mathcal{R}={({p}_{{B}^{0}} /{p}_{{B}^{+}})}^{3}$$ , upon which previous measurements rely, is strongly disfavored by our fit; the measured mass-difference value for the phase-space hypothesis also differs significantly from our measurement. We constrain $$\mathcal{R}$$ in a broader energy range than covered by the direct measurement and extract the energy dependence of $$\mathcal{R}$$ in the range from the $$B\overline{B }$$ threshold up to 10.59 GeV. We interpret the results using a phenomenological model and constrain the parameters of the $$B\overline{B }$$ potential in the isovector channel.

M. Abumusabh

I. Adachi

L. Aggarwal

H. Ahmed

Y. Ahn

H. Aihara

N. Akopov

S. Alghamdi

M. Alhakami

A. Aloisio

N. Althubiti

K. Amos

N. Anh Ky

C. Antonioli

D. Asner

H. Atmacan

T. Aushev

R. Ayad

V. Babu

N. Baghel

S. Bahinipati

P. Bambade

Sw. Banerjee

M. Barrett

M. Bartl

J. Baudot

A. Beaubien

F. Becherer

J. Becker

J. Bennett

F. Bernlochner

V. Bertacchi

M. Bertemes

E. Bertholet

M. Bessner

S. Bettarini

V. Bhardwaj

F. Bianchi

T. Bilka

D. Biswas

D. Bodrov

A. Bondar

G. Bonvicini

J. Borah

A. Boschetti

A. Bozek

M. Bračko

P. Branchini

R. Briere

T. Browder

A. Budano

S. Bussino

Q. Campagna

M. Campajola

G. Casarosa

C. Cecchi

P. Chang

P. Cheema

L. Chen

B. Cheon

C. Cheshta

H. Chetri

K. Chilikin

J. Chin

K. Chirapatpimol

H.E. Cho

K. Cho

S.J. Cho

S.K. Choi

S. Choudhury

S. Chutia

J. Colorado-Caicedo

Measurements of the mass difference $\textit{m}$($\textit{B}$ 0) $\textit{− m}$($\textit{B}$ +) and the energy dependence of the cross-section ratio $$\sigma ({e}^{+}{e}^{-}\to {B}^{0}{\overline{B} }^{0})/\sigma ({e}^{+}{e}^{-}\to {B}^{+}{B}^{-})$$ at Belle and Belle II