arXiv : Feebly Interacting Particles: FIPs 2022 workshop report

Antel, C.; Stadnik, Y.V.; Drewes, M.; Cladè, P.; Carenza, P.; Goudzovski, E.; Coloma, P.; Petcov, S.T.; Paoloni, A.; Velghe, B.; Guellati-Khelifa, S.; Samsonov, I.B.; Heuchel, D.; Lantwin, O.; Boehm, C.; De Roeck, A.; Trevisani, N.; Gonzalez-Garcia, M.C.; Beacham, J.; Junius, S.; Lopez-Pavon, J.; Tastet, J.-L.; Giannotti, M.; Zorbilmez, C.; Lindner, A.; Wong, Y.Y. Y.; Ulmer, S.; Söldner-Rembold, S.; Toro, N.; Song, N.; Zurek, K.; Foldenauer, P.; Kwon, O.; Granelli, A.; Calore, F.; Dandoy, V.; Flambaum, V.V.; Hearty, C.; Sun, C.; Oceano, I.; Middleton, S.; Crivelli, P.; Lanfranchi, G.; Li, L.; Deppisch, F.F.; Knolle, J.; Ripellino, G.; Sandner, S.; Raggi, M.; Klose, P.; Klaric, J.; Pascoli, S.; Shelton, J.; Pospelov, M.; Milstead, S.; Hajer, J.; Battaglieri, M.; Wallisch, B.; Marocco, J.; Tran, N.; Dey, B.; Kopp, J.; Hostert, M.; Echenard, B.; Golutvin, A.; Gori, S.; Gatti, C.; Urrea, S.; Buchmüller, O.; Grote, H.; Darmé, L.; Pöttgen, R.; Martin, J.W.; Chauhan, B.; Kahlhoefer, F.; O’Hare, C.A. J.; Kling, F.; Harris, P.

doi:10.1140/epjc/s10052-023-12168-5

Article
Report number	arXiv:2305.01715 ; CERN-TH-2023-061 ; DESY-23-050 ; FERMILAB-PUB-23-149-PPD ; INFN-23-14-LNF ; JLAB-PHY-23-3789 ; LA-UR-23-21432 ; MITP-23-015
Title	Feebly Interacting Particles: FIPs 2022 workshop report
Author(s)	Antel, C. (Geneva U.) ; Battaglieri, M. (INFN, Genoa) ; Beacham, J. (Duke U.) ; Boehm, C. (Sydney U.) ; Buchmüller, O. (Imperial Coll., London) ; Calore, F. (Annecy, LAPTH) ; Carenza, P. (Stockholm U., OKC) ; Chauhan, B. (U. Iowa, Iowa City) ; Cladè, P. (Paris, Lab. Kastler Brossel) ; Coloma, P. (Madrid, IFT ; Madrid, Autonoma U.) ; Crivelli, P. (Zurich, ETH) ; Dandoy, V. (KIT, Karlsruhe, IAP) ; Darmé, L. (IP2I, Lyon) ; Dey, B. (Eotvos U.) ; Deppisch, F.F. (University Coll. London) ; De Roeck, A. (CERN) ; Drewes, M. (Louvain U., CP3) ; Echenard, B. (Caltech) ; Flambaum, V.V. (New South Wales U.) ; Foldenauer, P. (Madrid, IFT ; Madrid, Autonoma U.) ; Gatti, C. (Frascati) ; Giannotti, M. (Barry U.) ; Golutvin, A. (Imperial Coll., London) ; Gonzalez-Garcia, M.C. (Barcelona U. ; ICREA, Barcelona ; Barcelona, Autonoma U. ; YITP, Stony Brook) ; Gori, S. (UC, Santa Cruz ; UC, Santa Cruz, Inst. Part. Phys.) ; Goudzovski, E. (Birmingham U.) ; Granelli, A. (Bologna U. ; INFN, Bologna) ; Grote, H. (China West Normal U.) ; Guellati-Khelifa, S. (Paris, Lab. Kastler Brossel ; CNAM, Paris) ; Hajer, J. (Lisbon, CFTP) ; Harris, P. (MIT) ; Hearty, C. (British Columbia U.) ; Heuchel, D. (DESY) ; Hostert, M. (Cambridge U., DAMTP ; Perimeter Inst. Theor. Phys. ; Minnesota U. ; Minnesota U., Theor. Phys. Inst.) ; Junius, S. (Brussels U.) ; Kahlhoefer, F. (KIT, Karlsruhe, IKP ; KIT, Karlsruhe, TTP) ; Klaric, J. (Louvain U., CP3) ; Kling, F. (DESY) ; Klose, P. (Bern U.) ; Knolle, J. (Gent U.) ; Kopp, J. (CERN ; U. Mainz, PRISMA ; Mainz U., Inst. Phys.) ; Kwon, O. (IBS, Daejeon, CAPP) ; Lantwin, O. (Unlisted) ; Lanfranchi, G. (Frascati) ; Li, L. (Brown U.) ; Lindner, A. (DESY) ; Lopez-Pavon, J. (Valencia U. ; Valencia U., IFIC) ; Marocco, J. (LBL, Berkeley) ; Martin, J.W. (Winnipeg U.) ; Middleton, S. (Caltech) ; Milstead, S. (Stockholm U.) ; Oceano, I. (DESY) ; O’Hare, C.A. J. (Sydney U.) ; Paoloni, A. (Frascati) ; Pascoli, S. (Bologna U. ; INFN, Bologna) ; Petcov, S.T. (SISSA, Trieste ; INFN, Trieste ; Tokyo U., IPMU) ; Pospelov, M. (Cambridge U., DAMTP ; Perimeter Inst. Theor. Phys. ; Minnesota U. ; Minnesota U., Theor. Phys. Inst.) ; Pöttgen, R. (Lund U.) ; Raggi, M. (INFN, Rome ; U. Rome La Sapienza (main)) ; Ripellino, G. (Uppsala U.) ; Samsonov, I.B. (New South Wales U.) ; Sandner, S. (Valencia U. ; Valencia U., IFIC) ; Söldner-Rembold, S. (Manchester U.) ; Shelton, J. (Illinois U., Urbana) ; Song, N. (Liverpool U., Dept. Math.) ; Sun, C. (Los Alamos Natl. Lab., Theor. Div.) ; Stadnik, Y.V. (Sydney U.) ; Tastet, J.-L. (Madrid, IFT) ; Toro, N. (SLAC) ; Tran, N. (Fermilab) ; Trevisani, N. (KIT, Karlsruhe) ; Ulmer, S. (Heinrich Heine U., Dusseldorf ; Wako, RIKEN) ; Urrea, S. (Valencia U. ; Valencia U., IFIC) ; Velghe, B. (TRIUMF) ; Wallisch, B. (Stockholm U., OKC ; U. Texas, Austin (main)) ; Wong, Y.Y. Y. (New South Wales U.) ; Zorbilmez, C. (Mersin U.) ; Zurek, K. (Caltech)
Publication	2023-12-11
Imprint	2023-05-02
Number of pages	266
In:	Eur. Phys. J. C 83 (2023) 1122
In:	Workshop on Feebly-Interacting Particles (FIPs 2022), CERN, Geneva, Switzerland, 17 - 21 Oct 2022, pp.1122
DOI	10.1140/epjc/s10052-023-12168-5
Subject category	hep-ph ; Particle Physics - Phenomenology
Abstract	Particle physics today faces the challenge of explaining the mystery of dark matter, the origin of matter over anti-matter in the Universe, the origin of the neutrino masses, the apparent fine-tuning of the electro-weak scale, and many other aspects of fundamental physics. Perhaps the most striking frontier to emerge in the search for answers involves new physics at mass scales comparable to familiar matter, below the GeV-scale, or even radically below, down to sub-eV scales, and with very feeble interaction strength. New theoretical ideas to address dark matter and other fundamental questions predict such feebly interacting particles (FIPs) at these scales, and indeed, existing data provide numerous hints for such possibility. A vibrant experimental program to discover such physics is under way, guided by a systematic theoretical approach firmly grounded on the underlying principles of the Standard Model. This document represents the report of the FIPs 2022 workshop, held at CERN between the 17 and 21 October 2022 and aims to give an overview of these efforts, their motivations, and the decadal goals that animate the community involved in the search for FIPs.
Copyright/License	publication: © 2023-2024 The Author(s) (License: CC BY 4.0), sponsored by SCOAP³ preprint: (License: CC BY 4.0)

$Global $3\nu$ oscillation analysis from fit to global data NuFIT~5.1. We show $\Delta\chi^2$ profiles minimized with respect to all undisplayed parameters. The red (blue) curves correspond to Normal (Inverted) Ordering. Solid (dashed) curves are without (with) adding the tabulated SK-atm $\Delta\chi^2$. Note that as atmospheric mass-squared splitting we use $\Delta m^2_{31}$ for NO and $\Delta m^2_{32}$ for IO.$ $(Upper left) Example Feynman diagram for HNL production via the DY process in type-I seesaw models. (Lower left) Exclusion limits on the mixing parameter $|V_{\mathrm{N}\mu}|^2$ between HNL and muon in type-I seesaw models as a function of the HNL mass $m_{\mathrm{N}}$ from Ref.~\cite{CMS:2022fut}. (Right) Exclusion limits on the mixing parameter $|U|^2$ in type-I seesaw models with different mixing assumptions as a function of the HNL mass $m_{\mathcal{N}}$ from Ref.~\cite{ATLAS:2022atq}.$ $(Upper left) Example Feynman diagram for HNL production via the DY process in type-I seesaw models. (Lower left) Exclusion limits on the mixing parameter $|V_{\mathrm{N}\mu}|^2$ between HNL and muon in type-I seesaw models as a function of the HNL mass $m_{\mathrm{N}}$ from Ref.~\cite{CMS:2022fut}. (Right) Exclusion limits on the mixing parameter $|U|^2$ in type-I seesaw models with different mixing assumptions as a function of the HNL mass $m_{\mathcal{N}}$ from Ref.~\cite{ATLAS:2022atq}.$ Show more plots

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