scholarly journals One-loop corrections to ALP couplings

2021 ◽  
Vol 2021 (11) ◽  
Author(s):  
J. Bonilla ◽  
I. Brivio ◽  
M. B. Gavela ◽  
V. Sanz
Keyword(s):  
Dark Matter ◽  
Renormalization Group ◽  
Direct Detection ◽  
Top Quarks ◽  
Order Dimension ◽  
Leading Order ◽  
Theoretical Understanding ◽  
Anomalous Couplings ◽  
The One

Abstract The plethora of increasingly precise experiments which hunt for axion-like particles (ALPs), as well as their widely different energy reach, call for the theoretical understanding of ALP couplings at loop-level. We derive the one-loop contributions to ALP-SM effective couplings, including finite corrections. The complete leading-order — dimension five — effective linear Lagrangian is considered. The ALP is left off-shell, which is of particular impact on LHC and accelerator searches of ALP couplings to γγ, ZZ, Zγ, WW, gluons and fermions. All results are obtained in the covariant Rξ gauge. A few phenomenological consequences are also explored as illustration, with flavour diagonal channels in the case of fermions: in particular, we explore constraints on the coupling of the ALP to top quarks, that can be extracted from LHC data, from astrophysical sources and from Dark Matter direct detection experiments such as PandaX, LUX and XENON1T. Furthermore, we clarify the relation between alternative ALP bases, the role of gauge anomalous couplings and their interface with chirality-conserving and chirality-flip fermion interactions, and we briefly discuss renormalization group aspects.

scholarly journals Direct detection of supersymmetric dark matter and the role of the target nucleus spin

1994 ◽  
Vol 50 (12) ◽  
pp. 7128-7143 ◽  
Author(s):  
V. A. Bednyakov ◽  
H. V. Klapdor-Kleingrothaus ◽  
S. G. Kovalenko
Keyword(s):  
Dark Matter ◽  
Target Nucleus ◽  
Direct Detection

Searching for Dark Matter: Background Discrimination in the PICO detector

2018 ◽  
Author(s):  
Simon Daley
Keyword(s):  
Dark Matter ◽  
Image Analysis ◽  
Direct Detection ◽  
Pressure Sensors ◽  
Weakly Interacting Massive Particles ◽  
Acoustic Sensors ◽  
Good Discrimination ◽  
Bubble Chambers ◽  
Background Events

The PICO experiment uses superheated bubble chambers located at SNOLAB for direct detection of Weakly Interacting Massive Particles (WIMPs), one of the candidate particles for dark matter. Bubbles form in the detector when a particle interacts with a nucleus of the target fluid, and the recoiling deposits enough energy to nucleate a bubble in the superheated fluid. Much of the data analysis for PICO focuses on determining what type of particle caused a bubble to form. The differentiation is made by analysing signals from pressure sensors, piezoelectric acoustic sensors, and stereoscopic cameras. This talk will present an overview of the sensors and analysis which are used to discriminate between WIMP interactions and background events in the PICO 2L detector, with a focus on the role of image analysis and the potential sensitivity of the detector if good discrimination can be realized.

Neuropsychological Investigations of Human Amnesia: Insights Into the Role of the Medial Temporal Lobes in Cognition

2017 ◽  
Vol 23 (9-10) ◽  
pp. 732-740 ◽  
Author(s):  
Mieke Verfaellie ◽  
Margaret M. Keane
Keyword(s):  
Long Term Memory ◽  
Medial Temporal Lobes ◽  
Theoretical Understanding ◽  
Temporal Lobes ◽  
The Past ◽  
Clinical Disorders ◽  
Nuanced Understanding ◽  
The One

AbstractThe past 30 years of research on human amnesia has yielded important changes in our understanding of the role of the medial temporal lobes (MTL) in memory. On the one hand, this body of evidence has highlighted that not all types of memory are impaired in patients with MTL lesions. On the other hand, this research has made apparent that the role of the MTL extends beyond the domain of long-term memory, to include working memory, perception, and future thinking. In this article, we review the discoveries and controversies that have characterized this literature and that set the stage for a new conceptualization of the role of the MTL in cognition. This shift toward a more nuanced understanding of MTL function has direct relevance for a range of clinical disorders in which the MTL is implicated, potentially shaping not only theoretical understanding but also clinical practice. (JINS, 2017, 23, 732–740)

scholarly journals SUSY INTO DARKNESS: HEAVY SCALARS IN THE CMSSM

2013 ◽  
Vol 28 (15) ◽  
pp. 1350061 ◽  
Author(s):  
VAN E. MAYES
Keyword(s):  
Dark Matter ◽  
Parameter Space ◽  
Cross Sections ◽  
Higgs Mass ◽  
Cold Dark Matter ◽  
Direct Detection ◽  
Percent Level ◽  
Relic Density ◽  
The One ◽  
Near Future

A survey of the mSUGRA/CMSSM parameter space is presented. The viable regions of the parameter space which satisfy standard experimental constraints are identified and discussed. These constraints include a 124–127 GeV mass for the lightest CP-even Higgs and the correct relic density for cold dark matter. The superpartner spectra corresponding to these regions fall within the well-known hyperbolic branch and are found to possess sub-TeV neutralinos and charginos, with mixed Bino/Higgsino LSP's with 200–800 GeV masses. In addition, the models possess ~3–4 TeV gluino masses and heavy squarks and sleptons with masses [Formula: see text]. Spectra with a Higgs mass mh≅125 GeV and a relic density 0.105 ≤ Ωχ0h2≤ 0.123 are found to require EWFT at around the one-percent level, while those spectra with a much lower relic density require EWFT of only a few percent. Moreover, the spin-independent neutralino–proton direct detection cross-sections are found to be below or within the XENON100 2σ limit and should be experimentally accessible now or in the near future. Finally, it is pointed out that the supersymmetry breaking soft terms corresponding to these regions of the mSUGRA/CMSSM parameter space (m0∝ m1/2with [Formula: see text] and A0= -m1/2) may be obtained from general flux-induced soft terms in Type IIB flux compactifications with D3 branes.

scholarly journals PRIVATE HIGGS AT THE LHC

2013 ◽  
Vol 28 (28) ◽  
pp. 1350149 ◽  
Author(s):  
YONI BENTOV ◽  
A. ZEE
Keyword(s):  
Dark Matter ◽  
Degrees Of Freedom ◽  
Vacuum Expectation ◽  
Mass Hierarchy ◽  
Neutrino Mixing ◽  
Leading Order ◽  
Expectation Values ◽  
Mixing Angles ◽  
Yukawa Couplings

We study the LHC phenomenology of a general class of "Private Higgs" (PH) models, in which fermions obtain their masses from their own Higgs doublets with [Formula: see text] Yukawa couplings, and the mass hierarchy is translated into a dynamical chain of vacuum expectation values. This is accomplished by introducing a number of light gauge-singlet scalars, the "darkons," some of which could play the role of dark matter. These models allow for substantial modifications to the decays of the lightest Higgs boson, for instance through mixing with TeV-scale PH fields and light darkons: in particular, one could accommodate [Formula: see text] flavor-uncorrelated deviations from the SM [Formula: see text] vertices with TeV-scale degrees of freedom. We also discuss a new implementation of the PH framework, in which the quark and neutrino mixing angles arise as one-loop corrections to the leading order picture.

scholarly journals Fat brane, dark matter and localized kinetic terms in six dimensions

2020 ◽  
Vol 80 (2) ◽  
Author(s):  
Ricardo G. Landim
Keyword(s):  
Dark Matter ◽  
Particle Physics ◽  
Direct Detection ◽  
Kinetic Term ◽  
Finite Width ◽  
Complex Scalar ◽  
Abelian Gauge ◽  
Complex Scalar Field ◽  
Relic Abundance

Abstract Extra dimensions (ED) have been used as attempts to explain several phenomena in particle physics over the years. In this paper we investigate the role of an abelian gauge field as mediator of the interaction between dark matter (DM) and Standard Model (SM) particles, in a model with two flat and transverse ED compactified on the chiral square. DM is confined in a thin brane, localized at the origin of the chiral square, while the SM is localized in a finite width brane, lying in the opposite corner of the square. A brane-localized kinetic term is present in the DM brane, while in the fat brane it is not allowed. In this model the kinetic mixing is not required because we assume that the SM particles couple to the mediator through their $$B-L$$B-L charges, while DM couples to it via a dark charge. Assuming a complex scalar field as DM candidate it is possible to obtain the observed DM relic abundance and avoid direct detection constraints for some parameter choices.

scholarly journals Origins of Stellar Halos

2015 ◽  
Vol 11 (S317) ◽  
pp. 1-8
Author(s):  
Kathryn V. Johnston
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Stellar Populations ◽  
Observational Evidence ◽  
Dark Matter Halo ◽  
Theoretical Understanding ◽  
Stellar Halo ◽  
The One ◽  
Halo Population

AbstractThis contribution reviews ideas about the origins of stellar halos. It includes discussion of the theoretical understanding of and observational evidence for stellar populations formed “in situ” (meaning formed in orbits close to their current ones), “kicked-out” (meaning formed in the inner galaxy in orbits unlike their current ones) and “accreted” (meaning formed in a dark matter halo other than the one they currently occupy). At this point there is general agreement that a significant fraction of any stellar halo population is likely “accreted”. There is modest evidence for the presence of a “kicked-out” population around both the Milky Way and M31. Our theoretical understanding of and the observational evidence for an “in situ” population are less clear.

RG IMPROVEMENT OF THE EFFECTIVE POTENTIAL AT FINITE TEMPERATURE

1996 ◽  
Vol 11 (28) ◽  
pp. 2259-2269 ◽  
Author(s):  
HISAO NAKKAGAWA ◽  
HIROSHI YOKOTA
Keyword(s):  
Renormalization Group ◽  
Effective Potential ◽  
Finite Temperature ◽  
Renormalization Group Equation ◽  
Effective Procedure ◽  
Coefficient Function ◽  
Group Equation ◽  
Leading Order ◽  
Effective Potentials ◽  
The One

We present a simple and effective procedure to improve the finite temperature effective potential so as to satisfy the renormalization group equation (RGE). With the L-loop knowledge of the effective potential and of the RGE coefficient function, this procedure carries out a systematic resummation of large-T as well as large-log terms up to the Lth-to-leading order, giving an improved effective potential which satisfies the RGE and is exact up to the Lth-to-leading T and log terms. Applications to the one- and two-loop effective potentials are explicitly performed.

TECHNICAL ASPECTS IN DARK MATTER DIRECT DETECTION

2013 ◽  
Vol 23 ◽  
pp. 309-313
Author(s):  
R. BERNABEI ◽  
P. BELLI ◽  
A. DI MARCO ◽  
F. MONTECCHIA ◽  
F. CAPPELLA ◽  
...  
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Theoretical Models ◽  
The Other ◽  
Technical Aspects ◽  
Other Hand ◽  
The One

In the field of dark matter direct detection, on the one hand, it is predicted by theoretical models that many dark matter candidates and scenarios are possible. On the other hand, a variety of detectors has been proposed, but most of them — by the fact — are still at R&D stage. Such a situation leads to some considerations on technical aspects on dark matter direct detection.

scholarly journals The Role of Small Scale Experiments in the Direct Detection of Dark Matter

Universe ◽  
2021 ◽  
Vol 7 (4) ◽  
pp. 81
Author(s):  
Susana Cebrián
Keyword(s):  
Dark Matter ◽  
New Technologies ◽  
Direct Detection ◽  
Detection Methods ◽  
Small Scale ◽  
Detection Systems ◽  
Relevant Role ◽  
Low Mass ◽  
Complex Detection

In the direct detection of the galactic dark matter, experiments using cryogenic solid-state detectors or noble liquids play for years a very relevant role, with increasing target mass and more and more complex detection systems. But smaller projects, based on very sensitive, advanced detectors following new technologies, could help in the exploration of the different proposed dark matter scenarios too. There are experiments focused on the observation of distinctive signatures of dark matter, like an annual modulation of the interaction rates or the directionality of the signal; other ones are intended to specifically investigate low mass dark matter candidates or particular interactions. For this kind of dark matter experiments at small scale, the physics case will be discussed and selected projects will be described, summarizing the basics of their detection methods and presenting their present status, recent results and prospects.

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