In this talk, I shall discuss the present status of dark matter (DM) based on the existing astrophysical data and its future possibilities with upcoming observations. I shall show that a generalized analysis of available astrophysical data can allow a wide range of parameter space for thermal WIMP DM. An alternative way to constrain the WIMPs is to search for its signal using the upcoming radio telescope Square Kilometer Array (SKA). The SKA, as I shall present, can probe much deeper into the GeV-TeV scale DM parameter space. Furthermore, it will be shown that in the case of the MeV DM, too, the SKA will be able to probe such a range of the parameter space that is beyond the reach of the existing observations. In addition, the SKA can also detect the signatures of popular non-thermal DM candidates like PBHs. Another possible hunting ground for DM can be the compact celestial objects. I shall show that the data of compact stars like White Dwarves (WDs) and neutron stars can constrain the interactions of WIMP with the constituents of such stars, thereby providing useful information regarding the WIMP parameter space. This in principle can constrain some well motivated DM scenarios.
Hadronic matrix elements evaluated on the lattice can be converted to a continuum scheme such as MSbar using intermediate non-perturbative renormalisation schemes. A very popular choice is to employ the Rome-Southampton method, i.e. RI/MOM and its variants. In this work we explore various choices of kinematics which define non-exceptional interpolating momentum schemes (IMOM). Using flavour non-singlet quark bilinears, we compute the renormalisation factors of the quark mass and wave function for nf=3 flavours of dynamical quarks. We show our numerical results and discuss the potential of these schemes.
Multiple observations of phenomena which cannot be explained in the Standard Model suggest that we need new physics beyond what we already know. The proliferation of theories in the last decades and the absence of direct observation of new phenomena at the LHC suggests to develop analysis strategies as model-independent as possible, yet suitable to be applied in experimental searches at current or next-generation colliders. One of the critical points in performing this kind of phenomenological analyses is that, very often, large parameter scans are necessary: intensive and often redundant MC simulations have to be performed to cover relevant regions of signal parameter space and achieve enough accuracy in the determination of signal features. On the other hand, disk space and computing time are often limited, and the environmental impact of performing such computations is almost never taken into consideration. There is a growing need to devise strategies to optimise data production and share resources in the HEP community, both theory and experiment. I will describe a framework which allows such approach, where simulated signal samples are deconstructed into complete sets of basic elements to be combined a posteriori to perform different analysis. The framework is modular, collaborative, flexible and resource-friendly. I will describe it through concrete examples for specific phenomenological analyses and indicate possible short- and long-term developments and applications.
I will overview our recent advances in studies of various phenomenological implications of multi-Higgs extensions of the Standard Model constrained by additional horizontal (flavour) symmetries, both gauged and global. A particular focus would be on singlet-extended SM, 2HDMs + singlet and 3HDMs, with some of their basic implications on Higgs and flavour physics, as well as on possible detection of primordial gravitational waves.
Looking at the Earth's interior with neutrinos is a realistic possibility with current and future neutrino detectors, which is complementary to geophysics methods, but it is based purely on weak interactions. In this talk, I will discuss the two main approaches to perform Earth tomography with neutrinos: (i) neutrino absorption tomography, based on partial absorption of a neutrino flux as it propagates through the Earth (at energies about a few TeV) and (ii) neutrino oscillation tomography, based on coherent Earth matter effects on the neutrino oscillatory pattern (at energies below a few tens of GeV). I will first discuss (i) and present the first neutrino tomography of Earth using actual IceCube data. Then, I will discuss (ii) and, in particular, I will focus on supernova neutrinos with tens of MeV.