Grad School Physics Seminar 2025/26
from
Thursday, 2 October 2025 (09:15)
to
Friday, 26 June 2026 (18:00)
Monday, 29 September 2025
Tuesday, 30 September 2025
Wednesday, 1 October 2025
Thursday, 2 October 2025
Friday, 3 October 2025
Saturday, 4 October 2025
Sunday, 5 October 2025
Monday, 6 October 2025
Tuesday, 7 October 2025
Wednesday, 8 October 2025
Thursday, 9 October 2025
09:15
Welcoming Talk of the Graduate School Director¶
-
Michał Spaliński
Welcoming Talk of the Graduate School Director¶
Michał Spaliński
09:15 - 09:35
Room: Room 207
09:35
Discussion about the goals and organization of the PhD seminar¶
-
Jakub Wagner
(
National Centre for Nuclear Research
)
Anna Durkalec
(
National Centre for Nuclear Research
)
Michal Bluj
(
NCBJ
)
Discussion about the goals and organization of the PhD seminar¶
Jakub Wagner
(
National Centre for Nuclear Research
)
Anna Durkalec
(
National Centre for Nuclear Research
)
Michal Bluj
(
NCBJ
)
09:35 - 09:55
Room: Room 207
Friday, 10 October 2025
Saturday, 11 October 2025
Sunday, 12 October 2025
Monday, 13 October 2025
Tuesday, 14 October 2025
Wednesday, 15 October 2025
Thursday, 16 October 2025
09:15
Production of Self Interacting Scalars in the Early Universe
-
Juan Esau Cervantes Hernandez
(
NCBJ Warsaw
)
Production of Self Interacting Scalars in the Early Universe
Juan Esau Cervantes Hernandez
(
NCBJ Warsaw
)
09:15 - 09:35
Room: Room 207
In this talk, I will present an overview of my research on Dark Matter (DM). I will begin with a brief introduction to the study of DM across different approaches, before focusing on Cannibal DM produced via the freeze-in mechanism in the early Universe. I will discuss the non-trivial thermal dynamics of this scenario and the importance of tracking the DM temperature evolution. I will then outline the resulting detectability prospects, which become viable in non-standard cosmological histories, particularly when the early Universe is dominated by a cold inflaton field. In the second part, I will turn to cosmological phase transitions, emphasizing how first-order transitions can generate observable gravitational waves (GWs). Finally, I will show that an inverse phase transition can occur within the freeze-in framework, where cannibalization dynamics crucially modify the evolution of the transition and the associated GW phenomenology, potentially within reach of future interferometer experiments.
Friday, 17 October 2025
Saturday, 18 October 2025
Sunday, 19 October 2025
Monday, 20 October 2025
Tuesday, 21 October 2025
Wednesday, 22 October 2025
Thursday, 23 October 2025
09:15
Study of direct photon production in Pb-Pb collisions at $\sqrt {s_{NN}}$ = 5.02 TeV with ALICE experiment’s Photon Spectrometer (PHOS) at Large Hadron Collider
-
Sushobhan Mandal
(
NCBJ
)
Study of direct photon production in Pb-Pb collisions at $\sqrt {s_{NN}}$ = 5.02 TeV with ALICE experiment’s Photon Spectrometer (PHOS) at Large Hadron Collider
Sushobhan Mandal
(
NCBJ
)
09:15 - 09:35
Room: Room 207
The Quark-Gluon Plasma (QGP), a state of deconfined quarks and gluons, is believed to have existed in the early Universe shortly after the Big Bang. As the QGP cools, it transitions into the hadronic matter we observe today. In laboratory settings, small-scale "Big Bangs" are created through high-energy heavy-ion collisions, which heat the hadronic matter above the transition temperature, approximately 150 MeV, resulting in the formation of the QGP. Direct photons serve as unique probes in high-energy proton-proton and nucleus-nucleus collisions due to their weak interaction with the dense and hot quark-gluon medium. These photons escape the medium unaltered, providing undistorted information about the collision's evolution. In the ALICE experiment at the Large Hadron Collider (LHC), photons from lead-lead collisions are measured using techniques such as the Photon Conversion Method and Electromagnetic Calorimeter. The Photon Spectrometer (PHOS), offering high-precision photon detection, was used for our analysis (with Run 2 data in Pb-Pb collisions at $\sqrt {s_{NN}}$ = 5.02 TeV) to measure inclusive photons and simulate decay photons, aiding in the derivation of direct photon spectra. By disentangling the contributions of decay, prompt and thermal photons emitted during these collisions, we can estimate the effects of cold and hot nuclear matter and gain insights into the temperature, correlations, and collective phenomena within the QGP.
Friday, 24 October 2025
Saturday, 25 October 2025
Sunday, 26 October 2025
Monday, 27 October 2025
Tuesday, 28 October 2025
Wednesday, 29 October 2025
Thursday, 30 October 2025
09:15
CMB Lensing with TEReSiTA
-
Nicola Principi
(
NCBJ
)
CMB Lensing with TEReSiTA
Nicola Principi
(
NCBJ
)
09:15 - 10:15
Room: Room 207
We are currently living in the most scientifically active era of the human kind: cosmology makes no exception. Our understanding of the Universe has radically changed during the last decades. However, while many long-standing questions about the nature of the Universe have been answered, many others have emerged. Why is the Universe's expansion accelerating? What is dark energy? What is dark matter? How does inflation work? The study of the Cosmic Microwave Background, together with other cosmological probes, is one of the ways we can answer these new questions. In particular, studying the weak gravitational lensing effect of large-scale structure on the CMB photons, we can obtain information about both the primordial and the late-time Universe. I will show how. In this talk, I present the Tomographic Ensamble of Realistic Simulations of Tracers and Anisotropies (TEReSiTA): a set of simulations of correlated galaxy catalogues and CMB observations. TEReSiTA, my original work, is a very useful and versatile tool for testing new paths in the quest for high-precision cosmological parameter estimation.
Friday, 31 October 2025
Saturday, 1 November 2025
Sunday, 2 November 2025
Monday, 3 November 2025
Tuesday, 4 November 2025
Wednesday, 5 November 2025
Thursday, 6 November 2025
09:15
From gravitational symmetries to the area law
-
Ludovic Varrin
From gravitational symmetries to the area law
Ludovic Varrin
09:15 - 10:15
Room: Room 207
The complete structure of quantum gravity remains unknown to this day. A recent line of research proposes using the symmetries of gravity as a guiding principle in the search for its quantum formulation. In this talk, I will present our approach, which employs these symmetries to classify the possible quantum gravitational states associated with a subregion of spacetime. I will further show that our formalism naturally leads to a computation of the entanglement entropy of such subregions. Finally, I will argue that, in the classical limit, the leading term of this entanglement entropy scales with the area of the subregion’s boundary, thus recovering the famous Bekenstein–Hawking area law and strengthening the case for a symmetry-based approach to quantum gravity.
Friday, 7 November 2025
Saturday, 8 November 2025
Sunday, 9 November 2025
Monday, 10 November 2025
Tuesday, 11 November 2025
Wednesday, 12 November 2025
Thursday, 13 November 2025
09:15
Ultra-Diffuse Galaxies study
-
Antonio Vanzanella
(
National Centre for the Nuclear Research, Pasteura 7, 02-093 Warsaw, Poland
)
Ultra-Diffuse Galaxies study
Antonio Vanzanella
(
National Centre for the Nuclear Research, Pasteura 7, 02-093 Warsaw, Poland
)
09:15 - 10:15
Room: Room 207
Low Surface Brightness Galaxies (LSBGs) are defined as galaxies with an average central surface brightness, 𝜇(0,r), below the typical level of the night sky. LSBGs are estimated to contribute less than 1% to the luminosity of the local observable universe; however, their contribution to the total number density of galaxies is estimated to be around 40% to 50%. Exploring the standard evolution of LSBGs and investigating the reasons behind their faint nature could be crucial to understanding our universe. Among LSBGs, a subsample of objects has been identified: classified as Ultra Diffuse Galaxies (UDGs), which are LSBGs having a central surface brightness measured in g-band, 𝜇(0,g), larger than 24 mag per arcsec² and an extended half-light radius, r{1/2}, larger than 1.5 kpc. UDGs populate the distribution tail of the LSBGs' luminosity profile, inhabiting field, group and cluster environments. Previous studies have established substantial differences in the properties of UDGs according to their host environment. Comparing properties in different UDGs hosting environments would allow us to find the most likely evolutionary path of these galaxies, factoring out the episodic events due to their surroundings. In our work, we validated the performance of a Machine Learning model developed to find LSBGs and UDGs, extracting also physical properties of LSBGs/UDGs through redshift measurements such as star formation rates (SFRs) and stellar masses(Mstar).
Friday, 14 November 2025
Saturday, 15 November 2025
Sunday, 16 November 2025
Monday, 17 November 2025
Tuesday, 18 November 2025
Wednesday, 19 November 2025
Thursday, 20 November 2025
09:15
Multidimensional Framework for Modeling Fusion and Fission of Heaviest Nuclei
-
Aleksander Augustyn
(
NCBJ
)
Multidimensional Framework for Modeling Fusion and Fission of Heaviest Nuclei
Aleksander Augustyn
(
NCBJ
)
09:15 - 10:15
Room: Room 207
This work presents the development of a comprehensive computational framework for modeling fusion and fission processes in heavy and superheavy nuclei (Z ≥ 90). The framework is based on the Warsaw Macroscopic-Microscopic Model (WMMM), extended to incorporate multiple shape parameterizations, including the traditional beta parameterization and the Fourier-over-Spheroid (FoS) approach, which enables description of nuclear shapes from compact configurations to scission. The framework combines several methodological advances in shape parameterization conversion, model modernization, and large-scale computational capabilities to generate multidimensional potential energy surfaces spanning over 100 million configurations per nucleus. Stochastic shape evolution is described through both simplified and sophisticated formalisms, enabling predictions of fusion probabilities, ground state properties, fission barriers, and mass fragment distributions. Applications to superheavy elements and actinide systematics demonstrate the framework's ability to reproduce experimental observables without parameter fitting, suggesting promising prospects for a unified theoretical description of fusion-fission dynamics across the heavy element region.
Friday, 21 November 2025
Saturday, 22 November 2025
Sunday, 23 November 2025
Monday, 24 November 2025
Tuesday, 25 November 2025
Wednesday, 26 November 2025
Thursday, 27 November 2025
09:00
Probes of light dark matter in relativistic regime
-
Jyotismita Adhikary
(
NCBJ
)
Probes of light dark matter in relativistic regime
Jyotismita Adhikary
(
NCBJ
)
09:00 - 10:00
Room: Room 207
Dark matter interactions are traditionally probed in the non-relativistic regime characteristic of cold DM in the present-day universe. However, this strategy is insufficient for probing a class of important thermal DM targets for which non-relativistic scattering rates are highly suppressed. This opens an unexplored region of parameter space and motivates the development of detection strategies specifically tailored to low-mass dark matter. In this talk, I will discuss examples of such models and outline novel detection strategies designed to probe them — either directly, or indirectly through the detection of light dark-sector mediators.
Friday, 28 November 2025
Saturday, 29 November 2025
Sunday, 30 November 2025
Monday, 1 December 2025
Tuesday, 2 December 2025
Wednesday, 3 December 2025
Thursday, 4 December 2025
09:15
Search for hadron exotics in the new decay modes of the $B^0$ meson at LHCb
-
Salil Joshi
(
NCBJ
)
Search for hadron exotics in the new decay modes of the $B^0$ meson at LHCb
Salil Joshi
(
NCBJ
)
09:15 - 09:35
Room: Room 207
Spectroscopic studies of multi-quark hadrons in the charmonium sector are crucial in providing powerful insights into the intricacies of quantum chromodynamics (QCD) in the non-perturbative regime. Describing these hadrons as bound quark systems from first principles is challenging, but experimental observations in the last 20 years have driven the progress, with the discovery of nearly 30 exotic hadron candidates. It is this pattern of one unexpected result after another, with the emergence of desperately few connections, that has characterized the studies in this field. The LHCb experiment, with its unique capability to cover the large heavy-quark production cross-section at the LHC, offers a great window of opportunity to explore heavy hadron spectroscopy, in both the conventional and exotic sectors. This presentation is a synopsis of our work in search of QCD exotica in two new decay modes of the $B^0$ meson, which are $B^0 \rightarrow J/\psi\pi^+\pi^-\pi^0K^-\pi^+$ and $B^0 \rightarrow J/\psi\omega K^-\pi^+$. In each case we measure the Branching fraction and search for higher charmonium exotics as intermediate states in the LHCb data, collected from Run 1 (2011-2012) and Run 2 (2015-2018) in proton-proton collisions.
Friday, 5 December 2025
Saturday, 6 December 2025
Sunday, 7 December 2025
Monday, 8 December 2025
Tuesday, 9 December 2025
Wednesday, 10 December 2025
Thursday, 11 December 2025
09:15
Study of recurrent activity in radio sources
-
ANUPAMA MOHANAN
Study of recurrent activity in radio sources
ANUPAMA MOHANAN
09:15 - 10:15
Room: Room 207
Peaked-spectrum (PS) radio sources are widely regarded as tracers of the earliest stages of radio jet evolution. Milliarcsecond VLBI imaging frequently reveals compact double morphologies embedded within kiloparsec-scale cocoons, suggesting that many PS sources have the potential to grow into large FR I or FR II radio galaxies. However, a key open question remains: Do PS sources typically evolve into large-scale radio galaxies, or do they instead undergo short, intermittent bursts of activity separated by long quiescent phases? Over the past three decades, only a handful of PS AGN have been found inside older, faint radio cocoons, leaving the duty cycle of young radio jets poorly constrained. Earlier wide-area surveys lacked the surface-brightness sensitivity and angular resolution to identify these “compact core + relic emission” systems in statistically significant numbers. Recent advances in low-frequency radio interferometry have made it possible to detect faint, low-surface-brightness emission that was previously inaccessible. In this talk, I will first introduce the fundamental concepts of radio astronomy, AGN, radio galaxy morphology, and the evolutionary role of compact peaked-spectrum sources. I will then present the motivation and scientific goals of my PhD research, which aims to probe the duty cycle and restarted activity of radio sources. Using multi-frequency radio surveys, including LoTSS, we search for diffuse, relic emission around compact PS cores providing direct evidence of earlier cycles of jet activity and offering new insights into the episodic nature of young radio galaxies.
Friday, 12 December 2025
Saturday, 13 December 2025
Sunday, 14 December 2025
Monday, 15 December 2025
Tuesday, 16 December 2025
Wednesday, 17 December 2025
Thursday, 18 December 2025
09:15
Study of the Vector Boson Scattering $W^{\pm}W^{\pm}$ production at $\sqrt{s}=13.6~\mathrm{TeV}$
-
Monika Ghimiray
Study of the Vector Boson Scattering $W^{\pm}W^{\pm}$ production at $\sqrt{s}=13.6~\mathrm{TeV}$
Monika Ghimiray
09:15 - 10:15
Room: Room 207
In this seminar, I will present a study of Vector Boson Scattering (VBS) at the Compact Muon Solenoid (CMS) experiment at CERN, focusing on same-sign $W^{\pm}W^{\pm}$ scattering and its sensitivity to physics beyond the Standard Model. The analysis targets the leptonic final state with two same-sign charged leptons, two neutrinos, and two forward tagging jets, providing a clean handle on the electroweak nature of VBS and its characteristic event topology. I will outline the main experimental challenges, emphasizing the dominant background contributions and the strategies used to control them — particularly reducible backgrounds from non-prompt leptons, which are among the most significant sources of contamination. I will also present the expected cross-section measurements for this channel. Finally, I will introduce the interpretation within the Standard Model Effective Field Theory (SMEFT) framework, highlighting some preliminary results from the phenomenology part of my project, and conclude with an outlook on future SMEFT studies.
Friday, 19 December 2025
Saturday, 20 December 2025
Sunday, 21 December 2025
Monday, 22 December 2025
Tuesday, 23 December 2025
Wednesday, 24 December 2025
Thursday, 25 December 2025
Friday, 26 December 2025
Saturday, 27 December 2025
Sunday, 28 December 2025
Monday, 29 December 2025
Tuesday, 30 December 2025
Wednesday, 31 December 2025
Thursday, 1 January 2026
Friday, 2 January 2026
Saturday, 3 January 2026
Sunday, 4 January 2026
Monday, 5 January 2026
Tuesday, 6 January 2026
Wednesday, 7 January 2026
Thursday, 8 January 2026
09:15
Hierarchical Cosmology Constraints through Strong Gravitational Lensing
-
Shuaibo Geng
(
National Center for Nuclear Research
)
Hierarchical Cosmology Constraints through Strong Gravitational Lensing
Shuaibo Geng
(
National Center for Nuclear Research
)
09:15 - 10:15
Room: Room 207
Strong gravitational lensing, a phenomenon where the gravitational field of a massive foreground galaxy distorts and magnifies the light from a distant background source, provides a unique astrophysical laboratory. It uniquely bridges studies of the very large and the very small, enabling simultaneous investigation of the internal structure of galaxies and the global geometry of the universe. This dual capability makes it a powerful tool for probing the two most significant constituents of the modern universe: dark matter and dark energy. Research on galaxy mass distributions via strong lensing pertains to the nature of dark matter, while the use of lensing as a cosmological probe informs our understanding of dark energy. However, these two lines of inquiry are inherently intertwined. This thesis focuses on developing a self-consistent framework to investigate both the redshift evolution of galaxy mass distributions and cosmological parameters, with the aim of decoupling their mutual dependencies. We first present a model-independent method to study the mass profile evolution in lens galaxies. By training a non-parametric artificial neural network (ANN) on Type Ia supernova data to reconstruct the distance-redshift relation, we compare the inferred distance ratios with predictions from lens models. Applied to a combined sample of 161 lenses, this approach measures a significant redshift evolution in the extended power-law mass density slope, with the total mass profile steepening at lower redshifts. The method was validated with mock data based on LSST forecasts, which also project high precision for future large samples. We subsequently extend this framework to a hierarchical cosmological analysis using distance ratios derived from strong lensing. A Fisher-based sensitivity study identifies "sensitivity valleys" in the lens-source redshift plane where cosmological constraining power diminishes. By incorporating the prior on mass-profile evolution calibrated in the first part of the study, we reconstruct distance ratios from lensing observables and compare them to cosmological predictions. This hierarchical scheme allows for joint constraints on both mass-profile evolution and cosmological parameters within a single, unified analysis. The degeneracies between these probes are broken by incorporating external datasets. In a flat $w$CDM model, combining strong lensing distance ratios with \textit{Planck} CMB data yields a constraint on the dark energy equation of state parameter of $w=-1.52^{+0.18}_{-0.19}$. In the flat $w_{\phi}$CDM model, adding DESI BAO data provides a measurement of the matter density parameter $\Omega_m=0.256^{+0.031}_{-0.018}$. This work establishes a robust, integrated methodology for advancing our understanding of galaxy evolution and cosmology through the large sample of strong gravitational lensing.
Friday, 9 January 2026
Saturday, 10 January 2026
Sunday, 11 January 2026
Monday, 12 January 2026
Tuesday, 13 January 2026
Wednesday, 14 January 2026
Thursday, 15 January 2026
09:15
From theory to automation: Decoupling renormalization for BSM Higgs decays
-
Jonas Lang
(
National Center for Nuclear Research Poland
)
From theory to automation: Decoupling renormalization for BSM Higgs decays
Jonas Lang
(
National Center for Nuclear Research Poland
)
09:15 - 10:15
Room: Room 207
High-precision calculations of Higgs boson observables can be used to constrain models of Beyond the Standard Model (BSM) physics. Motivated by the non-observation of light BSM particles at the LHC, in this talk I will discuss a renormalization scheme for precise predictions of Higgs boson decays in the presence of moderately heavy BSM physics at the 1-loop level. I will cover the basics of regularization and renormalization. Special focus will be on the decoupling renormalization scheme, where I will present the renormalization conditions for a generic model. I will also show application of the decoupling scheme in the two Higgs doublet model (THDM) to explore its caveats and effects. Finally, I will sketch how this calculation becomes automatized as a part of FlexibleSUSY spectrum-generator generator.
Friday, 16 January 2026
Saturday, 17 January 2026
Sunday, 18 January 2026
Monday, 19 January 2026
Tuesday, 20 January 2026
Wednesday, 21 January 2026
Thursday, 22 January 2026
09:15
First dust and gas insight in late stage galaxy evolution
-
Giuliano Lorenzon
(
NCBJ
)
First dust and gas insight in late stage galaxy evolution
Giuliano Lorenzon
(
NCBJ
)
09:15 - 10:15
Room: Room 207
Quiescent galaxies (QGs) have traditionally been viewed as the endpoint of galaxy evolution, characterized by the cessation of star formation and the rapid depletion of gas and dust in the interstellar medium (ISM). However, over the past decade, infrared and sub-millimeter observations have challenged this picture by revealing the presence of dust or cold gas in a subset of quiescent systems, particularly at high redshift. The James Webb Space Telescope (JWST) began operations at the start of my PhD and has since transformed this field by uncovering a larger and earlier population of QGs than previously expected. These discoveries have opened new questions about QGs: how do they form? Do they evolve after quenching? Does quiescence truly represent a terminal phase of galaxy evolution? In this short seminar, I will provide an overview of this emerging field and its implications for galaxy evolution and population studies. I will place particular emphasis on the survey we performed with the sub-mm ALMA telescope, which constitutes the first large sample of quiescent galaxies with simultaneous detections of both cold molecular gas and dust beyond the local universe. I will discuss how these data, in synergy with JWST observations and state-of-the-art simulations, offer new insight into the residual ISM of quiescent galaxies and its role in their post-quenching evolution.
Friday, 23 January 2026
Saturday, 24 January 2026
Sunday, 25 January 2026
Monday, 26 January 2026
Tuesday, 27 January 2026
Wednesday, 28 January 2026
Thursday, 29 January 2026
Friday, 30 January 2026
Saturday, 31 January 2026
Sunday, 1 February 2026
Monday, 2 February 2026
Tuesday, 3 February 2026
Wednesday, 4 February 2026
Thursday, 5 February 2026
Friday, 6 February 2026
Saturday, 7 February 2026
Sunday, 8 February 2026
Monday, 9 February 2026
Tuesday, 10 February 2026
Wednesday, 11 February 2026
Thursday, 12 February 2026
Friday, 13 February 2026
Saturday, 14 February 2026
Sunday, 15 February 2026
Monday, 16 February 2026
Tuesday, 17 February 2026
Wednesday, 18 February 2026
Thursday, 19 February 2026
Friday, 20 February 2026
Saturday, 21 February 2026
Sunday, 22 February 2026
Monday, 23 February 2026
Tuesday, 24 February 2026
Wednesday, 25 February 2026
Thursday, 26 February 2026
Friday, 27 February 2026
Saturday, 28 February 2026
Sunday, 1 March 2026
Monday, 2 March 2026
Tuesday, 3 March 2026
Wednesday, 4 March 2026
Thursday, 5 March 2026
Friday, 6 March 2026
Saturday, 7 March 2026
Sunday, 8 March 2026
Monday, 9 March 2026
Tuesday, 10 March 2026
Wednesday, 11 March 2026
Thursday, 12 March 2026
Friday, 13 March 2026
Saturday, 14 March 2026
Sunday, 15 March 2026
Monday, 16 March 2026
Tuesday, 17 March 2026
Wednesday, 18 March 2026
Thursday, 19 March 2026
Friday, 20 March 2026
Saturday, 21 March 2026
Sunday, 22 March 2026
Monday, 23 March 2026
Tuesday, 24 March 2026
Wednesday, 25 March 2026
Thursday, 26 March 2026
Friday, 27 March 2026
Saturday, 28 March 2026
Sunday, 29 March 2026
Monday, 30 March 2026
Tuesday, 31 March 2026
Wednesday, 1 April 2026
Thursday, 2 April 2026
Friday, 3 April 2026
Saturday, 4 April 2026
Sunday, 5 April 2026
Monday, 6 April 2026
Tuesday, 7 April 2026
Wednesday, 8 April 2026
Thursday, 9 April 2026
Friday, 10 April 2026
Saturday, 11 April 2026
Sunday, 12 April 2026
Monday, 13 April 2026
Tuesday, 14 April 2026
Wednesday, 15 April 2026
Thursday, 16 April 2026
Friday, 17 April 2026
Saturday, 18 April 2026
Sunday, 19 April 2026
Monday, 20 April 2026
Tuesday, 21 April 2026
Wednesday, 22 April 2026
Thursday, 23 April 2026
Friday, 24 April 2026
Saturday, 25 April 2026
Sunday, 26 April 2026
Monday, 27 April 2026
Tuesday, 28 April 2026
Wednesday, 29 April 2026
Thursday, 30 April 2026
Friday, 1 May 2026
Saturday, 2 May 2026
Sunday, 3 May 2026
Monday, 4 May 2026
Tuesday, 5 May 2026
Wednesday, 6 May 2026
Thursday, 7 May 2026
Friday, 8 May 2026
Saturday, 9 May 2026
Sunday, 10 May 2026
Monday, 11 May 2026
Tuesday, 12 May 2026
Wednesday, 13 May 2026
Thursday, 14 May 2026
Friday, 15 May 2026
Saturday, 16 May 2026
Sunday, 17 May 2026
Monday, 18 May 2026
Tuesday, 19 May 2026
Wednesday, 20 May 2026
Thursday, 21 May 2026
Friday, 22 May 2026
Saturday, 23 May 2026
Sunday, 24 May 2026
Monday, 25 May 2026
Tuesday, 26 May 2026
Wednesday, 27 May 2026
Thursday, 28 May 2026
Friday, 29 May 2026
Saturday, 30 May 2026
Sunday, 31 May 2026
Monday, 1 June 2026
Tuesday, 2 June 2026
Wednesday, 3 June 2026
Thursday, 4 June 2026
Friday, 5 June 2026
Saturday, 6 June 2026
Sunday, 7 June 2026
Monday, 8 June 2026
Tuesday, 9 June 2026
Wednesday, 10 June 2026
Thursday, 11 June 2026
Friday, 12 June 2026
Saturday, 13 June 2026
Sunday, 14 June 2026
Monday, 15 June 2026
Tuesday, 16 June 2026
Wednesday, 17 June 2026
Thursday, 18 June 2026
Friday, 19 June 2026
Saturday, 20 June 2026
Sunday, 21 June 2026
Monday, 22 June 2026
Tuesday, 23 June 2026
Wednesday, 24 June 2026
Thursday, 25 June 2026
Friday, 26 June 2026