BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Is the Hubble tension a mystery of the small-scale Universe? DTSTART;VALUE=DATE-TIME:20260915T091000Z DTEND;VALUE=DATE-TIME:20260915T095000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31275@indico.ific.uv.es DESCRIPTION:Speakers: Jens Chluba (University of Manchester)\nhttps://indi co.ific.uv.es/event/8160/contributions/31275/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31275/ END:VEVENT BEGIN:VEVENT SUMMARY:Role of large-scale structures in cosmological evolution with mult i-messenger signatures DTSTART;VALUE=DATE-TIME:20260915T150000Z DTEND;VALUE=DATE-TIME:20260915T152500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31280@indico.ific.uv.es DESCRIPTION:Speakers: Archan S Majumdar (S. N. Bose National Centre for Ba sic Sciences)\nRecent observations have revealed the presence of cosmic st ructures at even very large scales in the Universe. This\, along with cos mological tensions\, motivates re-examination of the standard paradigm of the concordance model based on assumptions of homogeneous matter distribut ion at various cosmological scales. The observed large-scale matter inhomo geneities may possibly impact the background Hubble evolution through the ir backreaction on the cosmological metric. We compute the effects of bac kreaction through the Buchert formalism for averaging on spatial hypersurf aces\, employing various physically motivated ansatzes for multiple-domain cosmic inhomogeneities. The resulting altered Hubble evolution\, when co nfronted with data from various recent observations\, leads to tight const raints on the backreaction models. Remarkably\, our analysis predicts inte resting signatures on various kinds of astronomical signals\, such as the \, (a) red-shift drift\, (b) 21-cm brightness temperature\, and (c) amplit ude of gravitational waves from compact binaries. Moreover\, we show how t he Hubble tension gets alleviated through the obtained best-fit parameters of our backreaction models. \n\n\nReferences:\n[1] Effect of inhomogenei ties on the propagation of gravitational waves from binaries of compact ob jects\, S. S. Pandey\, A. Sarkar\, A. Ali\, A. S. Majumdar\, JCAP 06\, 021 (2022).\n[2] Global 21-cm brightness temperature in viscous dark energy models\, A. Halder\, S. S. Pandey\, A. S. Majumdar\, JCAP 10\, 049 (2022). \n[3] Viscous attenuation of gravitational waves propagating through an i nhomogeneous background\, S. S. Pandey\, A. Sarkar\, A. Ali\, A. S. Majumd ar\, Eur. Phys. J. C 83\, 435 (2023).\n[4] Future deceleration due to bac kreaction in a Universe with multiple inhomogeneous domains\, A. Halder\, S. S. Pandey\, A. S. Majumdar\, JCAP 08\, 064 (2023).\n[5] Analyzing the 21-cm signal brightness temperature in the Universe with inhomogeneities\, S. S. Pandey\, A. Halder\, A. S. Majumdar\, Phys. Rev. D 110\, 043531 (20 24).\n[6] Constraining the Hubble parameter with the 21-cm brightness tem perature signal in a universe with inhomogeneities\, S. Mukherjee\, S. S. Pandey\, A. S. Majumdar\, Phys. Rev. D 112\, 063520 (2025).\n[7] Optical d epth to reionization in a Universe with multiple inhomogeneous domains\, S . S. Pandey\, Ruchika\, S. Mukherjee\, A. S. Majumdar\, arXiv: 2604.13718 [astro-ph.CO].\n\nhttps://indico.ific.uv.es/event/8160/contributions/31280 / LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31280/ END:VEVENT BEGIN:VEVENT SUMMARY:The Distance Network: a unified analysis of local H0 measurements DTSTART;VALUE=DATE-TIME:20260915T121000Z DTEND;VALUE=DATE-TIME:20260915T125000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31282@indico.ific.uv.es DESCRIPTION:Speakers: Stefano Casertano (Space Telescope Science Institute )\nThe Distance Network provides a unified\, statistically rigorous framew ork for a robust combined statistical analysis of a broad variety of local measurements of the Hubble constant. This approach provides full error p ropagation\, accounting for commonalities between measurements\, and stati stical tests to identify possible outliers. We obtain an improved determi nation of the Hubble constant\, with a baseline value of 73.50+/-0.81 km/s /Mpc\, over 7 sigma from current Lambda-CDM based estimates. We test many variants that include\, exclude\, or modify various methods\; all yield v alues between 72.5 and 74.0 km/s/Mpc. The algorithm and data are publicall y available and allow the inclusion of future measurements in this framewo rk.\n\nhttps://indico.ific.uv.es/event/8160/contributions/31282/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31282/ END:VEVENT BEGIN:VEVENT SUMMARY:Investigating Expansion-History Mismatch with Diverse Dark Energy Parametrization Frameworks DTSTART;VALUE=DATE-TIME:20260917T134500Z DTEND;VALUE=DATE-TIME:20260917T141000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31313@indico.ific.uv.es DESCRIPTION:Speakers: Upala Mukhopadhyay (University of Luxembourg)\nThe $ \\Lambda$CDM model successfully explains a wide range of cosmological obse rvations\; however\, persistent discrepancies most notably the $H_0$ tensi on between early and late time measurements challenge its completeness. No proposed extension has yet resolved this tension while retaining the over all success of $\\Lambda$CDM. We have investigated whether the $H_0$ tensi on can be associated with a specific epoch in the cosmic expansion history and identify the redshift range most relevant for understanding its origi n. In addition to the cosmological constant\, we have considered three phe nomenological models based on general parametrizations of key quantities g overning cosmic expansion: the dark energy (DE) equation of state\, the DE pressure density\, and the scale factor. Using early time Planck data and late time Pantheon+ (with and without SH0ES calibration) and DESI measure ments\, we have constrained model parameters and examined the evolution of the Hubble parameter H(z). We have found that $\\Lambda$CDM exhibits disc repancies across all redshifts\, whereas the other models show them mainly at low redshifts. Further analysis at low redshifts reveals significantly larger deviations in $H(z)$ at $z$=0.51 and 0.706 compared to other range s. We have also found that the pressure density parametrization alleviates the $H_0$ tension\, reducing it to $\\sim 2.7\\sigma$\, while the other m odels do not provide significant improvements.\n\nhttps://indico.ific.uv.e s/event/8160/contributions/31313/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31313/ END:VEVENT BEGIN:VEVENT SUMMARY:An Agnostic Exploration of Novel Equation Structures for Dynamical Dark Energy DTSTART;VALUE=DATE-TIME:20260917T143500Z DTEND;VALUE=DATE-TIME:20260917T150000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31314@indico.ific.uv.es DESCRIPTION:Speakers: Rebecca Briffa (University of Malta)\nCosmological t ensions between early- and late-Universe probes\, most notably the Hubble tension in $H_0$ have intensified scrutiny of the ΛCDM paradigm and motiv ated flexible dark-energy scenarios beyond a cosmological constant. A pers istent obstacle is that the functional form of the dark-energy equation of state $w(a)$ is usually chosen by hand (e.g.wCDM or CPL)\, so potentially viable models may never be tested.\n\nWe present an automated pipeline th at searches a large combinatorial space of dynamical dark-energy parametri sations using a mask-based genetic algorithm coupled to the CLASS Boltzman n code. Each candidate is a sum of coefficient–shape terms $w(a)=\\sum c _i f_j(a)$\, the genetic algorithm selects which terms are active\, while coefficients are constrained with datasets via Cobaya (with optional neur al-network acceleration through CLiENT). Fitness is driven by $\\chi^2$\, enabling evolutionary discovery of competitive $w(a)$ structures without f ixing a single parametric ansatz a priori.\n\nThis approach sits at the in tersection of data-analysis and fundamental-physics themes: it uses evolut ionary optimisation and likelihood-driven model search to explore dark-ene rgy phenomenology that may help interpret\, and ultimately alleviate\, ten sions with the concordance model. We discuss validation against standard b aselines (including CPL)\, the best-performing symbolic forms found so far \, and the path toward multi-probe analyses (CMB\, BAO/DESI) needed to ass ess tension relief robustly.\n\nhttps://indico.ific.uv.es/event/8160/contr ibutions/31314/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31314/ END:VEVENT BEGIN:VEVENT SUMMARY:Primordial Black Holes as Cosmic Expansion Accelerators DTSTART;VALUE=DATE-TIME:20260917T150000Z DTEND;VALUE=DATE-TIME:20260917T152500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31315@indico.ific.uv.es DESCRIPTION:Speakers: Konstantinos Dialektopoulos (University of Malta)\nI n this seminar\, I will present a novel mechanism for cosmic acceleration driven by primordial black holes with effective repulsive behavior. Using a new Swiss Cheese cosmological framework\, I will discuss four black hole spacetimes—Hayward\, Bardeen\, Dymnikova\, and de Sitter-Schwarzschild —to show that this acceleration emerges naturally from the geometry itse lf. The results suggest that ultra-light PBHs could drive inflation withou t requiring an inflaton\, while PBHs with masses $m \\sim 10^{12}\\mathrm{ g}$ and abundances $0.107 \n\nhttps://indico.ific.uv.es/event/8160/contrib utions/31315/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31315/ END:VEVENT BEGIN:VEVENT SUMMARY:Connecting Early Dark Energy to Late Dark Energy by the Diluting M atter Potential DTSTART;VALUE=DATE-TIME:20260917T141000Z DTEND;VALUE=DATE-TIME:20260917T143500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31316@indico.ific.uv.es DESCRIPTION:Speakers: Eduardo Guendelman (Ben Gurion University)\nIn this work we study a scale invariant gravity theory containing two scalar field s\, dust particles and a measure defined from degrees of freedom independe nt of the metric. The integration of the degrees of freedom that define th e measure spontaneously break the scale symmetry\, leaving us in the Einst ein frame with an effective potential that is dependent on the density of the particles. The potential contains three flat regions\, one for inflati on\, another for early dark energy and the third for late dark energy. At a certain point\, as the matter dilutes\, tunneling from the early dark en ergy to the late dark energy can start efficiently. \nThis mechanism natur ally alleviated the observed Hubble tension by modifying the sound horizon prior to recombination while preserving late-time cosmology. Moreover\, t he model predictions are consistent with observations from the reduced CMB \, BAO\, and local measurement of $H_0$\, providing a coherent and unified description of the universe. In this context\, the Bayesian analysis of t hese datasets confirms the viability of our scenario\, with the best-fit p arameters indicating an early dark energy fraction of $f_{\\rm NEDE}\\appr ox 0.3$ at a redshift \nof $z^{\\prime}=5000$. This preliminary estimate\, obtained \nusing the reduced CMB dataset\, is expected to be tightened \n once the full CMB likelihood is considered.\n\nhttps://indico.ific.uv.es/e vent/8160/contributions/31316/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31316/ END:VEVENT BEGIN:VEVENT SUMMARY:Coffee Break DTSTART;VALUE=DATE-TIME:20260917T131500Z DTEND;VALUE=DATE-TIME:20260917T134500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31312@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31312/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31312/ END:VEVENT BEGIN:VEVENT SUMMARY:The inertial mass density : Cosmology\, Post-Newtonian Physics\, a nd Galactic Kinematics DTSTART;VALUE=DATE-TIME:20260917T122500Z DTEND;VALUE=DATE-TIME:20260917T125000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31309@indico.ific.uv.es DESCRIPTION:Speakers: Nihan Katirci (Dogus University)\nThe persistent  tension and the improved supernova–BAO consistency under dynamical dark energy after DESI DR2 motivate rethinking how dark energy evolution is pa rametrized. We formulate it directly through the inertial mass density (IM D)\, $\\rho+p$IMD\, and show that an IMD evolving from a negative to an equal positive constant toward z->0 can induce a past sign change in  itself\, with background constraints from SimpleMC and a full perturbative analysis using CAMB and COBAYA underway. We then turn to the face that co smology leaves dormant — the genuinely inertial role of IMD — in self- gravitating systems\, where at first post-Newtonian order the IMD acquires pressure and gravitational-self-energy contributions whose rescaling by t wo parameters breaks the strong equivalence principle. The resulting local effects\, a Nordtvedt effect and a non-conservation of momentum\, are sma ll enough to pass tight Solar-System and pulsar-timing tests\, yet the sam e corrections accumulate on large scales and reshape galactic kinematics a s an alternative to dark matter. In short\, we present IMD as a single\, f undamental variable connecting the dark sector across scales.\n\nhttps://i ndico.ific.uv.es/event/8160/contributions/31309/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31309/ END:VEVENT BEGIN:VEVENT SUMMARY:Can a slime mould help us with cosmological tensions? DTSTART;VALUE=DATE-TIME:20260917T120000Z DTEND;VALUE=DATE-TIME:20260917T122500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31310@indico.ific.uv.es DESCRIPTION:Speakers: Vincenzo Salzano ()\nModern cosmology is confronted with persistent observational tensions that challenge the standard cosmol ogical model. While most proposed solutions rely on extending existing the oretical frameworks\, we are developing an alternative\, model-independent approach inspired by the collective dynamics of biological systems. We pr esent the motivation\, methodology\, and current status of a proof-of-conc ept project aimed at investigating whether a slime-mould-inspired algorith m can extract cosmological information directly from the large-scale distr ibution of matter without assuming a specific theory of gravity. The ongoi ng work focuses on transforming this algorithm from an interpolation tool into a predictive framework through systematic calibration against numeric al cosmological simulations\, followed by its application to observational data. We will discuss the planned validation strategy\, including tests o f its ability to reproduce cosmic structures\, generate realistic mock obs ervations\, and infer statistically robust information about the underlyin g cosmological model. By introducing this research programme and its first developments\, we aim to open a novel avenue for model-independent studie s of gravity and the origin of current cosmological tensions.\n\nhttps://i ndico.ific.uv.es/event/8160/contributions/31310/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31310/ END:VEVENT BEGIN:VEVENT SUMMARY:Beyond j=1: Observational Constraints on Almost-ΛCDM Cosmologies DTSTART;VALUE=DATE-TIME:20260917T125000Z DTEND;VALUE=DATE-TIME:20260917T131500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31311@indico.ific.uv.es DESCRIPTION:Speakers: Jess Worsley (1Department of Mathematics and Applied Mathematics\, University of Cape Town\, 7 University Ave N\, 7700\, Sout h Africa.)\nThe cosmographic condition $j(z)=1$ provides the kinematical s ignature of the spatially flat $\\Lambda$CDM model independently of any sp ecific dark-energy or modified-gravity theory. We investigate the extent t o which current observations permit departures from this condition by cons idering three phenomenological ``almost-$\\Lambda$CDM'' cosmographic closu res in which the cosmic jerk differs slightly from unity through a small d eformation parameter $\\epsilon$. The models are constrained using Markov Chain Monte Carlo analyses of recent DESI baryon acoustic oscillation meas urements together with compressed Planck cosmic microwave background likel ihoods and the Union3\, Pantheon+\, and DESY5 Type Ia supernova compilatio ns.\n\nUnlike conventional analyses that infer the expansion history after imposing an explicit parameterization of the dark-energy equation of stat e\, our cosmographic framework reconstructs the expansion history directly from observations\, with the effective dark-energy equation of state emer ging as a derived quantity rather than an assumed one. We find that all th ree cosmographic closures are confined by current observations to a remark ably small neighbourhood of the $\\Lambda$CDM cosmographic fixed point\, w ith the inclusion of Planck data driving the preferred evolution toward $j _0\\simeq1$ and $w_{\\rm DE\,0}\\simeq-1$. Despite their distinct kinemati cal constructions\, the reconstructed dark-energy evolution consistently e xhibits a smooth freezing behaviour that remains close to $w=-1$ without c rossing the phantom divide.\n\nModel comparison using the Akaike and Bayes ian information criteria shows that the almost-$\\Lambda$CDM cosmographic models remain statistically competitive with standard dark-energy paramete rizations while relying on fewer assumptions regarding the functional form of $w(z)$. Our analysis demonstrates that current observations constrain the cosmic expansion history more robustly than the detailed evolution of the dark-energy equation of state\, which remains sensitive to the reconst ruction methodology employed. These results highlight the importance of mo del-independent cosmographic approaches for interpreting current evidence for dynamical dark energy and provide a natural framework for future studi es of cosmological perturbations and structure formation.\n\nhttps://indic o.ific.uv.es/event/8160/contributions/31311/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31311/ END:VEVENT BEGIN:VEVENT SUMMARY:Lunch DTSTART;VALUE=DATE-TIME:20260917T103500Z DTEND;VALUE=DATE-TIME:20260917T120000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31308@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31308/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31308/ END:VEVENT BEGIN:VEVENT SUMMARY:Timescape versus ΛCDM — precision tests of emerging spatial cur vature DTSTART;VALUE=DATE-TIME:20260917T100500Z DTEND;VALUE=DATE-TIME:20260917T103000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31306@indico.ific.uv.es DESCRIPTION:Speakers: David Wiltshire ()\nThe timescape cosmology returns to first principles\, to explain apparent cosmic acceleration in the stati stical regime of general relativity. As inhomogeneities in density and exp ansion grow\, they back react on the average cosmic expansion\, which diff ers from conventional FLRW models. Crucially\, dynamical spatial curvature arises as time-varying gradients of the kinetic energy of expansion\, dep ending directly on the volume fraction of cosmic voids.\n\nThe timescape e xpansion history is close to ΛCDM\, but with differences at a precision w hich we are now finally probing. Whereas ΛCDM is increasingly challenged\ , independent observational tests now favour timescape. In particular\, th e recent DESI evidence for "evolving dark energy" gives a dark energy "equ ation of state" w(z) consistent with timescape's non-FLRW evolution\, as p redicted in 2009. Projections made in 2014 for the Euclid mission showed t hat Euclid will distinguish FLRW expansion histories from those with emerg ing spatial curvature\, including timescape\, by the definitive Clarkson-B assett-Lu (CBL) test. The CBL test consists of two parts: the first part r equiring over 1000 precise type Ia supernova luminosity distance measureme nts was completed in our recent analysis of the Pantheon+ data\, finding v ery strong Bayesian evidence (ln B > 5) in favour of timescape over ΛCDM. Furthermore\, even restricting the sample to redshifts beyond any convent ional scale of statistical homogeneity\, z > 0.075\, timescape is preferre d over ΛCDM with ln B > 1. This was confirmed independently by the DES su rvey.\n\nThe second part of the CBL test involving Euclid BAOs over a reds hift range\, 0.7 \n\nhttps://indico.ific.uv.es/event/8160/contributions/31 306/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31306/ END:VEVENT BEGIN:VEVENT SUMMARY:Multifield cosmology with higher curvature terms DTSTART;VALUE=DATE-TIME:20260917T094000Z DTEND;VALUE=DATE-TIME:20260917T100500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31307@indico.ific.uv.es DESCRIPTION:Speakers: Lilia Anguelova (INRNE\, Bulgarian Academy of Scienc es)\nEffective actions with higher curvature terms can have cosmological s olutions exhibiting a transient phantom regime. I will discuss a generaliz ation of multifield cosmology in the presence of a higher curvature term\, namely the Gauss-Bonnet term. I will show that in this context there are novel features of the so called rapid turn regime\, in which multifield mo dels of cosmic acceleration (i.e. of inflation or dark energy) are phenome nologically distinct from single-scalar ones.\n\nhttps://indico.ific.uv.es /event/8160/contributions/31307/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31307/ END:VEVENT BEGIN:VEVENT SUMMARY:TBA DTSTART;VALUE=DATE-TIME:20260917T090000Z DTEND;VALUE=DATE-TIME:20260917T094000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31305@indico.ific.uv.es DESCRIPTION:Speakers: Martina Gerbino (INFN Ferrara)\nhttps://indico.ific. uv.es/event/8160/contributions/31305/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31305/ END:VEVENT BEGIN:VEVENT SUMMARY:Coffee Break DTSTART;VALUE=DATE-TIME:20260917T083000Z DTEND;VALUE=DATE-TIME:20260917T090000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31304@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31304/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31304/ END:VEVENT BEGIN:VEVENT SUMMARY:Dynamical dark energy from exponential f(R) gravity: cosmological tensions and neutrino mass after DESI DR2 DTSTART;VALUE=DATE-TIME:20260917T080500Z DTEND;VALUE=DATE-TIME:20260917T083000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31302@indico.ific.uv.es DESCRIPTION:Speakers: Simone D'Onofrio (ICE - CSIC)\nThe latest DESI DR2 B AO data favor a dynamical dark energy equation of state\, reviving the que stion of whether late-time modifications of gravity can ease the tensions of the standard model. We test a generalized exponential $f(R)$ model with massive neutrinos\, which produces an effective dynamical dark energy at low redshift while recovering $\\Lambda$CDM at early times. Through a Baye sian MCMC analysis combining cosmic chronometers\, DESI DR2 BAO\, the CMB acoustic scale\, and Pantheon+ supernovae\, we constrain the model jointly with the total neutrino mass and compare it with $\\Lambda$CDM and w0waCD M. The exponential $f(R)$ model is statistically favored over $\\Lambda$CD M\, partially alleviates the Hubble tension\, and mildly relaxes the cosmo logical neutrino mass bound\, while retaining the theoretical foundation t hat the phenomenological CPL parameterization lacks. These results show ho w the interplay between modified gravity and neutrino physics offers a via ble route to addressing cosmological tensions.\n\nhttps://indico.ific.uv.e s/event/8160/contributions/31302/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31302/ END:VEVENT BEGIN:VEVENT SUMMARY:Augmenting Galaxy Catalogues in FLAMINGO using Machine Learning DTSTART;VALUE=DATE-TIME:20260917T074000Z DTEND;VALUE=DATE-TIME:20260917T080500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31303@indico.ific.uv.es DESCRIPTION:Speakers: Elliot Scott (Newcastle University)\nRobust hydrodyn amic simulations are necessary for placing strong constraints on cosmologi cal parameters through the analysis pipelines of observations of statistic s such as galaxy clustering. However\, for these purposes\, the simulation s need both large box size and high resolution\, which is computationally prohibitive. In this work we use the connection between galaxies and their host dark matter halos to populate dark-matter-only simulations\, using d ata from the FLAMINGO simulations suite. We employ the Extremely Randomize d Trees algorithm to model the connection between the mass profile\, histo ry and environment of dark matter halos and the probability distribution o f the stellar mass of the galaxy contained in the halo. However\, we also demonstrate that dark matter properties which probe the centre of the dark matter profile are highly predictive when applied to data from hydrodynam ic simulations but are also sensitive to the baryonic feedback missing fro m dark-matter-only simulations. We use a Gaussian Processes emulator that simultaneously optimises the hyperparameters of our model and selects for the dark matter features which are predictive of the stellar mass while be ing insensitive to the differences between the hydrodynamic and dark-matte r-only simulations. Using this combination of features\, we produce novel catalogues from large box dark-matter-only simulations in FLAMINGO. Our ca talogue from the FLAMINGO-10k simulation reproduces the galaxy stellar mas s function in the hydrodynamic simulations to within 0.1 dex in the range of stellar masses to which the FLAMINGO stellar mass function was calibrat ed. We also reproduce the mean and scatter of the stellar mass-halo mass r elation to within 0.2 dex over a large range of halo masses. Furthermore w e find agreement in the two-point correlation function within several stel lar mass ranges to match to within 0.1 dex over a large range of length sc ales.\n\nhttps://indico.ific.uv.es/event/8160/contributions/31303/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31303/ END:VEVENT BEGIN:VEVENT SUMMARY:TBA DTSTART;VALUE=DATE-TIME:20260917T070000Z DTEND;VALUE=DATE-TIME:20260917T074000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31301@indico.ific.uv.es DESCRIPTION:Speakers: Willem Elbers (Institute for Computational Cosmology \, Durham University)\nhttps://indico.ific.uv.es/event/8160/contributions/ 31301/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31301/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing dark energy evolution with Quaia quasars through the integ rated Sachs-Wolfe effect DTSTART;VALUE=DATE-TIME:20260916T150000Z DTEND;VALUE=DATE-TIME:20260916T152500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31293@indico.ific.uv.es DESCRIPTION:Speakers: Mina Ghodsi Yengejeh (Konkoly Observatory)\nThe Inte grated Sachs--Wolfe (ISW) effect probes the late-time evolution of gravita tional potentials and provides a complementary test of the nature of dark energy. We investigate whether the redshift evolution of the ISW effect ca n provide new constraints on the time evolution of dark energy. We conside r theoretical predictions for the standard ΛCDM cosmology and alternative w0waCDM models favoured by recent DESI BAO and DES Y6 constraints. We per form a tomographic cross-correlation analysis of the Quaia quasar catalogu e and \\textit{Planck} CMB temperature maps to measure the ISW signal over a broad redshift range\, spanning about (10h−1 Gpc)3 comoving volume. W e assess the robustness of the inferred ISW amplitude against variations i n sky coverage\, multipole range\, and tomographic binning. We detect the ISW effect at a significance of 2.8σ\, corresponding to an amplitude of A ISW≃1.69±0.61 relative to the Planck ΛCDM prediction. The inferred sig nal remains stable against various analysis choices\, including various CM B maps (SMICA\, NILC\, SEVEM)\, different choices of ℓmax and the number of multipole bins\, and an alternative quasar bias model. The measured IS W amplitude is moderately stronger than predicted by the fiducial ΛCDM co smology\, and the alternative w0waCDM models do not account for this discr epancy. Future tomographic ISW measurements with improved quasar catalogue s from Gaia and forthcoming wide-area galaxy surveys such as Euclid and DE SI will help clarify the origin of this difference.\n\nhttps://indico.ific .uv.es/event/8160/contributions/31293/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31293/ END:VEVENT BEGIN:VEVENT SUMMARY:Pseudo-scalar dark energy and cosmic birefringence DTSTART;VALUE=DATE-TIME:20260916T141000Z DTEND;VALUE=DATE-TIME:20260916T143500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31294@indico.ific.uv.es DESCRIPTION:Speakers: Marco Regis (University of Torino and INFN)\nA cosmo logical pseudo-scalar field provides a compelling realization of dynamical \ndark energy (DE). If its coupling to photons is non-negligible\, the cos mic microwave background acquires a rotation of its polarization plane\, k nown as cosmic birefringence. We discuss pseudo-scalar models that can sim ultaneously account for the recent hints of evolution in the equation of s tate of DE and of the presence of cosmic birefringence.\n\nhttps://indico. ific.uv.es/event/8160/contributions/31294/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31294/ END:VEVENT BEGIN:VEVENT SUMMARY:The Universal Rotation Curve of disk galaxies: probing dark matter and the local expansion rate DTSTART;VALUE=DATE-TIME:20260916T143500Z DTEND;VALUE=DATE-TIME:20260916T150000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31297@indico.ific.uv.es DESCRIPTION:Speakers: Tiziano Schiavone (SISSA\, Trieste)\nThe Universal R otation Curve provides a powerful empirical framework to investigate the d istribution of luminous and dark matter in disk galaxies. By adopting norm alized radial and velocity coordinates\, we investigate the emergence of u niversal kinematic properties across galaxies with different masses and lu minosities. The resulting co-added rotation curves will be analyzed throug h different dark matter mass models to constrain the halo density profiles . Finally\, we discuss the use of the radial Tully–Fisher relation to ob tain an independent estimate of the Hubble constant in the local Universe. This work represents a first step toward a unified analysis of galaxy rot ation curves and their cosmological applications.\n\nhttps://indico.ific.u v.es/event/8160/contributions/31297/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31297/ END:VEVENT BEGIN:VEVENT SUMMARY:Safe Phantom Divide Crossing from Unscreened Non-Minimal Coupling to Gravity DTSTART;VALUE=DATE-TIME:20260916T134500Z DTEND;VALUE=DATE-TIME:20260916T141000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31299@indico.ific.uv.es DESCRIPTION:Speakers: Adrià Gómez-Valent (Institut de Ciències del Cosm os\, Universitat de Barcelona)\nRecent hints of dynamical dark energy\, in cluding a possible crossing of the phantom divide inferred from the latest cosmological data\, have motivated the search for viable theoretical expl anations. Scalar fields non-minimally coupled to gravity with a coupling o f the form $F(\\varphi)=1+\\alpha\\varphi^2$ are physically motivated and have emerged as promising candidates\, providing a significantly improved fit to the data compared to $\\Lambda$CDM and even outperforming the $w_0w _a$CDM parametrization. However\, in the absence of a screening mechanism\ , the regions of parameter space examined exhaustively so far in the liter ature (with $\\alpha0$) that realizes a crossing of the phantom divide whi le remaining consistent with Cassini–Huygens bounds and the most recent (and tightest) Lunar Laser Ranging measurements\, without introducing high er-derivative terms in the action. This setup\, which admittedly is subjec t to some degree of fine-tuning\, fully respects the BBN constraints and l eads only to mildly larger values of the effective gravitational coupling in the past\, peaking at the onset of dark energy domination at approximat ely 0.5\\% above Newton's constant. We review the background and linear pe rturbation dynamics of the model\, deriving illustrative analytical result s that provide physical insight into its behavior\, and update the constra ints on the model using the latest cosmological data\, including the DES-D ovekie supernova sample. We perform for the first time a full-fledged Mont e Carlo analysis with $\\alpha>0$\, studying also the impact of the variat ion of $G$ on the supernovae likelihood\, and compare the results obtained with $\\alpha\n\nhttps://indico.ific.uv.es/event/8160/contributions/31299 / LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31299/ END:VEVENT BEGIN:VEVENT SUMMARY:Coffee Break DTSTART;VALUE=DATE-TIME:20260916T131500Z DTEND;VALUE=DATE-TIME:20260916T134500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31300@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31300/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31300/ END:VEVENT BEGIN:VEVENT SUMMARY:Addressing the DESI DR2 Phantom-Crossing Anomaly and Enhanced $H_0 $ Tension with Reconstructed Scalar-Tensor Gravity DTSTART;VALUE=DATE-TIME:20260916T125000Z DTEND;VALUE=DATE-TIME:20260916T131500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31295@indico.ific.uv.es DESCRIPTION:Speakers: Leandros Perivolaropoulos ()\nRecent cosmological da ta\, including DESI DR2\, highlight significant tensions within the $\\Lam bda$CDM paradigm. When analyzed in the context of General Relativity (GR)\ , the latest DESI data favor a dynamical dark energy (DDE) equation of sta te\, $w(z)$\, that crosses the phantom divide line $w=-1$. However\, this framework prefers a lower Hubble constant\, $H_0$\, than Planck 2018\, the reby worsening the tension with local measurements. This phantom crossing is a key feature that cannot be achieved by minimally coupled scalar field s (quintessence) within GR. This suggests the need for a new degree of fre edom that can simultaneously: (A) increase the best-fit value of $H_0$ in the context of the DESI DR2 data\, and (B) allow the crossing of the $w=-1 $ line within a new theoretical approach. In this talk I will demonstrate that both of these goals may be achieved in the context of Modified Gravit y (MG)\, and in particular\, Scalar-Tensor (ST) theories\, where phantom c rossing is a natural and viable feature.\n\nhttps://indico.ific.uv.es/even t/8160/contributions/31295/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31295/ END:VEVENT BEGIN:VEVENT SUMMARY:Reconstructing the Type Ia Supernova Absolute Magnitude with Two-P robe Physics-Informed Neural Networks DTSTART;VALUE=DATE-TIME:20260916T120000Z DTEND;VALUE=DATE-TIME:20260916T122500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31296@indico.ific.uv.es DESCRIPTION:Speakers: Denitsa Staicova (Institute for Nuclear Research and Nuclear Energy)\nWe apply two variants of Physics-Informed Neural Network s (PINNs) to reconstruct the Type Ia supernova absolute magnitude M_B(z) f rom joint BAO and supernova data under four cosmological models (\\LambdaC DM\, CPL\, GEDE\, \\Lambda_sCDM) and two DESI DR2 fiducial sets. A heteros cedastic single-network method tested across four constraint configuration s establishes that the Etherington distance duality relation is more funda mental constraint than cosmological model priors\, with DDR violations of 30--52 mmag under physical constraints versus 85--2330 mmag without. Under full constraints all models recover M_B \\approx -19.3 mag with biases be low 0.05 mag. A Fisher information-weighted two-network variant trains ind ependent networks on BAO and SN data\, providing clean probe separation an d finding no significant M_B evolution in z \\in [0.3\, 1.5]. The heterosc edastic method identifies a persistent 2-3\\sigma residual at z \\sim 0.4- 0.5 that is consistent across all four models and both fiducials\; the Fis her method finds no significant pointwise deviation in z\\in[0.3\,1.5] but shows a systematic separation of redshift-binned M_B distributions consis tent with the same underlying tension. While the origin of this feature re mains ambiguous\, its model-independence and cross-method consistency warr ant further investigation with forthcoming data.\n\nhttps://indico.ific.uv .es/event/8160/contributions/31296/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31296/ END:VEVENT BEGIN:VEVENT SUMMARY:Defocusing dark energy: Raychaudhuri diagnostics beyond $w<-1/3$ a nd the phantom divide DTSTART;VALUE=DATE-TIME:20260916T122500Z DTEND;VALUE=DATE-TIME:20260916T125000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31298@indico.ific.uv.es DESCRIPTION:Speakers: Ozgur Akarsu (Istanbul Technical University (ITU))\n In general relativity\, cosmic acceleration is a statement about geometry- --the timelike defocusing of the comoving congruence---and the field equat ions source it with mass--energy combinations\, not with any equation-of-s tate ratio. Evolving dark energy is now back at the center of cosmology\, and several scenarios under active discussion---sign-switching $\\Lambda_{ \\rm s}$CDM and AdS-to-dS transitions\, which simultaneously ease the $H_0 $ and $S_8$ tensions and restore $\\sum m_\\nu$ to physical values\, as we ll as modified-gravity backgrounds recast in GR-like form---feature an eff ective dark-energy density that is negative in the past and crosses zero a t some redshift $z_\\dagger$. Our standard language quietly assumes this n ever happens: $w_{\\rm de}0$ and the inequality reverses on the negative b ranch\; the phantom divide $w_{\\rm de}=-1$ stops separating anything once the density changes sign\; at $\\rho_{\\rm de}=0$ the ratio $w_{\\rm de}$ does not exist\, though nothing physical is singular there\; and sign-pre serving parametrizations such as $w_0$--$w_a$ cannot represent the crossin g at all. In this talk\, based on arXiv:2607.18008\, we ask what defines d ark energy when $w$ cannot\, and answer with the two combinations the fiel d equations actually use: the active gravitational mass density $\\mathcal {M}=\\rho+3p$\, which drives Raychaudhuri defocusing\, and the inertial ma ss density $\\mathcal{I}=\\rho+p$\, whose zero---the null energy condition (NEC) boundary---replaces the phantom divide as the regular separator. Sh arp results follow: any smooth sign switch is phantom-like and repulsive a t the crossing\, with the total NEC intact\; the pole in $w_{\\rm de}$ is purely kinematic\, with universal residue $n(1+z_\\dagger)/3$\, so $w_{\\r m de}=-1$ is never attained and the two sides of the divide connect only t hrough the pole\; repulsion begins strictly before the switch\, at $z_{\\r m rep}>z_\\dagger$\; an exact window in $\\rho_{\\rm de}'(z_\\dagger)$ per mits acceleration at the crossing itself\; and the deceleration parameter admits exactly one or three sign-changing zeros. An analytic $\\Lambda_{\\ rm s}$CDM profile\, exponential infrared $f(T)$ gravity\, and the minimal phantom brane realize the pattern. The practical moral for reconstructions : across $\\rho_{\\rm de}=0$ the regular targets are $(\\rho_{\\rm de}\,p_ {\\rm de}\,\\mathcal{I}_{\\rm de}\,\\mathcal{M}_{\\rm de})$---kinematic to tals need no dark-sector split---and parametrizations should be allowed to change sign.\n\nhttps://indico.ific.uv.es/event/8160/contributions/31298/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31298/ END:VEVENT BEGIN:VEVENT SUMMARY:Lunch DTSTART;VALUE=DATE-TIME:20260916T103500Z DTEND;VALUE=DATE-TIME:20260916T120000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31292@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31292/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31292/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraining primordial gravitational wave amplitude and de-lensin g of CMB maps - influence of Galactic foregrounds DTSTART;VALUE=DATE-TIME:20260916T100500Z DTEND;VALUE=DATE-TIME:20260916T103000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31286@indico.ific.uv.es DESCRIPTION:Speakers: Pawel Bielewicz (National Centre for Nuclear Researc h)\nDetecting primordial gravitational waves (PGWs) is one of the main goa ls for upcoming Cosmic Microwave Background (CMB) experiments. Achieving t his objective requires precise removal of the CMB gravitational lensing si gnal from polarisation maps -- so-called de-lensing -- as well as cleaning the maps from diffuse Galactic foregrounds. In this talk\, I will present studies on influence of the Galactic emission on the reconstruction of th e CMB lensing potential and de-lensing of the divergence-free component of CMB polarization maps. Using realistic foreground models of varying compl exity\, we test the sensitivity of constraints on the primordial gravitati onal wave amplitude and the $\\sigma_8$ parameter to residual Galactic con tamination and its interplay with de-lensing. Our results highlight that p recise modelling and removal of Galactic emission will be crucial for reli ably estimating the amplitude and $\\sigma_8$ parameter in next-generation CMB experiments.\n\nhttps://indico.ific.uv.es/event/8160/contributions/31 286/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31286/ END:VEVENT BEGIN:VEVENT SUMMARY:Systematic uncertainties in optimal de-lensing of CMB B modes with cross-correlation of CMB and galaxy survey DTSTART;VALUE=DATE-TIME:20260916T094000Z DTEND;VALUE=DATE-TIME:20260916T100500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31287@indico.ific.uv.es DESCRIPTION:Speakers: Kishan Deka ()\nIn the era of high-precision Cosmic Microwave Background (CMB) anisotropy measurements\, detection of primordi al gravitational waves (PGWs) will be one of the main goals of current CMB experiments. Detection of a divergence-free (B-mode) component in CMB pol arisation will provide direct evidence of inflationary PGWs in the early u niverse. However\, weak gravitational lensing of CMB photons due to interv ening mass distributions of the Universe distorts the primordial polarisat ion patterns\, introducing an additional lensing-induced B-mode signal. Re moving these lensing-induced B-modes is essential for improving constraint s on the amplitude of PGWs. In this work\, we test a tomographic delensing method on simulations of the Rubin Observatory LSST galaxy catalogue and Simons Observatory (SO) CMB maps. A significant improvement in delensing e fficiency is achieved by using a multi-tracer approach\, where we split th e galaxy dataset into tomographic redshift bins. However\, uncertainties i n photometric redshift measurements pose a problem for optimal weighting o f the tracers. We explore the impact of photometric redshift errors with r ealistic simulations and build a pipeline to propagate these uncertainties to constraints on the amplitude of primordial gravitational waves. Additi onally\, we explore constraints on the galaxy bias\,b(z)\, and the amplitu de of matter fluctuations parameter\,σ8\, through tomographic cross-corre lations using realistic simulations of photometric measurements from LSST 10-year datasets.\n\nhttps://indico.ific.uv.es/event/8160/contributions/31 287/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31287/ END:VEVENT BEGIN:VEVENT SUMMARY:Cobaya development updates DTSTART;VALUE=DATE-TIME:20260916T090000Z DTEND;VALUE=DATE-TIME:20260916T094000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31291@indico.ific.uv.es DESCRIPTION:Speakers: Jesus Torrado (Instituto de Estructura de la Materia (IEM-CSIC))\nhttps://indico.ific.uv.es/event/8160/contributions/31291/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31291/ END:VEVENT BEGIN:VEVENT SUMMARY:Coffee Break DTSTART;VALUE=DATE-TIME:20260916T083000Z DTEND;VALUE=DATE-TIME:20260916T090000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31290@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31290/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31290/ END:VEVENT BEGIN:VEVENT SUMMARY:Revisiting the Hubble Constant with FRBs: Evidence for Redshift Ev olution DTSTART;VALUE=DATE-TIME:20260916T080500Z DTEND;VALUE=DATE-TIME:20260916T083000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31289@indico.ific.uv.es DESCRIPTION:Speakers: Surajit Kalita (University of Warsaw)\nFast Radio Bu rsts (FRBs) are millisecond radio transients with high dispersion measures \, making them powerful tracers of ionized matter across cosmological dist ances. In this talk\, I will present two complementary approaches\, Bayesi an analysis and machine learning\, applied to a set of localized FRBs to r igorously test the consistency of the $\\Lambda$CDM model at late cosmic e poch. Our results reveal a redshift evolution of the Hubble constant\, a b ehavior that stands in contradiction to the core postulate standard cosmol ogy. I will further show that this discrepancy can be resolved for alterna te cosmological models. These findings suggest a fundamental inadequacy in the standard cosmological framework and necessitate a deeper revision of the theoretical underpinnings of cosmology to resolve the Hubble tension.\ n\nhttps://indico.ific.uv.es/event/8160/contributions/31289/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31289/ END:VEVENT BEGIN:VEVENT SUMMARY:Geometric Constraints on the Pre-Recombination Expansion History f rom the Hubble Tension DTSTART;VALUE=DATE-TIME:20260916T074000Z DTEND;VALUE=DATE-TIME:20260916T080500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31288@indico.ific.uv.es DESCRIPTION:Speakers: Davide Pedrotti (TIFPA-INFN\, Università di Trento) \nI perform a model-independent reconstruction of the background pre-recom bination expansion history of the Universe. I find that purely early-time resolutions to the Hubble tension\, satisfying the geometric CMB constrain ts\, exist at the background level. This class of solutions requires a smo oth transition around matter-radiation equality\, characterized by a ≃15 % expansion rate enhancement prior to recombination. This result serves as a blueprint for future model-building approaches\, providing a background stress-test for Hubble tension proposals.\n\nhttps://indico.ific.uv.es/ev ent/8160/contributions/31288/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31288/ END:VEVENT BEGIN:VEVENT SUMMARY:H0 (+other things) from GW Sirens DTSTART;VALUE=DATE-TIME:20260916T070000Z DTEND;VALUE=DATE-TIME:20260916T074000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31285@indico.ific.uv.es DESCRIPTION:Speakers: Tessa Baker (University of Portsmouth)\nhttps://indi co.ific.uv.es/event/8160/contributions/31285/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31285/ END:VEVENT BEGIN:VEVENT SUMMARY:Wising up to CatWISE: using simulation-based inference to measure the cosmic dipole DTSTART;VALUE=DATE-TIME:20260915T141000Z DTEND;VALUE=DATE-TIME:20260915T143500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31277@indico.ific.uv.es DESCRIPTION:Speakers: Oliver Oayda (The University of Sydney)\nWe apply Si mulation-Based Inference ('SBI') to the cosmic dipole problem for the firs t time\, measuring the distribution of quasar counts over the sky in the i nfrared CatWISE2020 sample. Our SBI-based approach alleviates systematic e ffects arising from the WISE instrument itself and enables direct inferenc e of the sample's dipole. We find a dipole that is twice as large as the C MB expectation but more seriously misaligned with the CMB direction (≈3 σ)\, adding further evidence to the persistent 'dipole tension'. This rem ains a serious challenge for ΛCDM. However\, our result highlights the po wer of SBI at machine-inferring a likelihood function in the presence of d ifficult systematics\, which will make it a natural choice for robust infe rence with new datasets. For example\, in the radio regime\, the Rapid ASK AP Continuum Survey contains a wealth of unexplored information but has po ssible systematics that must be understood before measuring the dipole. SB I will be a natural technique to disentangle the signal from the systemati c\, shedding new light on the dipole tension.\n\nhttps://indico.ific.uv.es /event/8160/contributions/31277/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31277/ END:VEVENT BEGIN:VEVENT SUMMARY:Simulation-based tension quantification of the cosmic dipole anoma ly DTSTART;VALUE=DATE-TIME:20260915T143500Z DTEND;VALUE=DATE-TIME:20260915T150000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31278@indico.ific.uv.es DESCRIPTION:Speakers: Mali Land-Strykowski (UNIVERSITY OF SYDNEY)\nThe co smic dipole observed in the matter distribution of galaxy surveys consiste ntly disagrees with the kinematic expectation set by the cosmic microwave background\, posing a serious challenge to the Cosmological Principle and the standard model of cosmology. However\, the fidelity of the dipoles we infer rests on our understanding of the systematics present in the surveys . For many systematics\, their analytical effect on the source counts is u nknown\, rendering the likelihood function intractable. We demonstrate tha t Simulation-Based Inference (SBI) is an effective tool for quantifying te nsions between cosmic dipole data sets\, enabling inference when likelihoo ds are intractable. Here\, we apply neural-ratio estimation to the cosmic dipole for the first time\, recovering tensions between Planck\, NVSS\, RA CS\, and CatWISE under different treatments of systematics. Our SBI archit ecture provides a robust machinery for future dipole analyses with LSST\, Euclid\, and the SKA\, where it will be essential to model complex observa tional systematics.\n\nhttps://indico.ific.uv.es/event/8160/contributions/ 31278/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31278/ END:VEVENT BEGIN:VEVENT SUMMARY:Beyond LCDM with future surveys: Rubin LSST\, SKAO and Simons Obse rvatory DTSTART;VALUE=DATE-TIME:20260915T134500Z DTEND;VALUE=DATE-TIME:20260915T141000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31279@indico.ific.uv.es DESCRIPTION:Speakers: Chandra Shekhar Saraf (Korea Astronomy and Space Sci ence Institute)\nRecent results from the Dark Energy Spectroscopic Instrum ent has shifted our understanding about dark energy\, preferring about 2-3 sigma evidence for evolving dark energy. The phantom crossing of the dark energy equation of state has motivated the search of new cosmological mod els. In this talk\, I will discuss how combinations of data from Rubin Obs ervatory LSST\, Simons Observatory and SKAO can assist in better understan ding the nature of dark energy and solutions to cosmological tensions. I w ill present forecasts on Rapid Transition Dark Energy and Early Dark Energ y models\, and discuss the challenges and systematics in different dataset s. Specifically\, I will present which combinations to datasets generate b est constraints on extended models.\n\nhttps://indico.ific.uv.es/event/816 0/contributions/31279/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31279/ END:VEVENT BEGIN:VEVENT SUMMARY:Coffee Break DTSTART;VALUE=DATE-TIME:20260915T131500Z DTEND;VALUE=DATE-TIME:20260915T134500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31283@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31283/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31283/ END:VEVENT BEGIN:VEVENT SUMMARY:Convergence in the value of H0 from Type Ia Supernovae DTSTART;VALUE=DATE-TIME:20260915T125000Z DTEND;VALUE=DATE-TIME:20260915T131500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31281@indico.ific.uv.es DESCRIPTION:Speakers: PIlar Ruiz-Lapuente (Instituto de Física Fundamenta l (CSIC) and ICCUB)\nConvergence in the value of H0 from Type Ia Supernova e\n\n In this talk\, I will review new findings that point towards a\n c oncordant value of the Hubble constant (H0) from data based in\n the SH0 ES collaboration and the Chicago--Carnegie Supernova Project\n using the ''SNe Ia twins method'' and using\, as well\, the common\n ''SNe Ia ligh t curve method''.\n There has been usually a discrepancy in the H0 value given by the\n two collaborations. Here we show that such disagreement sh ould not exist. \n I will present the advancement to convergence in the v alue of H0 and\n the improvements being made in the field.\n\nhttps://ind ico.ific.uv.es/event/8160/contributions/31281/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31281/ END:VEVENT BEGIN:VEVENT SUMMARY:Lunch DTSTART;VALUE=DATE-TIME:20260915T104000Z DTEND;VALUE=DATE-TIME:20260915T121000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31276@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31276/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31276/ END:VEVENT BEGIN:VEVENT SUMMARY:Coffee Break DTSTART;VALUE=DATE-TIME:20260915T084000Z DTEND;VALUE=DATE-TIME:20260915T091000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31274@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31274/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31274/ END:VEVENT BEGIN:VEVENT SUMMARY:AMICO galaxy clusters in KiDS-1000: cosmological constraints from the two-point correlation function DTSTART;VALUE=DATE-TIME:20260915T101500Z DTEND;VALUE=DATE-TIME:20260915T104000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31271@indico.ific.uv.es DESCRIPTION:Speakers: Massimiliano Romanello (University of Bologna)\nWe study the clustering of an optically identified galaxy cluster catalogue f rom the fourth data release of the Kilo Degree Survey (KiDS-1000). The pho tometric sample was identified by the Adaptive Matched Identifier of Clust ered Objects (AMICO) algorithm and consists of 9049 clusters with $S/N\\ge q3.5$\, in redshift range $0.1\\leq z\n\nhttps://indico.ific.uv.es/event/8 160/contributions/31271/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31271/ END:VEVENT BEGIN:VEVENT SUMMARY:CORN - Chronometers Of Relic Nature: Estimate of the expansion rat e of the Universe using compact relic galaxies DTSTART;VALUE=DATE-TIME:20260915T081500Z DTEND;VALUE=DATE-TIME:20260915T084000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31272@indico.ific.uv.es DESCRIPTION:Speakers: Krzysztof Lisiecki (National Centre for Nuclear Rese rach\, Poland)\nThe persistent discrepancy between the locally measured Hu bble constant\, derived from Cepheids and Type Ia supernovae\, and the val ue inferred from the cosmic microwave background underscores the need for independent cosmological probes. Cosmic chronometers provide a direct\, mo del-independent measurement of the expansion history\, but their accuracy is currently limited by systematic uncertainties in stellar population mod elling\, particularly when the full red and quiescent population is used. \nI propose an alternative chronometer strategy based on relic galaxies: t he oldest\, most compact\, and most dynamically evolved systems at a given epoch. These galaxies are expected to host uniformly old\, rapidly formed stellar populations with minimal subsequent mass growth\, making them clo ser to ideal single-burst populations. By focusing on this population\, we can reduce uncertainties associated with composite star formation histori es and mitigate biases arising from late-time rejuvenation.\nIn this work I use the largest catalogue of relics\, to construct a cleaner differentia l age–redshift relation. Particular emphasis will be placed on assessing the limitations of current single stellar population models\, including m etallicity\, initial mass function\, and alpha-enrichment. By quantifying how these ingredients affect absolute and differential age estimates\, we aim to establish a more robust systematic floor for the chronometer method . A relic-based approach has the potential to tighten stellar age constrai nts at fixed redshift\, refine the expansion history measurement\, and pro vide an independent perspective on the Hubble tension.\n\nhttps://indico.i fic.uv.es/event/8160/contributions/31272/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31272/ END:VEVENT BEGIN:VEVENT SUMMARY:New Constraints on the Varying Electron Mass Solution to the Hubbl e Tension DTSTART;VALUE=DATE-TIME:20260915T095000Z DTEND;VALUE=DATE-TIME:20260915T101500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31273@indico.ific.uv.es DESCRIPTION:Speakers: Yo Toda (Kochi University of Technology)\nDespite it s remarkable success\, the standard cosmological model\, $\\Lambda$CDM\, f aces several serious challenges. Among them\, the “Hubble tension”—t he discrepancy between the value of the Hubble constant inferred from obse rvations of the early Universe and that obtained directly from local measu rements—is one of the most important problems in modern cosmology. As a possible solution to this tension\, models in which the electron mass vari es with time around the epoch of recombination have been proposed.\n\nIn t his talk\, I will provide an overview of how a time-varying electron mass modifies the recombination history and affects the sound-horizon scale\, t hereby potentially alleviating the Hubble tension. I will then present the observational constraint $\\frac{m_e}{m_{e\,0}} = 1.0101 \\pm 0.0046$\, o btained using the Markov Chain Monte Carlo code COBAYA from a combined ana lysis of the latest cosmic microwave background data from Planck\, baryon acoustic oscillation data from DESI\, and Type Ia supernova data from Pant heon+. Finally\, I will discuss the physical implications of this result.\ n\nhttps://indico.ific.uv.es/event/8160/contributions/31273/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31273/ END:VEVENT BEGIN:VEVENT SUMMARY:Evidence of deviations from LCDM from a new Hubble Diagram of Qua sars DTSTART;VALUE=DATE-TIME:20260915T075000Z DTEND;VALUE=DATE-TIME:20260915T081500Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31270@indico.ific.uv.es DESCRIPTION:Speakers: Guido Risaliti (Università di Firenze)\nI present n ew cosmological fits to a Hubble diagram built from supernovae and a homog eneous quasar sample spanning a redshift interval z = 0.7--3.5. The quasar distances are derived from the non-linear relation between X-ray and UV l uminosities\, and the sample is selected to minimize dust reddening\, gas obscuration\, host-galaxy contamination\, and selection biases as describe d in the companion paper. This provides high-quality constraints in a reds hift range otherwise poorly covered by Type~Ia supernovae. The main result s are: (1) the combined Hubble diagram shows strong (> 4 σ) tension with the standard flat ΛCDM model at z ≥ 1.5\; (2) in the overlap region\, t he quasar and supernova Hubble diagrams are fully consistent\, supporting a common distance scale\; (3) allowing for an evolving dark-energy equatio n of state yields a significantly better fit\, with w_0 and w_a values com patible with those favored by recent DESI results\; (4) our quasar Hubble diagram and cosmological constraints agree closely with an independent ana lysis based on ~6\,000 quasars standardized via variability distances (Dut ra et al.~2026). The convergence of two independent quasar methods strengt hens the case that the deviation from flat lcdm at high redshift is not dr iven by sample-specific systematics.\n\nhttps://indico.ific.uv.es/event/81 60/contributions/31270/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31270/ END:VEVENT BEGIN:VEVENT SUMMARY:Overview of the ESA Euclid mission DTSTART;VALUE=DATE-TIME:20260915T071000Z DTEND;VALUE=DATE-TIME:20260915T075000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31269@indico.ific.uv.es DESCRIPTION:Speakers: Valeria Pettorino (ESA ESTEC)\nTBA\n\nhttps://indico .ific.uv.es/event/8160/contributions/31269/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31269/ END:VEVENT BEGIN:VEVENT SUMMARY:Opening Talks DTSTART;VALUE=DATE-TIME:20260915T070000Z DTEND;VALUE=DATE-TIME:20260915T071000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31268@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31268/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31268/ END:VEVENT BEGIN:VEVENT SUMMARY:Registration DTSTART;VALUE=DATE-TIME:20260915T061500Z DTEND;VALUE=DATE-TIME:20260915T070000Z DTSTAMP;VALUE=DATE-TIME:20261012T033636Z UID:indico-contribution-8160-31266@indico.ific.uv.es DESCRIPTION:https://indico.ific.uv.es/event/8160/contributions/31266/ LOCATION: URL:https://indico.ific.uv.es/event/8160/contributions/31266/ END:VEVENT END:VCALENDAR