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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:20260922T160947Z
UID:indico-contribution-5707-31313@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/
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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:20260922T160947Z
UID:indico-contribution-5707-31314@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/
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BEGIN:VEVENT
SUMMARY:Primordial Black Holes as Cosmic Expansion Accelerators
DTSTART;VALUE=DATE-TIME:20260917T150000Z
DTEND;VALUE=DATE-TIME:20260917T152500Z
DTSTAMP;VALUE=DATE-TIME:20260922T160947Z
UID:indico-contribution-5707-31315@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/
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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:20260922T160947Z
UID:indico-contribution-5707-31316@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/
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BEGIN:VEVENT
SUMMARY:Coffee Break
DTSTART;VALUE=DATE-TIME:20260917T131500Z
DTEND;VALUE=DATE-TIME:20260917T134500Z
DTSTAMP;VALUE=DATE-TIME:20260922T160947Z
UID:indico-contribution-5707-31312@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:20260922T160947Z
UID:indico-contribution-5707-31309@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/
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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:20260922T160947Z
UID:indico-contribution-5707-31310@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:20260922T160947Z
UID:indico-contribution-5707-31311@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/
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