CosmoVerse@Kraków

9 Jul 2024, 08:00 → 11 Jul 2024, 20:00 Europe/Warsaw

Kraków

CosmoVerse@Krakow (9 July - 11 July 2024) is the second annual conference in a series of conferences that aim to establish a link between the different research areas in cosmology with the main focus on challenges of tensions in cosmological survey data.

 

This conference is organized within the COST Action initiative CA21136 - Addressing observational tensions in cosmology with systematics and fundamental physics (CosmoVerse). Learn more about CosmoVerse action at https://cosmoversetensions.eu/

The first conference called CosmoVerse@Lisbon 2023 took place in Lisbon. All of the recorded talks and presentations are public at (https://cosmoversetensions.eu/event/first-cosmoverse-conference-cosmoverselisbon/)

The conference is organized together with Jagiellonian University in Kraków, and National Centre for Nuclear Research in Warsaw.

 

Main topics:

• Observational cosmology and Systematics (cross-correlation of data, systematic effects)  
• Data analysis (astrostatistics; data science in astronomy; Bayesian analysis; machine learning and artificial intelligence)  
• Fundamental Physics (challenge of the cosmological hypothesis, dark energy and modified gravity, neutrino physics, dark energy, and dark matter interaction)

 

** WARNING: Regarding hotel bookings: conference organizers HAVE NEVER AUTHORISED ANY COMPANY to send any requests regarding accommodation or travel. We strongly advise you NOT TO reply to any emails or calls from such companies and we do not accept any responsibility for adverse consequences should you choose to do so.

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Invited speakers

Stefano Anselmi, INFN, Sezione di Padova, Italy
Ariel Goobar, Stockholm University, Sweden
Wendy Freedman, University of Chicago, USA (online)
Tanvi Karwal, Kavli Institute for Cosmological Physics, The University of Chicago, USA
Lloyd Knox, UC Davis, USA
Adam Riess, Johns Hopkins University, USA
Mairi Sakellariadou, King’s College London, UK

 

 

Venue:

The conference will take place in Kraków at Faculty of Physics, Astronomy and Applied Computer Science of the Jagiellonian University in the period 9 July - 11 July 2024.

 

Important dates:

2023 December 18th: Registration and abstract submission opens
2024 May 10th: Registration and abstract submission deadline
2024 July 9th-11th: Conference days 
2024 July 10th Conference Dinner
2024 July 11th Public Lecture

(2024 July 12th MC meeting for the committee)

 

 

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Tuesday, 9 July

Morning 1

Convener: Jackson Said (University of Malta)

1 Welcome talks

2 Plenary 1: Time-domain Cosmology in the Era of Large Surveys

Speaker: Ariel Goobar

3 Updating cosmological tensions using the most recent datasets from early and late Universe probes

In the recent years, with the improvement on the precision of the different cosmological probes, the rise of some of the tensions and anomalies that affect the standard model of cosmology, like the H0-tension, the sigma_8-tension and the lensing anomaly, has motivated the study of alternative models to the standard LCDM model in order to reconcile these tensions. In this talk, I will show some re-analysis of some of the most common extensions of LCDM with different combinations of the latest datasets such as Planck PR4, type Ia SN and the DESI BAO 2024, in order to see if it is possible to alleviate the tensions

Speaker: Jacobo Asorey Barreiro (Universidad Complutense de Madrid & IPARCOS)

4 New insights on neutrino interactions with dark matter from CMB data

In the talk, I will revisit the possibility of using cosmological observations to constrain models that involve interactions between neutrinos and dark matter. I will show that small-scale measurements of the cosmic microwave background with a few percent accuracy are critical to uncovering unique signatures from models with small couplings that would require a much higher sensitivity at lower multipoles. In order to test this, the currently available high-multipole data have been analyzed, both independently and in combination with low-multipole CMB and Baryon Acoustic Oscillation measurements, finding a preference for a non-vanishing coupling at 68% CL. This aligns with other CMB-independent probes, such as Lyman-α. I will illustrate how this coupling could be accounted for in dark matter interactions with a sterile neutrino.

Speaker: Sebastian Trojanowski (National Centre for Nuclear Research (NCBJ))

Cosmoverse_July2024_Trojanowski.pdf

10:50 Coffee Break

Morning 2

Convener: Elsa Teixeira

5 Breaking the cosmic degeneracies with non-standard probes

Classical LSS probes of growth rate/gravity relies on clustering statistics, RSD and lensing. Most observables related to those techniques suffer from various biases and degeneracies. To the most severe problems include: theoretical bias related to the way how the signal is modelled and extracted and baryonic effects leading to degeneracy of the clustering strength signal with the efficiency of various galaxy formation processes.

I will discuss some non-standard probes (including peculiar velocities and clustering amplitudes) and their combination that can be used for cross-correlating with standard probes to estimate the unknown systematic errors. This opens an avenue to mitigate mentioned problems and used better accuracy for cosmological constraints on gravity and the growth-rate. Using non-standard probes offers also an unique way for a cosmology self-consistency test of the current data sets. Such tests can significantly help in hunting of unknown systematics - a crucial topic in the context of existing observational tensions in the LCDM (like S8 and H0 tensions).

Speaker: Wojciech Hellwing (Center for Theoretical Physics PAS)

6 Distance measurements with Active Galactic Nuclei

Measuring cosmic distances accurately is a critical challenge in astrophysics, pivotal for our understanding of the Universe expansion history and for testing cosmological models. In this talk, I will explore two innovative methods for using Active Galactic Nuclei (AGN) as tools for distance measurement. AGN, notable for their extreme luminosity, can be observed even at high redshifts; however, their variable emission precludes straightforward distance estimations based on flux measurements alone. I will describe two techniques developed to standardize AGN and use them for distances. Firstly, I will examine the X-ray – UV luminosity relation in quasars—the most luminous types of AGN. I will discuss recent advancements in enhancing the reliability and precision of distance estimates obtained with this relation and how they challenge the standard ΛCDM cosmological model's predictions when implemented with SNe in the Hubble Diagram. Secondly, I will explore the correlation between AGN X-ray variability and black hole mass, utilizing the BASS dataset at low redshifts to characterize it. Additionally, I will discuss the potential impacts of forthcoming data from the Euclid, LSST, and Athena missions.

Speaker: Matilde Signorini (University of Roma 3)

7 Is the cosmological principle in trouble?

I will present our recent results exploring the integrity of the cosmological principle, the idea that, on sufficient scales, the universe is homogeneous and isotropic. Recent tensions have arisen between the dipole of cosmological sources and its interpretation from the CMB as a kinematic departure from the local Hubble Flow, bringing the cosmological principle into doubt. With a Bayesian-based approach, I explore the cosmological dipole in optical/IR catalogues of quasars, using Bayesian evidence to assess differing hypotheses. The conclusion is, that whilst the picture is not completely clear, the results support the veracity of the cosmological principle.

Speaker: Prof. Geraint Lewis (The University of Sydney)

12:35 Lunch Break

Afternoon 1

Convener: Agnieszka Pollo (National Centre for Nuclear Research, Warsaw, Poland)

8 Marginalization approach in Baryonic Acoustic Oscillation - what we have learned so far?

Baryonic Acoustic Oscillations (BAO), with their intrinsic connection to the physics of both the early and late universe, offer a great opportunity to gain insights into the Hubble tension. This talk will summarize recent results obtained by analyzing BAO datasets. We will discuss the challenges in using BAO, particularly the degeneracy between the Hubble constant (H_0) and the sound horizon (r_d) and we will then present our marginalization technique to overcome this problem. We will discuss the results from the application of this method in constraining different dark energy models, including our most recent work dedicated to the interacting dark energy (IDE).

Speaker: Denitsa Staicova (INRNE, Bulgarian Academy of Sciences)

DStaicova_BAO_Krakow.pdf

9 Inflation and the Hubble Tension

CMB temperature and polarization measurements from the Planck satellite and the BICEP/Keck collaboration have established stringent constraints on the amplitude of primordial gravitational waves (r < 0.036) and the spectral index of scalar modes (ns = 0.9649 ± 0.0044), severely limiting a multitude of inflationary models. In this talk, I will discuss if and to what extent the Hubble tension represents an element of uncertainty surrounding these results. I will argue that solutions involving new physics at early times (i.e., before recombination) could have significant implications for inflation. Even mild deviations from an early-time ΛCDM cosmology (potentially supported by current data) could significantly change our conclusions regarding which inflationary models are favored/disfavored by current data. Based on these results, there is solid ground to assert that the constraints on inflationary parameters may be influenced by the cosmological model, potentially to a greater degree than commonly realized, and therefore that the presence of the Hubble tension could represent a non-negligible source of uncertainty for inflation.

Speaker: William Giarè (University of Sheffield)

Giare_Krakow.pdf

10 Reconnaissance with JWST of the J-region Asymptotic Giant Branch in Distance Ladder Galaxies: From Irregular Luminosity Functions to Approximation of the Hubble Constant

We study stars in the J-regions of the asymptotic giant branch (JAGB) of near-infrared color magnitude diagrams in the maser host NGC 4258 and 4 hosts of 6 Type~Ia~supernovae (SN~Ia): NGC 1448, NGC 1559, NGC 5584, and NGC 5643. These clumps of stars are readily apparent near $1.0

Speaker: Siyang Li (Johns Hopkins University)

15:45 Coffee Break

Afternoon 2

Convener: Ariel Goobar

11 Planery 3: The Hubble Tension: New Results from JWST [Online]

Speaker: Wendy Freedman

12 Detection of the lensed quasars by the Nancy Grace Roman Space Telescope

Strong gravitational lensing is a powerful tool for mapping the distribution of dark matter and testing various cosmological parameters. One such parameter is the Hubble Constant, which can be determined by measuring the time delay between lensed images. Our study focuses on the detection of lensed quasars by forthcoming Nancy Grace Roman Space Telescope (Roman) survey. Based on the capability of the Roman telescope and the recent results for the Quasar Luminosity Function (QLF) in the infrared band of Spitzer Space Telescope imaging survey, we find the number of quasars that will be observed by Roman telescope. Also, we develop Monte Carlo simulations using the mass-luminosity distribution function of galaxies and the redshift distributions of galaxies and quasars to find the efficiency that a quasar to be lensed by foreground galaxies. Even though this survey is not primarily designed as a strong lensing detection experiment, it will still provide a large complementary catalogue to forthcoming lensing discovery projects.

Speaker: Lindita Hamolli (University of Tirana)

13 Hubble tension and its redshift tomography

I will review the essence of the Hubble tension, its current observational status and the three classes of theoretical models that attempt to address it. Then I will focus on the level of the tension in redshift bins as expressed by the mismatch between distances measured by BAO data and by SnIa data calibrated respectively by the CMB sound horizon scale and by the Cepheid based distance ladder. The variation of the tension with redshift will be discussed and its possible implications for theoretical models will be analysed.

Speaker: Prof. Leandros Perivolaropoulos (University of Ioannina)

leandros-peri1.pdf

17:45 Welcome Party + Poster Session

Wednesday, 10 July

Morning 1

Convener: Leandros Perivolaropoulos (University of Ioannina)

14 Plenary 1 Mairi Sakellariadou

Speaker: Prof. Mairi Sakellariadou

15 Plenary: The challenges of using Baryon Acoustic Oscillations distances for cosmology

Speaker: Prof. Stefano Anselmi

10:20 Coffee Break

Morning 2

Convener: Tanvi Karval

16 Talk 1

Speaker: Daniela Grandón

17 A dark matter solution to the H0 and S8 tensions, and the integrated Sachs-Wolfe void anomaly

We consider a phenomenological model of dark matter with an equation-of-state that is negative and changing at late times. We show that this couples the $H_{0}$ and $\sigma_8$ tensions, providing an explanation for both simultaneously, while also providing an explanation for the anomalously large integrated Sachs-Wolfe (ISW) effect from cosmic voids. Observations of high ISW from cosmic voids may therefore be evidence that dark matter plays a significant role in the $H_{0}$ and$\sigma_8$ tensions. We predict the ISW from cosmic voids to be a factor of $\sim2$ greater in this model than what is expected from the standard model $\Lambda$CDM.

Speaker: Mariana Jaber Bravo (CFT Polish Academy of Sciences)

18 BAO Anomalies after DESI Release

In the era of tensions, when precision cosmology is blooming, numerous new theoretical models are emerging. However, it's crucial to pause and question the extent to which the observational data we rely on are model-dependent. In this work, we study the comoving position of the acoustic peak, a cornerstone standard ruler in cosmology. We considered BAO observational datasets from two distinct teams and calculated $r_d$ sound horizon value with the help of each BAO data set along with SN I-a data from the Pantheon Plus sample. Our conclusion at present is there is a significant amount of tension within two independent BAO datasets. We further go on to say that while one BAO data set allows solutions like Early Dark Energy, the other completely rules out $r_d$ tension and hence the possibility of early modifications of $r_d$ such as EDE as a solution to Hubble Tension.

Speaker: Ruchika Ruchika (INFN, Rome)

12:05 Conference Photo + Lunch Break

Afternoon 1

Convener: Denitsa Staicova (INRNE, Bulgarian Academy of Sciences)

19 BREAKING PLANCK’S LENSING ANOMALY: A PARAMETRIC APPROACH

Parametrising the growth of large scale structure is a powerful tool, as it allows us to detect deviations from the Standard Model of cosmology - SM in a general way, without having to make limiting assumptions about their fundamental nature. We will be presenting the results of a series of analyses carried on two such parametrisations: the growth index - ‘$\gamma$’, a precise modification of the growth of linear, sub-horizon matter perturbations in the SM, and the ‘$\mu_0$ − $\Sigma_0$’ framework, a modification of the Poisson and lensing equations from General Relativity - GR. Notably, Planck’s 2018 analysis has shown a $2\sigma$ evidence of Modified Gravity - MG (i.e., $\mu_0$, $\Sigma_0 \neq 0$), while other Cosmic Microwave Background - CMB experiments such as ACT and SPT showed consistency with GR. Could Planck’s lensing anomaly be responsible for this? The goal of our work is to show if the link between the loss of power at high multipoles in the anisotropy power spectra of Planck and the detected evidence for MG stands the test of alternative approaches to analyse Planck’s data, as the one taken by the HiLLiPoP team who, consistently with other CMB experiments, have found no sign of abnormal lensing signals. We find that the usage of the HiLLiPoP likelihood on Planck data does not reveal any deviation from the SM, suggesting that the lensing anomaly could plausibly explain the MG detection by Planck.

Speaker: Enrico Specogna

20 Lighting Dark Ages with ISW Effect

The integrated Sachs-Wolfe effect (ISW) describes how CMB photons pick up a net blue or redshift when traversing the time-varying gravitational potentials between the last scattering surface and us. Deviations from its standard amplitude could hint new physics. We show that reconstructing the amplitude of the ISW effect as a function of the redshift may provide a unique tool to probe the gravity sector during the era of dark ages, inaccessible via other cosmological observables. Exploiting Planck CMB temperature, polarization and lensing observations, we find a $2\sigma$ deviation from the standard ISW amplitude at redshift $z=500$. Barrying a systematic origin, our findings could point to either possibly new physics or a departure from the standard picture of structure formation under the General Relativity framework. Assuming the simplest two-redshift-bin scenario, we ensure $38\sigma$ and $2\sigma$ evidences of the early and late ISW effects, respectively, despite a priori possible degeneracy with the CMB lensing amplitude. Using a multiple tomographic method, we present the first complete characterization of the ISW effect over $k$-space and time. Future tomographic ISW analyses are therefore crucial to probe the dark ages at redshifts otherwise unreachable via other probes.

Speaker: Deng Wang (IFIC, CSIC-University of Valencia)

21 Slicing Through the Tension: The Future of Cosmological Weak Lensing

Cosmological information contained within the non-linear regime of the Universe may prove crucial in solving the tension currently observed between weak lensing and CMB probes. However, this information lies beyond the reach of our conventional analyses which use two-point statistics. In this talk, I present the improvements in cosmological constraining power offered by an alternative weak lensing statistic, the projected matter density PDF. For realistic lensing survey specifications, this statistic yields >50% improvements in the constraints on the matter energy density parameter,  $Ω_m$, and the amplitude of the matter power spectrum, $σ_8$.  We also find significantly improved precision for the Hubble parameter, $H_0$, and the dark energy equation of state parameter, $w_0$. I will demonstrate how these gains in cosmological constraining power can be made reality with tailored numerical simulations paired and machine learning.

Speaker: Benjamin Giblin (University of Edinburgh)

22 A dark standard siren measurement of the Hubble constant following LIGO/Virgo/KAGRA O4a and the Legacy Survey

We present a new constraint on the Hubble constant (H0) from the standard dark siren method using a sample of 5 well-covered gravitational wave (GW) alerts reported during the first part of the fourth LIGO/Virgo/KAGRA observing runs in combination with standard dark sirens from the first three runs. Our methodology relies on the galaxy catalog method alone. We use the full probability density estimation of photometric redshifts derived by a deep learning method using the DESI Legacy Survey and DELVE galaxy catalogs. We add the constraints from 5 new well-localized binary black hole mergers to the sample of standard dark sirens analyzed in Alfradique et al. (2024). We combine the H0 posterior for 5 new standard sirens with other 10 previous events (3 with updated posteriors), finding H0=69.9^{+13.3}{−12.0} km s−1 Mpc−1 (68% Highest Density Interval) with the catalog method alone. This result represents an improvement of ∼23% comparing the new 15 dark siren constrain with the previous 10 dark siren constraint, and a reduction in uncertainty of ∼40% from the combination of 15 dark and bright sirens compared with the GW170817 bright siren alone. The combination of dark and bright siren GW170817 with recent jet constraints yields H0 of 68.0^{+4.3}{−3.8} km s−1 Mpc−1, a ∼6% precision from Standard Sirens, reducing the previous constraint uncertainty by ∼10% .

Speaker: Prof. Clecio Bom (Centro Brasileiro de Pesquisas Físicas)

15:40 Coffee Break

Afternoon 2

Convener: Eleonora Di Valentino (University of Sheffield)

23 Plenary 3 The Hubble Tension: JWST and HST Agree [Online]

Speaker: Prof. Adam Riess

24 KiDS-SBI: Simulation-Based Inference Analysis of KiDS-1000 Cosmic Shear

Cosmic shear, the weak gravitational lensing effect on distant galaxies due to matter in the foreground, is a powerful tool to study the distribution of matter, to probe its large-scale structure, and infer the cosmological model of the Universe. Standard analyses are typically based on the assumption of a Gaussian likelihood with a parameter-independent covariance, but these assumptions may not hold for all observables, scales and/or all systematics. Simulation-based inference (SBI) addresses this by evaluating an effective likelihood from forward-simulations which map parameters to data vectors. To this end, I will present a novel application of SBI to a cosmic shear analysis of the Kilo-Degree Survey's KiDS-1000 data release. The forward model is based on lognormal random fields which take into consideration systematics which are typically not modelled in standard inference, such as variable depth, point-spread function variations, shear biases, etc. I will also describe how the simulated galaxy catalogues are compressed to shear-shear angular two-point statistics which are further compressed using score compression. I will show how we train a 12-dimensional neural likelihood estimation to obtain a converged and unbiased posterior of the cosmological parameters within $\Lambda$CDM. We achieve this with only 10,000 model evaluations which run in a time comparable to a standard MCMC. We find that our constraints on the weak lensing parameter, $S_8$, are similar to constraints from previous analyses of KiDS-1000. We note a non-negligible parameter-dependence in the learnt likelihood which is consistent with cosmic variance. At the same time, we find that systematics such as variable depth can have significant impacts on the posterior estimates. Lastly, I will highlight how these findings and SBI will help address the modelling/inference challenges facing upcoming stage IV galaxy surveys.

Speaker: Dr Maximilian von Wietersheim-Kramsta (University College London)

25 PolySwyft: a sequential simulation-based nested sampler

We present recent advances in combining Nested Sampling and Simulation Based Inference, and show these are performant for cosmological scale problems. Nested sampling [1,2] is a numerical Bayesian inference tool for performing model comparison and parameter estimation, and has been widely applied across cosmology & particle physics. Simulation based inference (SBI) is an emerging new paradigm for data analysis [3], which allows researchers to perform inference tasks such as parameter estimation, model comparison, and hypothesis testing directly from forward simulations without the need for an explicit likelihood function, and has already had successful application in weak lensing [4] and 21cm cosmology [5]. By removing the need for an explicit likelihood, SBI frees us from assumptions such as fiducial cosmological model (typically ΛCDM) and comprises a next-generation tool for disentangling tensions from systematics.

At its heart, the nested sampling meta-algorithm requires sampling from the prior subject to a hard likelihood constraint. It is therefore challenging to apply nested sampling if the likelihood is not explicitly available, as is the case in simulation based inference. To address this, we propose a sequential algorithm which iteratively runs nested sampling on a ratio estimator whose training data are progressively informed by the dead points of the previous nested sampling runs. This replaces truncation with nested sampling's dead measure, and allows training of neural ratio estimators without marginalisation for generative models with around 10 free parameters without marginalisation.

As an example of this synthesis, we use PolyChord [6] for nested sampling and swyft [7] for the neural ratio estimator (forming PolySwyft), but emphasise the generality of this approach throughout. We showcase it on CMB and 21cm toy examples, and discuss potential future extensions to higher numbers of parameters and a deeper integration of the two algorithms.

[1] https://arxiv.org/abs/2205.15570
[2] https://arxiv.org/abs/2101.09675
[3] https://arxiv.org/abs/1911.01429
[4] https://arxiv.org/abs/2403.02314
[5] https://arxiv.org/abs/2403.14618
[6] https://github.com/PolyChord/PolyChordLite
[7] https://swyft.readthedocs.io/en/stable/
[Paper to be released at around the time of the talk]

Speaker: Will Handley (University of Cambridge)

TeX & Python source

will_handley_cosmoverse_2024.pdf

18:30 Conference Dinner

Thursday, 11 July

Morning 1

Convener: Marika Asgari (Newcastle University)

26 Plenary 1 Tanvi Karval

Speaker: Tanvi Karval

Karwal_Cosmoverse_Krakow.pdf

27 Plenary 2 Barriers to A Concordance Cosmology

Speaker: Lloyd Knox

10:20 Coffee Break

Morning 2

28 Recent theoretical and observational developments in LsCDM Cosmology: On track to a new concordance model

Sign-switching cosmological constant cold dark matter ($\Lambda_{\rm s}$CDM) cosmology has emerged as a compelling new paradigm, demonstrating unprecedented success in aligning with observational data from various datasets and effectively resolving major cosmological tensions. This model is characterized by a minimal deviation from the standard $\Lambda$CDM model, proposing a rapid Anti-de Sitter (AdS) to de Sitter (dS) transition in the late universe ($z_\dagger\sim 1.7$), inspired by the graduated dark energy (gDE) model. In this talk, we will first provide a concise introduction to $\Lambda_{\rm s}$CDM cosmology. We will then discuss the latest theoretical and observational developments that underscore $\Lambda_{\rm s}$CDM as a promising candidate or guide for a new concordance cosmological model of the Universe.

Speaker: Ozgur Akarsu (Istanbul Technical University)

Akarsu_Krakow_2024_wide.pdf

29 Multifield Cosmology and the Dark Universe

Multifield cosmology, arising from the interaction of multiple scalar fields with gravity, can lead to qualitatively new features, when the background solutions have strongly non-geodesic trajectories in field space. This is the so called rapid-turn regime. We outline the reasons why rapid-turning can produce novel effects relevant for inflation, dark matter or dark energy. Then we focus on a particular class of multifield dark energy models in the rapid-turn regime. We show that the speed of sound of the dark energy perturbations, in these models, is reduced compared to the speed of light, which can have implications for the large-scale clustering of matter. Furthermore, we argue that this class of models holds significant promise for alleviating the Hubble and $\sigma_8$ tensions simultaneously.

Speaker: Lilia Anguelova (INRNE, Bulgarian Academy of Sciences)

30 Constraints on Tensor Perturbations from Cosmological Data Using Teleparallel Gravity

In this study, we explore novel observational constraints within the framework of $f(T)$ gravity, focusing on the impact of primordial gravitational waves on the Cosmic Microwave Background (CMB) anisotropies and the B-mode polarization spectrum. Our investigation incorporates a teleparallel formulation for the background cosmology, enabling us to extend our analysis to include late-time cosmological datasets such as the Hubble data, Pantheon plus data, and Baryon Acoustic Oscillations (BAO) data from the DESI collaboration. By integrating these diverse datasets, we obtain a more comprehensive understanding of tensor perturbations within the $f(T) $ framework. Additionally, our study sheds light on the behaviour of cosmological tensions within this framework at late-time epochs. This approach enhances our grasp of $f(T) $ gravity's implications for the late-time universe, contributing to a deeper comprehension of its underlying dynamics.

Speaker: Rebecca Briffa (Institute of Space Sciences and Astronomy, University of Malta)

12:05 Poster Award + Lunch Break

Afternoon 1

Convener: Gonzalo Olmo (Universidad de Valencia)

31 Model Independent reconstruction of an Interacting Dark Energy

In this talk I will explain what is a Model Independent reconstruction and how it can be used to study Dark Energy models, particularly in a scenario where Dark Energy can interact with Dark Matter.

Speaker: Luis Adrián Escamilla Torres (SoMaS, The University of Sheffield)

32 Cosmology from weak-lensing shear-selected galaxy clusters in the Hyper Suprime-Cam Subaru Strategic Program

We present cosmological constraints using the abundance of shear-selected galaxy clusters in the Hyper Suprime-Cam (HSC) Subaru Strategic Program. The clusters are selected on the mass maps constructed using the three-year (Y3) weak-lensing data with an area of ≈ 500 deg2, resulting in a sample size of 129 clusters with a high signal-to-noise ratio 𝜈 of 𝜈 ≥ 4.7. Owing to the deep, wide-field, and uniform imaging of the HSC survey, this is by far the largest sample of shear-selected clusters, in which the selection solely depends on gravity and is free from any assumptions about the dynamical state. Informed by the optical counterparts, the shear-selected clusters span a redshift range of 𝑧 ≲ 0.7 with a median of 𝑧 ≈ 0.3. We carefully account for (1) the bias in the photometric redshift of sources, (2) the bias and scatter in the weak-lensing mass using a simulation-based calibration, and (3) the measurement uncertainty that is directly estimated on the mass maps. The results present the first cosmological constraints from the shear-selected clusters, paving a way forward for cluster cosmology in the future LSST era.

Speaker: I-Non Chiu (National Cheng Kung University)

33 Unexplored regions in teleparallel gravity: Sign-changing dark energy density

In this talk, we will discuss construction of $\Lambda_{\rm s}$CDM-type cosmologies within teleparallel gravity, $f(T)$ gravity to address major cosmological tensions such as $H_0$ and $S_8$ tensions.

Speaker: Nihan Katırcı (Doğuş University)

NKatırcı_CosmoverseKrakow1107.pdf

15:00 Coffee Break

Afternoon 2

34 Constraining Dark Energy from the Local Group Dynamics

In this talk I will develop a method to constrain the Cosmological Constant Λ from binary galaxies, focusing on the Milky Way and Andromeda. I will provide an analytical solution to the two-body problem with Λ and show that the ratio between the Keplerian period and TΛ = 2π/(c √ Λ) ≈ 63.2 Gyr controls the importance of effects from the Cosmological Constant. The Andromeda-Milky Way orbit has a period of ∼ 20 Gyr and so Dark Energy has to be taken into account. Using the current best mass estimates of the Milky Way and Andromeda galaxies, I find the Cosmological Constant value based only on the Local Group dynamics to be lower then 5.44 times the value obtained by Planck. With future astrometric measurements, the bound on the Cosmological Constant can be reduced to (1.67 ± 0.79) ΛPL. The results offer the prospects of constraints on Λ over very different scales than previously. With other binary systems I show that the upper bound on the cosmological constant decreases when the orbital period of the system increases, emphasizing that Λ is a critical period in binary motion.

based on Astrophys.J.Lett. 953 (2023) 1, L2 & Astrophys.J.Lett. 928 (2022) 1, L5

Speaker: Dr David Benisty (Frankfurt Institue for Advanced Studies)

KrakowLocalLambda.pdf

35 An interacting dark sector from fluid approximations

The persistent discrepancy between theoretical predictions of the standard cosmological model and precision measurements from diverse observational probes remains a pressing challenge in modern cosmology. Over the past decade, mounting evidence for persistent discrepancies in the inferred values of cosmological parameters derived from both model-dependent and -independent methodologies has motivated the proposal of alternatives to the standard paradigm. In this seminar, I will focus on the exploration of potential missing physics within the standard model, focusing on the enigmatic dark sector comprising dark matter and dark energy, and any potential interactions between them. Leveraging on fluid approximations for the physical nature of the dark sector and its underlying dynamics, we assess the viability of various models in reconciling the observed cosmological tensions

Speaker: Elsa Teixeira

36 Dark energy in light of the early JWST observations: indicating a negative cosmological constant?

Early data from the James Webb Space Telescope (JWST) has uncovered the
existence of a surprisingly abundant population of very massive galaxies at extremely high redshift, which are hard to accommodate within the standard ΛCDM cosmology. We explore whether the JWST observations may be pointing towards more complex dynamics in the dark energy (DE) sector. Motivated by the ubiquity of anti-de Sitter vacua in string theory, we consider a DE sector consists of a negative cosmological constant (nCC) and a evolving component with positive energy density on top, whose equation of state is allowed to cross the phantom divide. We show that such a scenario can drastically alter the growth of structure compared to ΛCDM, and accommodate the otherwise puzzling JWST observations if the dynamical component evolves from the quintessence-like regime in the past to the phantom regime today: in particular, we demonstrate that the presence of a nCC (which requires a higher density for the evolving component) plays a crucial role in enhancing the predicted cumulative comoving stellar mass density. Our work reinforces the enormous potential held by observations of the abundance of high-z galaxies in probing cosmological models and new fundamental physics, including string-inspired ingredients.

Speaker: Upala Mukhopadhyay (Center for Theoretical Physics, Jamia Millia Islamia University)

37 Cosmology in the Realm of Gamma-Ray Bursts and Quasars

Despite decades of research, cosmology still lacks reliable probes to study the Universe in the intermediate redshift regime (from z = 1 up to z = 1100). Very few astronomical objects observed at such high distances can be standardized. We present the case of two such sources: Gamma-Ray Bursts (GRBs, $z<9.4$) and Quasars (QSOs, $z<7.4$). For GRBs, the observational luminosity distance can be derived using an empirical log-linear relation between the luminosity at the end of the plateau phase ($L_{a}$), rest-frame time at the end of the plateau ($T^{*}_{a}$), and luminosity during the peak phase ($L_{peak}$). This relation was first formulated by Dainotti et al. (2016) as $\log_{10}L_{a} = a\times \log_{10}T^{*}_{a} + b\times \log_{10}L_{peak} +c$.
QSOs, on the other hand, follow a power-law correlation between the luminosity observed in the X-ray band ($L_{X}$) and the optical luminosity ($L_{UV}$). This correlation was presented by Risaliti & Lusso (2015) as $L_{X}=\beta \times L^{\gamma}_{UV}$. Although these correlations have been shown to result from the intrinsic physics of the sources rather than observational effects, applying them to cosmological computations remains challenging. A reliable fitting method must properly take into account selection bias and redshift evolution. We demonstrate that samples of GRBs and QSOs are significantly affected by these effects. Additionally, we present a circularity-free method for fitting the cosmological model based on a de-evolving procedure developed by Efron & Petrosian (1992). Lastly, we present our results of fitting cosmological parameters.

Speaker: Aleksander Lenart (Astronomical Observatory, Jagiellonian University in Kraków)

Cosmology in the Realm of QSOs and GRBs.pptx

38 Deep Learning and genetic algorithms for cosmological Bayesian inference speed-up

In this talk, we present a novel approach to accelerate the Bayesian inference process, focusing specifically on the nested sampling algorithms. Our method utilizes the power of deep learning, employing feedforward neural networks to approximate the likelihood function dynamically during the Bayesian inference process. Unlike traditional approaches, our method trains neural networks on-the-fly using the current set of live points as training data, without the need for pre-training. This flexibility enables adaptation to various theoretical models and datasets. We perform the hyperparameter optimization using genetic algorithms to suggest the initial neural network architectures for learning each likelihood function. Once sufficient accuracy is achieved, the neural network replaces the original likelihood function.

Speaker: J Alberto Vazquez (ICF-UNAM)

Public Lecture (Polish - prof. Sebastian Szybka)

Public Lecture (English - prof. Mairi Sakellariadou)