Abstract:<\/strong> The search for particle dark matter has seen tremendous progress and developments in the last decade. One of the primary methods for understanding the particle nature of dark matter is through direct detection. In this talk, I will provide an overview of the progress made in dark matter direct detection, discuss the synergies with other probes for dark matter, and give a look at what we can hope to see in the next decade.<\/p><\/div>\n\t\t\t<\/div> ABSTRACT: <\/strong>New physics particles beyond the reach of terrestrial experiments are expected to play important roles in the early universe. In particular, they can leave unique signals in non-Gaussianity observables. I will give an overview of the connection between particle physics models and these so-called cosmological collider signals, and highlight some recent developments and future directions.<\/p><\/div>\n\t\t\t<\/div> ABSTRACT:<\/strong> I will talk about cosmological results from the completed observations of the Atacama Cosmology Telescope, including polarized measurements of the cosmic microwave background that significantly extend the angular range probed by the Planck satellite. I will discuss implications for the LCDM model and the early universe. I will then talk about the status of new observations underway with the Simons Observatory in Chile, using a suite of telescopes to test the inflationary model, and to probe the physics of the later-time universe through correlations with overlapping large scale structure surveys.<\/p><\/div>\n\t\t\t<\/div> ABSTRACT:<\/strong> In this talk I will overview the progression of Dark Energy Survey's (DES) journey from the Science Verification to the final cosmological analysis with the full 6-year dataset. I will present some of the latest results from the Year 6 analysis. I will also describe how DES\u2019s legacy will carry on into the next steps in our pursuit of understanding the nature of the Universe.<\/p><\/div>\n\t\t\t<\/div> Abstract:<\/strong> I will introduce the Vera C. Rubin Observatory and its 10-year Legacy Survey of Space and Time (LSST), which is due to start by the end of this year. I will report on the construction, commissioning and operations of the Rubin system, describe the data that the LSST Dark Energy Science Collaboration will be using for cosmology, and give some indications of what we might hope to measure, and when.<\/p><\/div>\n\t\t\t<\/div> Parallel 1a. Theme: Topology\/COMPACT Chair: Asier Lopez-Eiguren (Euskal Herriko U) Room: Danforth<\/strong><\/p>\n Parallel 1b. Theme: LSS I: WL Chair: Claire Lamman (Ohio State U) Room: McKenna-Peter-Wright<\/strong><\/p>\n Parallel 1c. Theme: Theory I Chair: Angelo Esposito (Sapienza U) Room: Connan<\/strong><\/p>\n Parallel 1d. Theme: DM I Chair: Matteo Cremonesi (CMU) Room: McConomy<\/strong><\/p>\n Parallel 2a. Theme: CMB\/ML Chair: Hy Trac (CMU) Room: Danforth<\/strong><\/p>\n Parallel 2b. Theme: LSS II Chair: Tianqing Zhang (U Pitt) Room: McKenna-Peter-Wright<\/strong><\/p>\n Parallel 2c. Theme: Theory II Chair: Francesco Serra (Johns Hopkins) Room: Connan<\/strong><\/p>\n Parallel 2d. Theme: DM II Chair: Valentina Dutta (CMU) Room: McConomy<\/strong><\/p>\n Abstract:<\/strong> I will overview a program of extracting cosmological information from clustering data using large-scale structure perturbation theory or effective field theory (EFT). The application of EFT allows for sub-percent precision analytic understanding of galaxy clustering on quasi-linear scales and provides an unmatched flexibility in testing new physics scenarios beyond the standard cosmological model. I will share some results of this program that include new measurements of fundamental cosmological parameters and novel constraints on dark energy, dark matter, and the physics of the early universe from public BOSS and DESI data. Finally, I will discuss the prospects of new discoveries in fundamental cosmology with EFT in the era of high-redshift surveys such as DESI-II and Spec-S5.<\/p><\/div>\n\t\t\t<\/div> Abstract:<\/strong> Cosmological models and predictions rely extensively on the well-established field theory framework of particle physics. However, a qualitatively new challenge arises: cosmological systems inherently contain substances with poorly constrained macroscopic properties and entirely unknown microphysics, such as the inflaton sector, dark matter, and dark energy. This results in a rich array of novel phenomena, including dissipation, stochastic fluctuations, out-of-equilibrium dynamics, and non-unitary macroscopic evolution. Moreover, since gravitational observables are of primary interest, and gravity universally couples to all forms of matter, a close system approach requires precise description of all cosmic constituents\u2014something feasible only in the simplest toy models. To address these challenges, I propose an open system approach to cosmology.<\/p>\n I begin with a pedagogical introduction to open quantum systems. Then, I present the open effective field theory of inflation as a general class of theories of single-field inflation in the presence of an unknown medium. This local, dissipative theory yields a new class of predictions for cosmological correlators, generalizing existing models. I then tackle the challenge of formulating general relativity in the presence of an unspecified medium. As a warmup, I present a formulation of electromagnetism in a medium, incorporating dissipation and fluctuations while ensuring a consistent treatment of gauge symmetries. Building on these results, I introduce the general and systematic construction of dissipative extensions of general relativity and explore their implications for modeling open dark matter, dark energy and the late-time evolution of the universe. Finally, I study the implications for the dissipative propagation of gravitational waves through the dark sector medium.<\/p><\/div>\n\t\t\t<\/div> Abstract:<\/strong> I will review some recent developments in the study of quantum field theory in cosmological spacetimes. I will particularly focus on aspects of correlation functions and how they encode the physics of the early universe.<\/p><\/div>\n\t\t\t<\/div> Abstract:<\/strong> The accuracy of the interpretation of the current generation of late-time cosmology probes is greatly limited by the theorists' ability to predict the response of baryons. This will only get more difficult in the coming years with the upcoming surveys (DESI-BGS, Euclid, LSST, 4-most, Simons) mapping our sky with unprecedented precision. In this talk, I will discuss some of the efforts towards this challenge on the simulation side. I will, in particular, focus on the new generation of simulations, the FLAMINGO suite, designed to be virtual twins of the Stage IV cosmology surveys. This suite includes the largest simulation ever run to z=0 and exploits a state-of-the-art baryon physics model calibrated to the relevant data. Variations in the physics, trained via machine learning techniques, allow us to encompass the uncertainty in the modeling. Outputs in observer space, such as X-ray, stellar light and SZ lightcones are produced and are used to validate the simulations. I will present some of the main results obtained by exploiting the simulations. This talk is also an invitation to collaborate and make use of this data for your research.<\/p><\/div>\n\t\t\t<\/div> Abstract:<\/strong> In this talk I will present how AI is changing cosmology. Machine learning algorithms can now classify millions of astronomical objects, reconstruct complex physical properties from photometric data, and identify cosmologically significant events in real-time. I will introduce recent applications of AI to cosmological analyses.<\/p>\n Using Type Ia supernova cosmology with the Dark Energy Survey (DES) as an example, I will show how machine learning enables the photometric classification of large samples of SN Ia that probe fainter magnitudes and higher redshifts than spectroscopically classified samples. These larger samples help reduce systematic uncertainties by including previously discarded supernovae in more diverse environments. However, applying AI in cosmology presents unique challenges: calibration, physical interpretability, and bias mitigation. I will present strategies for validating AI predictions and quantifying the impact of algorithmic choices on derived cosmological parameters.<\/p>\n I will conclude by discussing how AI methods will be essential for the Vera C. Rubin Observatory LSST, enabling unprecedented cosmological constraints and opening a new era for understanding Dark Energy.<\/p><\/div>\n\t\t\t<\/div> Parallel 3a. Theme: Methods\/sims\/ML Chair: Laura Herold (JHU) Room: Danforth<\/strong><\/p>\n Parallel 3b. Theme: DESI Results Chair: Alexandra Amon (Princeton U) Room: McKenna-Peter-Wright<\/strong><\/p>\n Parallel 3c. Theme: Theory III Chair: Savvas Koushiappas (Brown U) Room: Connan<\/strong><\/p>\n Parallel 3d. Theme: DM III Chair: Andrew Zentner (U Pitt) Room: McConomy<\/strong><\/p>\n Parallel 4b. Theme: LSS III: Clusters, Baryonic effects Chair: Sayan Mandal (CMU) Room: McKenna-Peter-Wright<\/strong><\/p>\n Parallel 4c. Theme: LSS IV \/Theory IV Chair: Alice Garoffolo (U Penn) Room: Connan<\/strong><\/p>\n Parallel 4d. Theme: DM IV Chair: Robert Scherrer (Vanderbilt U) Room: McConomy<\/strong><\/p>\n10:00-10:30 | Liantao Wang \u2014 Cosmological collider as a probe for new physics in the early universe<\/h4>\n\t\t\t\t
10:30-11:00 | Jo Dunkley \u2014 Cosmology from the CMB<\/h4>\n\t\t\t\t
11:00-11:30 | Coffee Break<\/h5>\n\t\t\t\t
PLENARY SESSION 1b CHAIR: Rachel Mandelbuam<\/h4>\n\t\t\t\t
11:30-12:00 | Chihway Chang \u2014 Dark Energy Survey: 10+ years of cosmology<\/h4>\n\t\t\t\t
12:00-12:30 | Phil Marshall \u2014 Looking Forward to the Next 10 Years with Rubin\/LSST<\/h4>\n\t\t\t\t
12:30-14:00 | Lunch<\/h5>\n\t\t\t\t
14:00-15:30 | Parallel Session 1<\/h4>\n\t\t\t\t
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15:30-16:00 | Coffee Break<\/h5>\n\t\t\t\t
16:00-17:30 | Parallel Session 2<\/h4>\n\t\t\t\t
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17:30-18:00 | Break<\/h5>\n\t\t\t\t
18:00-20:00 | Reception + Poster Session @ Rangos 2-3<\/h4>\n\t\t\t\t
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\n First<\/strong><\/td>\n Last<\/strong><\/td>\n Title<\/strong><\/td>\n<\/tr>\n \n Molly<\/td>\n Abramson<\/td>\n <\/td>\n<\/tr>\n \n Aiza<\/td>\n Ali<\/td>\n Dark Matter Decay and optical emission lines.<\/td>\n<\/tr>\n \n Arhum<\/td>\n Ansari<\/td>\n The Large Scale Structure Bootstrap<\/td>\n<\/tr>\n \n Marcus<\/td>\n Bosca<\/td>\n High-Z: A New Method of Detecting Primordial 21-cm Signals<\/td>\n<\/tr>\n \n Siyu<\/td>\n Chen<\/td>\n <\/td>\n<\/tr>\n \n Shreya<\/td>\n Dayal<\/td>\n Parallels Between Brain and Cosmic Networks: A Graph-Based Machine Learning Study<\/td>\n<\/tr>\n \n Isabele<\/td>\n de Souza Vitorio<\/td>\n Exploring the Core-galaxy Connection<\/td>\n<\/tr>\n \n Jessie<\/td>\n Hammond<\/td>\n Integrated effects in Large-scale Structure<\/td>\n<\/tr>\n \n Meagan<\/td>\n Herbold<\/td>\n Generating Synthetic Lyman-alpha Forest Spectra with Lognormal Simulations for P1D Analysis<\/td>\n<\/tr>\n \n Tanisha<\/td>\n Jhaveri<\/td>\n Turning a negative neutrino mass into a positive optical depth<\/td>\n<\/tr>\n \n Nathaniel<\/td>\n Johnson<\/td>\n Sub-halo Alignment's Dependence on Halo Clustering<\/td>\n<\/tr>\n \n Joann<\/td>\n Jones<\/td>\n Constraints on Spatially Varying Dark Energy using LSST Forecasts<\/td>\n<\/tr>\n \n Wonkyung<\/td>\n Kim<\/td>\n Light WIMP Search with COSINE-100<\/td>\n<\/tr>\n \n Kei-ichiro<\/td>\n Kubota<\/td>\n Unusual Characteristics of Quasinormal Modes in Kerr spacetime<\/td>\n<\/tr>\n \n Ash<\/td>\n Lassonde<\/td>\n Rolling in the Deep: Testing Time-Evolving Dark Energy in Light of New DESI Data<\/td>\n<\/tr>\n \n Seung Mok<\/td>\n Lee<\/td>\n Status of COHERENT D2O Detector and its Implications for CEVNS Precision and Supernova Detection<\/td>\n<\/tr>\n \n Carmella<\/td>\n Li<\/td>\n Searching for Dark Matter with ML in LDMX<\/td>\n<\/tr>\n \n Jinzheng<\/td>\n Li<\/td>\n Cosmological FOPT aspects: supercooling and gauge invariance<\/td>\n<\/tr>\n \n Victoria<\/td>\n Lloyd<\/td>\n Modeling nonlinear scales for dynamical dark energy cosmologies with COLA<\/td>\n<\/tr>\n \n Dylan<\/td>\n McCauley<\/td>\n Exploring Neutrino-Assisted EDE Models as a Resolution to the Hubble Tension<\/td>\n<\/tr>\n \n Kimihiro<\/td>\n Nomura<\/td>\n Signature of ultralight dark matter in pulsar timing arrays<\/td>\n<\/tr>\n \n Aline<\/td>\n Pereyra Flores<\/td>\n Impact of dark sector preheating on CMB<\/td>\n<\/tr>\n \n Rodrigo<\/td>\n Pinheiro<\/td>\n Cosmological forecast from 21cm intensity mapping's power spectrum and bispectrum<\/td>\n<\/tr>\n \n Joyce<\/td>\n Qiu<\/td>\n Reconstructing and Classifying DESI Spectra with Variational Autoencoders<\/td>\n<\/tr>\n \n Abhinav<\/td>\n Raghavan<\/td>\n Exploring Neutrino-Assisted EDE Models as a Resolution for the Hubble Tension<\/td>\n<\/tr>\n \n Anmol<\/td>\n Raina<\/td>\n Non-Gaussianities in Multifield Inflation models with Torsion and Turning<\/td>\n<\/tr>\n \n Evan<\/td>\n Saraivanov<\/td>\n Forcasting Modified Growth with Effective Field Theory of Large Scale Structure for Roman Space Telescope<\/td>\n<\/tr>\n \n Fran<\/td>\n Stedman<\/td>\n Searching for Dark Matter with ML in LDMX<\/td>\n<\/tr>\n \n Yijie<\/td>\n Zhu<\/td>\n Emulators for Cosmological Data vectors, and application to Beyond LCDM model<\/td>\n<\/tr>\n<\/tbody>\n<\/table><\/div>\n\t\t\t<\/div>\n\t\t\t<\/div> Tue, Oct 14<\/h2><\/div>\n\t\t\t<\/div>
COSMO-25 Tuesday events<\/h5>\n\t\t\t\t
PLENARY SESSION 2a CHAIR: Rachel A. Rosen<\/h5>\n\t\t\t\t
9:30-10:00 | Mikhail Ivanov \u2014 Large-scale structure theory: successes, challenges, and new frontiers <\/h4>\n\t\t\t\t
10:00-10:30 | Enrico Pajer \u2014 An Open System Approach to Cosmology<\/h4>\n\t\t\t\t
10:30-11:00 | Austin Joyce \u2014 Quantum Field Theory in Our Universe<\/h4>\n\t\t\t\t
11:00-11:30 | Coffee Break<\/h5>\n\t\t\t\t
PLENARY SESSION 2b CHAIR: Tiziana DiMatteo<\/h5>\n\t\t\t\t
11:30-12:00 | Mathieu Schaller \u2014 The FLAMINGO suite of cosmological simulations: A stage IV cosmology proves virtual twin<\/h4>\n\t\t\t\t
12:00-12:30 | Anais Moeller \u2014 A New Era for Cosmology with AI<\/h4>\n\t\t\t\t
12:30-14:00 | Poster prizes \/ Lunch<\/h5>\n\t\t\t\t
14:00-15:30 | Parallel Session 3<\/h4>\n\t\t\t\t
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15:30-16:00 | Coffee Break<\/h5>\n\t\t\t\t
16:00-17:30 | Parallel Session 4<\/h4>\n\t\t\t\t
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