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hv.dekanaat [at] ut.ee

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Jakobi 2, rooms 116–121, 51005 Tartu
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Ülikooli 18–310, 50090 Tartu
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J. Liivi 4, 50409, Tartu
Viljandi Culture Academy

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Dean's Office

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Lossi 36, 51003 Tartu
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Salme 1a–29, 50103 Tartu
Johan Skytte Institute of Political Studies

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Narva mnt 18, 51009 Tartu
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Näituse 2, 50409 Tartu
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Näituse 20–324, 50409 Tartu
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Lossi 36, 51003 Tartu
Narva College

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+372 740 1900

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college [at] narva.ut.ee

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Raekoja plats 2, 20307 Narva
Pärnu College

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+372 445 0520

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info [at] pc.ut.ee

Faculty address:
Ringi 35, 80012 Pärnu

Dean's Office

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+372 737 5326

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med [at] ut.ee

Faculty address:
Ravila 19, 50411 Tartu
Institute of Biomedicine and Translational Medicine

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biomeditsiin.ut.ee

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+372 737 4210

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bsmi [at] ut.ee

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Biomeedikum, Ravila 19, 50411 Tartu
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+372 737 5286

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pharmacy [at] ut.ee

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Nooruse 1, 50411 Tartu
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hambaarstiteadus.ut.ee

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+372 731 9856

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Puusepa 1a, 50406 Tartu
Institute of Clinical Medicine

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clinicalmedicine.ut.ee

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+372 737 5323

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kmi [at] ut.ee

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L. Puusepa 8, 50406 Tartu
Institute of Family Medicine and Public Health

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tervis.ut.ee

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+372 737 4190

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dph [at] ut.ee

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Ravila 19, 50411 Tartu
Institute of Sport Sciences and Physiotherapy

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+372 737 5360

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kkdek [at] ut.ee

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Ujula 4, 51008 Tartu

Dean's Office

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+372 737 5820

Faculty email:
ltt [at] ut.ee

Faculty address:
Vanemuise 46–208, 51003 Tartu
Institute of Computer Science

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+372 737 5445

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ics [at] ut.ee

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Narva mnt 18, 51009 Tartu
Estonian Marine Institute

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mereinstituut.ut.ee

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Employee contacts

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+372 671 8902

Faculty address:
Mäealuse 14, 12618 Tallinn
Institute of Physics

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W. Ostwaldi 1, 50411 Tartu
Institute of Chemistry

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chem.ut.ee

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+372 737 5261

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chemistry [at] ut.ee

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Ravila 14a, 50411 Tartu
Institute of Genomics

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genomics.ut.ee

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+372 737 4000

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info.genoomika [at] ut.ee

Faculty address:
Riia 23b, 51010 Tartu
Institute of Mathematics and Statistics

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+372 737 5860

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ltms [at] ut.ee

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Narva mnt 18, 51009 Tartu
Institute of Molecular and Cell Biology

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tymri.ut.ee

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+372 737 5027

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Riia 23, 23b–134, 51010 Tartu
Tartu Observatory

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www.kosmos.ut.ee

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+372 737 4510

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kosmos [at] ut.ee

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Observatooriumi 1, Tõravere, 61602 Tartumaa
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Nooruse 1, 50411 Tartu
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Vanemuise 46, 51003 Tartu

Institutions

Library

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W. Struve 1, 50091 Tartu
Youth Academy

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Uppsala 10, 51003 Tartu
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muuseum [at] ut.ee

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Lossi 25, 51003 Tartu
University of Tartu Natural History Museum and Botanical Garden

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Support Units

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Employeescontacts

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Rector's Office
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University of Tartu Press

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Tartu University Hospital

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University of Tartu Foundation

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Ülikooli 18, 50090 Tartu
View all other units

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Seminar and event videos

On this page, you can find videos of recorded seminars or other events on various topics. The list is constantly updated. To find the event you would like to watch, scroll down the page or click on the title of the event in the following list.

Galaxies and non-galactic baryons in cosmic filaments (15.09.2021)
ESTHub information webinar (23.03.2021)
The Corona handshake: connectivity, collapse, and evolution in the Corona Borealis supercluster (17.02.2021)
On the effects of Initial Mass function on the galactic chemical enrichment: the role of Pair Instability Supernovae (10.02.2021)
Non-relativistic stars as a probe of modified gravity (13.01.2021)
The symmetry of planets and life in the Universe (2.12.2020)
An EAGLE view of the missing baryons (25.11.2020)
Evolution of galaxies on the cosmic web (1.10.2020)
Cosmic web topology – From DM density fields, halos and (at some point) observations (16.9.2020)
Modelling of phytoplankton and water quality in Biebrza river (10.9.2020)
Virtual excursion to Tartu Observatory (14.5.2020)
Probing heating in the IGM and proto-clusters (13.5.2020)
NIVA – introduction and project overview (30.4.2020)
Single tree detection using template matching and convolutional neural networks (23.4.2020)
Estimating the prediction accuracy in remote sensing applications (26.3.2020)
Optimizing the performance of statistical analysis of large raster images (19.3.2020)
RITA remote sensing: Fire (12.3.2020)

Galaxies and non-galactic baryons in cosmic filaments

ESTHub information webinar

Martin Menert, Ave Ansper-Toomsalu, Liis Sipelgas, Kaupo Voormansik, Thomas Storm
23.03.2021

Summary

The aim of the seminar is to introduce the possibilities of ESTHub and to share the experience of using remote sensing data in science and teaching as well in the development of services necessary for the state. ESThub was opened in the Estonian Land Board in cooperation with the European Space Agency in 2019 and offers services to companies, the public sector, research and development institutions and academy.

The development of ESTHub in the framework of the Coperncius program will enable the expansion of active dialogue with users and promote national innovation actions the international space and downstream community.

Moderator: prof. Anu Noorma (Estonian representative in Copernicus User Forum, University of Tartu, Tartu Obseravtory)

Presentations:
Martin Menert (Estonian Land Board) - Designing ESTHub services
Ave Ansper-Toomsalu (University of Tartu, Tartu Obseravtory) - Using ESTHub for science and studies
Liis Sipelgas (TalTech, Department of Marine Systems) - Upgrading the ice charting service in Estonia
Kaupo Voormansik (KappaZeta) - How to make ESTHub even more attractive for EO and GIS companies? / KappaZeta Sentinel-1 easy-to-use data layers for B2B and B2G users
Thomas Storm (Brockmann Consult, Germany) - presentation of examples for how to use the facility

Seminar materials

Ave Ansper-Toomsalu - Using ESTHub for science and studies
Kaupo Voormansik - Sentinel-1 analysis ready data layers for B2B and B2G users
Martin Menert - From expert oriented system to open data service for everyone
Liis Sipelgas - Upgrading Estonian Ice charting service
Thomas Storm - ESTHub usage examples

Video

The Corona handshake: connectivity, collapse, and evolution in the Corona Borealis supercluster

On the effects of Initial Mass function on the galactic chemical enrichment: the role of Pair Instability Supernovae

Sabyasachi Goswami
10.02.2021

Summary

There is mounting evidence that the stellar initial mass function (IMF) could extend much beyond the canonical Mi ~100, Msun limit, but the impact of such hypothesis on the chemical enrichment of galaxies still remains to be clarified. We aim to address this question by analysing the observed abundances of thin- and thick-disc stars in the Milky Way with chemical evolution models that account for the contribution of very massive stars dying as pair-instability supernovae. We built new sets of chemical yields from massive and very massive stars up to Mi ~ 350 Msun, by combining the wind ejecta extracted from our hydrostatic stellar evolution models with explosion ejecta from the literature.

Jätka lugemist

Using a simple chemical evolution code we analyse the effects of adopting different yield tables by comparing predictions against observations of stars in the solar vicinity. After several tests, we focus on the [O/Fe] ratio which best separates the chemical patterns of the two Milky Way components. We find that with a standard IMF, truncated at Mi ~ 100 Msun, we can reproduce various observational constraints for thin-disc stars, but the same IMF fails to account for the [O/Fe] ratios of thick-disc stars. The best results are obtained by extending the IMF up to Mi = 350 Msun and including the chemical ejecta of very massive stars, in the form of winds and pair-instability supernova explosions.

Our study indicates that PISN played a significant role in shaping the chemical evolution of the Milky Way thick disc. By including their chemical yields it is easier to reproduce not only the level of the alpha-enhancement but also the observed slope of thick-disc stars in the [O/Fe] vs [Fe/H] diagram. The bottom line is that the contribution of very massive stars to the chemical enrichment of galaxies is potentially quite important and should not be neglected in chemical evolution models.

Seminar video

Non-relativistic stars as a probe of modified gravity

The symmetry of planets and life in the Universe

An EAGLE view of the missing baryons

Toni Tuominen
25.11.2020

Summary

With the use of the EAGLE simulation, I present the spatial and thermal distribution of the baryons within the filaments of the Cosmic Web. In particular, I characterise the properties of the hottest (log T(K) > 5.5) Warm-Hot Intergalactic Medium (WHIM). As observations of the diffuse intergalactic medium at these temperatures are extremely challenging, the hot WHIM remains largely undetected and is a candidate to solve the cosmological missing baryon problem. Indeed, the EAGLE simulation predicts a large fraction of baryons to be in the hot WHIM. I demonstrate how we located the hot WHIM and examined its radial temperature and density profiles by using the Bisous and MMF/NEXUS+ filament finders, and show how the galaxy luminosity density can aid in selecting the most promising filaments for future observations.

Video

Evolution of galaxies on the cosmic web

Ruchika Seth (IUCAA)
1.10.2020

Summary

We take a close look at the galaxies in the Coma Supercluster and assess the role of the environment (in the form of cluster, group and supercluster filament) in their evolution, in particular examining the role of groups. We characterise the groups according to intrinsic properties such as richness and halo mass, as well as their position in the supercluster and proximity to the two rich clusters, Abell 1656 (Coma) and Abell 1367. We devise a new way of characterising the local environment using a kernel density estimator. We find that the impact of the environment on galaxies is a complex combination of the overdensities on various scales and that Abell 1367 end of the supercluster is in the process of assembly at present, leading to heightened star formation activity in galaxies, in contrast with the Coma-end of the filament system.

Video

Cosmic web topology – From DM density fields, halos and (at some point) observations

Georg Wilding (University of Groningen)
16.9.2020

Summary

The structure of the cosmic web, its connectivity and multiscale, geometric nature, has been of the centre of extensive research in the past decades. We study the underlying dark matter distribution in LCDM using persistent homology. It provides information on characteristic densities of topological features, their hierarchical interactions, multiscale connectivity and percolation. With elements of homology theory, such as Betti numbers to count holes of various dimensions, we trace the evolution of the hierarchical structure, geometry and connectivity of the cosmic web in a set of cosmological N-body simulations.

Within homology theory, persistence quantifies the longevity and stability of topological features. Features with high persistence can be associated with the prominent structural components in the multicomponent, multidimensional cosmic web. Together with another homological feature, the Betti curves, this concisely and richly describes the evolution of the topological shape of the cosmic web. Taking a step back, we then use this information to discern differences in the cosmic web topology between various dark energy cosmologies, as well as to identify a topological bias in the DM halo distribution.

Video

Modelling of phytoplankton and water quality in Biebrza river

Virtual excursion to Tartu Observatory

Probing heating in the IGM and proto-clusters

Robin Kooistra
13.5.2020

Summary

Neutral hydrogen gas on large scales provides an excellent probe for various sources of heating. At low redshift (z < 0.1), I will discuss the prospect of detecting the intergalactic medium (IGM) in large-scale filaments through 21-cm emission with the upcoming Square-Kilometre Array (SKA). Such a detection would provide constraints on the strength of the cosmic UV background. Furthermore, the Lyman alpha forest is currently one of the best probes of the neutral gas in the IGM at high redshift (z ~ 2-3). Recently, the Lyman alpha forest has been used to generate 3D tomographic maps of the large-scale absorption field in surveys such as CLAMATO. Using simulations, we explore the potential of these maps for constraining the thermal and ionization properties of the gas through the distribution of Lyman alpha transmission as a function of reconstructed dark-matter density. I will show that this can potentially be used as a direct probe of preheating in proto-clusters. This will help to constrain the various models of galaxy and AGN feedback, both in the IGM and in clusters.

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Seminar and event videos

Galaxies and non-galactic baryons in cosmic filaments

ESTHub information webinar

The Corona handshake: connectivity, collapse, and evolution in the Corona Borealis supercluster

On the effects of Initial Mass function on the galactic chemical enrichment: the role of Pair Instability Supernovae

Non-relativistic stars as a probe of modified gravity

The symmetry of planets and life in the Universe

An EAGLE view of the missing baryons

Evolution of galaxies on the cosmic web

Cosmic web topology – From DM density fields, halos and (at some point) observations

Modelling of phytoplankton and water quality in Biebrza river

Virtual excursion to Tartu Observatory

Probing heating in the IGM and proto-clusters

NIVA – introduction and project overview

Single tree detection using template matching and convolutional neural networks

Estimating the prediction accuracy in remote sensing applications

Optimizing the performance of statistical analysis of large raster images

RITA remote sensing: Fire