Seminar 1:  Bulk flow measurement and Hubble tension

Parinaz Sheikhansari

Department of Physics, Sharif University of Technology

Seminar 2: Mergers of primordial black holes in extreme clusters and the H0 tension

Yasaman Khalaj Masoumi

Department of Physics, Sharif University of Technology

Abstract 1: The standard cosmological model has been successful in describing many observations from widely different epochs of the Universe, from primordial nucleosynthesis to the accelerating expansion of the present day. With the improvement of the number and the accuracy of observations, some inconsistencies among key cosmological parameters of the model have emerged. One of these discrepancies is between the early and late time measurements of H0.

Some alternative models are proposed to alleviate H0. The question is how these models predict other cosmological observations. In this work, we measured bulk flow in the LCDM model and the uLCDM model to see how bulk flow changes in uLCDM and investigate whether it can reconcile H0 tension.

Abstract 2: The simplest ΛCDM model provides a good fit to a large span of cosmological data. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant. There are many proposals beyond the ΛCDM model to reconcile the tension, like early dark energy (EDE model), primordial magnetic field, mergers of primordial black holes in extreme clusters. The model which we have been focused on is the mergers of primordial black holes in extreme clusters. In this talk, I will discuss several models which proposed PBHs are clustered, therefore, the gravitational waves emitted by collisions of such PBH binaries could resolve the Hubble tension

یکشنبه 31 مرداد 1400، ساعت 19:00

Sunday 22 August 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Seminar 1: Hierarchical Classification of Variable Stars Using Deep Convolutional and Recurrent Neural Networks

Mahdi Abdollahi

Department of Physics, Sharif University of Technology

Seminar 2: Accretion disk dynamics and luminosity

Amirhossein Mohammadi

Department of Physics, Sharif University of Technology

Abstract 1: The importance of using fast and automatic methods to classify variable stars for a large amount of data is undeniable. There have been many attempts at classifying Variable Stars by traditional algorithms, which require long pre-processing times. In recent years, neural networks as classifiers have come to notice. This paper proposes the Hierarchical Classification technique, which contains several models with the same network structure. We use two pre-processing methods, which produce input data by using light curves and the period. We use the OGLE variable stars’ database to train and test the performance with different models based on the Hierarchical Classification technique. Further, we use Convolutional Neural Networks and Recurrent Neural Networks in the network structure. We see these neural networks work faster than traditional methods and have more accurate predictions. We obtain the best accuracy of 98% for class classification and 92% for subclasses classification.

Abstract 2: Accretion disks are disk-like flows of materials that are orbiting a central object in a gravitational potential. We can see these disks as a fluid and discuss their dynamics which we will do in steady and decaying states. The central body of the accretion disks can be stars which, we will discuss the effect of the accretion disk on the luminosity of the star in the steady-state.

یکشنبه 24 مرداد 1400، ساعت 19:00

Sunday 15 August 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Mohammad Amin Hejazi

Department of Physics, Sharif University of Technology

Periodic step-like features in the inflationary potential

Abstract: Primordial black holes (PBH) are at the forefront of theoretical cosmology since they can explain dark matter, gravitational waves, and more. The enhanced power spectrum of small scales can result in the production of primordial black holes that could be dark matter candidates. In this talk, we discuss step-like features of the inflationary potential resulting in an increase in the power spectrum of curvature perturbations by several orders of magnitude. As part of this research, we apply a number of these features at the same distances periodically in the inflationary slow-roll potential. Furthermore, we apply the floquet theory to better understand how these features optimize power spectrum enhancements. Finally, we estimate the floquet exponent using both analytical and numerical methods in different ranges of feature parameters.

یکشنبه 17 مرداد 1400، ساعت 19:00

Sunday 8 August 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Ehsan Ebrahimian

Department of Physics, Sharif University of Technology

The mad halos, reasonable evidence for the Tidal Locking Theory

Abstract: Many previous studies have shown that the direction of the angular momentum of structures is aligned with their environment.  Some studies tried to explain this with the Tidal Torque Theory (TTT). The TTT is the accepted theory for explaining the origin of the angular momentum of structures. However, we suggested another mechanism that could change the angular momentum of the dark matter halos. This mechanism is called the Tidal Locking Theory (TLT). It is similar to the mechanism that locked the Moon to the Earth via tidal forces. We investigate the IllustrisTNG simulation to find evidence of the TLT and how it affects the spin alignment of the halos. We suggest that the mad halos, halos with high velocity, provide clear evidence of the TLT. Therefore, we recommend that to understand the spin-LSS alignment better, one must look at the halos’ speed and not at their masses.

 یکشنبه 10 مرداد 1400، ساعت 19:00

Sunday 1 August 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Samaneh Sarbaz

Department of Physics, Sharif University of Technology

Frequency shift in binary lensing system

Abstract: In the gravitational microlensing phenomenon, multiple responses are obtained for the parameters of the gravitational lens. There are many ways to solve this problem. One of the recent techniques proposed is by the use of source starlight spectroscopy, in which shifts in the absorption lines of the source star can be considered as the reason for the relative motion of the lens. In this research, our objective is to study the frequency shifts in binary lenses. Therefore, after reviewing the frequency shift in single gravitational lens systems, we will study this phenomenon in binary systems.

In binary lenses, which are mainly used to detect extrasolar planets, the problem of degeneracy is causing multiple responses, and we want to use this technique to detect extrasolar planets better than before.

 یکشنبه 3 مرداد 1400، ساعت 19:00

Sunday 25 July 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Nonlinear astrophysical probes of gravity beyond General Relativity

David F. Mota

Institute of Theoretical Astrophysics, University of Oslo

Abstract:x Extending General Relativity by adding extra degrees of freedom is a popular approach to explain the accelerated expansion of the universe and to build high energy completions of the theory of gravity. The presence of such new degrees of freedom is, however, tightly constrained from observations and experiments. The viability of a given modified theory of gravity therefore strongly depends on the existence of screening mechanisms that suppresses the extra degrees of freedom in certain scales and regimes. I describe how one can use nonlinear structure formation to probe extensions to General Relativity, and will present a set of astrophysical observables that could give smoking guns of screening mechanism.

یکشنبه 27 تیر 1400، ساعت 19:00

Sunday 18 July 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Mohammadreza Ayromlou

Max Planck Institute for Astrophysics

Galaxy formation with L-Galaxies: galaxy evolution meets large-scale structure

Abstract: I first describe the standard theory of galaxy formation and evolution and introduce different kinds of galaxy formation modeling, including semi-analytical models and hydrodynamical simulations.

I then introduce a local background environment (LBE) estimator to quantify environment locally for all galaxies within cosmological simulations. Analyzing the LBE properties, I show that there should be no boundary for dark matter haloes when modeling galaxy evolution. I use the time-evolving LBE of galaxies to develop a method to better account for environmental processes within the Munich semi-analytical model of galaxy formation, L-Galaxies. Using this new method, I remove the artificial halo boundary and extend environmental processes to all galaxies in the simulation. I recalibrate the updated model using a Markov Chain Monte Carlo (MCMC) method and a few observational constraints. By comparing our results to data on galaxy properties in different environments from different surveys (e.g. SDSS, HSC), I demonstrate that the updated model significantly improves the agreement with the observations. Overall, in the vicinity of massive dark matter haloes, the new model produces stronger environmental dependencies, better recovering observed trends with halocentric distance up to scales much beyond the halo virial radius. This is likely to influence the correlations between galaxies up to tens of Megaparsecs. This presentation is based on the following papers: arXiv 1903.01988, 2004.14390, 2011.05336

یکشنبه 20 تیر 1400، ساعت 19:00

Sunday 11 July 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Mahya Sadaghiani

Physikalisches Institut, Universität zu Köln

Unveiling the properties of the clusters in the NGC6334 filamentary cloud, including the physics of shocked gas and accretion

Abstract: NGC6334 is a nearby high-mass star-forming complex that has been the target of multiple studies at different wavelengths. This filamentary cloud contains several massive protoclusters at different stages of evolution which are likely pinpointing sites of high mass star formation activity. In order to investigate the kinematics of the dense gas at the scales of the clusters (<1 pc), we conducted ALMA observations towards the two high-mass protoclusters NGC6334-I and NGC6334-I(N) embedded in the filamentary star-forming complex NGC6334, as well as the gas connecting them to the large-scale filament. The observations cover the spatial scales from 1800au to 0.25 pc and are sensitive to the 3 mm continuum emission and different molecular species. The intensity maps of dense gas tracers reveal a network of filamentary structures converging at the positions of these two clusters. The analysis of the velocity fields results in similar mass accretion rates for both clusters, suggesting that they are competing for the mass reservoir in the main filament.

The ALMA continuum map at 3 mm revealed a total of 142 cores in the observed region. The compact cores are grouped in four main clusters identified by machine learning algorithms.

The typical separations (4000-12000 au) together with the core masses (0.2-100 Msun) are in agreement with turbulent fragmentation at scales of 0.1 pc. We find that the CMF of the clusters show an excess of high-mass cores compared to the IMF, which can be due to effect of temperature and the unresolved multiplicity.

The evidence of mass-segregation is found in NGC6334-I and NGC6634-I(N) with locating the massive cores close to the center.

The accretion process via the filamentary network possibly generates slow shocks due to the transport of material. On the other side, a large population of star-forming cores can produce high-velocity shocks due to the outflows. The SiO emission map obtained with ALMA is an ideal tracer of shocked gas and exhibits a complex morphology with a broad variety of line profiles and a large number of overlapping emission features towards the clusters NGC6334-I and NGC6334-I(N). As an attempt to decompose the slow shocks from the high-velocity shocks, I took advantage of spectral decomposition and wavelet analysis. The spectral decomposition separates the two types of shocks based on the width of the SiO line profile. The complex wavelet analysis isolates the slow shocks based on the probability density function (PDF) of their wavelet coefficients. The decomposition analysis reveals that 30% of the shock energetics in the region are generated in slow shocks, while for the remaining 70%, outflows are responsible. The widespread emission generated by slow shocks dominates at scales >0.1 pc.

یکشنبه 13 تیر 1400، ساعت 19:00

Sunday 4 July 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

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Sara Rezaei Khoshbakht

Chalmers University of Technology, Department of Space, Earth and Environment, Gothenburg, Sweden

Max Planck Institute for Astronomy (MPIA), Heidelberg, Germany.

3D mapping of dust in the Milky Way in the Gaia era

Abstract: The unprecedented astrometry from the Gaia mission provides us with an opportunity to study the solar neighbourhood in the finest details ever possible. Extracting the wealth of information in these data remains a challenge, however. We have developed a state-of-the-art, three-dimensional dust mapping technique using the Gaussian process that provides detailed 3D maps of the Milky Way. We obtain the 3D positions of stars from Gaia, and their individual extinction using 2MASS and WISE photometry, which are then used as the input for our model. Taking into account both distance and extinction uncertainties, together with the 3D spatial correlation between neighbouring points, we produce detailed 3D maps of the local molecular clouds, revealing the 3D shapes of individual clouds for the first time.

In this talk, I will start by introducing dust and why it is an important component of the interstellar medium, followed by some of the most recent literature works in the field. Then I will introduce you to our technique and its application to mapping both the Galactic-scale structures and the local molecular clouds. I will finish by showing some of our latest results towards Orion A and California molecular clouds that solved a long-standing mystery of their contrasting star formation rates.

یکشنبه 30خرداد 1400، ساعت 19:00

Sunday 20 June 2021 – 19:00 Tehran Time

اتاق سمینار مجازی –Virtual Seminar Room

https://vc.sharif.edu/ch/cosmology

گزینه ورود به صورت مهمان – Enter as a Guest