| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:30 to 09:45 | Rajesh Gopakumar (ICTS, India) | Welcome address | ||
| 09:45 to 10:45 | D Pogosyan (University of Alberta, Canada) | Cosmological Perturbation Theory / CMB (Lecture 1) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | S Bharadwaj (IITK, India) | 21cm Physics and Cosmology (Lecture 1) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | D Pogosyan (University of Alberta, Canada) | Cosmological Perturbation Theory / CMB (Lecture 2) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | -- | FREE | ||
| 16:15 to 17:00 | -- | Coffee |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | D Pogosyan (University of Alberta, Canada) | Cosmological Perturbation Theory / CMB (Lecture 3) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Aseem Paranjape (IUCAA, India) | Cosmological Structure Formation (Lecture 1) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Alan Heavens (Imperial College, UK) | Gravitational Lensing (Lecture 1) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | S Bharadwaj (IIT Kharaghpur, India) | 21cm Physics and Cosmology (Lecture 2) | ||
| 16:15 to 17:00 | -- | Coffee |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | D Pogosyan (University of Alberta, Canada) | Cosmological Perturbation Theory / CMB (Lecture 4) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | S Bharadwaj (IIT Kharagpur, India) | 21cm Physics and Cosmology (Lecture 3) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Alan Heavens (Imperial College, UK) | Gravitational Lensing (Lecture 2) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | S Bharadwaj (IIT Kharagpur, India) | 21cm Physics and Cosmology (Lecture 4) |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Alan Heavens (Imperial College, UK) | Gravitational Lensing (Lecture 3) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Paolo Creminelli (ICTP, Italy) | Inflation (Lecture 1) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Alan Heavens (Imperial College, UK) | Gravitational Lensing (Lecture 4) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Shadab Alam (University of Edinburgh, UK) | LSS Hands-on (Lecture 1) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | -- | Informal Student Talks |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | D Pogosyan (University of Alberta, Canada) | Cosmological Perturbation Theory / CMB (Lecture 5) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Aseem Paranjape (IUCAA, India) | Cosmological Structure Formation (Lecture 2) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Paolo Creminelli (ICTP, Italy) | Inflation (Lecture 2) | ||
| 15:15 to 16:15 | Aseem Paranjape (IUCAA, India) | Cosmological Structure Formation (Lecture 3) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | -- | Informal Student Talks |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Aseem Paranjape (IUCAAP, India) | Cosmological Structure Formation (Lecture 4) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | John Peacock (University of Edinburgh, UK) | Cosmology with LSS (Lecture 1) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | D Pogosyan (University of Alberta, Canada) | Cosmological Perturbation Theory / CMB (Lecture 6) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | John Peacock (University of Edinburgh, UK) | Cosmology with LSS (Lecture 2) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | -- | Informal Student Talks |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | John Peacock (University of Edinburgh, UK) | Cosmology with LSS (Lecture 3) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Paolo Creminelli (ICTP, Italy) | Inflation (Lecture 3) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | John Peacock (University of Edinburgh, UK) | Cosmology with LSS (Lecture 4) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Stefano Borgani (INAF - OATS, Italy) | Galaxy Clusters (Lecture 1) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | -- | Informal Student Talks |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Paolo Creminelli (ICTP, Italy) | Inflation (Lecture 4) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Stefano Borgani (INAF - OATS, Italy) | Galaxy Clusters (Lecture 2) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Paolo Creminelli (ICTP, Italy) | Inflation (Lecture 5) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Stefano Borgani (INAF - OATS, Italy) | Galaxy Clusters (Lecture 4) |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Aseem Paranjape (IUCAA,India) | Cosmological Structure Formation (Lecture 5) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Shadab Alam (University of Edinburgh, UK) | LSS Hands-on (Lecture 2) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Aseem Paranjape (IUCAA, India) | Cosmological Structure Formation (Lecture 6) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | -- | FREE |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Archishman Ghosh (Nikhef, Amsterdam, Netherlands) | Cosmology with Gravitational Waves (Lecture 1) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Kandaswamy Subramanian (IUCAA, India) | Galaxy Formation (Lecture 1) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Varun Sahni (IUCAA, India) | Dark Energy (Lecture 1) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Archishman Ghosh (Nikhef, Amsterdam, Netherlands) | Cosmology with Gravitational Waves (Lecture 2) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | Archishman Ghosh (Nikhef, Amsterdam, Netherlands) | Cosmology with Gravitational Waves (Lecture 3) |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | -- | FREE | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Kandaswamy Subramanian (IUCAA, India) | Galaxy Formation (Lecture 2) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Varun Sahni (IUCAA, India) | Dark Energy (Lecture 2) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Kandaswamy Subramanian (IUCAA, India) | Galaxy Formation (Lecture 3) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | J. Richard Bond (University of Toronto, Canada) | Quantum Inflation in the Planck Era and Beyond |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Rishi Khatri (TIFR, India) | CMB Physics | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Jens Chluba (University of Manchester, UK) | Recombination Physics (Lecture 1) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Varun Sahni (IUCAA, India) | Dark Energy (Lecture 3) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | T R Choudhury (NCRA, India) | Reionization (Lecture 1) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | -- | FREE |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | T R Choudhury (NCRA, India) | Reionization (Lecture 2) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Jens Chluba (University of Manchester, UK) | Recombination Physics (Lecture 2) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | T R Choudhury (NCRA, India) | Reionization (Lecture 3) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Shadab Alam (University of Edinburgh, UK) | LSS Hands-on (Lecture 3) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 18:00 | Rashid Sunyaev (Max-Planck-Institut für Astrophysik, Garching, Germany) | X-Ray and microwave cosmology: synergy and competition: What do we expect from the next generation X-ray and microwave telescopes? (Infosys-ICTS Chandrasekhar Lectures) |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Jens Chluba (University of Manchester, UK) | Recombination Physics (Lecture 3) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Benjamin D Wandelt (Institut D'Astrophysique de Paris, France) | Statistics / Data Analysis (Lecture 1) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Raul E Angulo (DIPC, San Sebastian, Spain) | Cosmological Simulations (Lecture 1) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Benjamin D Wandelt (Institut D'Astrophysique de Paris, France) | Statistics / Data Analysis (Lecture 2) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 16:30 to 18:00 | Rashid Sunyaev (Max-Planck-Institut für Astrophysik, Garching, Germany) | Physics of the radiation spectra formation due to Thomson scattering of low frequency photons on hot Maxwellian electrons (Infosys-ICTS Chandrasekhar Lectures) |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:45 to 10:45 | Raul E Angulo (DIPC, San Sebastian, Spain) | Cosmological Simulations (Lecture 2) | ||
| 10:45 to 11:30 | -- | Coffee | ||
| 11:30 to 12:30 | Benjamin D Wandelt (Institut D'Astrophysique de Paris, France) | Statistics / Data Analysis (Lecture 3) | ||
| 12:30 to 14:00 | -- | Lunch | ||
| 14:00 to 15:00 | Raul E Angulo (DIPC, San Sebastian, Spain) | Cosmological Simulations (Lecture 3) | ||
| 15:00 to 15:15 | -- | Short Break | ||
| 15:15 to 16:15 | Benjamin D Wandelt (Institut D'Astrophysique de Paris, France) | Statistics / Data Analysis (Lecture 4) | ||
| 16:15 to 17:00 | -- | Coffee | ||
| 17:00 to 17:30 | Raul E Angulo (DIPC, San Sebastian, Spain) | Cosmological Simulations (Lecture 4) | ||
| 17:30 to 18:00 | N Khandai | -- |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:00 to 09:25 | François R. Bouchet (IAP, Paris, France) |
Plank cosmological legacy: a basis for an exciting future I will describe the observational status of Cosmology after the final delivery of the Planck satelitte, with a short overview of the main achievements and open questions and describe the ambitious plans to move forward. |
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| 09:25 to 09:40 | Subhajit Ghosh (TIFR, India) | Dark neutrino interactions make gravitational waves blue | ||
| 09:40 to 09:55 | Anirban Roy (SISSA, Italy ) |
B-Mode Signal From Patchy reionization I'll talk about how detachability of patchy reionization by future CMB experiments. I'll discuss how secondary CMB B mode can be generated due to patchy reionization. reference link: https://arxiv.org/abs/1801.02393 |
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| 09:55 to 10:20 | Jens Chluba (University of Manchester, UK) | Can we neglect relativistic temperature corrections in the Plank SZ analysis? | ||
| 10:20 to 10:35 | Sandeep Kumar Acharya (TIFR, India) |
Beyond y, i, and mu: Rich structure of non-thermal relativistic CMB spectral distortions from high energy particle cascades It is generally assumed that for energy injection before recombination, all of the injected energy is dissipated as heat in the baryon-photon plasma, giving rise to the y-type, i-type, and mu-type distortions in the CMB spectrum. We show that this assumption is incorrect when the energy is injected in the form of energetic (i.e. energy much greater than the background CMB temperature) particles. We evolve the electromagnetic cascades, from the injection of high energy particles, in the expanding Universe and follow the CMB spectral distortion resulting from the interaction of the electromagnetic shower with the background photons, electrons, and ions. The electromagnetic shower loses a substantial fraction of its energy to the CMB spectral distortions before the energy of the particles in the shower has degraded to low enough energies that they can thermalize with the background plasma. This spectral distortion is the result of the interaction of non-thermal energetic electrons in the shower with the CMB and thus has a shape that is substantially different from the y-type or i-type distortions. The shape of the final \emph{non-thermal relativistic} (ntr-type) CMB spectral distortion depends upon the initial energy spectrum of the injected electrons, positrons, and photons and thus has information about the energy injection mechanism e.g. the decay or annihilation channel of the decaying or annihilating dark matter particles. The shape of the spectral distortion is also sensitive to the redshift of energy injection. Our calculations open up a new window into the energy injection at z. |
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| 10:35 to 11:05 | -- | Coffee Break | ||
| 11:05 to 11:20 | Matt Hilton (University of KwaZulu-Natal, Durban) |
The Atacama Cosmology Telescope Sunyaev-Zel'dovich Galaxy Clusters Survey The Atacama Cosmology Telescope (ACT) is conducting an effectively mass-limited search for galaxy clusters using the redshift-independent Sunyaev-Zel'dovich (SZ) effect. In this talk I will describe our recent work on constructing the two-season ACTPol galaxy cluster catalog (arXiv:1709.05600), and discuss mass calibration of this sample using weak-lensing observations. I will also describe ongoing work with Advanced ACT (AdvACT), which has surveyed approximately 14,000 square degrees of the southern sky, and at the time of writing has detected more than 1500 galaxy clusters out to z = 2. With its clean, well-defined selection function, it is an ideal sample to use to study galaxy evolution in clusters, constrain cosmological parameters, and measure the evolution of both thermal and non-thermal emission by the intracluster medium. |
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| 11:20 to 11:45 | Tarun Souradeep (IUCAA, India ) |
CMB-Bhārat: A Comprehensive next-gen CMB mission proposal The observations of the spectrum and anisotropies of the primordial cosmic microwave background (CMB) radiation has spearheaded the transition into an era of precision cosmology, with accurate determination of the cosmological parameters, critical inferences of the early universe and origin of structures. However, over 90% of the polarisation information and an almost untouched spectral information remains to be mapped out with more capable mission with high value returns for Cosmology and ultra-High Energy Physics. I present a case for an next generation CMB space mission as an unique opportunity for India that has presented itself to partake in potentially path breaking discovery, together with a number of guaranteed high science dividends and providing a rich legacy astronomical data. |
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| 11:45 to 12:10 | Jacques Delabrouille (IAP, Paris, France) | The Cosmic Origins Explorer | ||
| 12:10 to 12:35 | Shaul Hanany (University of Minnesota, USA) |
The Probe of Inflation and Cosmic Origins The Probe of Inflation and Cosmic Origins (PICO) is a concept for a probe-scale mission that we studied over the last 18 months as part of NASA's preparations for the US 2020 decadal panel. PICO is an imaging polarimeter with a 1.4 m aperture telescope, and 21 frequency bands between 20 and 800 GHz. If flown, PICO will be the most sensitive cosmic microwave background instrument implemented in the next decade. I will describe PICO's science goals and its design. |
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| 12:35 to 14:00 | -- | Lunch Break | ||
| 14:00 to 14:25 | Ritoban Basu Thakur (California Institute of Technology, USA) |
The BICEP-Array Telescope, searching for primordial inflation from the South Pole Our comprehensive understanding of early universe of physics strongly indicates an epoch of rapid inflation. Detection of a curl-type (B-mode) polarization at degree scales would be a direct proof of inflation. The BICEP/Keck collaboration, with ever improving generations of telescopes operating at the South Pole, has been leading this search for inflation. The new BICEP Array (BA) set of telescopes will begin observing at the South Pole starting in 2020. BA will measure polarized CMB in bands centered at 30, 40, 90, 150, 220 and 270 GHz respectively. The first re ceiver to be deployed will perform the 30/40 GHz measurements, enabling us to understand and therefore model synchrotron contamination to the CMB with high confidence. The following receivers (ranging 90-270 GHz) will focus on the CMB and dust emissions. Therefore with data-driven parametric modeling of all the foregrounds, we will deliver extremely deep and clean CMB polarization maps furthering the search for inflation. This talk will present an overview of the design and expected performance of the BICEP Array instruments, focusing on the 30/40 GHz receiver. I will also outline how BICEP Array will inform the future CMB ‘Stage 4’ experiments, and the “delensing” science case being developed with our neighbor, the South Pole Telescope (SPT-3G). |
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| 14:25 to 14:50 | Lyman Page (Princeton University, USA) |
Measuring the CMB from Chile: a look ahead Chile is an excellent site from which to measurement the CMB. One benefit is the ability to observe large regions of sky. For sub-degree scale measurements, there is excellent overlap with optical surveys such as LSST and DESI. For measuring primordial B-modes, modulators are likely necessary and have been demonstrated. We describe in broad terms the observing program for Chile for the next few years, in particular the Simons Observatory, and its complementarity to other efforts in space and on the ground. |
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| 14:50 to 15:20 | -- | Coffee Break | ||
| 15:20 to 15:45 | Zeeshan Ahmed (SLAC National Accelerator Laboratory, California) |
CMB-S4, the ultimate ground-based CMB polarization survey Ground-based CMB imaging instrumentation is continuing generational leaps in photon-noise-limited sensitivity, while our understanding and mitigation of systematic errors and biases advances for the most difficult CMB measurements such as that of tensor-to-scalar ratio. CMB-S4 is an ambitious multi-frequency, ground-based CMB polarization survey program over 40% of the Southern sky proposed to be built and operated in Chile and Antarctica in the 2020s. It aims to detect or rule out most models of inflation that naturally explain the scalar spectral index (r>0.001); distinguish neutrino mass hierarchy at high significance; search for thermal relics in the early history of the universe before the QCD phase transition; significantly tighten constraints on the epoch of reionization; probe baryonic feedback in galaxy evolution; provide a legacy catalog of clusters and mm-wave sources; and open a new window of discovery in mm-wav e time-domain astrophysics including imaging of gamma-ray bursts and active galaxies. In this talk I will provide a brief introduction to CMB-S4 and a broad overview of its science goals. |
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| 15:45 to 16:10 | Francesco Piacentini |
LSPE and COSMO instrumentos for CMB measurements The Observational Cosmology group at University of Rome in working on measurements of the CMB since years. The next generation of instruments under development are the Large Scale Polarisation Explorer (LSPE) for CMB polarisation, and COSmic Monopole Observer (COSMO), for absolute spectrum of the CMB. I briefly present the two instruments, their status and prospectives. |
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| 16:10 to 17:30 | -- | Discussion |
| Time | Speaker | Title | Resources | |
|---|---|---|---|---|
| 09:00 to 09:25 | Marat Gilfanov (Max Planck Institute for Astrophysics, Germany) | Cosmological studies with wide-field X-ray surveys | ||
| 09:25 to 09:50 | R. Srianand (IUCAA, India) | Science with Thirty Meter Telescope | ||
| 09:50 to 10:15 | Tirthankar Roy Choudhury (NCRA, India) |
Cosmology and high-redshift universe with the Square Kilometre Array The Square Kilometre Array (SKA) is an international effort to build the largest radio telescope in the world with the aim of studying different problems in astrophysics, cosmology and fundamental physics. India is one of the eleven countries participating in the project. In this talk, we will discuss the specifications and capabilities of the SKA along with the anticipated timeline. Some specific contributions made by Indian community towards the development of the project will also be highlighted. Finally, we will discuss some of the most interesting problems in cosmology and high-redshift universe that can be studied using the SKA. |
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| 10:15 to 10:30 | Moumita Aich (University of KwaZulu-Natal, South Africa) |
Cosmology with HIRAX: combining 21-cm and large-scale structure surveys The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) is a radio telescope array led by University of KwaZulu-Natal, South Africa, that will map nearly all of the southern sky in radio continuum and neutral hydrogen line emission over a frequency range of 400 to 800 MHz. Optical surveys such as Large Synoptic Survey Telescope (LSST), Dark Energy Spectroscopic Instrument (DESI), EUCLID and the Wide Field Infrared Survey Telescope (WFIRST) will also probe the large-scale structure of the universe with much higher precision and depth by mapping the galaxy distribution. Tracing out the visible universe provides a tracer of the underlying matter distribution which in principle correlates with 21-cm cosmology surveys. Both provide us with tracers of dark matter distributions, therefore we expect cross-correlations between the overlapping surveys will provide novel constraints on cosmological parameters, redshift-dependent neutral hydrogen fraction and bias, and probe the relationship between stars and gas in their dark matter halos. |
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| 10:30 to 11:00 | -- | Coffee Break | ||
| 11:00 to 11:15 | Pavan Kumar Aluri (IITV, India) |
Parity-wise alignments of CMB multipoles In our recent work, we explored the alignments among even and odd multipoles separately. We found that the common alignment axes form two distinct groups, one in the northern hemisphere and the other in the southern hemisphere contrary to our expectation that they should be randomly oriented over the sky. The even multipoles' common alignment axes are pointing roughly in the same direction as the dipole-quadrupole-octopole alignment and the maximum even mirror parity axis. The odd multipoles' common alignment axis span the region containing the low-l dipole power asymmetry axis and the axis of odd mirror parity maximum. Results of our study are part of the paper : Alignments of parity even/odd-only multipoles in CMB, Pavan K. Aluri, John P. Ralston and Amanda Weltman, Monthly Notices of the Royal Astronomical Society (2017), v472, p2410 https://arxiv.org/abs/1703.07070 |
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| 11:15 to 11:30 | Sumanta Chakraborty (IACS, India) | Galileon Cosmology with Torsion | ||
| 11:30 to 11:45 | Anjan Ananda Sen (Jamia Millia Islamia Central University, India) | Resolving Hubble Tension With New Energy Density Component | ||
| 11:45 to 12:00 | Pranjal Trivedi (University of Hamburg, Germany) |
Axion-like Dark Matter Constraints from CMB Birefringence Axion-like particles (ALPs) are leading dark matter candidates which also arise in effective field theories. We present a sensitive probe for ultra-light dark matter or ALPs - birefringence in the cosmic microwave background (CMB). Birefringence arises from the oscillating ALPs' effective refractive index and is also relevant for laboratory dark matter searches. Constraints derived from the CMB on axion-photon coupling represent three or four orders of magnitude improvement over prior constraints, with further prospects for upcoming cosmological birefringence observations. These constraints on significant regions of coupling vs. ALP mass parameter space and ultra-light dark matter models, are independent of assumed magnetic fields and relatively robust to ALP dark matter fraction limits. |
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| 12:00 to 12:15 | Anirban Das (TIFR, India) |
Cosmology of Late-forming Ballistic Dark Matter Various cosmological observations tell us that about 24% of the total energy density of the universe exists in the form of nonrelativistic dark matter. But they fail to provide any information about the epoch or method of formation of the dark matter. There are particle physics models where the cold dark matter is formed late after a phase transition during the history of the universe. A model independent way to probe these models is to study their cosmological aspects. We shall try to compute the matter power spectrum of this delayed dark matter model and discuss the new effects originating due to the late formation of cold dark matter. We shall also try to identify the nature of the dark sector prior to the phase transition from its imprints on the matter power spectrum. |
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| 12:15 to 12:30 | Shreya Banerjee (Ben Gurion University of the Negev, Israel) | Can there be Bounce in weakly broken Galileon Theories? | ||
| 12:30 to 12:45 | Pravabati Chingangbam (IIA, India) | The shape of quantum fluctuations | ||
| 12:45 to 14:00 | -- | Lunch Break | ||
| 14:00 to 14:25 | Shiv Sethi (RRI, India) | Detecting EoR in redshifted H1 emission | ||
| 14:25 to 14:50 | Jonathan Sievers (McGill University, Canada) |
HIRAX and Fast Radio Bursts The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) is a planned 1024-element radio array that will be built in the South African Karoo desert. While it's primary focus is on observing baryon acoustic oscillations, HIRAX will also be a premiere instrument for discovering fast radio bursts (FRBs). With the addition of outrigger stations across southern Africa, HIRAX will also be able to localize a large fraction of its non-repeating FRBs to ~30 mas. With the dramatic increase in FRB discovery rate promised by instruments like CHIME and HIRAX, FRBs can also be used to help probe cosmology. |
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| 14:50 to 15:15 | Biman B. Nath (RRI, India) |
Diffuse matter in the universe: CGM to IGM Most of the baryons in the Universe is in a diffuse state. It is either confined to halos around galaxies (circumgalactic medium), or to galaxy clusters (intracluster medium) or it traces the large scale structure of the universe (intergalactic medium). The evolution of structures in the universe has left imprints on this diffuse gas, in the form of its thermal properties, ionisation state and metallicity. We will discuss different physical processes that are important for the diffuse matter in the universe, and what they tell us about the evolution of galaxies and structures. |
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| 15:15 to 15:30 | Mousumi Das (IIA, India) |
A Radio/X-ray Study of the Hot and Warm Gas around Isolated Galaxies in Voids We present low frequency radio observations of the extended emission around galaxies lying within voids. Voids contain a sparse but significant population of galaxies that show signatures of ongoing star formation and AGN activity. They are generally late type, gas rich disk galaxies and appear to be similar in nature to normal galaxies in denser environments but are evolving at a much slower rate. The sparse environment of voids allows us to study the evolution of the circum galactic medium (CGM) around AGN or starburst host galaxies in isolated environments. It also allows us to estimate how star forming void galaxies contribute to the hot gas within voids. In this presentation we show that there can be significant radio emission around void galaxies, especially from those lying within larger voids, and in some cases there can be extended X-ray emission as well. The hot/warm gas around these galaxies is due to stellar and AGN feedback processes associated with void galaxies, both of which are triggered by either galaxy interactions or gas accretion from the intergalactic medium. We discuss the implications of our results for understanding the evolution of void galaxies and the hot gas within voids. |
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| 15:30 to 15:45 | Niladri Paul (IUCAA, India) |
Calibration of satellite red fraction using colour-dependent clustering measurement from SDSS Colour of galaxies is a key towards understanding galaxy evolution and star-formation history. In all the statistical models depending on colour, one also needs the red fraction of the central and satellite galaxies separately. One can compute them using a galaxy group catalogue as e.g. Yang catalogue, but these catalogues suffer from issues related to incompleteness and impurity. Another way to model this quantity is from the colour-dependent clustering measurements from SDSS. In this work, the speaker will talk about this second approach within a precision halo model framework which incorporates measurement of halo correlation function directly from N-body simulations. |
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| 15:45 to 16:00 | Vikram Rentala (IITB, India) | Dark Matter microlensing with GAIA | ||
| 16:00 to 16:15 | Girish Kulkarni (TIFR, India) |
Large Lyman-alpha opacity fluctuations in models of late reionization High-redshift QSO spectra show large spatial fluctuations in the Lyman-alpha opacity of the intergalactic medium on surprisingly large scales at z>= 5.5. In this talk, I will present a radiative transfer simulation of cosmic reionization driven by galaxies that reproduces this large scatter and the rapid evolution of the Lyman-alpha opacity distribution at 5=6. Reionization is complete at z=5.3 in our model, and 50% of the volume of the Universe is ionized at z=7. Agreement with the Lyman-alpha forest data in such a late reioniza tion model requires a rapid evolution of the ionizing emissivity of galaxies that peaks at z~6.8. The late end of reionization results in a large scatter in the photoionisation rate and the neutral hydrogen fraction at redshifts as low as z<~5.5 with large residual neutral "islands" that can produce very long Gunn-Peterson troughs resembling those seen in the data. |
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| 16:15 to 16:30 | -- | Closing Remarks | ||
| 16:30 to 17:00 | -- | Coffee |