## Error message

• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Undefined offset: 0 in include() (line 36 of /home/it/www/www-icts/sites/all/themes/riley/templates/views/views-view-fields--related-file-field-collection-view.tpl.php).
• Notice: Use of undefined constant qftgrt2021 - assumed 'qftgrt2021' in __lambda_func() (line 2 of /home/it/www/www-icts/sites/all/modules/contrib/views_php/plugins/views/views_php_handler_area.inc(39) : runtime-created function).
• Notice: Undefined index: und in __lambda_func() (line 3 of /home/it/www/www-icts/sites/all/modules/contrib/views_php/plugins/views/views_php_handler_area.inc(39) : runtime-created function).
Monday, 13 March 2023
Time Speaker Title Resources
09:30 to 10:10 David Marsh (King's College London, UK) Axion Star Explosions

Axion stars form in the centres of DM halos. If the axion is coupled to electromagnetism, then axion stars are unstable above a critical mass, and explode releasing low energy photons. Explosions are simulated in full (3+1)d numerical General Relativity. For axion masses in the range 1e-11 eV and couplings of order 1e-12 GeV^-1, axion star instability is predicted to happen in the first DM structures formed, with masses of order 1 Msol at redshifts z~30. The rate of such explosions is computed from halo merger histories in standard cosmology. Axion star explosions lead to enhanced DM decay during the dark ages, which heats the intergalactic medium. Constraints on anomalous heating from the CMB optical depth lead to new and powerful constraints on axion parameter space. Future 21cm measurements can provide complementary probes of axion parameter space to the DMRadio direct detection program.

10:10 to 10:50 Subhabrata Majumdar (TIFR, India) The 'observed' phase-space of Dark Matter in galaxies

I will talk about the `observed' phase-space of dark matter in Milky Way, from the very centre to outer edge, and also from nearby galaxies. I will also discuss the implications for dark matter searches.

12:00 to 12:15 Ravi Kumar Sharma (IIA, India) Signatures of Light Massive Relics on nonlinear structure formation

Cosmologies with Light Massive Relics (LiMRs) as a subdominant component of the dark sector are well-motivated from a particle physics perspective, and can also have implications for the Ïƒ8 tension between early and late time probes of matter clustering. The effects of LiMRs on the Cosmic Microwave Background (CMB) and structure formation on large (linear) scales have been investigated extensively. In this paper, we initiate a systematic study of the effects of LiMRs on smaller, nonlinear scales using cosmological N -body simulations; focusing on quantities relevant for photometric galaxy surveys. For most of our study, we use a particular model of nonthermal LiMRs but the methods developed easily generalize to a large class of models of LiMRs â€” we explicitly demonstrate this by considering the Dodelson-Widrow form of the velocity distribution. We find that, in general, the effects of LiMR on small scales are distinct from those of a Î›CDM universe, even when the value of Ïƒ8 is matched between the models. We show that weak lensing measurements around massive clusters, between âˆ¼ 0.1hâˆ’1Mpc and âˆ¼ 10hâˆ’1Mpc, should have sufficient signal-to-noise in future surveys to distinguish between Î›CDM and LiMR models that are tuned to fit both CMB data and large (linear) scale structure data at late times. Furthermore, we find that different LiMR cosmologies which are indistinguishable by conventional linear probes can be distinguished by these probes if their velocity distributions are sufficiently different. LiMR models can, therefore, be best tested and constrained by jointly analyzing data from CMB and late-time structure formation on both large and small scales.

12:15 to 12:30 Richa Arya (IISc, India) Primordial black holes and secondary gravitational waves from warm inflation

The inflationary paradigm of the early Universe has been extraordinarily consistent with the observations of the cosmic microwave background radiation, however, the microphysics governing it is not well understood. In this talk, I will focus on the warm inflation scenario and investigate its imprint on the observations. Warm inflation is a well-motivated and general description of inflation, in which the dissipative effects in a coupled inflaton-radiation system govern the dynamics of the Universe. Here, the inflaton interactions with radiation fields are not neglected; thus, there is a non-zero temperature during the inflationary phase. As a result, the dynamics of the Universe is modified, and the primordial power spectrum in warm inflation has distinct signatures compared to the standard cold inflation. I will discuss my study on some models of warm inflation and generation of primordial black holes (PBH) from them. PBH refers to the black holes that could have been produced in the very early Universe. Unlike the astrophysical black holes, which are the end products of stellar evolution, PBH spans a wide mass range. In particular, we focus on generating PBHs with mass in the range ($10^{17}-10^{23}$ ) g, which can explain the full dark matter abundance. Further, we calculate the scalar-induced secondary gravitational waves spectrum associated with the PBH formation and explore their signatures in the gravitational wave detectors. This is crucial for understanding the physics of inflation, dark matter and gravitational waves.

12:30 to 12:45 Amlan Chakraborty (IIA, India) Formation and Abundance of Late Forming Primordial Black Holes as Dark Matter

The Dark Matter (DM) is one of the mysterious components of our universe that accounts for almost 27% of matter-energy content in it. Out of all the proposed dark matter candidates, ’WIMP’ was thought to be the best-fitted one, yet its undetectability despite two decades of search, has propelled us to look for new candidate of dark matter beyond WIMPs. Recently Primordial Black Holes (PBHs) have emerged as one of the most potent and well-studied candidates, even though there are theoretical and observational constraints on PBHs. In our recent work, a late PBH formation mechanism has been proposed where a natural phase transition (around redshift ∼ 10^6) in a strongly interacting fermion-scalar fluid allows formation of an early dense halo that finally collapse into PBH. We find that the PBHs formed (within a mass range of ∼ 10^—16 – 10^—14M☉) in this manner indeed account for the entire DM density of the universe. We numerically compute the the mass function of DM PBHs in our scenario and its implication on cosmological observables.

14:30 to 16:00 -- Discussion
16:30 to 18:00 Shiv Sethi (RRI, India) Cosmological Perturbation Theory (Lecture 1)
Tuesday, 14 March 2023
Time Speaker Title Resources
09:30 to 10:10 Vera Gluscevic (University of Southern California, USA) Uncovering dark matter physics:from the early universe to near field cosmology

Cosmological observables, from the CMB anisotropy to the census of galaxies in the early and local universe, offer the most direct and broad tests for the nature of dark matter, including a number of scenarios that are challenging or even impossible to test in a laboratory setting. I will review the status of the recent early-universe and late-universe searches for the identity of dark matter, summarizing the best current limits on scattering between dark matter and baryons, the non-thermal production mechanisms for sterile neutrinos, and mass bounds on thermal-relic dark matter. I will highlight the interplay between complementary probes of dark matter physics, using the example of the 21-cm signal from the Cosmic Dawn, the CMB primary anisotropy, and substructure in the Milky Way. Finally, I will discuss the prospects for unveiling the physics of dark matter in the coming decade.

10:10 to 10:50 Thomas Abel (Stanford University, USA) Practical, Fast, Beyond 2-pt Statistics for Large Scale Structure Clustering
10:50 to 11:30 Mousumi Das (IIA, India) The Distribution of Dark Matter in Galaxies : from observations to cosmological simulations

One of the most well known evidences for the presence of dark matter is the flat rotation curves of galaxies, which was discovered several decades ago. Since then there have been several studies of the dark matter distribution in galaxies using both observations and simulations. In this talk I will cover the astrophysical detection of dark matter in galaxies and present the different methods that are used to determine the dark matter distribution in galaxies. I will also discuss how theoretical and simulation studies predict the morphology of galaxy halos and their evolution with time.

12:15 to 12:30 Sudipta Das (Visva-Bharati University, India) Imprints of interacting dark universe on cosmological perturbations

In this paper we have considered an interacting model of dark energy where the dark sectors are allowed to interact among themselves through an assumed relation. By solving the perturbation equations numerically, we have studied the imprints on the growth of matter as well as dark energy fluctuations. It has been found that for higher rate of interaction strength for the coupling term, visible imprints on the dark energy density fluctuations are observed at the early epochs of evolution. In order to check the viability of the model, we have tested the interacting model with different observational datasets and have looked into the evolution of the density contrast, and the effects on the CMB temperature fluctuation as well as matter power spectrum.

12:30 to 12:45 Arpan Kar (cQUEST, South Korea) Halo-independent bounds on the non-relativistic effective theory of WIMP-nucleon scattering from direct detection and neutrino observations

In my presentation I will talk about the halo-independent bounds on the WIMP-nucleon couplings of the non-relativistic effective Hamiltonian that drives the scattering process off nuclei of a WIMP of spin 1/2. We will see that for most of the couplings the degree of relaxation of the halo-independent bounds compared to those obtained by assuming the Standard Halo Model is with few exceptions relatively moderate in the low and high WIMP mass regimes, where it can be as small as a factor of 2, while in the intermediate mass range (10 -- 200 GeV) it can be as large as 1000. An exception to this general pattern, with more moderate values of the bound relaxation, is observed in the case of the spin-dependent type WIMP-proton couplings with no or a comparatively small momentum suppression, for which WIMP capture in the Sun is strongly enhanced because it is driven by scattering events off Hydrogen, the most abundant target in the Sun. Within this class of operators the relaxation is particularly small for interactions that are driven by only the velocity-dependent term, for which the solar capture signal is enhanced because of the high speed of scattering WIMPs inside the strong gravitational field of the Sun.

12:30 to 12:45 Khursid Alam (IISER Kolkata, India) Effects of reheating on moduli stabilization

Moduli potential loses its minima due to external energy sources of inflaton energy density or radiation produced at the end of inflation. But, the non-existence of minima does not necessarily mean destabilization of moduli. In fact, the destabilization of moduli is always dependent on the initial field values of the fields. In this work, we study carefully how the effects of reheating ease the problem of moduli destabilization. The associated time scale to produce the thermal bath allows a larger initial field range to stabilize the field. Contrary to the usual notion, the allowed initial field range is larger for higher temperatures when the effective potential is of a run-away nature. This eases the moduli destabilization problem for heavy mass moduli. For low mass moduli (≲ 30 TeV), the allowed field range still causes the cosmological moduli problem by violating the BBN constraints unless its initial abundance is suppressed.

14:30 to 16:00 -- Discussion
16:30 to 18:00 Shiv Sethi (RRI, India) Cosmological Perturbation Theory (Lecture 2)
Wednesday, 15 March 2023
Time Speaker Title Resources
09:30 to 10:00 Subhendra Mohanty (PRL, Ahmedabad, India) Gravitational wave Memory Signals from Binary orbits and Soft-Graviton Theorems

I will explain the calculation of memory effect from orbits of compact binaries and show the connection with calculations of amplitudes from soft graviton theorems.

10:10 to 10:50 Tathagata Ghosh (HRI, India) Di-Higgs Blind Spots in Gravitational Wave Signals

Conditions for strong first-order phase transition and generation of observable gravitational wave (GW) signals are very restrictive to the profile of the Higgs potential. Working in the minimal extension of the SM with a new gauge singlet real scalar, I’ll show that the production of signals relevant for future GW experiments, such as LISA, can favor depleted resonant and non-resonant di-Higgs rates at colliders for phenomenologically relevant regimes of scalar mixing angles and masses for the heavy scalar. I’ll discuss the emergence of these di-Higgs blind spot configurations in GWs and also show that di-boson channels, ZZ and WW , can restore the phenomenological complementarities between GW and collider experiments in these parameter space regimes.

10:50 to 11:30 Susmita Adhikari (IISER Pune, India) From the Edge of a Dark Matter Halo
12:00 to 12:15 Animesh Sah (TIFR, India) Cosmological Studies with Pantheon+ Compilation of Type 1a Supernovae

Type 1a supernovae have been used as distance rulers to study the kinematics of the universe and serve as the primary evidence of dark energy and the recently growing Hubble tension. The latest type 1a compilation released is Pantheon+, but there is some debate within the literature about the many corrections employed in the dataset and its treatment of uncertainties. We examine the peculiar velocity corrections in the Pantheon+ dataset and estimate the cosmological parameters using the Maximum Likelihood technique.

12:15 to 12:30 Himanshu Verma (IIT Bombay, India) Astrometric Microlensing of Primordial Black Holes with Gaia

The Gaia space telescope allows for unprecedented accuracy for astrometric measurements of stars in the Galaxy. In this work, we explore the sensitivity of Gaia to detect primordial black hole (PBH) dark matter through the distortions that PBHs would create in the apparent trajectory of background stars, an effect known as astrometric microlensing (AML). We present a novel calculation of the lensing probability, and we combine this with the existing publicly released Gaia eDR3 stellar catalog to predict the expected rate of AML events that Gaia will see. We also compute the expected distribution of a few event observables, which will be useful for reducing backgrounds. We argue that the astrophysical background rate of AML like events due to other sources is negligible (except possibly for very long duration events), and we use this to compute the potential exclusion that could be set on the parameter space of PBHs with a monochromatic mass function. We find that Gaia is sensitive to PBHs in the range of 0.4 Msun - 5\times10^7 Msun, and has peak sensitivity to PBHs of ~10 Msun for which it can rule out as little as a fraction 3\times10^{-4} of dark matter composed of PBHs. With this exquisite sensitivity, Gaia has the potential to rule out a PBH origin for the gravitational wave signals seen at LIGO. Our novel calculation of the lensing probability includes for the first time, the effect of intermediate duration lensing events, where the lensing event lasts for a few years, but for a period which is still shorter than the Gaia mission lifetime. The lower end of our predicted mass exclusion is especially sensitive to these type of lensing events. As and when time-series data for Gaia is released, our prediction of the lensing rate and event observable distributions will be useful to estimate the true exclusion/discovery of the PBH parameter space utilizing this data.

12:30 to 12:45 Md Riajul Haque (IIT Madras, India) WIMPs, FIMPs, and Inflaton phenomenology via reheating: the possibility of purely Gravitational reheating

My talk will mainly focus on the reheating dynamics after inflation and its possible implication on dark matter (DM) and inflaton phenomenology. We consider reheating through various possible channels of inflaton going into massless scalars (bosonic reheating) and fermions (fermionic reheating) via non-gravitational and gravity-mediated decay processes. We further include the finite temperature effect on the decay process. Along with their precise roles in governing the dynamics, we compared the relative importance of different temperature-corrected decay channels in the gradual process of reheating depending on the reheating equation of state (EoS), which is directly related to inflaton potential. Particularly, the universal gravitational decay of inflaton is observed to play a crucial role in the reheating process for a large range of inflaton decay parameters. For our study, we consider typical Î±-attractor inflationary models. We further establish the intriguing connection among those different inflaton decay channels and the CMB power spectrum that can have profound implications in building up a unified model of inflation, reheating, and DM. We analyze both fermion and scalar DM with different physical processes being involved, such as gravitational scattering, thermal bath scattering, and direct inflaton decay. Gravitational decay can again be observed to play a crucial role in setting the maximum limit on DM mass, especially in the FIMP scenario. Depending on the coupling strength, we have analyzed in detail the production of both FIMP and WIMP-like DM during reheating, and their detailed phenomenological implications from the perspective of various cosmological and laboratory experiments. References: 1. Phys.Rev.D 106 (2022) 2, 023506, 2.e-Print: 2301.01641 3. e-Print: 2201.02348 (Accepted in Phys.Rev.D )

14:30 to 16:00 -- Discussion
16:30 to 18:00 David Marsh (King's College London, UK) Cosmology of Ultralight Dark Matter: Searches and Constraints

Topics: Production of ultralight dark matter from vacuum realignment. Linear theory structure formation. Bounds from the CMB and large scale structure. Schrodinger-Poisson equation inside galaxies. Looking to the future with intensity mapping. Formation and structure of axion stars. Superradiance.

Thursday, 16 March 2023
Time Speaker Title Resources
09:30 to 10:10 Anjan Ananda Sen (JMI, India) Cosmological Tensions: Signals for New Physics beyond ΛCDM?
10:10 to 10:50 Rajeev Kumar Jain (IISc, India) Primordial Black Holes from Inflation:dark matter, Gravitational waves and Imprints from Evaporation
10:50 to 11:30 Mayuri S. Rao (RRI, India) Cosmology Experiments - the present day landscape

There have been tremendous advancements in cosmology in the past decades, coming from a combination of theory and measurement. There exist aspects of the standard cosmological model that remain poorly understood. Among these are inflation, cosmic dawn, and the epoch of reionization. Modern day experiments, on-going and upcoming are working towards making measurements to understand these periods, and thus constrain relevant parameters. In this talk I will give a brief overview of the existing constraints on some of these poorly constrained cosmological and astrophysical parameters, and lay out the landscape of some current and next-generation experiments and their targeted sensitivities.

12:00 to 12:15 Ragavendra H.V. (RRI, India) Unique observational imprints of ultra slow roll inflation

Recent literature is replete with models and mechanisms for the production of primordial black holes (PBHs) that could constitute significant fraction of dark matter in the current universe. Among the various models, a class of inflationary models known as ultra slow roll (USR) inflation stands as a promising candidate. These models generate significant population of PBHs along with enhanced strengths of secondary gravitational waves (GWs). Given the plethora of models in the literature, it is imperative to look for unique features of USR, to distinguish it from other contenders. USR models, besides enhancing the primordial scalar power over small scales, lead to nulling of scalar power at a specific scale close to the location of the peak in the spectrum. Further, the scalar bispectra arising from USR models have non-trivial amplitudes and shapes, such that they may alter the observational predictions that are computed using Gaussian assumptions. For instance, they lead to significant corrections to the spectral density of secondary GWs around the peak amplitude. In this talk, I shall highlight these characteristic signatures of USR and discuss the prospect of observing them through different cosmological probes such as the upcoming GW and 21-cm missions. Reference: [1] H. V. Ragavendra and L. Sriramkumar, an invited review accepted in Galaxies [arXiv:2301.08887 [astro-ph.CO]]

12:15 to 12:30 Aparajita Sen (IISER Thiruvananthapuram, India) Optimum Frequency Range for thermal dust removal and r-recovery in CMB-BHARAT

Detecting CMB B-modes, one of the major scientific goals of CMB-BHARAT, is challenging as the signal is deeply buried under the dominant astrophysical foreground emissions from the thermal-dust and the synchrotron. To facilitate the adequate subtraction of thermal-dust, the instrument design of CMB-BHARAT has included nine dust-dominated high-frequency bands over the frequency range of 220-850 GHz. In this talk, I will present our recent work. We have closely re-examined the utility of the high-frequency bands in foreground subtraction using a non-parametric component separation method.

12:30 to 12:45 Anoma Ganguly (TIFR, India) EDGES of the Dark Forest: A new absorption window into the composite dark matter and large scale structure

We propose a new method to hunt for dark matter using dark forest/absorption features across the full electromagnetic spectrum, especially in the bands where there is a desert i.e. regions where no strong lines from baryons are expected. Such unique signatures can arise for dark matter models with a composite nature and internal electromagnetic transitions. In the presence of a background source, such as a quasar, such interactions in the dark matter halos can produce a series of closely spaced absorption lines, which we call the dark forest. The dark forest feature is a sensitive probe of the dark matter self-interactions and the halo mass function, especially at the low mass end. Moreover, the absorption of CMB photons by dark matter gives rise to a global absorption signal in the CMB spectrum which can explain the anomalous absorption feature detected by the EDGES collaboration.

14:30 to 16:00 -- Discussion
16:30 to 18:00 David Marsh (King's College London, UK) The Postinflation QCD Axion

Topics: Focus on the QCD axion. Basics of particle physics and direct detection. Symmetry breaking after inflation and relic density from topological defects. Formation of miniclusters. Phenomenology of miniclusters.

Friday, 17 March 2023
Time Speaker Title Resources
09:30 to 10:10 Bhuvnesh Jain (University of Pennsylvania, USA) Large-scale structure: weak lensing and the S8 tension
10:10 to 10:50 Alexandre Refregier (ETH Zürich, Switzerland) Cosmological Weak Lensing
10:50 to 11:30 Tarun Souradeep (RRI, India) Structured test of the cosmological principle
12:00 to 12:15 Navin Chaurasiya (IUCAA, India) Galaxy-Dark matter halo connection and evolution using HSC photometric galaxies

In the paradigm of hierarchical structure formation, the galaxies are thought to form and evolve inside a potential well environment (halos) of 'collisionless' and 'only gravitationally interacting' form of matter. These dark halos have formed at the peaks of initial density fluctuations due to gravitational instability and as observations have revealed, are the sites of most of the galaxy formation and evolution. Estimating the presence of these dark structures of halos by using available galaxy surveys itself is an important and challenging task. This information can then be used to find out the connection between the galaxy and halo properties. Our current understanding of the structure formation and evolution is driven by simulations. At large scales the full hydrodynamic simulations are not feasible due to computational cost. However using 'the connection' (scaling relations) between galaxy properties like for example, 'stellar mass' versus the 'halo mass', semi-analytical models of structure formation can constrain the effectiveness of physical processes as a function of redshift, thus bypassing the need of full simulation from scratch. In our work, to estimate the masses of dark matter halos which host - (the lens galaxies) the photometric galaxies from HSC survey, we employ the technique of measurement of 'weak gravitational lensing' signals. Weak lensing being purely gravitational phenomena, directly and fully probes the total matter content responsible for lensing of the background source galaxies. Thus we are able to probe this matter content associated with lens galaxies responsible for lensing. We show the halo-mass vs stellar mass relation as our concluding scaling relation from low to high redshift bins of lens galaxies further split into bins of stellar masses, and in doing so we represent the power of wide layer of HSC survey for statistical studies like weak lensing.

12:15 to 12:30 Sambo Sarkar (IIT Kharagpur, India) Bound on self-interacting dark matter from galactic cores

Self-interactions between dark matter particles can induce core formation in galaxies and lead to thermalization of their central regions. The strength of self-interactions between dark matter particles is correlated to the size of the thermalized regions. The possibility of placing a conservative limit on the self-interaction cross-section by analyzing the distribution of core radius in isolated galactic haloes is explored in this work. We systematically use dark matter only N-body simulations of spherically symmetric isolated haloes incorporating isotropic self-scattering. We report a conservative upper limit on the self-interaction cross-section, σ/m< 9.8 cm^2/gm at 95% confidence level by comparing the generated distributions with the observed data.

12:30 to 12:45 Harshda Saxena (IIT Bombay, India) Kinetic Field Theory: Effects of modified gravity theories with screening mechanisms on non-linear cosmic density fluctuations

In a mean-field approximation within Kinetic Field Theory, it is possible to derive an accurate analytic expression for the power spectrum of resent-day, non-linear, cosmic density fluctuations. It depends on the gravity theory and the cosmological model via the expansion function of the background space-time, on the growth factor derived from it, and on the gravitational coupling strength, which may deviate from Newton’s constant in a manner depending on time and scale. In earlier work, we introduced a functional Taylor expansion around general relativity and the cosmological standard model to derive the effects of a wide class of modified-gravity theories on the non-linear power spectrum, assuming that such effects need to be small given the general success of the standard model. Here, we extend this class towards theories with small-scale screening, modelling screening effects by a suitably flexible interpolating function. We compare the Taylor expansion with exact solutions and find good agreement where expected. We find typical relative enhancements of the non-linear power spectrum between a few and a few ten per cent in a broad range of wave numbers between k ≳ 0.1 − 10 h Mpc, in good qualitative agreement with results obtained from numerical simulations.

14:30 to 15:10 P. Ajith (ICTS, India) Gravitational lensing of gravitational waves: A new probe of primordial black holes
15:10 to 16:00 -- Discussion
16:30 to 18:00 Thomas Abel (Stanford University, USA) Formation of first stars in the Universe
Monday, 20 March 2023
Time Speaker Title Resources
09:30 to 10:10 Tirthankar Roy Choudhury (NCRA, India) Understanding the Nature of Dark Matter using Neutral Hydrogen
10:10 to 10:50 Anupreeta More (IUCAA, India) Gravitational Lensing and Gravitational Waves, Tensions in Standard Cosmology
10:50 to 11:30 Mansi Dhuria (Pandit Deendayal Energy University, India) Self-Interacting Neutrinos: Unified Path to Dark Matter and Cosmological Tensions
12:00 to 12:15 Rathul Nath Raveendran (IACS, India) Distinguishing cosmological models through quantum signatures of primordial perturbations

In this talk, I discuss the evolution of various measures of quantumness of the curvature perturbation by integrating out the inaccessible entropic fluctuations in the multi-field models of inflation. In particular, I discuss the following measures of quantumness, namely purity, entanglement entropy and quantum discord. The models being considered in this talk are ones that produce large scale curvature power spectra similar to those produced by single-field models of inflation. More specifically, I consider different multi-field models which generate nearly scale invariant and oscillatory curvature power spectrum and compare their quantum signatures in the perturbations with the corresponding single-field models. I will show that, even though different models of inflation may produce the same observable power spectrum on large scales, they have distinct quantum signatures arising from the perturbation modes. This may allow for a way to distinguish between different models of inflation based on their quantum signatures.

12:15 to 12:30 Antara Dey (ISI Kolkata, India) Constraints on Dark Matter-Neutrino Interaction from 21-cm Cosmology

We have done a thorough investigation of the possible effects of interaction between dark matter (DM) and neutrinos on reionization history. We have constrained the interaction strength using 21 cm Cosmology and found out possible deviations from standard, non-interacting Î›CDM scenario. Comparing the results with the existing constraints from present cosmological observations reveals that 21 cm observations are more competent to constrain the interaction strength by a few orders of magnitude. We have also searched for prospects of detecting any such interaction in the upcoming 21 cm mission SKA1-Low by doing a forecast analysis and error estimation.

12:30 to 12:45 Arpan Hait (IIT Kanpur, India) Dark matter production during reheating

During reheating coherent oscillations of a field dissipate its energy density and form a dominating thermal bath. In this talk, I will discuss the thermalization of the decay products produced via increasing dissipation rate and its implication on the production of dark matter in the reheating epoch.

14:30 to 16:00 -- Discussion
16:30 to 18:00 Tirthankar Roy Choudhury (NCRA, India) Reionization and 21 cm Cosmology
Tuesday, 21 March 2023
Time Speaker Title Resources
09:30 to 10:10 Debaprasad Maity (IIT Guwahati, India) Reheating and its cosmological consequenecs

Our present understanding of reheating phase is incomplete due to a lack of observations. Apart from its cosmological implications, the reheating should play a vital role in particle physics and inflation model building.  In this talk, we elaborately discuss about role played by gravitional interaction in the reheating dynamics. We further discuss its cosmological consequences in in gravitational waves and dark matter phenomenology.

10:10 to 10:50 Nirmal Raj (TRIUMF, USA) Catching Dark Matter Underground at the Planck Mass and Beyond

Dedicated metre-sized detectors on Earth looking for dark matter particles via "direct detection" have caught none so far. This is perhaps because these particles are at least kilometres apart, thus coming with scant flux. I will discuss new strategies to catch them, and a search I performed in collaboration with the DEAP-3600 experiment, placing the first laboratory limits on particle dark matter at the Planck mass (1.2 x 10^19 GeV). I will also describe how neutrino experiments, with much larger detectors, can be repurposed to look for dark matter orders of magnitude beyond the Planck mass.

10:50 to 11:30 Arun Thalapillil (IISER Pune, India) Hidden objects and hidden physics
12:00 to 12:15 Kuldeep Purohit (Vadodara, India) Rotating Scalar Field and Formation of Bose Stars

We study numerical evolution of an initial cloud of self-gravitating bosonic dark matter with finite angular momentum and self-interaction in kinetic regime. It is demonstrated that such a system can undergo gravitational condensation and form a Bose star. The results show that the gravitational condensation time is strongly influenced by the presence of finite angular momentum or the strength of self-interaction. We find that in the cases related with attractive or no self-interaction, there is no significant transfer of angular momentum from the initial cloud to the formed star. However, for the case repulsive interaction our results indicate that such a angular-momentum transfer is possible. These results are consistent with the earlier analytical work where the stability of the rotating boson star was considered

12:15 to 12:30 Tarak Nath Maity (IISc, India) Neutrinos from Sun as a discovery tool for dark matter-electron scattering

We will discuss a novel strategy to search for dark matter (DM)-electron scattering. DM interacting with electrons may get captured inside the Sun. These captured DM may annihilate to produce different Standard Models (SM) particles. Neutrinos produced from these SM states can be observed in IceCube and DeepCore. Although there is no excess of neutrinos from the Solar direction, we find that the current results of IceCube and DeepCore set the strongest constraint on DM-electron scattering cross section in the DM mass range ~10 GeV to 1 TeV. This implies that future observations of the Sun by neutrino telescopes have the potential to unravel DM-electron interactions.

12:30 to 12:45 Shouvik Roy Choudhury (IUCAA, India) Massive Neutrino Self-Interactions and Inflation

Based on: JCAP 10 (2022) 018 (arXiv: 2207.07142). Certain inflationary models like Natural inflation (NI) and Coleman-Weinberg inflation (CWI) are disfavoured by cosmological data in the standard Î›CDM+r model (where r is the scalar-to-tensor ratio), as these inflationary models predict the regions in the ns-r parameter space that are excluded by the cosmological data at more than 2Ïƒ (here ns is the scalar spectral index). Cosmological models incorporating strongly self-interacting neutrinos (with a heavy mediator) are, however, known to prefer lower ns values compared to the Î›CDM model. Considering such neutrino self-interactions can, thus, open up the parameter space to accommodate the above inflationary models. In this work, we implement the massive neutrino self-interactions with a heavy mediator in two different ways: flavour-universal (among all three neutrinos), and flavour-specific (involving only one neutrino species). We implement the new interaction in both scalar and tensor perturbation equations of neutrinos. Interestingly, we find that the current cosmological data can support the aforementioned inflationary models at 2Ïƒ in the presence of such neutrino self-interactions.

14:30 to 16:00 -- Discussion
16:30 to 18:00 Lasha Berezhiani (Max Planck Institute for Physics, Germany) Dark Matter Superfluidity and Galactic Dynamics

After overviewing some of the short scale puzzles within the standard cold dark matter paradigm, I will discuss the idea of dark matter superfluidity as a tantalizing phenomenon in this context. One of the motivations is to provide a novel mechanism behind empirical correlations between dark and baryonic sectors within galaxies, by having an emergent long-range interaction between baryons mediated by superfluid phonons. I will discuss the challenges needed to be overcome for a successful realization of this paradigm. Another motivation is the superfluidity itself, without phonon-mediated forces. I will discuss the recent progress in understanding the structure of dark matter haloes in this scenario and the implications for the galactic dynamics.

Thursday, 23 March 2023
Time Speaker Title Resources
09:30 to 10:10 Surjeet Rajendran (Johns Hopkins University, USA) New Directions in the Search for Dark Matter
10:10 to 10:50 Saurabh Singh (RRI, India) Observing cosmic dawn through 21-cm signal

The emergence of the first stars and galaxies, often termed as cosmic dawn, and subsequent ionization of the Universe constitute crucial epochs in the cosmic timeline. Studying the nature of the first sources of radiation is essential to understanding their evolution. The spin-flip transition from neutral hydrogen, 21-cm signal, constitutes a powerful probe of the early Universe. Tracing its brightness at different cosmological redshifts and spatial scales can unravel several poorly constrained astrophysical properties of the first stars and galaxies and their interaction with the intergalactic medium. However, observing the elusive 21-cm signal from high redshifts is challenging due to multiple factors, which include exceptionally bright foregrounds and instrumental systematics. In this talk, I will discuss some of these challenges and how they are being addressed by experiments worldwide. I will draw examples from SARAS and HERA, 21-cm experiments aiming to detect the global and spatial fluctuations of the 21-cm signal, respectively. I will discuss their calibration techniques, unique systematic and foreground handling approaches, and how proposed space-based observations from PRATUSH can overcome several challenges. I will conclude with the latest results from these experiments, which include inference on the anomalous detection from the EDGES experiment, constraints on the properties of the galaxies in the early Universe, and the improved limits by a joint model for the interferometric and global signal experiments.

10:50 to 11:30 Urjit Yajnik (IIT Bombay, India) Emergent Dark Energy from hidden fermions and photons
12:00 to 12:15 Nilanjandev Bhaumik (IISc, India) Probing the early universe with gravitational wave background and primordial black holes

The expansion history between the end of inflation and big bang nucleosynthesis, is not accessible from any direct observations at our disposal. The advent of gravitational wave astronomy and recent developements involving primordial black holes (PBH) as a dark matter candidate has offered us a novel way to probe this intermediate phase. We find different reheating histories to leave distinct effects on both the PBH formation and associated second order stochastic gravitational wave background (SGWB). Particularly a matter dominated reheating causes an aditional amplification in SGWB spectrum. We further explore the possibility of ultra-low mass PBHs to dominate the universe for brief duration before evaporation. Taking into account both the inflationary and PBH density fluctuations, we show that such a scenario leads to an uniquely shaped doubly peaked SGWB spectrum, detectable in future GW observatories. Detection or non-detection of such a signal will confirm or constrain the PBH parameters, as well as PBH evaporation induced baryogenesis, dark matter and dark radiation.

12:15 to 12:30 Akash Kumar Saha (IISc, India) Sensitivities on non-spinning and spinning primordial black hole dark matter with global 21 cm troughs

21 cm line arising from neutral hydrogen is one of the most important tools for understanding the thermal and ionization history of the early universe. Primordial black holes (PBHs) are one of the oldest and well motivated DM candidates. Hawking radiating low-mass PBHs ($10^{15}$âˆ’$10^{18}$ g) can heat up the Intergalactic medium (IGM) by injecting all Standard Model particles and that can affect the global 21 cm signal. Recently, EDGES has claimed an excess in their detected global 21 cm signal, though more recently SARAS 3 has rejected that claim. By considering an EDGES-like measurement of the global 21 cm signal, we derive sensitivities on non-spinning and spinning PBH dark matter (DM). These sensitivities are competitive with existing bounds from various other astrophysical observables. Besides, we also investigate projected bounds on PBH DM abundance using the global 21 cm signal expected from the Dark Ages. We show that in future, unambiguous measurement of global 21 cm signal can either potentially discover or constrain PBH DM.

12:45 to 13:00 Bihag Dave (Ahmedabad University, India) Self-interactions of ultra-light dark matter and observations at galacticÂ scales

Recently, ultra-light Scalar Field Dark Matter (SFDM) has emerged as a promising alternative to the standard Cold Dark Matter (CDM) model. However, viability of models with no self-interactions (Fuzzy Dark Matter), in solving the small scale issues of CDM is under question while relevant masses are increasingly constrained using various astrophysical and cosmological observations. It is then interesting to consider the effects of self-interactions on these constraints. First we shall look at the impact of self-interactions on mass and radius of stable structures (solitons). Then we shall look at two astrophysical observations that can potentially constrain self-interactions: amount of mass contained within some region around the galactic center and galactic rotation curves of dwarf galaxies. We find that for the former, smaller values of attractive self-interactions are allowed compared to repulsive self-interactions. For the latter, repulsive self-interactions are preferred as compared to attractive or no self-interactions. For repulsive self-interactions, probed values of self-interaction strength is $\sim \mathcal{O}(10^{-90})$.

14:30 to 16:00 -- Discussion
16:30 to 18:00 Nishita Desai (TIFR, India) Looking for Dark Matter @ LHC
Friday, 24 March 2023
Time Speaker Title Resources
09:30 to 10:10 Nishita Desai (TIFR, India) DM searches at colliders
10:10 to 10:50 Ranjan Laha (IISc, India) Dark matter substructures affect dark matter-electron scattering in xenon-based direct detection experiments

Recent sky surveys have discovered a large number of stellar substructures. It is highly likely that there are dark matter (DM) counterparts to these stellar substructures. We examine the implications of DM substructures for electron recoil (ER) direct detection (DD) rates in dual phase xenon experiments. We have utilized the results of the LAMOST survey and considered a few benchmark substructures in our analysis. Assuming that these substructures constitute ∼10% of the local DM density, we study the discovery limits of DM-electron scattering cross sections considering one kg-year exposure and 1, 2, and 3 electron thresholds. With this exposure and threshold, it is possible to observe the effect of the considered DM substructure for the currently allowed parameter space. We also explore the sensitivity of these experiments in resolving the DM substructure fraction. For all the considered cases, we observe that DM having mass O(10)MeV has a better prospect in resolving substructure fraction as compared to O(100)MeV scale DM. We also find that within the currently allowed DM-electron scattering cross-section; these experiments can resolve the substructure fraction (provided it has a non-negligible contribution to the local DM density) with good accuracy for O(10)MeV DM mass with one electron threshold.

10:50 to 11:30 Suvodip Mukherjee (TIFR, India) Smoking gun signal of primordial black holes from gravitational wave observations
12:00 to 12:45 Vivian Poulin Status of Hubble tension
14:30 to 16:00 -- Discussion