Théorie

I will present a bit more extended version of the talk that I gave recently at the TAUP2021 conference, with overview of the recent developments in the multi-messenger astronomy.

Black holes (BHs) cover a wide range of mass: from the stellar BH binaries detected with LIGO / Virgo to the massive BHs residing at the center of galaxies. Both these populations will be detectable in future by LISA at low-frequency. In this talk, I will provide a general overview of the current detections from LIGO / Virgo, describing the current state-of-the-art and I will highlight the potential of the LISA mission.

The dawn of gravitational wave (GW) astronomy has enabled new probes of dark matter. In particular, the formation and abundance of primordial black holes (PBHs) can be probed through GWs. In this talk I will discuss different ways how GW observations can be used to probe PBHs and I will review the implications of LIGO-Virgo observations on PBHs.

Gravitational waves (GW) can be used to probe various epochs in the early Universe. In this talk I will discuss about the production of Gravitational waves in a particular model of inflationary magnetogenesis. In this model, we require a low energy scale for inflation and reheating (reheating temperature, TR < 104 GeV) and have a blue spectrum of electromagnetic (EM) field which peaks around the horizon scale of reheating.

Among the sources which the Laser Interferometer Space Antenna (LISA) will observe are the signals from Massive Black Hole Binaries during their inspiral, merger and ring-down phases. To estimate physical parameters of these systems and their localisations, one has to perform some form of Bayesian Inference. The most common approach to do it is through defining a likelihood function and producing posterior samples with some form of sampling technique. The disadvantage of such sampling methods is that they are slow.

In this talk, a tale of two separate studies on gravitational waves (GWs) will be briefly presented.

Gravitational waves have a periodic effect on the apparent positions of stars on the sky. This effect can be quantified and hence ultra-precise astrometric measurements (like the ones from Gaia) can provide a new method to search for gravitational signals.

Over the next few decades, we will have an exciting opportunity to test gravitational waves (GWs) from the early Universe with space interferometries. In this talk, we focus on GWs from first-order phase transitions and present recent efforts to improve the prediction on the GW spectrum. We first present an efficient numerical scheme to calculate GWs from sound waves (under the assumption that the system is in the linear regime) based on 2010.00971 (with T.Konstandin and H.Rubira).

The stochastic gravitational-wave background is a superposition of many astrophysical and cosmological sources, such as unresolved compact binaries, cosmic strings, and phase transitions in the early Universe. We highlight the importance of source separation in the case of a detection. By separating the individual sources, we can reveal remnants of early-universe processes. We use the data from the third LVK observing run to explore the parameter space of first-order phase transition models. We then investigate signs of parity violation in gravitational-wave data.