Conveners
Planning Gravitational Wave Detections form LISA: Block 1
- Philippe Jetzer (University of Zurich)
Description
LISA is a large ESA mission with an important NASA contribution. It is scheduled to be launced in 2034. The scope of LISA is to detect and study low-frequency gravitational waves (GW) from about 0.1 mHz to 1 Hz, and thus to complement ground-based GW observatories. LISA will allow to detect supermassive black holes (typically of 10^6 - 10^7 solar masses) merging at cosmological distances. Mergers of a supermassive black hole with another compact object (EMRI) produce a very clean GW signal which LISA will be able to measure with high precision. Another class of objects are ultra-compact binaries, in particular of white dwarfs in our Galaxy, since they are important sources of GW in the mHz frequency range. Moreover, it will be possible to detect or put strong constraints on the primordial gravitational wave background, which is just, as the cosmic microwave background, a leftover from the Big Bang. The aim of this parallel session is to discuss various aspects of the physics and astrophysics related to the above mentioned objects observable with LISA as well as issues related to the LISA data analysis.
We study hydrodynamical simulations of galaxy formation, based on the GADGET-3 code, and investigate supermassive black hole binaries coalescence at $5.5
The LISA detectability of GWs from supermassive black hole mergers will crucially depend on the physical properties of their host galaxies.
In this talk I will present a semi-analytic galaxy formation model, Delphi, that fully tracks the accretion- and merger-driven hierarchical assembly of the dark matter halo, gas, stellar, and black hole masses of high-redshift (z > 5) galaxies. We...
In 2034, within the rapidly changing landscape of gravitational-wave astronomy, the Laser interferometer Space Antenna will be the first space-based detector that will observe the gravitational spectra in the millihertz frequency band. It has recently been proposed that numerous LIGO/VIRGO sources will also be detectable by LISA. LISA will be able to detect binary black holes from our Milky...
This abstract is primarily based on my recent papers ApJ 909 (2021) 65 and ApJ 896 (2020) 69.
After predicting many sub- and super-Chandrasekhar limiting mass white dwarfs from the observations of peculiar type Ia supernovae, researchers have proposed various models to explain these two classes of white dwarfs separately. We showed that these two peculiar classes of white dwarfs, along with...
The future spaceborne gravitational wave detector LISA will probe a vast array of gravitational wave sources in the millihertz frequency band. Many of these sources will not be individually resolvable, instead adding incoherently to form stochastic gravitational wave backgrounds or foregrounds. The angular structure of these stochastic signals on the sky can be used to understand the spatial...
Close white dwarf binaries within our galaxy are promising sources of gravitational wave signals for Laser Interferometer Space Antenna (LISA). While the majority of such systems are expected to have circular orbits, a small portion of those formed through dynamical channels can have significant eccentricities. Analyzing the gravitational wave signals from these systems requires accurate...
