GIGA
Financiado
A Gamma-ray Infrastructure to Advance Gravitational Wave Astrophysics
When galaxies merge, do their central supermassive black holes also merge? How does the merger affect star formation and the evolution of galaxies? How does physics beyond the Standard Model of particles affect the Universe? The...
When galaxies merge, do their central supermassive black holes also merge? How does the merger affect star formation and the evolution of galaxies? How does physics beyond the Standard Model of particles affect the Universe? The detection and characterisation of low-frequency gravitational waves (GWs) will address these fundamental and longstanding questions of astronomy and cosmology.
Supermassive black holes at the centres of merging galaxies are expected to form binary systems whose orbital motion generates GWs. A cosmological population of such systems combine to build up a GW background (GWB). Such a GWB is also expected if the Universe went through an inflationary period, providing a GW map just moments after the Big Bang. Pulsar timing arrays (PTAs), which are ensembles of extremely stable millisecond pulsars (rotating neutron stars), can be used to study this GWB.
Searches for the GWB have typically used sensitive radio telescopes. However, radio data exhibit complex noise processes, predominantly arising from the interstellar medium (ISM), that limit its sensitivity and introduce bias. Gamma rays are immune to the effects of the ISM and a gamma-ray PTA can overcome several of the limitations affecting radio data. GIGA will (a) establish a gamma-ray PTA and independently detect the GWB, (b) develop advanced inference techniques to distinguish its astrophysical origins, (c) measure properties of the ISM through multiwavelength studies, and (d) explore energy-dependent couplings of dark matter. Through these avenues, GIGA will also maximise the sensitivity of radio PTAs and provide crucial validation of their measurements.
The detection of the GWB will provide the first stringent constraints on the dynamical evolution of supermassive black holes and their host galaxies while advanced inferences techniques will aid in disentangling weaker astrophysical sources including cosmic strings and phase transitions, thus probing physics beyond the Standard Model.
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Duración del proyecto: 60 meses
Fecha Inicio: 2023-12-05
Fecha Fin: 2028-12-31
Fecha Fin: 2028-12-31
Línea de financiación: concedida
El organismo HORIZON EUROPE notifico la concesión del proyecto el día 2023-12-05
Línea de financiación objetivo
El proyecto se financió a través de la siguiente ayuda:
ERC-2023-STG:
ERC STARTING GRANTS
Cerrada
hace 2 años
Presupuesto
El presupuesto total del proyecto asciende a
2M€
Líder del proyecto
STICHTING NEDERLANDSE WETENSCHAPPELIJK ONDERZ...
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Perfil tecnológico
TRL
4-5
Perfil tecnológico
TRL
4-5
237.31K€ |
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