Descrizione del progetto
Sfruttare i raggi gamma per gettare nuova luce sulle onde gravitazionali
La rilevazione e la caratterizzazione delle onde gravitazionali a bassa frequenza può chiarire importanti interrogativi non risolti in vari campi, quali fisica, astronomia e cosmologia. Gli scienziati si sono tradizionalmente avvalsi dei radiotelescopi per cercare un fondo di onde gravitazionali; il rumore, tuttavia, proveniente soprattutto dal mezzo interstellare, complica le misurazioni in tal ambito. Il progetto GIGA, finanziato dal CER, si prefigge di sfruttare i raggi gamma, che non sono influenzati da questo rumore, per superare tale barriera. Il progetto intende creare un insieme di stelle di neutroni rotanti estremamente stabili per studiare il fondo di onde gravitazionali, misurando inoltre le proprietà del mezzo interstellare ed esplorando gli accoppiamenti della materia oscura dipendenti dall’energia. I risultati offerti da GIGA dovrebbero fornire una visione pionieristica della dinamica dei buchi neri supermassicci e delle galassie che li ospitano.
Obiettivo
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.
Campo scientifico
- natural sciencesphysical sciencesastronomyobservational astronomygravitational waves
- natural sciencesphysical sciencesastronomyobservational astronomyradio astronomy
- natural sciencesphysical sciencesastronomyphysical cosmologybig bang
- natural sciencesphysical sciencesastronomyastrophysicsblack holes
- natural sciencesphysical sciencesastronomyplanetary sciencescelestial mechanics
Parole chiave
Programma(i)
- HORIZON.1.1 - European Research Council (ERC) Main Programme
Argomento(i)
Meccanismo di finanziamento
HORIZON-ERC - HORIZON ERC GrantsIstituzione ospitante
3526 KV Utrecht
Paesi Bassi