Gruppo Virgo MiB+PR (PI Bernuzzi) Gruppo Virgo TO (PI Nagar)
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1 Pisa, Sept 12th, 2017 Gruppo Virgo MiB+PR (PI Bernuzzi) Gruppo Virgo TO (PI Nagar) Planned activities: Extreme matter from CBC signals CBC waveform R&D Offline analysis R&D Astrophysical modeling of CBs Rates of R&D
2 Gruppi Virgo MiB+PR & TO Mission: Develop the theoretical knowledge and tools necessary for the GW data analysis and the interpretation of compact binaries events Top-players with unique expertises on all key aspects Waveform modeling [Bernuzzi, Nagar] Analytical & numerical relativity [Bernuzzi, Nagar] Multimessenger astrophysics [Bernuzzi, Colpi, Ghirlanda, Perego, Salafia] Formation channels & rates [Colpi, Mapelli, Spera] First Virgo group focusing on CBC waveform development, independent models [LIGO main players: AEI, Cardiff-Palma] DEVELOP state-of-art CBC models: GW from binary black holes [Nagar+ 14,17] GW from binaries with matter [Bernuzzi+ 15,17] EM counterparts and afterglows of [Colpi, Ghirlanda, Perego, Salafia +17] Dynamical formation channels in cosmological framework [Spera, Mapelli 17] Cosmography with multi-messenger signals [Colpi, Ghirlanda, Salafia +17] WANT TO: Interface and develop offline searches and PE pipelines Contribute to event interpretation and science
3 Virgo role in GW astronomy observations (< 2023) Network of detectors OBSERVATORIES Improved sensitivity for PE Enlarge the horizon (detection rate) Sky localization Multiple compact binaries (CB) events New sources: binary neutron stars (BNS) (and BH-NS binaries) Electromagnetic counterparts Key gap to fill amongst INFN activities Interface data-analysis & theoretical modeling
![2012 Nagar+ 2017] Is GR correct? Is the source a pair of black holes? Horizon?](/docs-images/72/66931043/images/4-2.jpg "No-hair theorem? How do these black holes form?")
4 Example: Extracting information from BBH events noise signal DATA ANALYSIS PIPELINES (Matched filtering) EOB MODELING: dynamics & waveforms Resummed EOB model: [Damour&Nagar 2012 Nagar+ 2017] Is GR correct? Is the source a pair of black holes? Horizon? No-hair theorem? How do these black holes form? Answer to each question requires waveforms and dedicated pipelines
5 Example: Multimessenger signals from BNS events Constraints on neutron star matter (EOS) Origin of heavy elements Identification of CBC as engines of GRB and kn Measure of H0 Strong-field modeling + nuclear & astrophysics input NUMERICAL RELATIVITY & RELATIVISTIC ASTROPHYSICS models: GW from CBC w\ tidal effects [Bernuzzi ] Kilonova (kn) emission [Perego, Colpi, Ghirlanda+ 2017]
6 Science output from CBCs Fundamental physics High-energy astrophysics Cosmology Strong field test of dynamical general relativity Constraints on structure of matter at supranuclear densities (NS EOS) Origin of heavy elements * Kilonovae and r-process site * Constraints on stellar evolution and BH and NS binary formation models Unveil short-gamma-ray-burst (SGRB) engines * Cosmography, H0 * GOAL OF THE MiB+PR & TO groups: Maximize this science outcome exploiting synergy with data-analysis * requires electromagnetic counterpart
7 Synergy & Collaborations Virgo Pisa (Del Pozzo) CBC data analysis (PE) Virgo Trento-Padova (Ciolfi, Giacomazzo, Prodi) Burst data analysis BNS modeling Virgo GSSI * (Branchesi) EM counterparts Virgo MIB+PR & TO (Bernuzzi, Colpi, Ghirlanda, Mapelli, Nagar) CBC waveform R&D Rates and population Astrophysical distribution Virgo NIKHEF (Van den Broeck) CBC data analysis (PE) Virgo Nejmengen * (Nissanke. Schimdt) Rates and population Astrophysical distribution Virgo Valencia & Paris * (Font, Porter) CBC data analysis LIGO Cardiff-Palma (Hannam, Husa) CBC waveform R&D * starting
8 People & Budget 2018 Bernuzzi, Sebastiano (0.6) TOT = 45.5k EURO (w/ startup cost ***) Colpi, Monica (0.4) Ghirlanda, Giancarlo (0.5) Mapelli, Michela (0.4) Perego, Albino * (0.5) Salafia, Om ** (0.4) Spera, Mario * (0.5) Messina, Francesco ** (0.8) Mangiagli, Alberto ** (0.8) Nagar, Alessandro (0.5). TOT = 15k EURO Riemenschneider, Gunnar ** (0.8) Note: * Assegnista fondi INFN/CIPE o Uni ** Dottorando Uni (Start Nov 2017, FTE included in preventivo) *** Missioni: ~ 8.5k / FTE *** Inventario (Next slide) + 4 assegni x 5 yr su fondi esterni ERC-StG BinGraSp (SB) assegno x 3 yr su fondi esterni FARE MIUR MeNeS (SB)
9 Local resources (not HPC!) Server [e.g. (2x) Xeon 8-Core 2,4GHz 20MB 128GB] Installed at UniPR data center and maintained there Storage 10TB, attached to the server Workstations (3x) Code development and preproduction Examples Development of waveform surrogate Hybrid waveform construction Pipeline development and testing Personal laptops insufficient Prerequisite to production URGENT! [Lackey,Bernuzzi+ 2016] PRODUCTION WILL BE THEN MOVED TO HPC FACILITIES CINECA/CNAF
10 Extra slides
11 NETWORK OF DETECTORS GW Observation GW MODELING (Source dynamics & Waveforms) noise signal DATA ANALYSIS PIPELINES (Matched filtering) RELATIVISTIC ASTROPHYSICS (Formation, Rates & Pop, interpretation, EM counterparts)
12 Binary neutron star waveform models (Bernuzzi, Nagar)
13 Multi-messenger & multiband (Colpi,Ghirlanda,Perego)
14 Progenitors & Formation channels (Spera,Mapelli) Binary black holes cosmic merger rate density Population synthesis (isolated) + N-body (dynamical formation) + cosmological simulations
![4 Msun, Radius~10 km] d ~ 50 km Inspiral merger postmerger Time Gravity field (~M/d)](/docs-images/72/66931043/images/15-1.jpg "Velocities (~0.")
15 Backup slide: ERC-StG BinGraSp (Bernuzzi) Modeling the Gravitational Spectrum of Neutron Star Binaries d ~ 150 km Collision of neutron stars [Mass~1.4 Msun, Radius~10 km] d ~ 50 km Inspiral merger postmerger Time Gravity field (~M/d) Velocities (~0.1 c) Densities D~200 Mpc ( far away ) from the source: Strain, dl/l = h ~ Frequency span Hz (broad band)
16 Status of ground-based GW observations AdvLIGO runs: O1 and O2; Virgo joined O2 Three binary black holes (BBH) events from Sept. 2015: - Direct gravitational-wave (GW) detection - Evidence for BH and merging BBH - GR tests in strong and dynamic regime - Evidence for population of stellar-mass BBH
17 Future of ground-based GW observations (< 2023) Network of detectors at improved accuracy Multiple compact binaries (CB) events New sources: binary neutron stars (BNS), and BH-NS binaries Sky loc. & Electromagnetic counterparts From DETECTORS to network of OBSERVATORIES key step: Interface data-analysis & theoretical efforts
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