EINSTEIN TELESCOPE probing the extreme through gravitational waves - PowerPoint PPT Presentation

EINSTEIN TELESCOPE probing the extreme through gravitational waves G Losurdo – INFN Pisa on behalf of the ET Collaboration Slide credits: S Hild, F Linde, H Lück, M Punturo, B Sathyaprakash, M Vasuth, …

TWO GROUND-BREAKING DISCOVERIES A NEW ERA IN THE OBSERVATION OF THE UNIVERSE GW170817 GW150914 Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 2

WHY 3G? WHY NOW? LIGO and Virgo both have facility-imposed limits on sensitivity q length, on surface site, obsolescence - At best a factor 3 in sensitivity can be gained wrt to the “advanced” LIGO/Virgo - We are ready to realize an infrastructure compatible with the q development of the interferometric detectors for decades 3G detector: q extend by ~10x the distance of sight wrt to the “advanced detectors” - entend the bandwidth towards lower frequencies (1 Hz target) - The first and second generations have required ~15 years between q the concept and the operation EINSTEIN TELESCOPE: concept developed in a FP7 Design Study, q involving France, Germany, Italy, the Netherlands, UK today the ET community also involves Belgium, Hungary, Poland, Spain, … - Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 3

SCIENCE CASE Extreme matter Extreme gravity Extreme universe Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 4

EXTREME MATTER Nucleons + Quark Nucleons exotic matter DEMOREST+, 2010 INTERNAL STRUCTURE AND COMPOSITION OF NS (LARGELY UNKNOWN) ENCODED IN THE EQUATION OF STATE Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 5

EXTREME MATTER WE ARE ABLE TO COMPUTE THE WAVEFORMS FOR THE VARIOUS EOS Takami, Rezzolla, Baiotti (2014) Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 6

EXTREME MATTER A 3G DETECTOR IS NEEDED TO MEASURE WHICH EOS IS THE RIGHT ONE Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 7

EXTREME GRAVITY Precision tests of alternative theories q polarizations - graviton mass - Lorentz invariance - Exotic compact objects q BH QNM q Pisa Meeting, Elba, May 31 2018 8 G Losurdo - INFN Pisa

EXTREME UNIVERSE Hubble parameter q Stochastic background q Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 9

WE HAVE THE RIGHT INSTRUMENT. NOW WE NEED TO MAKE IT BETTER AND BETTER AND BETTER… Galileo, 1610 Galileo, 1616 HST, 400 yrs later Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 10

DETECTOR CONCEPT Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 11

SENSITIVITY GOAL Advanced Virgo MERGER PHYSICS MASS ACCURACY LOCALIZATION HIGH MASS/HIGH Z NUMBER of SOURCES ET Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 12

WIDEN THE BAND: UNDERGROUND Limitations to LF sensitivity q rejection of seismic noise - newtonian noise - Both can be eased by going underground q noise at 2 Hz reduced by ~2 orders of magnitude Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 13

NEWTONIAN NOISE CREDIT: D Fiorucci Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 14

WIDEN THE BAND: XYLOPHONE Improving al low and high frequency with a single detector is very q challenging HF requires more laser power - LF requires cold mirrors - Idea: split the detection band over 3 “specialized” instruments q Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 15

Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 16

STAND-ALONE OBSERVATORY Start with a single 12%3#'2%45'6'3789' q :;689<8%'489#28%4=15)>? (xylophone) detector !"#$%&'('#()*%+*'&,%-*''.%".&%/01'2 #).343(3%)5%(6)%74#$'03).%4.('*8 5'*)9'('*3:%;$'%<=%&'('#()*3%.''& ).'%540('*#">4(?%'"#$,%6$40'%($'%@=% &'('#()*3%*'A14*'%B%540('*%#">4(4'3 '"#$%&1'%()%($'%13'%)5%&'(1.'& 34-."0%*'#?#04.-: -./0 -./0 $% -./0 !"# &'(),+ &'()*+ $% !"# Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 17

STAND-ALONE OBSERVATORY Start with a single 34%5#'4%67'.'589:' q ;<.9:=9%'69:#49%6>37)?@ (xylophone) detector !"#$%&'('#()*%+*'&,%-*''.%".&%/01'2 #).343(3%)5%(6)%74#$'03).%4.('*8 Add a second one to 5'*)9'('*3:%;$'%<=%&'('#()*3%.''& q ).'%540('*#">4(?%'"#$,%6$40'%($'%@=% fully resolve polarization &'('#()*3%*'A14*'%B%540('*%#">4(4'3 '"#$%&1'%()%($'%13'%)5%&'(1.'& 34-."0%*'#?#04.-: /012 /012 Antenna pattern for a polarized GW: $% !"# /012 !"# simple “L” (left) vs Triangle (right) -."),+ $% &'(),+ &'()*+ $% -.")*+ !"# $% !"# Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 18

STAND-ALONE OBSERVATORY !"# Start with a single 56%7#'6%89'.'7:;<' $% q =>.;<?;%'8;<#6;%8@59)AB (xylophone) detector C"4D'08;E8F.;%GF87"7<'%76;%78H8I18 /0%)*+ @$9JK859JK8L&JK8-LK8M&J8;E8*+)$+!7B !"#$%&'('#()*%+*'&,%-*''.%".&%/01'2 ;E8N?6:?81I8O0'8:0;G'%6:P8 #).343(3%)5%(6)%74#$'03).%4.('*8 Add a 2 nd one to fully 5'*)9'('*3:%;$'%<=%&'('#()*3%.''& C"4D'08;E8F%;04O.F87"7<'%76;%7 q @M&JK8-LK8-Q8O%(8+AB8H8RS8E;0 ).'%540('*#">4(?%'"#$,%6$40'%($'%@=% /0%),+ .6%'0O08E6.#'0:OT6#6'78O%(8SR8E;08 resolve polarization &'('#()*3%*'A14*'%B%540('*%#">4(4'3 #06O%G".O08E6.#'08:OT6#6'7 '"#$%&1'%()%($'%13'%)5%&'(1.'& 34-."0%*'#?#04.-: -'O478<'08#"%%'.8HU88 Add a 3 rd one for null q $% !"# stream and redundancy 1234 1234 $% !"# 1234 !"# -."),+ $% &'(),+ &'()*+ $% -.")*+ !"# $% !"# Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 19

ET INFRASTRUCTURE CONCEPT ET DESIGN STUDY, 2011 Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 20

ET AND THE INTERNATIONAL FRAMEWORK Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 21

ET COLLABORATION Call for interested launched at the ET Symposium (May 19-20) q Subscriptions by individual scientists (~450 so far) q Steering Committee nominated to write the Collaboration statute q and the governance rules Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 22

ESFRI It is crucial to enter in the 2020 update of the ESFRI roadmap q Update window: Jan-Aug 2019 q We need to define the political support and financial commitment: q Lead Country/Ent Lead Country/Entity ity - Participating countries/entities - Inclusion in National research infrastructure roadmap (when applicable) - Cost estimates and repartition - No need to choose the site in the proposal q Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 23

COST AND TIMELINE The realization of the ET observatory may cost 1-1.5 GEuros . Final q cost TBD on the basis of final choice of geometry and infrastructure features - Techincal Design Report - TIMELINE: q 2021-22: site selection - 2023-24: TDR - 2025: infrastructure realization start - 2030-31: commissioning start - 2032+: operation - Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 24

TOWARDS A 3G NETWORK ET-3G idea is spreading in the world q A similar scale GW observatory concept (Cosmic Explorer) is currently under - consideration in the US Or other designs that may emerge - A global approach to coordinate the efforts toward a Global q Research Infrastructure vision is underway Bottom-Up approach: GWIC-3G - Through the “Gravitational Wave International Committee”, scientists have established • a coordination team named GWIC-3G (see next slide) that is investigating the future network of 3G observatory from several points of view: addressing its scientific potential, the technological development needed, the opening and growing of the scientific community, the relationship with the funding agencies and the governance model to be adopted. Top-Down approach: GWAC - Funding agencies supporting or interested in GW research activities have established • the “Gravitational Wave Agencies Correspondents”, an information exchange forum to develop higher-level coordination Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 25

PLANS IN THE US 40 km ON-SURFACE DETECTOR Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 26

ET INFRASTRUCTURE FEASIBILITY STUDIES Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 27

TUNNEL Golden rules: q a new (and expensive) infrastructure must not be born short in space - avoid as much as possible complex arrangements - We tried to fit the ET xylophone configuration in a underground q infrastructure making realistic assumptions space required for working around the pipes (e.g. welding the modules) - avoid vertical arrangement of the ITF - include realistic tower footprint - WARNING: things might get even more complex (e.g. space required by - cryogenics) To further offload the tunnel we have moved the filter cavities into q shorter (1 km), dedicated tunnels this is a working hypothesis, to be discussed by the detector design teams - The resulting tunnel diameter is ~2x larger wrt ET book q Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 28

TUNNEL - ! in 10m Pisa Meeting, Elba, May 31 2018 G Losurdo - INFN Pisa 29