Antoine Petiteau AstroGR@Mallorca - 5th September ... - lisa-light wiki

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Antoine Petiteau AstroGR@Mallorca - 5th September ... - lisa-light wiki

Performance of the new spacebased gravitational wavedetector ("New LISA" / ELISA)Antoine Petiteau(APC-Paris & AEI-Potsdam)on a behalf of the science performance task forceAstroGR@Mallorca - 5th September 2011


Overview1. New context of space based gravitational wave detection.2. Configurations of the instrument : orbits, noises, sensitivity.3. Review of scientific results (current status) :3.1. Galactic binaries : confusion noise, resolvable source3.2. Verification binaries : SNR/detection, parameters estimation3.3. Supermassive Black Hole binaries :3.3.1. Detection,3.3.2. Parameters estimation,3.4. EMRIs.4. Conclusion2Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


New context of space basedgravitational wave detection3Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Official statement for thescientific communityDue to the recent adjustment in how L-class missions within the Cosmic Vision framework are chosen, ESAis currently investigating a design for a European-led variant of LISA that can be launched before 2022.After studying several configurations, a new baseline has been identified that will be refined in the comingmonth with the help of European industry. The new baseline simplifies the design of LISA, reducing thedistance between the satellites and employing only four instead of previously six laser links.The science team and a science task force, composed of members of the gravitational wave andastrophysics communities in both Europe and the US, have assessed the scientific validity of the newbaseline for the fields of physics, astrophysics and cosmology and have shown that the new configurationis very promising regarding sources such as galactic binaries, (super)massive black hole and extrememass ratio inspirals.Over the next few months, this work will continue until we have a finalised mission proposal by the fall of2011. The near future is very bright for astrophysics and cosmology using observations of gravitationalwaves in space.4Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


History of the last monthsApril : Adjustment of L-class missions within the Cosmic Vision : ESA start to investigate adesign for a European-led variant of LISA that can be launched before 2022.Creation of Science Team (ST) and Science Performance Task Force (SPTF)SPTF studied several options for the new detector to estimate which science can be done.ESA orders two technical studied to evaluate the viability of the options :Concurrent Design Facilities (CDF, ESA team) : no stopper, mission seems possible and fit inbudget ➡ new baseline.Astrium is doing a complementary study.ST and SPTF are currently working on/for the Yellow Book : proposal to ESA for selectionaround February 2012.5Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Science Performance Task ForcePau Amaro-Seoane (AEI)Sofiane Aoudia (AEI)Gerard Auger (APC)Stas Babak (AEI)Jon Gair (Cambridge)Oliver Jennrich (ESA)Philippe Jetzer (ETH)Ioannis Kamaretsos (Cardiff)Antoine Klein (ETH)Gijs Nelemans (Nijmengen)Frank Ohme (AEI)Antoine Petiteau (AEI) - coordinatorEric Plagnol (APC)Ed Porter (APC) - coordinatorEmma Robinson (AEI)B. S. Sathyaprakash (Cardiff)Bernard Schutz (AEI)Alberto Sesana (AEI)Carlos Sopuerta (IEEC)Alberto Vecchio (Birmingham)US contribution :Emanuele Berti (Mississippi)Neil Cornish (Montana)Ryan Lang (Goddard)Tyson Littenberg (Goddard)Sean McWilliams (Columbia)Ira Thorpe (Goddard)Michele Vallisneri (JPL)Marta Volonteri (Michigan)6Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Sensitivity : CDFLaunch with 2 Soyuz : 1 mother + 2 daughters : 4 links (2 arms)LISA baseline for the payload :telescope diameter = 40 cm ,laser power = 2 W.Change the armlength : 50 kg / million kmMore details and pictures (!)in the talk of Oliver Jennrichon TuesdayCurrent main configuration : 1 GmConfiguration with good potentiality : 2 GmNot completely excluded : 3 Gm and maybe 6 links .7Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Instrument :orbits, noises & sensitivity8Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


OrbitsLISA like orbits (from O. Jennrich) :10 degrees behind the Earth with 1 Gm,analytic with 1, 2 & 3 Gm,Closest to the Earth,From 8 to 22 degrees (after 5 years)Halo L1 orbits (V. Mueller) :SC1 small orbits around L1SC2 and SC3 on larger orbits shifted by 180 degLISA likeL19Earth+ MoonHalo L1Halo L1Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Acceleration noise :DRS : LISA requirements :LPF : LISAPathfinder requirements :Shot noise :δx SN =δx LPFacc7.7 × 10−120.65Noisesδx DRSacc= 1WP= 3 × 10−150.653.5 × 10−150.65 1/2 1+m/s 2 / √ Hz0.18 mHzfm/s 2 / √ Hz 2L 0.4 m5 × 10 9 m/ √ Hzm DLaser power:•2 W : LISA,•0.05 W : LISAPathfinder,•0.7 W : Highest power of laserin space until now.Other measurement noise (fixed noise):Armlength:(from orbits)δx OMS =Telescope :•0.4 m : LISA,•0.25 m : «new baseline»•0.28 m : optimized 2Gm6.2 × 10−120.65m/ √ Hz10Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Selected configurationsC2 - standard 1 Gm C5 - optimized ...Orbits 1 Gm - Numeric 10 o behind Earth Analytic - 2 GmLaser power 2 W 2 WTelescope 0.4 m 0.28 mInertial system DRS (LISA standard) DRS (LISA standard)SSN (δν/ν unit) 0.12 x 10 -38 f 2 2.05 x 10 -38 f 2SOMS (δν/ν unit) 2.81 x 10 -38 f 2Sacc (δν/ν unit) 6 x 10 -48 f -211Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SensitivityNoise response (δν/ν unit)Approximative sensitivity for 4 links(analytic)1e-141e-15PSD (Hz^{-1}) in relative frequency1e-341e-351e-361e-371e-381e-391e-401e-411e-421e-431e-44LISA standardC5 (Cdf2) : P=2.0W, D=0.28m, Orbits=LISA like 2.0Gm Ssn=4.66e-23 Soms=6.40e-23C2 (Cdf1) : P=2.0W, D=0.40m, Orbits=LISA like 1.0Gm Ssn=2.81e-24 Soms=6.40e-231e-451e-05 0.0001 0.001 0.01 0.1 1Approximative sensitivity for 4 linksTDI noise response in relative frequency unitLISA standardC2 (Cdf1) : P=2.0W, D=0.40m, Orbits=LISA like 1.0Gm Ssn=2.81e-24 Soms=6.40e-23C5 (Cdf2) : P=2.0W, D=0.28m, Orbits=LISA like 2.0Gm Ssn=4.66e-23 Soms=6.40e-23f (Hz)D = 0.4P = 2 W1 Gm C2D = 0.28P = 2 W2 Gm C5h (SNR=1, instantaneous)1e-161e-171e-181e-191e-20121e-211e-05 0.0001 0.001 0.01 0.1 1Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011f (Hz)


Noises contributionC2 : L = 1 Gm , D = 40 cmC5 : L = 2 Gm , D = 28 cm13Using simulation (LISACode/SyntheticLISA), checking of sensitivity, laser noisereduction by TDI 2 nd generation, ...Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Galactic binaries14Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Confusion noisePopulation of galactic binaries from G. Nelemans,D = 0.4P = 2 W1 Gm C2D = 0.28P = 2 W2 Gm C52 codes for estimating confusion noise iteratively :1- T. Littenberg & N. Cornish (Goddard,Montana) 2- M. Vallisneri (JPL)Almost negligible contribution for configuration with 1 Gm but for 2 Gm15Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Resolvable sources : detectionTypical number of resolvable source with standard LISA is about 17 000 :ΔΩ < 1 deg 2 : can be resolved on skyΔdf/dt < 20% : constrain on the luminosity distance3D postition : directly probe the 3D spatial distribution of the GalaxyJust source with Δdf 2 /dt 2 < 20% : characterize interaction between the two objects.C2 - 4 linksbaselineC5 - 4 linksoption 2GmC2 - 6 linksoption 6 linksC5 - 6 linksoption++SNR > 7 4586 6827 6204 11278ΔΩ < 1 deg 2 1107 1821 1892 3150Δdf/dt < 20% 1331 1814 1678 22843D position 370 628 457 81416Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Resolvable sources : parametersConfiguration C3 :(1Gm-)0.1 < σsky < 10 deg(LISA : [0.05, 5] deg)3 < σincl. < 100 deg(LISA : similar)10 %< σAmp< 100 %5 degResults are less good but still similar to LISA (continuous observation)17Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Verification binaries18Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Verification binaries - detectionDetection : source with SNR > 7Randomise over unknown parameters : inclination, ...Number of sourcesdetected :1000SNR = 7C2 - 4 linksC2 - 6 linksC5 - 4 linksC5 - 6 linksC2 C54 links 5 - 6 7 - 86 links 7 8SNR10010Results for C5(2 Gm) - 4links are similar to the onefor C2 (1Gm) - 6 links1V803 Cen CR Boo HP Lib AM CVn SDSS J0651 ES Cet V407 Vul RX J080619Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Verification binariesIdentification by sky positionIdentification of source using frequency and sky position :Number of sourcesidentified : alldetected sources1000100C2 - 4 linksC2 - 6 linksC5 - 4 linksC5 - 6 linksC2 C54 links 6 76 links 7 8 deg 21010.1V803 Cen CR Boo HP Lib AM CVn SDSS J0651 ES Cet V407 Vul RX J080620Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Verif. binaries - parameter estimationAmplitude & time derivative of frequency➡ information on distance, mass transfer1e-15C2 - 4 linksC2 - 6 linksC5 - 4 linksC5 - 6 linksInclination ➡ orientationAdditional informations to theelectromagnetic observation to understandthe system, ...df/dt Hz/s1e-161e-17V803 Cen CR Boo HP Lib AM CVnSDSS J0651 ES Cet V407 Vul RX J080610C2 - 4 linksC2 - 6 linksC5 - 4 linksC5 - 6 links1e-15C2 - 4 linksC2 - 6 linksC5 - 4 linksC5 - 6 links1A/Adf/dt Hz/s1e-160.1Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 20110.011e-1721V803 Cen CR Boo HP Lib AM CVn SDSS J0651 ES Cet V407 Vul RX J0806V803 Cen CR Boo HP Lib AM CVnSDSS J0651 ES Cet V407 Vul RX J0806


Supermassive Black Hole binaries22Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : waveformsee talk of Sean McWilliamsWe do not have a complete waveform at the moment ... but we have pieces :Inspiral / Full Higher harmonics spins eccentricity- Klein inspiral only yes yes yes- Lang / Cornish full yes precessing no- Petiteau / Babak / Aoudia inspiral only yes precessing no- McWilliams full yes aligned no- Babak & al. (PhenomC) full no aligned no- Kamarestos / Sathyaprakash ringdown yes ? no- Porter inspiral only yes no no- NR/GW group at AEI(restriction on parameters)full yes yes no23Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : horizonUsing phenomC, compute until which redshifta "standard" source with SNR = 10 can bedetected.Contours need to be superposed to theastrophysical expected distribution.24Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : populationWe compute parameter estimation using catalogues based on ...2 models for seed black holes :large seed (catalogues LE, LEm & LC),small seed (catalogues SE, SEm & SC).see talk of Alberto Sesana3 kinds for accretion model :coherent 1 spins perfectly aligned with high amplitude (catalogues LE & SE),coherent 2 spins slightly misaligned (0-10deg) with high amplitude (cataloguesLEm & SEm),chaotic spins direction random ; small amplitude (catalogues LC & SC)25Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : DetectionMean number of sources with C2 on an average catalogue (with PhenomCwaveform):34 in total12 at z6) for each catalogues and eachconfiguration using inspiral waveform : preliminary results of AEI - R. Lang - ...C2 - 4links C5 - 4 links C4 - 6 links All eventsLEm: Large seed / efficient acc. 38 40 40 72LC: Large seed / chaotic acc. 33 36 - 29 36 67SEm: Small seed / efficient acc. 39 50 47 243SC: Small seed / chaotic acc. 44 55 - 47 54 22726Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : Detection (Large seed)Large seed - efficient accretionLarge seed - chaotic accretion27Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : Detection (Small seed)Small seed - efficient accretionSmall seed - chaotic accretion28Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : distanceNumber of sources with estimation of distance (relative error < 50 %).Efficient accretionChaotic accretionSmall seedLarge seed29Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : sky positionNumber of sources with estimation of sky position (ΔΩ < 100 deg 2 )Efficient accretionChaotic accretionSmall seedLarge seed30Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : spin amplitudeNumber of sources with at least one measurable spin amp (error < 0.2).Efficient accretionChaotic accretionSmall seedLarge seed31Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : parameter estimationMasses : very good estimationsee talk of Sean McWilliamsRelative error on total mass < 0.1 - 1 % , error on mass ratio < 10 -2Relative error on individual masses < 1 - 10 %Spin direction : very hard to estimateBut some combinations can probably be constrained. Ex : L.SI which helps forunderstanding relative orientation between total angular momentum L and spins.Eccentricity : Can be estimated.Distribution for baseline (C2) on largeseed - chaotic accretion catalogue (LC)32Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb sciencePossible identification of electromagnetic counterpart (Sky < 10 deg 2 ) :C2 - 4 links : 2 - 5 events (z < 5 - 8) ,C5 - 4 links : 6 - 14 events (z < 5 - 9),C2 - 6 links : 13 - 15 events (z < 11 - 13).Estimation of luminosity distance :C2 - 4 links : 16 - 22 events (z < 8 - 12) ,C5 - 4 links : 25 - 33 events (z < 10 - 12),C2 - 6 links : 31 - 45 events (z < 11 - 15).Cosmology : seems hard due to the big size of the 3D box.Model selection ......33Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : Using more completewaveform and PE methodsMost part of the previous results are based on waveforms which do notinclude the full complexity and use Fisher Matrix approach (fast).But Fisher Matrix approach is not really valid when the errors are large andSNR small : need to use MCMC methods, ... see talk of Sean McWilliamsNew results show theprecision improves whenusing more completewaveforms.fullinspiral onlyC2 - LC34Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Model selectionsee talk of Alberto SesanaIt's still possible to differentiate between the models : due to the goodestimation of masses but should be better with a better resolution on distance.Ability for separating 2 models (ROC)Mixing models :recovery of mixing factorC2C235Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


EMRIssee talk of Jon GairUncertainties on population,Typically few tens with C2 (1 Gm) and around hundred with C5 (2 Gm) : tobe confirmed.Horizon distance (preliminary results) :detection until z < 0.3 (at MBH = 2x10 5 ) with C2,detection until z < 0.4 (at MBH = 2x10 5 ) with C5.Parameter estimation : if an EMRI can be detected, the parameterestimation is already good.36Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


ConclusionThe "new LISA" mission or "ELISA" mission will still do very nice science.A lot of tools have been set and studies done by the members of SPTF.Galactic binaries : few thousands of sources can still be detected with goodparameter estimation.Verification binaries : 5 to 8 sources detected.SMBHb : detection of few tens until z = 10EMRIs : seems possible ...Work in progress on science performance and technological studies.The near future is very bright for astrophysics and cosmology usingobservations of gravitational waves in space.37Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SensitivityChecking of sensitivity for configuration with numerical orbit ( from Oliver)has been done with LISACode.Checking of analytic formulation vs. simulationChecking of reduction of laser noise well below the other noises has beendone with LISACode & SynteticLISA.Note : the design of the optical bench used isthe old one (2004) ; the last design of LISAmeasurements system (including opticalbench and clock) has not been yet studied.39Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Analytic fitWe have analytic fit for eachconfiguration (except Halo L1)which have been checked againstthe simulation.40Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Selected configurationsC2 - std 1 Gm C5 - optimized C3 «new baseline» C4 - std 3 Gm ...Orbits Num. 10 o - 1 Gm Analytic - 2 Gm Num. 10 o - 1 Gm Analytic - 3 GmLaser power 2 W 2 W 0.7 W 0.7 WTelescope 0.4 m 0.28 m 0.25 m 0.25 mInertial system DRS DRS DRS DRSSSN (δν/ν unit) 0.06 x 10 -40 f 2 (1) 2.05 x 10 -38 f 2 2.31 x 10 -38 f 2 20.07 x 10 -38 f 2SOMS (δν/ν unit) 2.81 x 10 -38 f 2Sacc (δν/ν unit) 6 x 10 -48 f -2(1) : Mistake in the way of taking laser power into account41Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SensitivitySimulation by LISACode :Average of 60 sentivities generated on 12 days each one.P = 2 WD = 0.4P = 2 WD = 0.28 mP = 0.7 WD = 0.25 m1 Gm C2 C32 Gm C53 Gm C442Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SensitivitySimulation by LISACode :Average of 60 sentivities generated on 12 days each one.P = 2 WD = 0.4P = 2 WD = 0.28 mP = 0.7 WD = 0.25 m1 Gm C2 C32 Gm C53 Gm C442Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SensitivitySimulation by LISACode :Average of 60 sentivities generated on 12 days each one.P = 2 WD = 0.4P = 2 WD = 0.28 mP = 0.7 WD = 0.25 m1 Gm C2 C32 Gm C53 Gm C442Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SensitivitySimulation by LISACode :Average of 60 sentivities generated on 12 days each one.P = 2 WD = 0.4P = 2 WD = 0.28 mP = 0.7 WD = 0.25 m1 Gm C2 C32 Gm C53 Gm C442Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Sensitivity :Studied configurationsP = 2 WD = 0.4P = 2 WD = 0.28 m1 Gm C22 Gm C543Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Sensitivity : CDFP = 2 WD = 0.4P = 2 WD = 0.28 mP = 0.7 WD = 0.25 m1 Gm C2 C32 Gm C53 Gm C4Cdf vs. our config. :Cdf1 : C2 , C3 close-worstCdf2 : C5 close-worstCdf3 : C4 very-worstOur current results alreadygive a good approximation ofcurrent Cdf configurations44Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Check laser noise cancellationQuick checking of laser noise cancelation by TDI 2nd generation(SynthetyicLISA confirmed by LISACode)Configuration C1Configuration C245Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


Verification binariesDetection :Source with SNR > 7 :(Randomize over unknown parameters : inclination, ...)C2 C54 links 5 - 6 7 - 86 links 7 8C2 (1 Gm)4/6 linksC5 (2 Gm)4/6 links1000SNR = 7C2 - 4 linksC2 - 6 linksC5 - 4 linksC5 - 6 linksRX J0806.3+1527 48 / 67 79 / 111100V407_Vul - 17 / 24ES Cet 12 / 17 19 / 27SNRAM CVn 11 / 15 16 / 2310HP Lib 15 / 21 21 / 31SDSS J0651 11 / 17 19 / 27461V803 Cen CR Boo HP Lib AM CVn SDSS J0651 ES Cet V407 VulPerformance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th RX J0806Spetembery 2011


Parameters estimationSimilar precision as for resolvable binariesNumber of VB with sky error < 10 deg 2 :Raw estimate (for one realization) :LISA C2 C54 links 4 2 46 links 5 4 4Sky (deg 2 )4 / 6 linksinclination (radians)4 / 6 linksdf/dt (x10 -16 )4 / 6 linksC2 C5 C2 C5 C2 C5RX J0806.3+1527 0.07 / 0.03 0.03 / 0.01 14 / 9 8.9 / 5.7 0.05/0.03 0.02 / 0.02V407_Vul 15 / 7 5 / 2 62 / 44 37 / 27 0.23/ 0.17 0.15 / 0.11ES Cet 15 / 3.6 6 / 1.4 123 / 36 72 / 22 0.23/ 0.17 0.15 / 0.10AM CVn 89 / 23 43 / 11 158 / 25 109 / 17 0.21/0.15 0.14 / 0.10HP Lib 22 / 7 10 / 3 110 / 60 73 / 40 0.21/ 0.14 0.13 / 0.0947Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : SNRC2 = Cdf1 withPhenomC(Full / Nohigher harm. /spin aligned)48Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : Detection (Large seed)Large seed - efficient accretionLarge seed - chaotic accretion49Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : Detection (Small seed)Large seed - efficient accretionLarge seed - chaotic accretion50Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : distanceNumber of sources with measurable distance (relative error < 50 %).Efficient accretionChaotic accretionSmall seedLarge seed51Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : sky positionNumber of sources with measurable sky position (ΔΩ < 100 deg 2 )Efficient accretionChaotic accretionSmall seedLarge seed52Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : spin amplitudeNumber of sources with at least one measurable spin amp (error < 0.2).Efficient accretionChaotic accretionSmall seedLarge seed53Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : MassesEfficient accretionChaotic accretionSmall seed4 links - Full/No HH/Align spinInspiral/HH/spin rand. oriented54Large seed4 links - Full/No HH/Align spinPerformance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011Inspiral/HH/spin rand. oriented


SMBHb : Spin amplitudeEfficient accretionChaotic accretionSmall seed4 links - Full/No HH/Align spinInspiral/HH/spin rand. oriented55Large seed4 links - Full/No HH/Align spinPerformance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011Inspiral/HH/spin rand. oriented


SMBHb : Sky positionEfficient accretionChaotic accretionSmall seed10°x10°4 links - Full/No HH/Align spinInspiral/HH/spin rand. orientedLarge seed5610°x10°4 links - Full/No HH/Align spinInspiral/HH/spin rand. orientedPerformance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011


SMBHb : DistanceEfficient accretionChaotic accretionSmall seed4 links - Full/No HH/Align spinInspiral/HH/spin rand. oriented57Large seed4 links - Full/No HH/Align spinPerformance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011Inspiral/HH/spin rand. oriented


SMBHb : sky position & distanceFisher Matrixmethod limitation.Need other methodslike MCMC.Small seedLarge seed58Performance of the new space based GW detector - A. Petiteau on behalf of science performance task force - AstroGR@Mallorca - 5 th Spetembery 2011

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