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Inspiraling Compact Objects: Detection Expectations

Inspiraling Compact Objects: Detection Expectations. Vicky Kalogera Physics & Astronomy Dept. In this talk :. Gravitational Waves and Double Neutron Stars Meet PSR J0737-3039: a new strongly relativistic binary pulsar Inspiral Event Rates for NS-NS, BH-NS, BH-BH

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Inspiraling Compact Objects: Detection Expectations

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  1. Inspiraling Compact Objects: Detection Expectations Vicky Kalogera Physics & Astronomy Dept

  2. In this talk : • Gravitational Waves and Double Neutron Stars • Meet PSR J0737-3039: a new strongly relativistic binary pulsar • Inspiral Event Rates for NS-NS, BH-NS, BH-BH • Precessing Binaries: astrophysical expectations

  3. Double Neutron Star Inspiral What kind of signal ? Dotheyexist?YES! First known NS -NS: radio pulsarPSR B1913+16 inspiral chirp orbital decay GW emission causes orbital shrinkage leading to higher GW frequency and amplitude PSR B1913+16 Weisberg & Taylor 03

  4. detection rate ~ r3 strength ~ 1/r Sensitivity to coalescing binaries Dmax for each signal sets limits on the possible detection rate What is the expected detection rate out to Dmax ? Scaling up from the Galactic rate

  5. Inspiral Rates for the Milky Way Empirical Estimates Based on radio Theoretical Estimates Based on models of binary evolution until binary compact objects form. for NS -NS, BH -NS, and BH -BH pulsar properties and survey selection effects. for NS -NS only

  6. J0737-3039 Burgay et al. 2003 M15 (NGC 7078) Properties of known coalescing DNS pulsars 2127+11C Galactic Disk pulsars B1913+16 B1534+12

  7. . Ps (ms) (ss-1) L400 Ps B1913+16 59.03 8.6x10-18 270 B1534+12 37.90 2.5x10-18 9 J0737-3039 22.70 2.4x10-18 28 M15 (NGC 7078) Properties of known coalescing DNS pulsars 2127+11C 30.5 5.0x10 -18 670 Galactic Disk pulsars Burgay et al. 2003

  8. . Ps (ms) (ss-1) L400 B9 (G) Ps B1913+16 59.03 8.6x10-18 270 22.8 B1534+12 37.90 2.4x10-18 9 9.7 J0737-3039 22.70 2.4x10-18 340 7.4 M15 (NGC 7078) Properties of known coalescing DNS pulsars 2127+11C 30.5 5.0x10 -18 670 12.5 Galactic Disk pulsars Burgay et al. 2003

  9. . Ps (ms) (ss-1) L400 B9 (G) d(kpc) Ps B1913+16 59.03 8.6x10-18 270 22.8 7.3 B1534+12 37.90 2.4x10-18 9 9.7 0.5 J0737-3039 22.70 2.4x10-18 28 7.4 0.6 M15 (NGC 7078) Properties of known coalescing DNS pulsars 2127+11C 30.5 5.0x10-18 67 12.5 10.6 Galactic Disk pulsars Burgay et al. 2003

  10. . Ps (ms) (ss-1) Porb (hr) Ps B1913+16 59.03 8.6x10-18 7.8 B1534+12 37.90 2.4x10-18 10.0 J0737-3039 22.70 2.4x10-18 2.4 Properties of known coalescing DNS pulsars Galactic Disk pulsars Burgay et al. 2003 M15 (NGC 7078) 2127+11C 30.5 5.0x10 -18 8.0

  11. . Ps (ms) (ss-1) Porb (hr) e Ps B1913+16 59.03 8.6x10-18 7.8 0.61 B1534+12 37.90 2.4x10-18 10.0 0.27 J0737-3039 22.70 2.4x10-18 2.5 0.09 Properties of known coalescing DNS pulsars Galactic Disk pulsars Burgay et al. 2003 M15 (NGC 7078) 2127+11C 30.5 5.0x10-18 8.0 0.68

  12. . Ps (ms) (ss-1) Porb (hr) e Mtot ( ) Ps B1913+16 59.03 8.6x10-18 7.8 0.61 2.8 (1.39) B1534+12 37.90 2.4x10-18 10.0 0.27 2.7 (1.35) J0737-3039 22.70 2.4x10-18 2.5 0.09 2.6 (1.24) Properties of known coalescing DNS pulsars Mo Galactic Disk pulsars Burgay et al. 2003 M15 (NGC 7078) 2127+11C 30.5 5.0x10-18 8.0 0.68 2.7 (1.36)

  13. ·  B1913+16 110 65 300 4º.23 B1534+12 250 190 2700 1º.75 J0737-3039 160 100 85 16º.9 M15 (NGC 7078) Properties of known coalescing DNS pulsars 2127+11C 96 60 220 4º.46 c(Myr)sd(Myr)mrg(Myr)(yr-1) Galactic Disk pulsars Burgay et al. 2003

  14. Dominant sources of rate estimate uncertainties identified: (VK, Narayan, Spergel, Taylor '01) X small - number observed sample (2 NS - NS in Galactic field) PSR population dominated by faint objects 3 Robust lower limit for the MW (10-6 per yr) Upward correction factor for faint PSRs: ~ 1 - 500 Radio Pulsars in NS-NS binaries NS-NS Merger Rate Estimates Use of observed sampleand models for PSR surveyselection effects: estimates oftotalNS- NSnumbercombined withlifetime estimates (Narayan et al. '91; Phinney '91)

  15. (VK, Narayan, Spergel, Taylor '01) NG Nest pulsar luminosity function: ~ L-2 i.e., dominated by faint, hard-to-detect pulsars median 25% small-N sample is: > assumed to be representative of the Galactic population > dominated by bright pulsars, detectable to large distances total pulsar number is underestimated

  16. Radio Pulsars in NS-NS binaries NS-NS Merger Rate Estimates (Kim, VK, Lorimer 2002) It is possible to assignstatistical significance to NS-NSrate estimates with Monte Carlo simulations Bayesian analysis developed to derive the probability densityof NS-NS inspiral rate Small number bias and selection effects for faint pulsars are implicitly included in our method.

  17. Statistical Method Identify sub-populations of PSRs with pulse and orbital properties similar to each of the observed DNS Model each sub-population in the Galaxy with Monte-Carlo generations Luminosity distribution Spatial distribution power-law: f(L)  L-p, Lmin < L(Lmin: cut-off luminosity) 2. Pulsar-survey simulation considerselection effectsof all pulsar surveys generate ``observed’’ samples

  18. Earth Statistical Method fill a model galaxy with Ntotpulsars count the number of pulsars observed (Nobs) 3. Derive rate estimate probability distribution P(R)

  19. Statistical Analysis For a given total number of pulsars, Nobs follows a Poisson distribution. We calculate the best-fit value of <Nobs> as a function of Ntot and the probability P(1; Ntot) We use Bayes’ theorem to calculate P(Ntot) and finally P(R) P(Nobs) for PSR B1913+16

  20. statistical confidence levels expected GW detection rates Results: most probable rate Rpeak P(Rtot)

  21. Current Rate Predictions Burgay et al. 2003, Nature, 426, 531 VK et al. 2004, ApJ Letters, in press 3 NS-NS : a factor of 6-7 rate increase Initial LIGO Adv. LIGO per 1000 yr per yr ref model: peak 75 400 95% 15 - 275 80 - 1500 opt model: peak 20 1000 95% 35 - 700 200 - 3700

  22. Results:Rpeak vs model parameters

  23. Current expectations forLIGO II(LIGO I) detection rates of inspiral events NS -NS BH -NS BH -BH Dmax 350 700 1500 (Mpc)(20) (40) (100) Rdet 5 - 37001.5 -1500 15 -10,000 (1/yr)(10-3 - 0.7) (3x10-4 -0.3) (4x10-3 -3) from population synthesis • Use empirical NS-NS rates: constrain pop syn models > BH inspiral rates

  24. What do/will learn from PSR J0737-3039 ? • Inspiral detection rates as high as 1 per 1.5 yr (at 95% C.L.) are possible for initial LIGO ! Detection rates in the range 20-1000 per yr are most probable for advanced LIGO VK, Kim, Lorimer, et al. 2004, ApJ Letters, in press • NS #2 progenitor is constrained as less massive than ~4.7 Msolar NS #2 kick is constrained to be in excess of 60 km/s and its most probable value is 150 km/s Willems & VK 2003, ApJ Letters, submitted • Better confirmation of GR • First double pulsar with eclipses ! Lyne et al. 2004, Science, in press constraints on magnetic field and spin orientation pulsar magnetospheres measurement of new relativistic effects ?

  25. Parkes MultiBeam survey and acceleration searches Assuming that acceleration searches can perfectly correct for any pulse Doppler smearing due to orbital motion… How many coalescing DNS pulsars would we expect the PMB survey to detect ? VK, Kim et al. 2003 < Nobs > = 3.6 N.B. Not every new coalescing DNS pulsar will significantly increase the DNS rates … PMB Nobs

  26. Challenges in the near future... Technical:achieve target noise level Data analysis:optimal methods for signal retrieval detection of inspiral signal requires: template waveforms and matched filtering techniques

  27. Precession and Inspiral Waveforms Compact object binaries can precessif spins are of significant magnitude and misalignedwith respect to the orbital angular momentum. Precession can modify inspiral waveforms and decrease thedetection efficiency of standard non-precession searches. Precession effects are more important for binaries of high mass ratios (BH-NS)and with spin tilt angles of the massive object in excess of ~30°. (Apostolatos 95)

  28. BH Asymmetric supernova explosions can tilt the orbital plane relative to the spin of the non-exploding star. BH NS Q: What is the origin of spin tilt angles in compact object binaries ? Mass transfer episodes in binaries tend to align spin and orbital angular momentum vectors. SN + NS kick

  29. Grandclement et al. 2003 BH-NS Q: What are the expected spin tilt angles ? > model BH-NS progenitors and SN kick effects VK 2000 10 Mo BH 1.4 Mo NS BH-NS binaries are expected to have significant spin tilt angles

  30. Grandclement, VK, Vecchio 2002 Grandclement & VK 2003 Grandclement, Ihm, VK, Belczynski 2003 Buonanno et al. 2003 Pan et al. 2003 Precessing inspiral binaries with non-precessing templates: detection rate decreases Rdet decrease depends on spin magnitude and tilt angle: templates that can mimic the precession effects can increase the detection rate: For a 10-1.4 Mo BH-NS binary Maximum BH spin cos(spin tilt angle) cos(spin tilt angle)

  31. Grandclement, Ihm, VK, Belczynski 2003 Rate drop expected from astrophysical predictions for spin tilts in BH-NS binaries rate drop by 20-30% Expected rates: BH-NS 1.5 -1500 per yr 3x10-4 -0.3 BH-BH 15 -10,000 per yr 4x10-3 -3 3 BH-NS BH-NS BH spin magnitude

  32. In the near and distant future ... Initial LIGO 3 NS-NS ---> detection possible BH-BH ---> possible detection too Advanced LIGO expected to detect compact object inspiral as well as NS or BH birth events, pulsars, stochastic background past experience from EM: there will be surprises! Laser Interferometry in space: LISA sources at lower frequencies supermassive black holes and background of wide binaries

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