J/ApJ/716/615Binary compact object coalescence rates (O'Shaughnessy+, 2010)

Binary compact object coalescence rates: the role of elliptical galaxies. O'Shaughnessy R., Kalogera V., Belczynski K. <Astrophys. J., 716, 615-633 (2010)> =2010ApJ...716..615OADC_Keywords: Pulsars ; Models, evolutionary ; Galaxies, nearbyKeywords: binaries: close - gravitational waves - pulsars: generalAbstract: In this paper, we estimate binary compact object merger detection rates for LIGO, including the potentially significant contribution from binaries that are produced in elliptical galaxies near the epoch of peak star formation. Specifically, we convolve hundreds of model realizations of elliptical- and spiral-galaxy population syntheses with a model for elliptical- and spiral-galaxy star formation history as a function of redshift. Our results favor local merger rate densities of 4x10^{-3}Mpc^{-3}/Myr for binary black holes (BHs), 3x10^{-2}Mpc^{-3}/Myr for binary neutron stars (NSs), and 10^{-2}Mpc^{-3}/Myr for BH-NS binaries. Assuming a detection signal-to-noise ratio threshold of 8 for a single detector (in practice as part of a network, to reduce its noise), corresponding to radii Dbns of the effective volume inside of which a single LIGO detector could observe the inspiral of two 1.4M_{☉}NSs of 14Mpc and 197Mpc, for initial and advanced LIGO, we find event rates of any merger type of 2.9x10^{-2}-0.46 and 25-400yr^{-1}(at 90% confidence level), respectively.Description: To summarize, by fully simulating the past history of the local universe, this paper develops models for the present-day detection rate of short-range (z≪1) and long-range (z not much less than 1) gravitational-wave detectors. Our results are rate distributions, where each distribution includes some normalization uncertainties (SFR and fraction of stars born in binaries), certain population synthesis model parameters, and our simulation Monte Carlo uncertainty.File Summary:

FileName Lrecl Records Explanations

ReadMe 80 . This file table1.dat 159 489 Parameters of all binary evolution simulations used in this paper, along with predicted merger rates R, detection rates R, and (for spiral simulations) posterior probabilities

See also: J/ApJ/713/671 : Gravitational waves from pulsars (Abbott+, 2010) J/ApJ/675/1459 : Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)Byte-by-byte Description of file: table1.dat

Bytes Format Units Label Explanations

1 A1 --- T [E/S] Galaxy type (E)lliptical or (S)piral 3- 6 F4.2 Sun Z Metallicity relative to the Sun 8- 12 F5.2 --- p Inital Mass Function slope 14- 17 F4.2 --- r Mass ratio distribution exponent (1) 19- 22 F4.2 --- w Wind strength 24- 29 F6.2 km/s v1 Maxwellian velocity dispersion 1 (2) 31- 36 F6.2 km/s v2 Maxwellian velocity dispersion 2 (2) 38- 41 F4.2 --- wt [0/1] Relative proportions of two o maxwellian distributions 43- 46 F4.2 --- alpha [0/1] α*λ, the common envelope efficiency 48 I1 --- beta [1] Specific angular momentum of matter lost (3) 50- 53 F4.2 --- fa Nonconservative mass transfer fraction accreted (4) 55- 62 I8 --- N Number of binaries simulated 64- 69 I6 --- N(bh-hb) Number of BH-BH binaries formed 71- 75 I5 --- N(bh-ns) ? Number of BH-NS binaries formed (5) 77- 82 I6 --- N(ns-ns) ? Number of NS-NS binaries formed (5) 84- 86 I3 --- m(bh-bh) Number of BH-BH binaries that merge within 13.7 Gyr 88- 92 I5 --- m(bh-ns) ? Number of BH-NS binaries that merge within 13.7 Gyr (5) 94- 98 I5 --- m(ns-ns) ? Number of NS-NS binaries that merge within 13.7 Gyr (5) 100-104 F5.2 [Myr-1/Mpc3] r(bh-bh) Log Rate density for BH-BH mergers (6) 106-110 F5.2 [Myr-1/Mpc3] r(bh-ns) ? Log Rate density for BH-NS mergers (7) 112-116 F5.2 [Myr-1/Mpc3] r(ns-ns) ? Log Rate density for BH-NS mergers (5,7) 118-122 F5.2 [Myr-1/Mpc3] r*(bh-bh) Log Rate density for BH-BH mergers (8) 124-128 F5.2 [Myr-1/Mpc3] r*(bh-ns) ? Log Rate density for BH-BH mergers (8) 130-134 F5.2 [Myr-1/Mpc3] r*(ns-ns) ? Log Rate density for BH-BH mergers (5,8) 136-140 F5.2 yr-1 R(bh-bh) LIGO detection rate for BH-BH mergers (9) 142-146 F5.2 yr-1 R(bh-ns) ? LIGO detection rate for BH-NS mergers (9) 148-152 F5.2 yr-1 R(ns-ns) ? LIGO detection rate for NS-NS mergers (9) 154-159 F6.4 --- Ppost ? Posterior probability factor (10)

Note (1): p(q)∼q^{(-r)}at large q.Note (2): for two-component velocity distribution.Note (3): Podsiadlowski et al (1992ApJ...391..246P).Note (4): see Belczynski et al (2002ApJ...572..407B) Eq. 9.Note (5): Black Hole (BH) / Neutron Star (NS) lergers. Blank entries are not provided or used in this work, per the discussion near Fig. 9 and in PSgrbs. These simulations have few merging binaries of one type or another.Note (6): At present, due to this model, assuming the star formation history associated with type type (E or S).Note (7): At present. Provided only for the 250+ models where the rates are drawn from an unbiased distribution, per the discussion near Fig. 9 and in PSgrbs.Note (8): At present, due to this model, assuming all star formation occurs according to this model.Note (9): Expected single-interferometer initial LIGO detection rate. The single-interferometer advanced LIGO detection rate incorporates the time-dependent merger history and cosmological reach of the detector. The ratio of initial to advanced detection rates is nearly constant for BH-NS and NS-NS binaries; only for BH-BH binaries are corrections significant.Note (10): Only provided for the 241 (out of 282) spiral galaxy models where BH-BH, BH-NS, and NS-NS merger rates are each drawn from an unbiased distribution, per the discussion near Fig. 9 and in PSgrbs.

History: From electronic version of the journal(End)Greg Schwarz [AAS], Emmanuelle Perret [CDS] 30-May-2012

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