Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements

Dietz, A.

doi:10.1051/0004-6361/201016166

Cited by 35 publications

(39 citation statements)

References 65 publications

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“…The observed rate of shGRBs suggests that their rate could be once per year within z ∼ 0.5 [13]. The reach of the network can be significantly larger for a search that is focussed around an event like a GRB, than it is for a "blind" search in the entire data set.…”

Section: Advanced Gravitational Wave Detectorsmentioning

confidence: 93%

Scientific objectives of Einstein Telescope

Sathyaprakash¹,

Abernathy²,

Acernese³

et al. 2012

Class. Quantum Grav.

465

413

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Abstract. The advanced interferometer network will herald a new era in observational astronomy. There is a very strong science case to go beyond the advanced detector network and build detectors that operate in a frequency range from 1 Hz-10 kHz, with sensitivity a factor ten better in amplitude. Such detectors will be able to probe a range of topics in nuclear physics, astronomy, cosmology and fundamental physics, providing insights into many unsolved problems in these areas.PACS numbers: 95.36.+x, 97.60.Lf, 98.62.Py, 04.80.Nn, 95.55.Ym, 97.60.Bw, 97.60.Jd

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Section: Advanced Gravitational Wave Detectorsmentioning

confidence: 93%

Scientific objectives of Einstein Telescope

Sathyaprakash¹,

Abernathy²,

Acernese³

et al. 2012

Class. Quantum Grav.

465

413

View full text Add to dashboard Cite

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“…This approach is complementary to attempts to explore the DTD by comparing the rate of short GRBs (believed to be associated with BNS mergers) and the SFR (see e.g. Guetta & Piran 2005Guetta & Stella 2009;Leibler & Berger 2010;Dietz 2011;Coward et al 2012;Wanderman & Piran 2015). An independent single observation arises from GW170817.…”

Section: Introductionmentioning

confidence: 99%

The Gravitational waves merger time distribution of binary neutron star systems

Beniamini

Piran

2019

Monthly Notices of the Royal Astronomical Society

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Binary neutron stars (BNS) mergers are prime sites for r-process nucleosynthesis. Their rate determines the chemical evolution of heavy elements in the Milky Way. The merger rate of BNS is a convolution of their birth rate and the gravitational radiation spiral-in delay time.Using the observed population of Galactic BNS we show here that the lifetimes of pulsars in observed BNSs are sufficiently short that the ages of BNSs have little to no effect on the observed merger time distribution. We find that at late times (t ∼ > 1 Gyr) the gravitational wave delay time distribution (DTD) follows the expected t −1 . However, a significant excess of rapidly merging systems (between 40 − 60% of the entire population) is apparent at shorter times. Although the exact shape of the DTD cannot be determined with the existing data, in all models that adequately describe the data we find at least 40% of BNSs with merger times less than 1Gyr. This population of rapid mergers implies a declining deposition rate of r-process materials that is consistent with several independent observations of heavy element abundances in the Milky Way. At the same time this population that requires initial binary separations of roughly one solar radius clearly indicates that these binaries had common envelope progenitors. Our results suggest that a significant fraction of future LIGO/Virgo BNS mergers would reside in star forming galaxies.

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“…Guetta & Piran () find an SGRB rate density of

8 - 30 {Gpc}^{- 3} {yr}^{- 1}

, assuming isotropic emission. Another study (Dietz ) calculates a higher NS‐NS merger rate of about 7800 Gpc −3 yr −1 , but assuming the emissions are beamed with small opening angles.…”

Section: Introductionmentioning

confidence: 99%

The Swift short gamma-ray burst rate density: implications for binary neutron star merger rates

Coward

Howell

Piran

et al. 2012

Monthly Notices of the Royal Astronomical Society

132

143

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Short gamma-ray bursts (SGRBs) observed by Swift potentially reveal the first insight into cataclysmic compact object mergers. To ultimately acquire a fundamental understanding of these events requires pan-spectral observations and knowledge of their spatial distribution to differentiate between proposed progenitor populations. Up to 2012 April, there are only some 30 per cent of SGRBs with reasonably firm redshifts, and this sample is highly biased by the limited sensitivity of Swift to detect SGRBs. We account for the dominant biases to calculate a realistic SGRB rate density out to z ≈ 0.5 using the Swift sample of peak fluxes, redshifts and those SGRBs with a beaming angle constraint from X-ray/optical observations. We find an SGRB lower rate density of 8-3+5 Gpc -3 yr -1 (assuming isotropic emission) and a beaming corrected upper limit of 1100-470+700 Gpc -3 yr -1. Assuming a significant fraction of binary neutron star mergers produce SGRBs, we calculate lower and upper detection rate limits of (1-180) yr-1 by an Advanced LIGO (aLIGO) and Virgo coincidence search. Our detection rate is similar to the lower and realistic rates inferred from extrapolations using Galactic pulsar observations and population synthesis

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Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements

Cited by 35 publications

References 65 publications

Scientific objectives of Einstein Telescope

Scientific objectives of Einstein Telescope

The Gravitational waves merger time distribution of binary neutron star systems

The Swift short gamma-ray burst rate density: implications for binary neutron star merger rates

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