Erratum: "The Cosmic Coalescence Rates for Double Neutron Star Binaries"([URL ADDRESS="/cgi-bin/resolve?2004ApJ...601L.179K" STATUS="OKAY"]ApJ, 601, L179 [2004][/URL])

Kalogera, V.; Kim, C.; Lorimer, D. R.; Burgay, M.; D’Amico, N.; Possenti, A.; Manchester, R. N.; Lyne, A. G.; Joshi, B. C.; McLaughlin, M. A.; Krämer, M.; Sarkissian, J. M.; Camilo, F.

doi:10.1086/425868

Cited by 131 publications

(156 citation statements)

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“…This rate is substantially higher than the predicted astrophysical rate of 8:3 10 ÿ5 y ÿ1 MWEG ÿ1 [27]. However, the rate limit obtained in this paper is comparable with the rate limit of 47 y ÿ1 MWEG ÿ1 obtained from the LIGO-only S2 search [7], which was performed on a complementary data set.…”

supporting

confidence: 63%

Joint LIGO and TAMA300 search for gravitational waves from inspiralling neutron star binaries

Abbott¹,

Abbott²,

Adhikari³

et al. 2006

Phys. Rev. D

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We search for coincident gravitational wave signals from inspiralling neutron star binaries using LIGO and TAMA300 data taken during early 2003. Using a simple trigger exchange method, we perform an intercollaboration coincidence search during times when TAMA300 and only one of the LIGO sites were operational. We find no evidence of any gravitational wave signals. We place an observational upper limit on the rate of binary neutron star coalescence with component masses between 1 and 3M[sun] of 49 per year per Milky Way equivalent galaxy at a 90% confidence level. The methods developed during this search will find application in future network inspiral analyses

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supporting

confidence: 63%

Joint LIGO and TAMA300 search for gravitational waves from inspiralling neutron star binaries

Abbott¹,

Abbott²,

Adhikari³

et al. 2006

Phys. Rev. D

Self Cite

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“…In this picture the age of the remnant can be estimated from the source extension to t/1 kyr < ∼ 0.2 (d/1 kpc) 2 assuming typical values of Galactic cosmic ray diffusion (Atoyan et al 2006), which may be different outside the Galactic plane. The rate of merger-induced bursts in the Galaxy is found to be about one event every (0.5−7) × 10 4 years (Kalogera et al 2004;Guetta & Piran 2006). For an anticipated age of > ∼ 10 4 years the remnant has to be at a distance of > ∼ 7 kpc.…”

Section: Hadronic Scenario: Snr and Grb Remnantmentioning

confidence: 98%

Discovery and follow-up studies of the extended, off-plane, VHE gamma-ray source HESS J1507-622

Acero¹,

Aharonian²,

Akhperjanian³

et al. 2010

A&A

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Context. The detection of gamma-rays in the very-high-energy (VHE) range (100 GeV−100 TeV) offers the possibility of studying the parent population of ultrarelativistic particles found in astrophysical sources, so it is useful for understanding the underlying astrophysical processes in nonthermal sources. Aims. The discovery of the VHE gamma-ray source HESS J1507-622 is reported and possibilities regarding its nature are investigated. Methods. The H.E.S.S. array of imaging atmospheric Cherenkov telescopes (IACTs) has a high sensitivity compared with previous instruments (∼1% of the Crab flux in 25 h observation time for a 5σ point-source detection) and has a large field of view (∼5 • in diameter). HESS J1507-622 was discovered within the ongoing H.E.S.S. survey of the inner Galaxy, and the source was also studied by means of dedicated multiwavelength observations. Results. A Galactic gamma-ray source, HESS J1507-622, located ∼3.5 • from the Galactic plane was detected with a statistical significance >9σ. Its energy spectrum is well fitted by a power law with spectral index Γ = 2.24 ± 0.16 stat ± 0.20 sys and a flux above 1 TeV of (1.5 ± 0.4 stat ± 0.3 sys ) × 10 −12 cm −2 s −1 . Possible interpretations (considering both hadronic and leptonic models) of the VHE gamma-ray emission are discussed in the absence of an obvious counterpart.

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“…From field NSNS binaries a galactic merger rate to one event per (0.5-7) × 10 4 years is found (Kalogera et al 2004). For merger induced bursts which are formed in globular clusters a local rate of 20-90 events per Gpc −3 yr −1 (Salvatera et al 2008) or ∼4 Gpc −3 yr −1 (Guetta & Stella 2009) has been estimated.…”

Section: Age Of the Remnant And Rate Of Short Grbsmentioning

confidence: 96%

Finding short GRB remnants in globular clusters: the VHE gamma-ray source in Terzan 5

Domainko

2011

A&A

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Context. Globular cluster are believed to boost the rate of compact binary mergers that may launch a certain type of cosmological gamma-ray burst (GRB). Therefore globular clusters appear to be potential sites to search for remnants of such GRBs. Aims. The very-high-energy (VHE) gamma-ray source HESS J1747-248 recently discovered in the direction of the Galactic globular cluster Terzan 5 is investigated for being a GRB remnant. Methods. Signatures created by the ultrarelativistic outflow, the subrelativistic ejecta and the ionizing radiation of a short GRB are estimated for an expected age of such a remnant of t 10 4 years. Results. The kinetic energy of a short GRB could roughly be adequate for powering the VHE source in a hadronic scenario. The age of the proposed remnant estimated from its extension possibly agrees with the occurrence of such events in the Galaxy. Subrelativistic merger ejecta could shock-heat the ambient medium. Conclusions. Further VHE observations can probe for the presence of a break towards lower energies expected for particle acceleration in ultrarelativistic shocks. Deep X-ray observations would have the potential to examine whether there is any thermal plasma heated by the subrelativistic ejecta. The identification of a GRB remnant in our own Galaxy may also help to explore the effect of such a highly energetic event on the Earth.

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Erratum: "The Cosmic Coalescence Rates for Double Neutron Star Binaries"([URL ADDRESS="/cgi-bin/resolve?2004ApJ...601L.179K" STATUS="OKAY"]ApJ, 601, L179 [2004][/URL])

Cited by 131 publications

References 0 publications

Joint LIGO and TAMA300 search for gravitational waves from inspiralling neutron star binaries

Joint LIGO and TAMA300 search for gravitational waves from inspiralling neutron star binaries

Discovery and follow-up studies of the extended, off-plane, VHE gamma-ray source HESS J1507-622

Finding short GRB remnants in globular clusters: the VHE gamma-ray source in Terzan 5

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