Gravitational waves from the first stars

Sandick, Pearl; Olive, Keith A.; Daigne, F.; Vangioni, Elisabeth

doi:10.1103/physrevd.73.104024

Cited by 59 publications

(85 citation statements)

References 46 publications

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“…These include unresolved compact binary coalescences of both black holes and neutron stars [1][2][3][4][5], rotating neutron stars [6][7][8], supernovae [9][10][11][12], cosmic strings [13][14][15][16], inflationary models [17][18][19][20][21][22][23][24], phase transitions [25][26][27], and the pre-Big Bang scenario [28][29][30][31]. The variety of mechanisms potentially contributing to the background provides the opportunity to study a number of different environments within the Universe.…”

mentioning

confidence: 99%

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

255

268

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A wide variety of astrophysical and cosmological sources are expected to contribute to a stochastic gravitational-wave background. Following the observations of GW150914 and GW151226, the rate and mass of coalescing binary black holes appear to be greater than many previous expectations. As a result, the stochastic background from unresolved compact binary coalescences is expected to be particularly loud. We perform a search for the isotropic stochastic gravitational-wave background using data from Advanced LIGO's first observing run. The data display no evidence of a stochastic gravitational-wave signal. We constrain the dimensionless energy density of gravitational waves to be Ω0 < 1.7 × 10 −7 with 95% confidence, assuming a flat energy density spectrum in the most sensitive part of the LIGO band (20 − 86 Hz). This is a factor of ∼33 times more sensitive than previous measurements. We also constrain arbitrary power-law spectra. Finally, we investigate the implications of this search for the background of binary black holes using an astrophysical model for the background. The recent detections of binary black hole (BBH) coalescences by Advanced LIGO [32,33] suggest that the Universe may be rich with coalescing BBHs. While events like GW150914 and GW151226 are loud enough to be clearly detected, we expect there to be many more events that are too far away to be individually resolved and that contribute to the background. Since this BBH population originates from sources that are too distant to be individually detected, the stochastic search probes a distinct population of binaries compared to nearby sources [34]. The background from these binaries provides complementary information to individually resolved binary coalescences [35].In this Letter, we report on the search for an isotropic background using data from Advanced LIGO's first observing run O1. We search for the background by crosscorrelating data streams from the two separate LIGO detectors and looking for a coherent signal. We find no evidence for the background and place the best upper limits to date on the energy density of the background in the LIGO frequency band. We also update the impli-

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mentioning

confidence: 99%

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

255

268

View full text Add to dashboard Cite

show abstract

“…Stochastic backgrounds can be created from the superposition of astrophysical sources such as binary coalescences [1], magnetars [2,3], rotating neutron stars [4][5][6][7][8], and the first stars [9]. Cosmological signals may arise during or following inflation [10,11], from cosmic strings [12][13][14][15][16][17], phase transitions [18], and from nonstandard cosmologies [19,20].…”

Section: Introductionmentioning

confidence: 99%

Correlated noise in networks of gravitational-wave detectors: Subtraction and mitigation

et al. 2014

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One of the key science goals of advanced gravitational-wave detectors is to observe a stochastic gravitational-wave background. However, recent work demonstrates that correlated magnetic fields from Schumann resonances can produce correlated strain noise over global distances, potentially limiting the sensitivity of stochastic background searches with advanced detectors. In this paper, we estimate the correlated noise budget for the worldwide advanced detector network and conclude that correlated noise may affect upcoming measurements. We investigate the possibility of a Wiener filtering scheme to subtract correlated noise from Advanced LIGO searches, and estimate the required specifications. We also consider the possibility that residual correlated noise remains following subtraction, and we devise an optimal strategy for measuring astronomical parameters in the presence of correlated noise. Using this new formalism, we estimate the loss of sensitivity for a broadband, isotropic stochastic background search using 1 yr of LIGO data at design sensitivity. Given our current noise budget, the uncertainty with which LIGO can estimate energy density will likely increase by a factor of ≈12-if it is impossible to achieve significant subtraction. Additionally, narrow band cross-correlation searches may be severely affected at low frequencies f ≲ 70 Hz without effective subtraction.

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“…Cosmological models include inflationary models [1][2][3][4], models based on cosmic (super)strings [5][6][7][8][9][10], and models of alternative cosmologies [11,12]. Astrophysical models (see [13] for a review) integrate contributions from astrophysical objects across the universe including compact binary coalescences (CBC) of binary neutron stars (BNS) or binary black holes (BBH) [14][15][16][17][18][19][20][21][22][23][24], rotating neutron stars (NSs) [25][26][27][28][29][30][31][32][33][34], magnetars [34][35][36][37][38][39][40], the first stars [41], and white dwarf binaries [42].…”

Section: Introductionmentioning

confidence: 99%

Model of the stochastic gravitational-wave background due to core collapse to black holes

et al. 2015

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Superposition of gravitational waves generated by astrophysical sources is expected to give rise to the stochastic gravitational-wave background. We focus on the background generated by the ring-down of black holes produced in the stellar core collapse events across the universe. We systematically study the parameter space in this model, including the most recent information about the star formation rate and about the population of black holes as a function of redshift and of metallicity. We investigate the accessibility of this gravitational wave background to the upcoming gravitational-wave detectors, such as Advanced LIGO and Einstein Telescope.PACS numbers: 95.85. Sz, 97.60.Jd, 04.25.dg, 98.80.Cq

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Gravitational waves from the first stars

Cited by 59 publications

References 46 publications

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Correlated noise in networks of gravitational-wave detectors: Subtraction and mitigation

Model of the stochastic gravitational-wave background due to core collapse to black holes

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