Binary population synthesis with probabilistic remnant mass and kick prescriptions

Mandel, Ilya; Mueller, Bernhard; Riley, Jeff; de Mink, Selma E.; Vigna-Gomez, Alejandro; Chattopadhyay, Debatri

doi:10.48550/arxiv.2007.03890

Cited by 4 publications

(4 citation statements)

References 44 publications

(65 reference statements)

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“…Although the inferred component masses of GW190425's source are consistent with masses of known neutron stars [259][260][261][262], the total mass 3.4 +0.3 −0.1 M is greater than that of observed Galactic BNSs [263,264]. This raises the question of whether GW190425's source was formed in a different environment from the double neutron star systems observed to date [30,[265][266][267][268]. VII.…”

Section: Gw190425mentioning

confidence: 70%

GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run

Abbott,

Abraham

et al. 2020

Preprint

374

797

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UTC. By imposing a false-alarm-rate threshold of two per year in each of the four search pipelines that constitute our search, we present 39 candidate gravitational wave events. At this threshold, we expect a contamination fraction of less than 10%. Of these, 26 candidate events were reported previously in near real-time through GCN Notices and Circulars; 13 are reported here for the first time. The catalog contains events whose sources are black hole binary mergers up to a redshift of ∼ 0.8, as well as events which could plausibly originate from binary neutron stars, neutron star-black hole binaries, or binary black holes. For the latter group, we are unable to determine the nature based on estimates of the component masses and spins from gravitational wave data alone. The range of candidate events which are unambiguously identified as binary black holes (both objects ≥ 3 M ) is increased compared to GWTC-1, with total masses from ∼ 14M for GW190924 021846 to ∼ 150M for GW190521. For the first time, this catalog includes binary systems with asymmetric mass ratios, which had not been observed in data taken before April 2019. Given the increased sensitivity of Advanced LIGO and Advanced Virgo, the detection of 39 candidate events in ∼26 weeks of data (∼1.5 per week) is consistent with GWTC-1.

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Section: Gw190425mentioning

confidence: 70%

GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run

Abbott,

Abraham

et al. 2020

Preprint

374

797

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“…Moreover, close-binary interaction might in some cases lead to the stripping of a star's hydrogen and (most of its) helium envelope onto a companion NS, leaving behind a bare carbon-oxygen core (Nomoto et al 1994;Dewi et al 2002), undergoing subsequent iron-core collapse. The explosion of such ultrastripped SNe (Tauris et al 2013(Tauris et al , 2015Suwa et al 2015;Müller et al 2018) is discussed as the most likely evolutionary pathway leading to the formation of double NS systems (Tauris et al 2017;Mandel et al 2020).…”

Section: Additional Low-mass Componentmentioning

confidence: 99%

Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background

Kresse,

Ertl,

Janka

2020

Preprint

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The diffuse cosmic supernova neutrino background (DSNB) is observational target of the gadoliniumloaded Super-Kamiokande (SK) detector and the forthcoming JUNO and Hyper-Kamiokande detectors. Current predictions are hampered by our still incomplete understanding of the supernova (SN) explosion mechanism and of the neutron star (NS) equation of state and maximum mass. In our comprehensive study we revisit this problem on grounds of the landscapes of successful and failed SN explosions obtained by Sukhbold et al. and Ertl et al. with parametrized one-dimensional neutrino engines for large sets of single-star and helium-star progenitors, with the latter serving as proxy of binary evolution effects. Besides considering engines of different strengths, leading to different fractions of failed SNe with black-hole (BH) formation, we also vary the NS mass limit, the spectral shape of the neutrino emission, and include contributions from poorly understood alternative NS-formation channels such as accretion-induced or merger-induced collapse events. Since the neutrino signals of our large model sets are approximate, we calibrate the associated degrees of freedom by using state-of-the-art simulations of proto-neutron star cooling. Our predictions are higher than other recent ones because of a large fraction of failed SNe with long delay to BH formation. Our best-guess model predicts a DSNB νe -flux of 28.8 +24.6 −10.9 cm −2 s −1 with 6.0 +5.1 −2.1 cm −2 s −1 in the favorable measurement interval of [10,30] MeV, and 1.3 +1.1 −0.4 cm −2 s −1 with νe energies > 17.3 MeV, which is roughly a factor of two below the current SK limit. The uncertainty range is dominated by the still insufficiently constrained cosmic rate of stellar core-collapse events.

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“…Furthermore, GWTC-2 includes the first systems with confidently asymmetric component masses, including GW190412 with mass ratio m 2 /m 1 ≡ q = 0.28 +0.12 −0.06 (Abbott et al 2020b) and GW190814 (Abbott et al 2020c), with q = 0.112 +0.008 −0.009 . Furthermore, the secondary mass of GW190814, m 2 = 2.59 +0.08 −0.09 M , is near the purported neutron-star -black-hole gap (Bailyn et al 1998;Özel et al 2011;Farr et al 2011), posing a challenge to our understanding of binary formation (Abbott et al 2020c;Zevin et al 2020;Mandel et al 2020). We can gain insight into these exceptional events by studying them in the context of the larger population of compact binaries (Fishbach et al 2020b).…”

Section: Introductionmentioning

confidence: 99%

Population Properties of Compact Objects from the Second LIGO-Virgo Gravitational-Wave Transient Catalog

Abbott,

Abraham

et al. 2020

Preprint

103

240

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We report on the population properties of the 47 compact binary mergers detected with a false-alarm rate (FAR) < 1 yr −1 in GWTC-2, including all Advanced LIGO-Virgo observing runs through the most recent observing run O3a. We investigate the mass distribution, spin distribution, and merger rate as a function of redshift. We observe several binary black hole (BBH) population characteristics not discernible until now. First, we find that the primary mass spectrum contains structure beyond a power-law distribution with a sharp high-mass cut-off; it is more consistent with a broken power law with a break at 39.7 +20.3 −9.1 M , or a power law with a Gaussian feature peaking at 33.5 +4.5 −5.5 M (90% credible interval). While the primary mass distribution must extend to ∼ 65 M or beyond, only 2.9 +3.4 −1.7 % of systems have primary masses greater than 45 M . At low masses, we find that the primary mass spectrum has a global maximum at 7.8 +2.2 −2.1 M , consistent with a gap between ∼ 2.6 M and ∼ 6 M . Second, we find evidence that a nonzero fraction of BBH systems have component spins misaligned with the orbital angular momentum, giving rise to precession of the orbital plane. Moreover, we infer that 12% to 44% of BBH systems have spins tilted by more than 90 • with respect to their orbital angular momentum, giving rise to a negative effective inspiral spin parameter. Third, we provide improved estimates for merger rates using astrophysically motivated mass distributions: for BBH, R BBH = 23.9 +14.9 −8.6 Gpc −3 yr −1 and for binary neutron stars (BNS), R BNS = 320 +490 −240 Gpc −3 yr −1 . We constrain the BBH merger rate as a function of redshift and find that the rate likely increases with redshift (85% credibility), but not faster than the star-formation rate (87% credibility). Additionally, we examine recent exceptional events in the context of our population models, finding that the asymmetric masses of GW190412 and the high component masses of GW190521 are consistent with our population models, but the low secondary mass of GW190814 makes it an outlier. We discuss the implications of these results for compact binary formation and for the evolution of massive stars.

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Binary population synthesis with probabilistic remnant mass and kick prescriptions

Cited by 4 publications

References 44 publications

GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run

GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run

Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background

Population Properties of Compact Objects from the Second LIGO-Virgo Gravitational-Wave Transient Catalog

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