TY - JOUR
T1 - The Time Delay Distribution and Formation Metallicity of LIGO-Virgo's Binary Black Holes
AU - Fishbach, Maya
AU - Kalogera, Vicky
N1 - Publisher Copyright:
© 2021. The American Astronomical Society. All rights reserved.
PY - 2021/6/20
Y1 - 2021/6/20
N2 - We derive the first constraints on the time delay distribution of binary black hole (BBH) mergers using the LIGO-Virgo Gravitational-Wave Transient Catalog. Assuming that the progenitor formation rate follows the star formation rate (SFR), the data favor that 43%-100% of mergers have delay times <4.5 Gyr (90% credibility). Adopting a model for the metallicity evolution, we derive joint constraints for the metallicity-dependence of the BBH formation efficiency and the distribution of time delays between formation and merger. Short time delays are favored regardless of the assumed metallicity dependence, although the preference for short delays weakens as we consider stricter low-metallicity thresholds for BBH formation. For a p(τ) ∝ τ -1 time delay distribution and a progenitor formation rate that follows the SFR without metallicity dependence, we find that τ min < 2.2 Gyr, whereas considering only the low-metallicity Z < 0.3 Z o˙ SFR, τ min < 3.0 Gyr (90% credibility). Alternatively, if we assume long time delays, the progenitor formation rate must peak at higher redshifts than the SFR. For example, for a p(τ) ∝ τ -1 time delay distribution with τ min = 4 Gyr, the inferred progenitor rate peaks at z > 3.9 (90% credibility). Finally, we explore whether the inferred formation rate and time delay distribution vary with BBH mass.
AB - We derive the first constraints on the time delay distribution of binary black hole (BBH) mergers using the LIGO-Virgo Gravitational-Wave Transient Catalog. Assuming that the progenitor formation rate follows the star formation rate (SFR), the data favor that 43%-100% of mergers have delay times <4.5 Gyr (90% credibility). Adopting a model for the metallicity evolution, we derive joint constraints for the metallicity-dependence of the BBH formation efficiency and the distribution of time delays between formation and merger. Short time delays are favored regardless of the assumed metallicity dependence, although the preference for short delays weakens as we consider stricter low-metallicity thresholds for BBH formation. For a p(τ) ∝ τ -1 time delay distribution and a progenitor formation rate that follows the SFR without metallicity dependence, we find that τ min < 2.2 Gyr, whereas considering only the low-metallicity Z < 0.3 Z o˙ SFR, τ min < 3.0 Gyr (90% credibility). Alternatively, if we assume long time delays, the progenitor formation rate must peak at higher redshifts than the SFR. For example, for a p(τ) ∝ τ -1 time delay distribution with τ min = 4 Gyr, the inferred progenitor rate peaks at z > 3.9 (90% credibility). Finally, we explore whether the inferred formation rate and time delay distribution vary with BBH mass.
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U2 - 10.3847/2041-8213/ac05c4
DO - 10.3847/2041-8213/ac05c4
M3 - Article
AN - SCOPUS:85109112826
SN - 2041-8205
VL - 914
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 2
M1 - L30
ER -