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Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.
Resolving The Peak Of The Black Hole Mass Spectrum (2022)

Gravitational wave (GW) detections of binary black hole (BH) mergers have begun to sample the cosmic BH mass distribution. The evolution of single stellar cores predicts a gap in the BH mass distribution due to pair-instability supernova (PISN). Determining the upper and lower edges of the BH mass gap can be useful for interpreting GW detections from merging BHs. In this article We use MESA to evolve single, non-rotating, massive helium cores with a metallicity of $Z = 10^{-5}$ until they either collapse to form a BH or explode as a PISN without leaving a compact remnant. We calculate the boundaries of the lower BH mass gap for S-factors in the range S(300 keV) = (77,203) keV b, corresponding to the $\pm 3\sigma$ uncertainty in our high resolution tabulated $^{12}$C($\alpha$,$\gamma$)$^{16}$O reaction rate probability distribution function. We extensively test the temporal and mass resolution to resolve the theoretical peak of the BH mass spectrum across the BH mass gap. We explore the convergence with respect to convective mixing and nuclear burning, finding that significant time resolution is needed to achieve convergence. We also test adopting a minimum diffusion coefficient to help lower resolution models reach convergence. We establish a new lower edge of the upper mass gap as M$_{\rm lower}$ $\simeq$ 60$^{+32}_{-14}$ M$_{\odot}$ from the $\pm 3\sigma$ uncertainty in the $^{12}$C($\alpha$,$\gamma$)$^{16}$O rate. We explore the effect of a larger 3-$\alpha$ rate on the lower edge of the upper mass gap, finding M$_{\rm lower}$ $\simeq$ 69$^{+34}_{-18}$ M$_{\odot}$. We compare our results with BHs reported in the Gravitational-Wave Transient Catalog.


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Observing Intermediate-mass Black Holes and the Upper Stellar-mass gap with LIGO and Virgo (2022)

In this article we probe the mass function of intermediate-mass black holes (IMBHs) wherein we also include BHs in the upper mass gap ∼60 - 130 M$_{\odot}$. Employing the projected sensitivity of the upcoming LIGO and Virgo fourth observing (O4) run, we perform Bayesian analysis on quasi-circular non-precessing, spinning IMBH binaries (IMBHBs) with total masses 50 - 500 M$_\odot$, mass ratios 1.25, 4, and 10, and dimensionless spins up to 0.95, and estimate the precision with which the source-frame parameters can be measured. We find that, at 2$\sigma$, the mass of the heavier component of IMBHBs can be constrained with an uncertainty of ∼10 - 40% at a signal-to-noise ratio of 20. Focusing on the stellar-mass gap with new tabulations of the $^{12}$C($\alpha$,$\gamma$)$^{16}$O reaction rate and its uncertanties, we evolve massive helium core stars using MESA, to establish the lower and upper edge of the mass gap as ∼59$^{+34}_{-13}$ M$_{\odot}$ and ∼139$^{+30}_{-14}$ M$_{\odot}$ respectively, where the error bars give the mass range that follows from the ±3$\sigma$ uncertainty in the $^{12}$C($\alpha$,$\gamma$)$^{16}$O nuclear reaction rate. We find that high resolution of the tabulated reaction rate and fine temporal resolution are necessary to resolve the peak of the BH mass spectrum. We then study IMBHBs with components lying in the mass gap and show that the O4 run will be able to robustly identify most such systems. Finally, we re-analyse GW190521 with a state-of-the-art aligned-spin waveform model, finding that the primary mass lies in the mass gap with 90% credibility.


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