Draghis: Exploring the Spin Distribution of Stellar Mass Black Holes /Raghunathan: Prospects for Kinematic Sunyaev-Zeldovich Measurements from future CMB surveys

Apr 25, 2023 - 10:40 am to 11:30 am

Campus, PAB 102/103

Paul Draghis (University of Michigan) / Srini Raghunathan (University of Illinois Urbana-Champaign) In Person and zoom https://stanford.zoom.us/j/550904854

Zoom info: https://stanford.zoom.us/j/550904854


The launch of NuSTAR and the increasing number of binary black hole (BBH) mergers detected through gravitational wave (GW) observations have exponentially advanced our understanding of black holes. Despite the simplicity owed to being fully described by their mass and angular momentum, black holes have remained mysterious laboratories that probe the most extreme environments in the Universe. While significant progress has been made in the recent decade, the distribution of spin in black holes has not yet been understood. The preferred spin measurement techniques are “continuum fitting” (see e.g., Gou et al. 2009) and “relativistic reflection” (see e.g., Miller 2007). Relativistic reflection is independent of black hole mass, accretion rate, and distance to the system, making it a more versatile technique. Up until now, spin measurements for the same black hole using the two methods did not always agree, and even measurements using the same method did not always adopt the same sets of assumptions and theoretical prescriptions. Our work provides a pipeline that uses state of the art relativistic reflection models to fully explore the entire physical parameter space and to provide a uniform treatment of a large sample of black holes. Using our pipeline on NuSTAR data, we measure more than a dozen new black hole spins in X-ray binary systems, significantly expanding the measured sample size, and begin to remeasure old black hole spins in order to compile a distribution of measurements made using entirely consistent methods and systematic uncertainties. Additionally, we analyze possible observational and modeling biases of the sample and compare the distribution to that of spins measured in mergers of binary black hole systems observed through gravitational waves, in order to offer a unified view of black hole spin evolution. We find that the observed spin distribution of black holes in X-ray binaries is sharply peaked at high values, incompatible with the spin distribution inferred based on GW signals from merging BBH, suggesting that the observed black hole distributions are inherently different. Understanding the distribution of black hole spins in X-ray binaries provides an insight into the formation of black holes, supernova events, collapsar models, gamma-ray bursts, the formation and evolution of X-ray binaries and binary black hole systems, the physics of accretion, and paves the way for future Gravitational Wave efforts and for future X-ray missions such as XRISM, HEX-P, AXIS, or ATHENA.