An 8 hour characteristic time-scale in submillimetre light curves of Sagittarius A*

TL;DR

This study identifies an approximately 8-hour characteristic variability time-scale in Sagittarius A*'s submillimetre light curves, providing insights into the physical processes near the black hole's event horizon.

Contribution

It introduces a stochastic damped random walk model to quantify the variability time-scale in submm light curves of Sagittarius A*, linking it to accretion flow dynamics.

Findings

Characteristic time-scale of 8 hours at 230 GHz

Variability persists down to the event horizon

Time-scale differs from those at other wavelengths

Abstract

We compile and analyse long term (~10 year) submillimetre (1.3, 0.87, 0.43 mm, submm) wavelength light curves of the Galactic centre black hole, Sagittarius A*. The 0.87 and 0.43 mm data are taken from the literature, while the majority of the 1.3 mm light curve is from previously unpublished SMA and CARMA data. We use Monte Carlo simulations to show that on minute to few hour time-scales the variability is consistent with a red noise process with a 230 GHz power spectrum slope of 2.3+0.8-0.6 at 95% confidence. The light curve is de-correlated (white noise) on very long (month to year) times. In order to identify the transition time between red and white noise, we model the light curves as a stochastic damped random walk process. The models allow a quantitative estimate of this physical characteristic time-scale of 8-4+3 hours at 230 GHz at 95% confidence, with consistent results at 345 and 690 GHz. This corresponds to ~10 orbital times or ~1 inflow (viscous) time at R = 3 Rs, a typical radius producing the 230 GHz emission as measured by very long baseline interferometry and found in theoretical accretion flow and jet models. This time-scale is significantly shorter (longer) than those measured at radio (near-infrared, NIR) wavelengths, and is marginally inconsistent with the same variability mechanism operating in the submm and NIR for the expected t ~ R^3/2 scaling. It is crudely consistent with the analogous time-scale inferred in studies of quasar optical light curves after accounting for the difference in emission radius. We find evidence that the submm variability persists at least down to the ISCO, if not the event horizon. These results can be compared quantitatively with similar analyses at different wavebands to test for connections between the variability mechanisms, and with light curves from theoretical models of accreting black holes.