MOMO IV: The complete Swift X-ray and UV/optical light curve and characteristic variability of the blazar OJ 287 during the last two decades

TL;DR

This paper presents the most comprehensive multiwavelength monitoring of blazar OJ 287 over two decades, revealing detailed variability patterns, characteristic timescales, and insights into its emission components and structure.

Contribution

It provides the first dense, long-term X-ray and UV/optical light curve of OJ 287, analyzing variability, lags, and structural features, advancing understanding of blazar emission mechanisms.

Findings

Optical-UV variability timescale of ~5 days during low activity

Zero lag between optical and UV emissions during dense monitoring

Detection of a deep UV-optical fade lasting 2 months in 2017

Abstract

We are carrying out a dense monitoring of the blazar OJ 287 with Swift since late 2015 as part of our project MOMO (Multiwavelength Observations and Modeling of OJ 287). This is the densest existing monitoring of OJ 287 involving X-ray and UV data. In this latest publication of a sequence, we characterize the multiwavelength variability of OJ 287 based on >4000 Swift single-wave-band data sets including archival data since 2005. A structure function analysis reveals a characteristic timescale of ~5 days in the optical-UV at epochs of low-level activity, and larger during outbursts. The discrete correlation function shows zero lag between optical and UV, with tau = 0+-1 days at the epoch of densest cadence. During outbursts (in 2016/17 and 2020) the X-rays follow the UV with near-zero lags. However, during quiescence, the delay is 7-18 days with X-rays leading or lagging, interpreted as due to a different X-ray component dominated by inverse Compton emission. Scaling relations are used to derive the characteristic length scales of broad-line region and torus in OJ 287. A remarkable, symmetric UV--optical deep fade is identified in late 2017, lasting for 2 months. We rule out occultation from the passage of a dusty cloud and a model where the secondary black hole deflects the jet between the primary and observer. We speculate about a temporary dispersion or jet swing event in the core or in a bright quasi-stationary jet feature. The deep fade reveals an additional, spatially distinct X-ray component. The epoch 2020.9-2021.1 was searched for precursor flare activity predicted by the binary black hole model of OJ 287.