Distribution of X-ray Emission from Jet Knots of 3C273

TL;DR

This paper investigates the X-ray emission mechanisms of the jet knots in quasar 3C273, proposing inverse Compton scattering models and estimating physical parameters based on multi-band observations.

Contribution

It introduces a scenario where X-ray emissions from jet knots are explained by inverse Compton scattering, providing constraints on jet orientation and physical parameters.

Findings

Inverse Compton scattering explains X-ray emissions in the nearest knots.

Constraints on the jet's angle to the line of sight were derived.

Physical parameters of the jet knots were estimated.

Abstract

The jet of the quasar 3C273 is observed at different spectral bands. This jet has a knot structure. Jet radiation in radio and optical bands are connected with synchrotron mechanism, while the emission mechanism producing the X-rays is controversial. We suppose that the X-rays observed for two knots nearest to the quasar can originate from the inverse Compton scattering of external source radiation on relativistic electrons. But in the jet region with constant low X-ray intensity the inverse Compton scattering on cosmic microwave background photons (IC/CMB) is essential because the energy density of external source decreases. Upon this scenario the constraints on the angle between the jet axis and line sight values have been obtained. Also, some physical parameters for two nearest knots of the jet of 3C273 have been estimated.