The Crab Nebula at 1.3 mm: evidence for a new synchrotron component

TL;DR

This study presents 1.3 mm observations of the Crab Nebula revealing a new synchrotron component, characterized by spectral flattening and spatial variations, suggesting complex electron populations beyond traditional models.

Contribution

It provides evidence for a second synchrotron component in the Crab Nebula, challenging existing models and linking millimetre and X-ray structures.

Findings

Detection of spectral flattening in the inner region.

Identification of a second synchrotron component.

Correlation between mm spectral steepening and radio filaments.

Abstract

We present the results of 1.3 mm observations of the Crab Nebula, performed with the MPIfR bolometer arrays at the IRAM 30-m telescope. The maps obtained, of unprecedented quality at these wavelengths, allow a direct comparison with high-resolution radio maps. Although the spatial structure of the Crab Nebula does not change much from radio to millimetre wavelengths, we have detected significant spatial variations of the spectral index between 20 cm and 1.3 mm. The main effect is a spectral flattening in the inner region, which can be hardly explained just in terms of the evolution of a single population of synchrotron emitting electrons. We propose instead that this is the result of the emergence of a second synchrotron component, that we have tried to extract from the data. Shape and size of this component resemble those of the Crab Nebula in X rays. However, while the more compact structure of the Crab Nebula in X rays is commonly regarded as an effect of synchrotron downgrading, it cannot be explained why a similar structure is present also at mm wavelengths, where the electron lifetimes far exceed the nebular age. Our data, combined with published upper limits on spatial variations of the radio spectral index, also imply a low-energy cutoff for the distribution of electrons responsible for this additional synchrotron component. Although no model has been developed so far to explain the details of this component, one may verify that the total number of the electrons responsible for it is in agreement with what predicted by the classical pulsar-wind models, which otherwise are known to fail in accounting for the number of radio emitting electrons. We have also detected a spectral steepening at mm wavelengths in some elongated regions, whose positions match those of radio synchrotron filaments.