Loop I/NPS morphology predictions in the ultralong-wavelength band

TL;DR

This paper models the expected ultra-long wavelength radio sky morphology of Loop I/NPS under two origin scenarios, predicting observable differences that upcoming space missions could use to determine its true nature.

Contribution

It develops emissivity models for Loop I/NPS at ultra-long wavelengths considering free-free absorption, enabling scenario discrimination with future observations.

Findings

In the SNRs model, Loop I/NPS remains bright at ~1 MHz.

In the GC model, the arc is visible only above ~3 MHz.

Absorption effects cause the arc to be invisible at certain latitudes below ~3 MHz.

Abstract

Loop I/North Polar Spur (NPS) is the giant arc structure above the Galactic plane observed at radio wavelengths ($\lesssim 10$ GHz). There has been long-standing debate about its origin. While many people believe that it black consists of nearby supernova remnants (SNRs), some others consider it as a giant bubble close to the Galactic Center (GC), associated with the Fermi Bubble and the eROSITA X-ray bubble. At ultra-long wavelengths (wavelength $\gtrsim 10$ m or frequency $\lesssim 30$ MHz), particularly below $\sim 10$ MHz, the free-free absorption of the radio signal by diffuse electrons in the interstellar medium (ISM) becomes significant, resulting in different sky morphologies from those at higher frequencies. In this paper, we develop emissivity models for the two Loop I/NPS origin scenarios, and predict the Loop I/NPS morphology at ultra-long wavelengths in both scenarios, taking into account the free-free absorption effect.We find that in the SNRs model, the full Loop I/NPS will still be a bright arc even at $\sim 1$ MHz. In the GC model, the arc is fully visible only above $\sim 3$ MHz. While below this frequency, it is visible only at Galactic latitudes $b\gtrsim 30\degree$; the $b\lesssim 30 \degree$ part becomes invisible due to the absorption by the ISM electrons between the GC and the Sun. The upcoming space missions aiming at ultra-long wavelengths, such as the DSL and the FARSIDE, can potentially distinguish these two scenarios and provide decisive information about the origin of the Loop I/NPS.