Nature of the soft ULX in NGC 247: super-Eddington outflow and transition between the supersoft and soft ultraluminous regimes

TL;DR

This study investigates the spectral state transitions of the ULX in NGC 247, revealing super-Eddington outflows and challenging standard accretion disk models, with implications for understanding ULX emission mechanisms.

Contribution

It provides multi-epoch observations showing the transition between SSUL and SUL regimes, and proposes a super-Eddington outflow model for the soft X-ray emission.

Findings

Anti-correlation between blackbody radius and temperature ($R_{bb} \, \propto \, T_{bb}^{-2.8}$)

Greater variability in the SSUL regime compared to SUL

Flux dips possibly due to accretion rate changes or wind fluctuations

Abstract

We report on XMM-Newton/Chandra/Swift/HST observations of the ultraluminous X-ray source (ULX) in NGC 247, which is found to make transitions between the supersoft ultraluminous (SSUL) regime with a spectrum dominated by a cool ($\sim 0.1$ keV) blackbody component and the soft ultraluminous (SUL) regime with comparable luminosities shared by the blackbody and power-law components. Multi-epoch observations revealed an anti-correlation between the blackbody radius and temperature, $R_{\rm bb} \propto T_{\rm bb}^{-2.8 \pm 0.3}$, ruling out a standard accretion disk as the origin of the soft X-ray emission. The soft X-ray emission is much more variable on both short and long timescales in the SSUL regime than in the SUL regime. We suggest that the SSUL regime may be an extension of the ultraluminous state toward the high accretion end, being an extreme case of the SUL regime, with the blackbody emission arising from the photosphere of thick outflows and the hard X-rays being emission leaked from the embedded accretion disk via the central low-density funnel or advected through the wind. However, the scenario that the supersoft ULXs are standard ULXs viewed nearly edge-on cannot be ruled out. Flux dips on a timescale of 200 s were observed. The dips cannot be explained by an increase of absorption, but could be due to the change of accretion rate or related to thermal fluctuations in the wind or disk. The optical emission of NGC 247 ULX exhibits a blackbody spectrum at a temperature of 19,000 K with a radius of 20 $R_\odot$, likely arising from an OB supergiant companion star.