eROSITA All-Sky Survey Takes the Local Hot Bubble’s Temperature

About half a century ago, astronomers theorized that the Solar System is situated in a low-density hot gas environment. This hot gas emits soft X-rays that displace the dust in the local interstellar medium (ISM), creating what is known as the Local Hot Bubble (LHB). This theory arose to explain the ubiquitous soft X-ray background (below 0.2 keV) and the lack of dust in our cosmic neighborhood. This theory has faced some challenges over the years, including the discovery that solar wind and neutral atoms interact with the heliosphere, leading to similar emissions of soft X-rays.

Thanks to new research by an international team of scientists led by the Max Planck Institute for Extraterrestrial Physics (MPE), we now have a 3D model of the hot gas in the Solar System’s neighborhood. Using data obtained by the eROSITA All-Sky Survey (eRASS1), they detected large-scale temperature differences in the LHBT that indicate that the LHB must exist, and both it and solar wind interaction contribute to the soft X-ray background. They also revealed an interstellar tunnel that could possibly link the LHB to a larger “superbubble.”

The research was led by Michael C. H. Yeung, a PhD student at the MPE who specializes in the study of high-energy astrophysics. He was joined by colleagues from the MPE, the INAF-Osservatorio Astronomico di Brera, the University of Science and Technology of China, and the Dr. Karl Remeis Observatory. The paper that details their findings, “The SRG/eROSITA diffuse soft X-ray background,” was published on October 29th, 2024, by the journal Astronomy & Astrophysics.

The eROSITA telescope was launched in 2019 as part of the Russian–German Spektr-RG space observatory. It is the first X-ray observatory to observe the Universe beyond Earth’s geocorona, the outermost region of the Earth’s atmosphere (aka. the exosphere), to avoid contamination by the latter’s high-ultraviolet light. In addition, the eROSITA All-Sky Survey (eRASS1) was timed to coincide with the solar minimum, thus reducing contamination by solar wind charge exchanges.

For their study, the team combined data from the eRASS1 with data from eROSITA’s predecessor, the X-ray telescope ROSAT (short for Röntgensatellit). Also built by the MPE, this telescope complements the eROSITA spectra by detecting X-rays with energies lower than 0.2 keV. The team focused on the LHB located in the western Galactic hemisphere, dividing it into about 2000 regions and analyzing the spectra from each. Their analysis showed a clear temperature difference between the parts of the LHB oriented towards Galactic South (0.12 keV; 1.4 MK) and Galactic North (0.10 keV; 1.2 MK).

According to the authors, this difference could have been caused by supernova explosions that expanded and reheated the Galactic South portion of the LHB in the past few million years. Yeung explained in an MPE press release: “In other words, the eRASS1 data released to the public this year provides the cleanest view of the X-ray sky to date, making it the perfect instrument for studying the LHB.”

In addition to obtaining temperature data from the diffuse X-ray background spectra information, the combined data also provided a 3D structure of the hot gas. In a previous study, Yeung and his colleagues examined eRASS1 spectra data from almost all directions in the western Galactic hemisphere. They concluded that the density of the hot gas in the LHB is relatively uniform. Relying on this previous work, the team generated a new 3D model of the LHB from the measured intensity of X-ray emissions.

This model shows that the LHB extends farther toward the Galactic poles than expected since the hot gas tends to follow the path of least resistance (away from the Galactic disc). Michael Freyberg, a core author of this work, was a part of the pioneering work in the ROSAT era three decades ago. As he explained:

“This is not surprising, as was already found by the ROSAT survey. What we didn’t know was the existence of an interstellar tunnel towards Centaurus, which carves a gap in the cooler interstellar medium (ISM). This region stands out in stark relief thanks to the much-improved sensitivity of eROSITA and a vastly different surveying strategy compared to ROSAT.”

These latest results suggest the Centaurus tunnel may be a local example of a wider hot ISM network sustained by supernovae and solar wind-ISM interaction across the Galaxy. While astronomers have theorized the existence of the Centaurus tunnel since the 1970s, it has remained difficult to prove until now. The team also compiled a list of known supernova remnants, superbubbles, and dust and used these to create a 3D model of the Solar System’s surroundings. The new model allows astronomers to better understand the key features in the representation.

These include the Canis Major tunnel, which may connect the LHB to the Gum Nebula (the red globe) or the long grey superbubble (GSH238+00+09). Dense molecular clouds, represented in orange, are shown near the surface of the LHB in the direction of the Galactic Center (GC). Recent work suggests these clouds are moving away from the Solar System and likely formed from the condensation of materials swept up during the early formation of the LHB. Said Gabriele Ponti, a co-author of this work:

“Another interesting fact is that the Sun must have entered the LHB a few million years ago, a short time compared to the age of the Sun. It is purely coincidental that the Sun seems to occupy a relatively central position in the LHB as we continuously move through the Milky Way.”

Further Reading: MPE, Astronomy & Astrophysics