Origin of the companion’s mid-infrared photometric excess

Determine whether the slight mid-infrared photometric excess observed for HD 101452 B is caused by an astrophysical source, such as an unseen circumstellar disk or third companion, or by a systematic underestimation of the Gaia G-band photometry resulting from contamination by light from the nearby HD 101452 primary.

Background

The detected companion to HD 101452 was classified through a spectral-energy-distribution fit combining four JWST MIRI measurements with its Gaia DR3 G-band magnitude. Although the fit was broadly consistent with a late K- to early M-dwarf classification, the mid-infrared photometry appeared slightly brighter than expected from empirical stellar relations when the Gaia G-band measurement was used as an anchor.

The paper leaves unresolved whether this discrepancy reflects additional astrophysical emission from an unseen circumstellar disk or an additional companion, or instead results from a systematic error in the Gaia G-band photometry caused by contamination from the nearby primary star. Resolving this ambiguity would improve the physical interpretation and classification of HD 101452 B.

References

It is uncertain if this excess could be caused by an astrophysical source such as an unseen disk or third companion or if the Gaia G-band photometry could have a systematic error causing it to be slightly underreported due contamination from the light from the nearby host star.

— A Binary Flux Calibrator Reveals the Scientific Potential of Short-integration JWST MIRI Imaging to Directly Detect sub-Jupiter Exoplanets  (2609.19133 - Bowens-Rubin et al., 16 Sep 2026) in Section 4.4, “Classification of the Companion”