2026-10-28 アリゾナ大学
This study’s observations, made with the Hubble Space Telescope, revealed the “Cat’s Tail” structure for the first time in the visible light spectrum (white arrow). Unlike the original discovery observations made with the James Webb Space Telescope, which detected the dust grain’s heat emissions using infrared radiation, the tail appears shorter in the new images, because the further the trail of dust grains extends from the star, the less light they reflect. Avsar et al.
＜関連情報＞
- https://news.arizona.edu/news/enormous-cats-tail-tells-cosmic-collision-63-light-years-away
- https://iopscience.iop.org/article/10.3847/2041-8213/aeac4a
βピクトリス残骸円盤のHST/STISによる深層コロナグラフ画像：猫の尾の散乱光成分について Deep HST/STIS Coronagraphic Imaging of the β Pictoris Debris Disk: On the Scattered Light Component of the Cat’s Tail
Arin M. Avsar, Kevin Wagner, Dániel Apai, Isabel Rebollido, Antranik A. Sefilian, Marshall D. Perrin, Christopher C. Stark, Gabriel Weible, and András Gáspár
The Astrophysical Journal Letters Published: 2026 October 7
DOI:10.3847/2041-8213/aeac4a
Abstract
The β Pictoris debris disk is a unique system where mid-infrared coronagraphic imaging with JWST/Mid-Infrared Imager (MIRI) revealed a new spatially resolved substructure known as the Cat’s Tail. We present deep Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph (STIS) coronagraphic imaging of β Pic in scattered light, combining six epochs of observations between 2012 and 2025, in search of the scattered light component of the Cat’s Tail. We detect the disk out to a projected separation of 500 au for the first time with HST/STIS, achieving a signal-to-noise ratio (SNR) > 100 across much of the midplane between 50 and 200 au. We report the detection of the visible/near-infrared scattered light component of the Cat’s Tail substructure. We find through injection-recovery analysis that the scattered light component of the Cat’s Tail has a total flux of 0.1%–0.4% of the MIRI F1550C flux. Using the measured STIS-to-MIRI flux ratio, we model the Cat’s Tail grain properties and find that the grains are highly porous and almost entirely composed of organic refractory material, which is in agreement with findings with JWST/MIRI. We use the organics content of solar system dwarf planets and dust in the local ISM as a proxy to estimate the size of the colliding progenitors that can produce enough organic refractory material seen in the Cat’s Tail. We find that each colliding progenitor must have a mass of at least 1–3 × 1021 kg, comparable to Charon and Makemake in our Kuiper Belt. Additionally, we find a prominent warped morphology and surface brightness asymmetry in the outer dust halo of β Pic. We compare the observed halo morphology and asymmetry to predicted vertical structures, which may arise from planet–disk interactions.
