The Beta Pictoris debris disk hosts a curious substructure called the Cat’s Tail that was first seen in mid-infrared images from the James Webb Space Telescope. This paper reports that deep Hubble Space Telescope (HST) imaging now detects the Cat’s Tail in visible and near‑infrared scattered light. That means the same dust feature is reflecting starlight as well as glowing in the mid‑infrared.

The team combined six epochs of HST imaging with the Space Telescope Imaging Spectrograph (STIS), taken between 2012 and 2025, and used coronagraphy to block the bright star and reveal faint dust. With these deep data they traced the disk out to 500 astronomical units (AU) in projection — the first time HST/STIS reaches that far for this system — and achieved signal‑to‑noise ratios above 100 across much of the disk midplane between roughly 50 and 200 AU. To measure how bright the Cat’s Tail is in scattered light they used an injection–recovery test: they put simulated signals into the data and tried to recover them. From that test they estimate the Cat’s Tail’s scattered‑light flux is very faint, only about 0.1–0.4% of the flux seen in the JWST MIRI F1550C mid‑infrared filter.

The authors used the measured ratio of HST scattered light to JWST mid‑infrared emission to model the dust grains. Their models favor grains that are highly porous and made almost entirely of organic refractory material — a kind of carbon‑rich, non‑volatile dust. This result agrees with what the earlier JWST mid‑infrared study found from thermal emission alone. “Organic refractory” here means carbonaceous solids, not biological material.

The paper also explores what kind of collisions could create the amount of organic material seen. Using the organic content of Solar System dwarf planets and of dust in the local interstellar medium as rough templates, the authors estimate that each colliding body would need a mass of at least 1–3 × 10^21 kilograms. That mass is similar to large Kuiper Belt objects in our Solar System, such as Charon or Makemake. These estimates rely on those proxy compositions and on the assumption that a single collision supplied most of the detected material.