Letter to the Editor

Type Ib supernovae are bluer than Type Ic supernovae

¹ Max Planck Institute for Astrophysics, Karl-Schwarzschild-Straße 1, 85748 Garching bei München, Germany
² European Southern Observatory, Karl-Schwarzschild-Str. 2, 85741 Garching, Germany
³ Technische Universität München, TUM School of Natural Sciences, Physics Department, James-Franck-Straße 1, 85748 Garching, Germany
⁴ Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea
⁵ The School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
⁶ Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA

^⋆ Corresponding author: This email address is being protected from spambots. You need JavaScript enabled to view it.

Received: 2 May 2026
Accepted: 12 July 2026

Abstract

Type Ib and Ic supernovae (SNe Ib/Ic) are the bright finale of massive stars that have lost their hydrogen envelopes, making them powerful probes of mass stripping in massive star evolution. The advent of modern large photometric and spectroscopic surveys presents a unique opportunity to investigate systematic differences between these two kinds of SNe. In this study, we analyze a large, homogeneous sample of SNe Ib/Ic light curves from the Zwicky Transient Facility. We find a systematic difference in their apparent optical colors at peak: SNe Ib are, on average, bluer than SNe Ic, with two-sample tests confirming that the distributions differ (p <  0.05). The difference in their host galaxy reddening, as currently constrained, is too small to fully explain it. The color difference therefore most likely has an intrinsic origin, reflecting progenitors with different degrees of stripping – helium-rich for SNe Ib and helium-poor for SNe Ic. In addition, we find that SNe Ib/Ic with narrow lines (SNe Ibn/Icn) are bluer than those without, which might originate from circumstellar matter interaction, with potential connection to fast blue optical transients. We demonstrate that SN colors offer a promising probe of mass stripping in massive stars, potentially providing a useful tool for analyzing large photometric data and improving predictions for the final outcomes of stripped massive stars.