| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 00h 45m 13.4750912760s |
| Declination | +41° 32′ 33.146683296″ |
| Apparent magnitude (V) | ~22 (pre-2014) |
| Characteristics | |
| Evolutionary stage | Red supergiant (progenitor) |
| Variable type | Failed supernova (candidate) |
| Astrometry | |
| Distance | 2.5M ly (770k pc) |
| Details | |
| Mass | 13-20 M☉ |
| Other designations | |
| M31-2014-DS1, M31-DS1 | |
| Database references | |
| SIMBAD | data |
M31-2014-DS1 is a failed supernova candidate located in the Andromeda Galaxy (M31). It is a massive star observed to have undergone a "silent" collapse directly into a black hole without a characteristic supernova explosion. The event, characterized by a brief infrared brightening followed by the total disappearance of the progenitor star in optical wavelengths, provides observational evidence for the failed supernova theory of stellar evolution. [1]
The progenitor star was identified in archival data as a luminous red supergiant with an initial mass estimated at approximately 13 M☉. [1] In 2014, the object underwent a significant mid-infrared outburst, increasing in luminosity as detected by the Spitzer Space Telescope and the Wide-field Infrared Survey Explorer (WISE).
Following this peak, the star began a steady decline in brightness. By 2023, deep imaging from the W. M. Keck Observatory and the Hubble Space Telescope confirmed that the star was no longer visible. Unlike a standard Type II supernova, no luminous optical transient was detected during the collapse. [1]
The disappearance of M31-2014-DS1 is attributed to the collapse of the stellar core after the exhaustion of nuclear fuel. In typical stars of this mass range, the collapse triggers a shockwave that expels the outer layers. However, in the case of M31-2014-DS1, the shock failed to overcome the material falling inward. [1]
Theoretical models of the collapse suggest a brief, intense burst of neutrinos occurred at the moment of event horizon formation. The abrupt cessation of the neutrino signal marks the exact point of black hole birth. [2]
The infrared signature observed in 2014-2016 is believed to be caused by a small fraction of the stellar envelope (~1 M☉) being ejected at low velocities, subsequently cooling and forming a shroud of dust. [1] The remaining mass collapsed into a stellar-mass black hole.
The discovery addresses the "missing supernova" problem, where the number of observed supernovae is lower than predicted by the star formation rate. M31-2014-DS1 suggests that a significant fraction of massive stars may end their lives as failed supernovae rather than in bright explosions. [1]
Recent studies have also used this event to calibrate neutrino detectors like Super-Kamiokande, as the energy profile of the neutrinos provides data on the mass of the progenitor and the state of matter during collapse. [2]
Several researchers have proposed alternative models to explain the star's infrared behavior and subsequent disappearance in optical wavelengths.
Some models suggest the 2014 infrared outburst was not a precursor to the collapse, but rather a luminous red nova event caused by the merger of two stars. In this scenario, the "disappearance" is actually the merged remnant being temporarily shrouded by a thick, expanding shell of ejected material. [3]
Observations in early 2026 using the James Webb Space Telescope (JWST) have detected a persistent, albeit faint, mid-infrared source at the progenitor's coordinates. This has led some astronomers to argue that the star has not vanished, but as instead entered a phase of extreme mass loss, creating a dust cocoon thick enough to block all visible light. [4]
A 2026 preprint suggests the event could be an unusually long-duration eruption of a luminous blue variable star, which can mimic the appearance of a "disappearing" star before eventually re-emerging decades later. [3]