SNhunt181

SNhunt181 is a stripped-envelope supernova (Type Ib), consistent with core collapse after loss of the outer hydrogen (and for Ic, helium) envelope. The specific progenitor channel for this object is not uniquely determined by the spectral type alone.

The specific progenitor of SNhunt181 has not been observed. Events of this spectroscopic class are generally associated with massive-star core collapse after successive nuclear burning stages (hydrogen → helium → carbon → neon → oxygen → silicon → iron). Typical lifetimes of such progenitors are tens of millions of years, but that is a class expectation—not a measured age or evolutionary track for this star. No pre-explosion imaging identification is cited in the available record for SNhunt181.

SNhunt181 has a luminosity distance of approximately 587.1 Million Light-Years (redshift z = 0.04, d_L = 180 Mpc). Under a flat ΛCDM cosmology (H₀≈70 km/s/Mpc, Ωₘ≈0.3), the corresponding lookback time is ≈543 Myr — when the light set out 542.9 million years ago during the Neoproterozoic, hundreds of millions of years before complex animal life diversified. Luminosity distance is larger than the light-travel distance because cosmic expansion stretches the path; the two must not be equated.

SNhunt181 exhibits a measured spectroscopic redshift of z = 0.0400. The cockpit reports a user-facing recession velocity of 11,752.0 km/s, computed as the redshift Doppler-equivalent v = c·((1+z)²−1)/((1+z)²+1). Cosmological redshift is not generally equivalent to special-relativistic motion through space; this number is a convenient velocity label for z, not a measured peculiar velocity and not supernova ejecta speed. Bare c·z (≈11,992 km/s) is a different low-z approximation and is not mixed here.

At peak brightness, SNhunt181 achieved an apparent magnitude of 19.4 around 2013/04/05. Corrected for cosmic distance and foreground interstellar dust, its intrinsic absolute magnitude was -17. At this peak, the exploding star radiated with the incandescent brilliance of approximately 539.5 million Suns combined, briefly outshining the cumulative starlight of entire dwarf galaxies!

Core-collapse events of this broad class are often discussed with a ~10⁵³ erg gravitational binding energy of which ~99% may escape as neutrinos—again a class scale, not a measured budget for SNhunt181.

Spectroscopic line blueshifts imply an ejecta velocity of approximately 10,000 km/s (~3.3% of c) for SNhunt181. This is distinct from cosmological recession velocity inferred from redshift.

Classified core-collapse light curves are often sustained after peak by radioactive ⁵⁶Ni → ⁵⁶Co → ⁵⁶Fe decay, with typical nickel yields of order 0.05–0.15 solar masses—again a class scale, not a measured yield for SNhunt181. Shock-breakout heating may dominate the earliest optical flash; without a published bolometric fit, neither nickel mass nor the dominant power source is established for this event.

Events of SNhunt181's broad spectroscopic class are discussed in galactic chemical evolution as sources of oxygen-group and intermediate-mass elements (and, for some channels, iron-peak material). No measured elemental yields are published for SNhunt181.

A core-collapse explosion associated with SNhunt181's class forges an ultra-dense compact stellar remnant at the center of the detonation. If the progenitor had an initial mass under ~20 solar masses, it left behind a neutron star (pulsar)—packing the mass of our entire Sun into a city-sized sphere barely 20 kilometers wide, spinning dozens or hundreds of times per second. If the progenitor exceeded ~25–30 solar masses, gravity overcame neutron degeneracy pressure, creating a permanent stellar-mass black hole.

Supernova remnants in general evolve through free-expansion, Sedov–Taylor, and radiative phases over centuries to millennia, sometimes becoming bright X-ray shells and occasionally compressing nearby molecular clouds. These are standard remnant-evolution models, not forecasts measured for SNhunt181. Whether this site will trigger star formation, reach particular X-ray temperatures, or match Cassiopeia A depends on local density and magnetic field—none of which are constrained by the data shown here.

SNhunt181 is cataloged with host galaxy IC 3128A. No secure nuclear offset is published in this record.

In the celestial sphere, SNhunt181 is located at Right Ascension 12:18:41.3 and Declination +11:43:53, situated in the constellation Coma Berenices (Berenice's Hair). Because its declination is +11:43:53, it is primarily placed in the Northern celestial hemisphere.

Along this line of sight, the catalog records a Milky Way foreground color excess of E(B−V) = 0.0237 mag (source: published extinction estimate), corresponding to roughly A_V ≈ 0.07 mag for R_V = 3.1. Band-specific corrections (e.g. A_r) differ from A_V and should be applied when available. Map-based values (IRSA / Schlafly & Finkbeiner 2011) must not be claimed unless that map was actually queried.

No calibrated photometry is published for SNhunt181. Without multi-epoch flux measurements, neither a light curve nor a peak magnitude can be established. Follow-up imaging from survey alert streams would be required to map its brightness evolution.

No spectrum has been published for SNhunt181. Without spectroscopy, its chemical composition, expansion velocity, and physical classification cannot be established. Classification spectra from follow-up observatories would be required to identify diagnostic absorption and emission lines.

SNhunt181 was officially reported on 2013/04/06 by Howerton. Discoveries are typically flagged by high-cadence robotic survey telescopes (such as ATLAS, ZTF, Pan-STARRS, ASAS-SN, or Gaia) and worldwide amateur astronomers scanning the night sky, followed by rapid spectroscopic classification by international observatories.

Data for SNhunt181 are compiled from international astronomical notices, the IAU Transient Name Server (TNS), and peer-reviewed astrophysical journals.

Throughout global alert streams and survey databases, SNhunt181 has also been designated as: PSN J12184129+1143531, LSQ13abk. These cross-matched identifiers allow astronomers to cross-reference observations across the Zwicky Transient Facility (ZTF), the Asteroid Terrestrial-impact Last Alert System (ATLAS), Pan-STARRS, Gaia Photometric Science Alerts, and the IAU Transient Name Server (TNS).

As a core-collapse supernova, SNhunt181 provides independent cosmological distance calibrations via the Expanding Photosphere Method (EPM) and the Standard Candle Method for Type II supernovae (SCM-II). By correlating the physical expansion speed of the photosphere (measured via spectroscopic Doppler shifts) with its photometric color temperature, astronomers determine direct geometric distances independent of secondary distance ladders.

Core-collapse supernovae like SNhunt181 are premier targets for multi-messenger astrophysics! During the collapse of the iron core, an intense burst of 10⁵⁸ neutrinos escaped into space hours before the shock broke out through the stellar surface (as famously seen in SN 1987A). Furthermore, violent core asymmetries and non-axisymmetric core bounce can emit high-frequency gravitational waves detectable by advanced interferometers (LIGO, Virgo, KAGRA) for events within the Milky Way and Local Group.

Compared to historical landmarks like SN 1987A in the Large Magellanic Cloud (168,000 light-years away, naked-eye peak m = 2.9) or the Crab Supernova of 1054 (6,500 light-years away), SNhunt181 occurred at a distance of 587.1 Million Light-Years. While historical naked-eye supernovae occurred within our Milky Way or its immediate satellites, modern discoveries like SNhunt181 allow astrophysicists to probe diverse galactic environments, metallicities, and stellar populations across the broader universe.

Unknown — no measured brightness. SNhunt181 was discovered 4971 days ago (2013/04/06), but no calibrated photometry is published for it, so its current apparent magnitude cannot be stated. Without a magnitude there is no basis for a telescope-aperture recommendation. Use the coordinates and airmass chart above to plan a follow-up observation and report what you measure.

No, Earth is in zero danger. Supernovae are violent events emitting powerful gamma rays, X-rays, and cosmic rays; however, the astrophysical 'lethal kill zone' for our planet's protective ozone layer is estimated at 50 to 100 light-years. At a distance of 587.1 Million Light-Years, the inverse-square law dilutes the radiation by quintillions of times, making SNhunt181 completely harmless to our biosphere and purely a fascinating spectacle for human exploration.