SN2025uma

SN2025uma is a stripped-envelope supernova (Type Ib/c), 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 SN2025uma 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 SN2025uma.

SN2025uma has a luminosity distance of approximately 251.3 Million Light-Years (redshift z = 0.017746, d_L = 77.04 Mpc). Under a flat ΛCDM cosmology (H₀≈70 km/s/Mpc, Ωₘ≈0.3), the corresponding lookback time is ≈245 Myr — when the light set out 244.7 million years ago during the Triassic period as the earliest dinosaurs and mammals were just evolving. Luminosity distance is larger than the light-travel distance because cosmic expansion stretches the path; the two must not be equated.

SN2025uma exhibits a measured spectroscopic redshift of z = 0.0177. The cockpit reports a user-facing recession velocity of 5,272.9 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 (≈5,320 km/s) is a different low-z approximation and is not mixed here.

Observed (single-epoch) magnitude of SN2025uma is 18.76 (r) on 2025/08/10 (MJD 60897.5). A single calibrated detection is not evidence of a peak; no rise, decline, or light curve can be established from one point. An absolute magnitude of -15.67 mag can be quoted only if distance is independently known.

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 SN2025uma.

No ejecta velocity is measured for SN2025uma. Blast-wave speed is obtained from Doppler shifts of spectral absorption features (e.g. Si II λ6355 for Type Ia), not from cosmological redshift. Any recession velocity derived from z describes Hubble flow, not the explosion debris. Type Ib/c events typically show ejecta speeds of order ~12,500 km/s near maximum, but that class scale is not a measurement of SN2025uma.

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 SN2025uma. 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 SN2025uma'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 SN2025uma.

A core-collapse explosion associated with SN2025uma'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 SN2025uma. 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.

No host galaxy is identified for SN2025uma in this catalog record. A blank host field means the association is unresolved here—it does not establish that the host is uncataloged, resolved in imaging, or securely linked by astrometry. Possible states (unidentified, hostless candidate, imaging detection without a catalog name, or a securely matched cataloged galaxy) require separate evidence that is not present in this field.

In the celestial sphere, SN2025uma is located at Right Ascension 06:24:30.176 and Declination +17:49:35.03, situated in the constellation Gemini (The Twins). Because its declination is +17:49:35.03, 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) = 0.4361 mag (source: Analytical Galactic Disk Model (IAU)), corresponding to roughly A_V ≈ 1.35 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.

SN2025uma has 1 calibrated photometric detection on record in r from ZTF. A single point is not a light curve: no rise, peak, or decline rate can be measured until additional epochs are published.

No spectrum has been published for SN2025uma. 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.

SN2025uma was officially reported on 2025/08/10 by Nabeel Rehemtulla (CIERA, NU), Kaustav Kashyap Das (Caltech), Mansi Kasliwal (Caltech), Theophile Du Laz (Caltech) on behalf of ZTF. 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.

SN2025uma is documented across 3 scientific references and archival data sources in the sne.space. These include discovery circulars and research datasets from Transient Name Server, 2025TNSTR3263....1R, The Open Supernova Catalog. All raw photometry and spectroscopy points are cross-indexed to their original bibliographic records for peer-reviewed verification.

Throughout global alert streams and survey databases, SN2025uma has also been designated as: 2025uma, AT2025uma, ATLAS25kza, SN 2025uma, ZTF25abitlgg. 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, SN2025uma 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 SN2025uma 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), SN2025uma occurred at a distance of 251.3 Million Light-Years. While historical naked-eye supernovae occurred within our Milky Way or its immediate satellites, modern discoveries like SN2025uma allow astrophysicists to probe diverse galactic environments, metallicities, and stellar populations across the broader universe.

Unknown — no measured brightness. SN2025uma was discovered 461 days ago (2025/08/10), 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 251.3 Million Light-Years, the inverse-square law dilutes the radiation by quintillions of times, making SN2025uma completely harmless to our biosphere and purely a fascinating spectacle for human exploration.