SN2022pjq

SN2022pjq is classified as a superluminous supernova (SLSN). Proposed power sources include magnetar spin-down and ejecta–CSM interaction; which engine applies to this object is not established from the classification label alone.

The specific progenitor of SN2022pjq 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 SN2022pjq.

SN2022pjq has a luminosity distance of approximately 2668.9 Million Light-Years (redshift z = 0.17, d_L = 818.29 Mpc). Under a flat ΛCDM cosmology (H₀≈70 km/s/Mpc, Ωₘ≈0.3), the corresponding lookback time is ≈2109 Myr — when the light set out 2109.0 million years ago in deep Precambrian time, well before multicellular animals dominated Earth. Luminosity distance is larger than the light-travel distance because cosmic expansion stretches the path; the two must not be equated.

SN2022pjq exhibits a measured spectroscopic redshift of z = 0.1700. The cockpit reports a user-facing recession velocity of 46,685.6 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 (≈50,965 km/s) is a different low-z approximation and is not mixed here.

The peak brightness of SN2022pjq is not recorded. No peak apparent magnitude and no calibrated photometry are published for this transient, so neither its apparent brightness nor its intrinsic luminosity can be stated. Any figure quoted here would be an estimate from a template rather than a measurement of this object. Follow-up photometry would establish the light curve and the peak.

SLSN radiated energies can exceed ordinary supernovae by large factors, but the power source (magnetar, CSM interaction, or other) is model-dependent. No object-specific energy release is published for SN2022pjq.

No ejecta velocity is measured for SN2022pjq. 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 SLSN-I events typically show ejecta speeds of order ~15,000 km/s near maximum, but that class scale is not a measurement of SN2022pjq.

SLSN light curves may be powered by magnetar spin-down, CSM interaction, or (in some models) large ⁵⁶Ni masses. Which engine powers SN2022pjq is not established here, and no object-specific nickel mass is published.

Events of SN2022pjq'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 SN2022pjq.

A core-collapse explosion associated with SN2022pjq'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 SN2022pjq. 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 SN2022pjq 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, SN2022pjq is located at Right Ascension 21:48:58.161 and Declination -26:22:36.88, situated in the constellation Piscis Austrinus (The Southern Fish). Because its declination is -26:22:36.88, it is favorably placed for Southern Hemisphere observatories.

Along this line of sight, the catalog records a Milky Way foreground color excess of E(B−V) = 0.0437 mag (source: Analytical Galactic Disk Model (IAU)), corresponding to roughly A_V ≈ 0.14 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 SN2022pjq. 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 SN2022pjq. 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.

SN2022pjq was officially reported on 2022/07/23 by K. C. Chambers, T. de Boer, J. Bulger, J. Fairlamb, M. Huber, C.-C. Lin, T. Lowe, E. Magnier, A. Schultz, R. J. Wainscoat, M. Willman (IfA, University of Hawaii), K. W. Smith, D. R. Young, O. McBrien, J. Gillanders, S. Srivastav, M. Fulton, S. J. Smartt, D. O'Neill, P. Clark, S. Sim (Queen's University Belfast), D. E. Wright (University of Minnesota). 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 SN2022pjq are compiled from international astronomical notices, the IAU Transient Name Server (TNS), and peer-reviewed astrophysical journals.

Throughout global alert streams and survey databases, SN2022pjq has also been designated as: 2022pjq, PS22ggy, AT2022pjq, ATLAS22xpx, SN 2022pjq, ZTF22aausnwr. 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).

SN2022pjq cannot currently be used for cosmological distance work because its classification is unresolved. The distance ladder relies on type-specific techniques: Type Ia supernovae use the Phillips relation between peak absolute magnitude and decline rate, while Type II events use the Expanding Photosphere Method or SCM-II. An unclassified transient fits neither, so no Hubble-constant constraint can be derived from it until a spectrum establishes its type.

No neutrino or gravitational-wave counterpart has been reported for SN2022pjq, and none is expected to be identifiable without a classification. The multi-messenger signature differs sharply by type: core-collapse events emit a neutrino burst at shock breakout (detected once, for SN 1987A), while thermonuclear Type Ia events produce negligible neutrinos and gravitational waves. Searching for a counterpart before knowing which mechanism applies would be unfocused.

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), SN2022pjq occurred at a distance of 2668.9 Million Light-Years. While historical naked-eye supernovae occurred within our Milky Way or its immediate satellites, modern discoveries like SN2022pjq allow astrophysicists to probe diverse galactic environments, metallicities, and stellar populations across the broader universe.

Unknown — no measured brightness. SN2022pjq was discovered 1566 days ago (2022/07/23), 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 2668.9 Million Light-Years, the inverse-square law dilutes the radiation by quintillions of times, making SN2022pjq completely harmless to our biosphere and purely a fascinating spectacle for human exploration.