SN2016C: What Happened, Distance & Viewing Guide

Q: What type of supernova is SN2016C and what kind of star exploded?

SN2016C is classified as a Type II supernova, consistent with core collapse of a massive star that retained hydrogen in its outer envelope. Typical progenitor mass ranges quoted for the class are model expectations, not a measured mass for this star.

Q: What was the progenitor star doing in the millions of years leading up to SN2016C?

The specific progenitor of SN2016C 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 SN2016C.

Q: How far away is SN2016C from Earth and how old is the light reaching us?

SN2016C has a luminosity distance of approximately 65.5 Million Light-Years (redshift z = 0.00452, d_L = 20.07). Under a flat ΛCDM cosmology (H₀≈70 km/s/Mpc, Ωₘ≈0.3), the corresponding lookback time is ≈63 Myr — when the light set out 62.9 million years ago during the early Cenozoic era, following the extinction of the non-avian dinosaurs. Luminosity distance is larger than the light-travel distance because cosmic expansion stretches the path; the two must not be equated.

Q: What does the cosmological redshift of SN2016C tell us about the expansion of space?

SN2016C exhibits a measured spectroscopic redshift of z = 0.0045. The cockpit reports a user-facing recession velocity of 1,352.0 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 (≈1,355 km/s) is a different low-z approximation and is not mixed here.

          🔭 Deep Field (~2.1′ FOV) · DSS2 Optical (China-VO mirror)
        

● SN2016C Explosion Site

High-magnification deep optical view into SN2016C's host environment. Pan and scroll to explore the cosmic neighborhood where this star exploded.

⚡ Quick Observer Facts & Telemetry

IAU Transients DB

🌐 Distance to Earth

65.5 Million Light-Years

Lookback Cosmic Time

✨ Peak Brightness

Mag 14.9

Astro Camera (CCD)

☀️ Peak Radiance

376.7 million Suns

Combined Stellar Energy

🚀 Shock Velocity

~1,350 km/s

~0.5% Speed of Light

🌌 Host Galaxy

NGC 5247

Center Coincident

🧭 Constellation

Virgo

The Maiden

💥 Explosion Physics

Type II P

Core-Collapse Supergiant

📅 Discovered On

2016/01/03

Masakatsu Aoki

CHAPTER I

A Core-Collapse Class Transient

On 2016/01/03, astronomers scanning the heavens flagged a sudden, violent pinpoint of light that had flared into visibility. Designated SN2016C, it represents a catastrophic stellar explosion classified as a Type II P supernova.

SN2016C is classified in a core-collapse spectroscopic family. Events of this class are generally linked to the death of a massive star after successive nuclear burning stages, but no unique progenitor mass, lifetime, or pre-explosion identification is established for this object. The narrative of onion-shell fusion ending in iron-core collapse describes the class model, not a measured biography of SN2016C.

Astrophysical Mechanism Summary

Type: Type II P • Progenitor: Massive Red/Stripped Supergiant Star • Velocity: ~1,350 km/s (~0.5% c)

CHAPTER II

A Message Across Deep Cosmic Time

SN2016C has a luminosity distance of approximately 65.5 Million Light-Years (redshift z = 0.00452). That figure is not the light-travel time: under flat ΛCDM the lookback time is ≈63 Myr, when the light set out 62.9 million years ago during the early Cenozoic era, following the extinction of the non-avian dinosaurs.

Luminosity distance incorporates cosmic expansion and exceeds the light-travel distance. The two quantities must be reported separately.

CHAPTER III

Incandescence of 376.7 million Suns

At the height of the outburst around 2016/01/03, SN2016C surged to a peak apparent magnitude of 14.9 and an intrinsic absolute magnitude of -16.61. At that instant, this single dying star radiated with the collective power of approximately 376.7 million Suns combined, outshining whole dwarf galaxies.

The total energy released by the cataclysm was on the order of 10⁵¹ to 10⁵³ ergs. Over 99% of this energy was emitted within the first 10 seconds as a dense burst of trillions of neutrinos, with only 1% driving the visible blast wave.

CHAPTER IV

The Radioactive Furnace: Why Supernovae Glow for Months

After peak, many supernovae are powered by the radioactive chain ⁵⁶Ni → ⁵⁶Co → ⁵⁶Fe. That is the standard model for Type II P light curves; an object-specific nickel mass for SN2016C is not published here.

Nickel-56 decays to Cobalt-56 (half-life ≈6.1 days), then to stable Iron-56 (half-life ≈77.2 days), heating the ejecta from within. Typical class yields must not be quoted as measured values for this event.

CHAPTER V

Cosmic Kiln: Seeding the Elements of Life

Supernovae enrich galaxies with heavy elements. Events of SN2016C's class are associated with oxygen-group and intermediate-mass products (O, C, Ne, Mg, Si) in galactic chemical-evolution models. No measured elemental yields are published for SN2016C.

As Carl Sagan observed, "We are made of star-stuff" — a statement about nucleosynthesis in general, not a claim that atoms from this specific remnant are identified in the Solar System.

CHAPTER VI

Galactic Setting in Virgo

SN2016C is associated with cataloged host NGC 5247 . In our terrestrial sky, it resides in the constellation Virgo (The Maiden) at Right Ascension 13:38:05.30 and Declination -17:51:15.3.

CHAPTER VII

The Scientific Surveillance Campaign

Following its discovery by Masakatsu Aoki, observatories worldwide swung their lenses toward SN2016C. In the sne.space, SN2016C is documented across 31 photometric measurements in passbands such as B, U, UVM2, UVW1, UVW2, V and 3 spectroscopic epochs. These multi-wavelength observations allow astrophysicists to model the expanding photosphere, measure shock velocities, and probe circumstellar interactions.

CHAPTER VIII

Stargazer's Field Guide: Can You See It Tonight?

Can I see it tonight? No reliable current brightness estimate.

Discovered 3969 days ago (2016/01/03). Cataloged peak 2016/01/03 (3969d ago; rest-frame phase +3951.1d). Cataloged/observed peak: m = 14.90 on 2016/01/03. Latest observed: m = 19.72 on 2016/01/13 (MJD 57400.4).

No reliable current brightness estimate — no event-specific brightness fit with documented uncertainty is published for this object. Class-average decay templates are not used as object-specific predictions. Latest observed magnitude: m = 19.72 on 2016/01/13 (MJD 57400.4). Current brightness trend is unknown (last observation 2016/01/13 (MJD 57400.4); same-band recent pair unavailable or stale).

Instrument Class & Aperture	Sensitivity Limit	Cataloged Peak (m=14.90 on 2016/01/03)	Current Brightness Tonight
Naked Eye Dark sky site (Bortle 1–3) with no optical aid	m ≤ 6.0	Requires larger aperture (limit m ≤ 6.0)	No reliable estimate
Binoculars (50mm) Standard 7x50 or 10x50 handheld binoculars	m ≤ 9.5	Requires larger aperture (limit m ≤ 9.5)	No reliable estimate
Small Backyard Scope (4" / 100mm) Entry 4-inch (100mm) refractor / reflector	m ≤ 12.0	Requires larger aperture (limit m ≤ 12.0)	No reliable estimate
Medium Amateur Scope (8"–12") 8-inch to 12-inch Dobsonian or Schmidt-Cassegrain	m ≤ 14.5	Requires larger aperture (limit m ≤ 14.5)	No reliable estimate
Amateur CMOS Rig Cooled monochrome/color CMOS camera with multi-hour stack	m ≤ 19.5	✅ Reachable	No reliable estimate
2m–3m Research Telescope University or regional observatory (e.g. Palomar 60", Calar Alto)	m ≤ 22.0	✅ Reachable	No reliable estimate
Giant 8m–10m Observatories Keck (10m), VLT (8.2m), Gemini, Subaru optical imaging	m ≤ 25.0	✅ Reachable	No reliable estimate
Space Observatories Only Hubble Space Telescope (WFC3) / JWST (NIRCam deep stack)	m ≤ 30.0	✅ Reachable	No reliable estimate

Planetary Safety Note: Even though SN2016C was a titanic explosion, our planet sits safely outside the lethal 50–100 light-year kill zone. At a distance of 65.5 Million Light-Years, the blast poses zero physical hazard to Earth's biosphere.

🌌 Cosmic Neighbors & Contemporaries 105,868+ transients indexed

Cataloged transients closest to SN2016C in discovery time, spatial sky neighborhood, and cosmological redshift:

⏱️ Closest in Time

ASASSN-16ab Exploded same day

Type II 2016/01/03

OGLE16aad Exploded same day

Type Candidate 2016/01/03 · Mag 19.44

CSS160103:005059-020914 Exploded same day

Type Transient 2016/01/03 · Mag 19.5

🔭 Closest on the Sky

SNhunt141 3.7′ away

Type II P Discovered 2012/07/24

AT2020oub 19.1′ away

Type Candidate Discovered 2020/04/27

GRB 161224A 19.9′ away

Type LGRB Discovered 2016/12/24

🌌 Same Cosmic Era (Redshift)

SN2019np z = 0.00452

Type Ia ~61.9 Mly (approx.)

SN1993Z z = 0.00452

Type Ia ~61.9 Mly (approx.)

SN2024inv z = 0.004528

Type Ia ~62.0 Mly (approx.)

❓ Frequently Asked Questions About SN2016C

Scientific & observational Q&As indexed from astronomical databases & the sne.space

What type of supernova is SN2016C and what kind of star exploded? Astrophysics & Progenitor

SN2016C is classified as a Type II supernova, consistent with core collapse of a massive star that retained hydrogen in its outer envelope. Typical progenitor mass ranges quoted for the class are model expectations, not a measured mass for this star.

What was the progenitor star doing in the millions of years leading up to SN2016C? Astrophysics & Progenitor

The specific progenitor of SN2016C 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 SN2016C.

How far away is SN2016C from Earth and how old is the light reaching us? Cosmic Distance & Time

SN2016C has a luminosity distance of approximately 65.5 Million Light-Years (redshift z = 0.00452, d_L = 20.07). Under a flat ΛCDM cosmology (H₀≈70 km/s/Mpc, Ωₘ≈0.3), the corresponding lookback time is ≈63 Myr — when the light set out 62.9 million years ago during the early Cenozoic era, following the extinction of the non-avian dinosaurs. Luminosity distance is larger than the light-travel distance because cosmic expansion stretches the path; the two must not be equated.

What does the cosmological redshift of SN2016C tell us about the expansion of space? Cosmic Distance & Time

SN2016C exhibits a measured spectroscopic redshift of z = 0.0045. The cockpit reports a user-facing recession velocity of 1,352.0 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 (≈1,355 km/s) is a different low-z approximation and is not mixed here.

How bright did SN2016C become at its peak, and how many Suns does that equal? Explosion Energetics

At peak brightness, SN2016C achieved an apparent magnitude of 14.9 around 2016/01/03. Corrected for cosmic distance and foreground interstellar dust, its intrinsic absolute magnitude was -16.61. At this peak, the exploding star radiated with the incandescent brilliance of approximately 376.7 million Suns combined, briefly outshining the cumulative starlight of entire dwarf galaxies!

How much total energy was released by SN2016C, and where did that energy go? Explosion Energetics

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 SN2016C.

How fast are the supernova ejecta and shockwave of SN2016C expanding through space? Explosion Energetics

Spectroscopic line blueshifts imply an ejecta velocity of approximately 1,350 km/s (~0.5% of c) for SN2016C. This is distinct from cosmological recession velocity inferred from redshift.

What powers the prolonged glow of SN2016C weeks and months after detonation? Radioactive Engine

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 SN2016C. 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.

What chemical elements did SN2016C create and disperse into the universe? Nucleosynthesis & Elements

Events of SN2016C'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 SN2016C.

Did SN2016C leave behind a black hole, a neutron star, or nothing at all? Cosmic Remnant

A core-collapse explosion associated with SN2016C'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.

What will SN2016C's explosion site look like in 1,000 to 10,000 years? Cosmic Remnant

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 SN2016C. 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.

In which galaxy did SN2016C explode, and where is it located relative to the galactic center? Galactic Environment

SN2016C is cataloged with host galaxy NGC 5247. No secure nuclear offset is published in this record.

Where is SN2016C located in the night sky and which constellation is it in? Sky Coordinates

In the celestial sphere, SN2016C is located at Right Ascension 13:38:05.30 and Declination -17:51:15.3, situated in the constellation Virgo (The Maiden). Because its declination is -17:51:15.3, it is favorably placed for Southern Hemisphere observatories.

How much Milky Way interstellar dust obscures our view of SN2016C? Interstellar Dust

Along this line of sight, the catalog records a Milky Way foreground color excess of E(B−V) = 0.0767 mag (source: 3,6), corresponding to roughly A_V ≈ 0.24 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.

Across which photometric filter bands was SN2016C monitored? Astronomical Observations

SN2016C was tracked across 31 photometric observations across a baseline of 9.9 days utilizing filter bands including B, U, UVM2, UVW1, UVW2, V. Data were captured by observatories and survey networks including Swift. Multi-color photometry tracks the temperature evolution of the fireball, verifying the rise time to peak and the rate of radioactive decline.

What did astronomical spectroscopy reveal about SN2016C's chemical makeup? Astronomical Observations

Astronomers obtained 3 spectroscopic epochs for SN2016C from 3600.0 Å to 9287.3 Å. Optical spectroscopy provides the definitive physical fingerprint of the transient: P-Cygni line profiles reveal the expansion speed of the ejecta, while characteristic absorption features (such as hydrogen Balmer lines Hα/Hβ in Type II, or Si II λ6355 in Type Ia) identify the stellar composition and physical mechanism of the explosion.

Who discovered SN2016C and how was it first detected? Discovery & History

SN2016C was officially reported on 2016/01/03 by Masakatsu Aoki. 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.

How many scientific publications and observatories have contributed data to SN2016C? Scientific Research

SN2016C is documented across 7 scientific references and archival data sources in the sne.space. These include discovery circulars and research datasets from 2016A&A...594A..13P, SOUSA, 2011ApJ...737..103S, Transient Name Server. All raw photometry and spectroscopy points are cross-indexed to their original bibliographic records for peer-reviewed verification.

What other names and survey identifiers exist for SN2016C? Cross-Identifications

Throughout global alert streams and survey databases, SN2016C has also been designated as: AT2016C. 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).

How does SN2016C contribute to measuring the Hubble Constant and the scale of the cosmos? Cosmology & Distance Ladder

As a core-collapse supernova, SN2016C 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.

Could gravitational waves or neutrinos from SN2016C be detected on Earth? Multi-Messenger Astronomy

Core-collapse supernovae like SN2016C 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.

How does SN2016C compare to famous historical supernovae like SN 1987A or the Crab Supernova? Historical Comparison

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), SN2016C occurred at a distance of 65.5 Million Light-Years. While historical naked-eye supernovae occurred within our Milky Way or its immediate satellites, modern discoveries like SN2016C allow astrophysicists to probe diverse galactic environments, metallicities, and stellar populations across the broader universe.

Can I see SN2016C tonight with a backyard telescope or binoculars? Backyard Observation

Unknown — no measured brightness. SN2016C was discovered 3969 days ago (2016/01/03), 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.

Does the radiation or shockwave from SN2016C pose any threat to Earth? Planetary Safety

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 65.5 Million Light-Years, the inverse-square law dilutes the radiation by quintillions of times, making SN2016C completely harmless to our biosphere and purely a fascinating spectacle for human exploration.

Data sourced from IAU TNS, ALeRCE, WISeREP, and the sne.space. View All General Astrophysics FAQs →

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The Story of Supernova SN2016C