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Type — Supernova

The Story of Supernova CSS110130:011755+211320

An extraordinary stellar explosion that occurred Millions of Light-Years away in deep space.

⏱️ ~6 min deep read 🔬 24 Astrophysical Q&As 🔭 Viewing Guide Included 🪐 Constellation Pisces
🔭 Deep Field (~2.1′ FOV) · DSS2 Optical (China-VO mirror)
● CSS110130:011755+211320 Explosion Site

High-magnification deep optical view into CSS110130:011755+211320'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
Millions of Light-Years
Lookback Cosmic Time
✨ Peak Brightness
Mag 19
Large Observatory
☀️ Peak Radiance
Hundreds of Millions of Suns
Combined Stellar Energy
🚀 Shock Velocity
Not measured
No spectral ejecta velocity
🌌 Host Galaxy
Field Transient Host
Center Coincident
🧭 Constellation
Pisces
The Fishes
💥 Explosion Physics
Type —
Core-Collapse Supergiant
📅 Discovered On
2011/01/30
CRTS
CHAPTER I

An Unclassified Astronomical Transient

On 2011/01/30, astronomers scanning the heavens flagged a sudden, violent pinpoint of light that had flared into visibility. Designated CSS110130:011755+211320, it is an unclassified astronomical transient whose physical nature is not yet established.

CSS110130:011755+211320 was reported as a changing source, but it has not been spectroscopically classified. Without a spectrum, the progenitor cannot be identified: a thermonuclear white-dwarf detonation and a core-collapse of a massive star are mutually exclusive histories that produce different spectra and light curves. No progenitor, explosion mechanism, or remnant outcome is established for this object.

Astrophysical Mechanism Summary
Type: Unclassified (no spectrum) • Progenitor: Unknown • Velocity: Not measured
CHAPTER II

A Message Across Deep Cosmic Time

CSS110130:011755+211320 has a luminosity distance of approximately Millions of Light-Years . Lookback time is unavailable without a usable redshift; do not equate luminosity distance with travel time.

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

CHAPTER III

Brightness Record

At the height of the outburst around 2011/01/29, CSS110130:011755+211320 surged to a peak apparent magnitude of 19.

The total energy release is unknown without a spectroscopic classification.

CHAPTER IV

The Radioactive Furnace: Why Supernovae Glow for Months

Without a classification, the power source of CSS110130:011755+211320 cannot be identified; radioactive ⁵⁶Ni decay powers many supernovae but is not established for this transient.

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 CSS110130:011755+211320'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 CSS110130:011755+211320.

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 Pisces

No host galaxy is identified for CSS110130:011755+211320 in this catalog record . In our terrestrial sky, it resides in the constellation Pisces (The Fishes) at Right Ascension 01:17:54.63 and Declination +21:13:20.3.

CHAPTER VII

The Scientific Surveillance Campaign

Following its discovery by CRTS, observatories worldwide swung their lenses toward CSS110130:011755+211320. In the sne.space, CSS110130:011755+211320 is documented across 0 photometric measurements and 0 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? Unknown — no measured brightness.

Discovered 15.8 years ago (2011/01/30). No reliable current brightness estimate — no photometry has been published.

Planetary Safety Note: Even though CSS110130:011755+211320 was a titanic explosion, our planet sits safely outside the lethal 50–100 light-year kill zone. At a distance of Millions of Light-Years, the blast poses zero physical hazard to Earth's biosphere.

🌌 Cosmic Neighbors & Contemporaries 105,868+ transients indexed

Cataloged transients closest to CSS110130:011755+211320 in discovery time, spatial sky neighborhood, and cosmological redshift:

⏱️ Closest in Time
SN2011ab Exploded same day
Type II P 2011/01/30 · Mag 19.3
CSS110130:095426+445811 Exploded same day
Type Transient 2011/01/30 · Mag 16.5
MLS110129:035607+192755 1d before
Type Candidate 2011/01/29
🔭 Closest on the Sky
SN2020sbx 2.6′ away
Type Ia Discovered 2020/08/26
AT2020rzp 12.3′ away
Type Candidate Discovered 2020/08/23
AT2020ong 22.6′ away
Type Candidate Discovered 2020/07/11
🌌 Same Cosmic Era (Redshift)
No redshift match available (target z missing or no comparable redshifts in index).

❓ Frequently Asked Questions About CSS110130:011755+211320

Scientific & observational Q&As indexed from astronomical databases & the sne.space
🔍 24 of 24
What type of supernova is CSS110130:011755+211320 and what kind of star exploded? Astrophysics & Progenitor
CSS110130:011755+211320 has not been spectroscopically classified. It was reported as an astronomical transient, which means an object was detected changing in brightness, but its nature is not yet established. Classification requires a spectrum: the presence or absence of hydrogen lines separates Type II from Type I, and Type Ia is identified by silicon absorption near 6150 Å combined with the absence of hydrogen. Until such a spectrum is published, claims about the progenitor star or explosion mechanism would be speculation. Check the sources below for follow-up spectroscopy.
What was the progenitor star doing in the millions of years leading up to CSS110130:011755+211320? Astrophysics & Progenitor
The progenitor of CSS110130:011755+211320 cannot be identified without a classification. Stellar evolutionary history depends entirely on the explosion type: a Type Ia event would require a carbon-oxygen white dwarf in a binary system, whereas a core-collapse event would require a massive star exhausting its fuel within tens of millions of years. These are mutually exclusive histories that produce different spectra and light curves. No progenitor or precursor has been reported for this transient in the available literature.
How far away is CSS110130:011755+211320 from Earth and how old is the light reaching us? Cosmic Distance & Time
The distance to CSS110130:011755+211320 has not been measured. No spectroscopic redshift or luminosity distance is published for this transient, so neither its distance from Earth nor its lookback time can be stated. A redshift requires a spectrum, and a photometric redshift requires multi-band imaging that has not been reported. Without a distance, its intrinsic luminosity and total energy release are also undetermined. Check the sources below for follow-up spectroscopy or host-galaxy identification.
What does the cosmological redshift of CSS110130:011755+211320 tell us about the expansion of space? Cosmic Distance & Time
No spectroscopic redshift has been measured for CSS110130:011755+211320. Without a published z, its place in the Hubble flow, recession velocity, and lookback time cannot be stated. A redshift requires a spectrum (or a well-calibrated photometric redshift from multi-band imaging). Check the sources below for follow-up spectroscopy.
How bright did CSS110130:011755+211320 become at its peak, and how many Suns does that equal? Explosion Energetics
At peak brightness, CSS110130:011755+211320 achieved an apparent magnitude of 19 around 2011/01/29.
How much total energy was released by CSS110130:011755+211320, and where did that energy go? Explosion Energetics
The total energy released by CSS110130:011755+211320 is unknown. Energy budgets differ by orders of magnitude depending on mechanism: a thermonuclear Type Ia liberates ~10⁵¹ ergs mostly as kinetic energy, while a core-collapse event liberates ~10⁵³ ergs of which ~99% escapes as neutrinos. Without a spectroscopic classification, neither figure applies to this transient.
How fast are the supernova ejecta and shockwave of CSS110130:011755+211320 expanding through space? Explosion Energetics
No ejecta velocity is measured for CSS110130:011755+211320. 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.
What powers the prolonged glow of CSS110130:011755+211320 weeks and months after detonation? Radioactive Engine
The power source sustaining CSS110130:011755+211320 cannot be identified without a classification. Classified supernovae are typically powered after peak by the radioactive decay of ⁵⁶Ni → ⁵⁶Co → ⁵⁶Fe, but nickel yields and whether a shock-breakout flash occurred depend on the explosion mechanism. No spectrum is published for this transient, so no ⁵⁶Ni mass or decay-powered light-curve narrative applies.
What chemical elements did CSS110130:011755+211320 create and disperse into the universe? Nucleosynthesis & Elements
The nucleosynthetic products of CSS110130:011755+211320 are unknown because its type is unresolved. Element yields depend directly on the explosion mechanism: a thermonuclear Type Ia produces mostly iron-peak elements such as 56Ni and 56Fe, whereas a core-collapse event produces large quantities of oxygen, neon, magnesium and silicon from successive burning shells. No spectrum has been published for this transient, so which of these occurred is not established.
Did CSS110130:011755+211320 leave behind a black hole, a neutron star, or nothing at all? Cosmic Remnant
Whether CSS110130:011755+211320 left a remnant is unknown. A thermonuclear Type Ia leaves no compact remnant (the white dwarf is fully disrupted), whereas a core-collapse event leaves a neutron star or black hole depending on progenitor mass. Without a spectroscopic classification, none of these outcomes can be asserted for this transient.
What will CSS110130:011755+211320'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 CSS110130:011755+211320. 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 CSS110130:011755+211320 explode, and where is it located relative to the galactic center? Galactic Environment
No host galaxy is identified for CSS110130:011755+211320 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.
Where is CSS110130:011755+211320 located in the night sky and which constellation is it in? Sky Coordinates
In the celestial sphere, CSS110130:011755+211320 is located at Right Ascension 01:17:54.63 and Declination +21:13:20.3, situated in the constellation Pisces (The Fishes). Because its declination is +21:13:20.3, it is primarily placed in the Northern celestial hemisphere.
How much Milky Way interstellar dust obscures our view of CSS110130:011755+211320? Interstellar Dust
Along this line of sight, the catalog records a Milky Way foreground color excess of E(B−V) = 0.0439 mag (source: published extinction estimate), 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.
Across which photometric filter bands was CSS110130:011755+211320 monitored? Astronomical Observations
No calibrated photometry is published for CSS110130:011755+211320. 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.
What did astronomical spectroscopy reveal about CSS110130:011755+211320's chemical makeup? Astronomical Observations
No spectrum has been published for CSS110130:011755+211320. 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.
Who discovered CSS110130:011755+211320 and how was it first detected? Discovery & History
CSS110130:011755+211320 was officially reported on 2011/01/30 by CRTS. 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 CSS110130:011755+211320? Scientific Research
Data for CSS110130:011755+211320 are compiled from international astronomical notices, the IAU Transient Name Server (TNS), and peer-reviewed astrophysical journals.
What other names and survey identifiers exist for CSS110130:011755+211320? Cross-Identifications
Throughout global alert streams and survey databases, CSS110130:011755+211320 has also been designated as: PSN J01175463+2113204. 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 CSS110130:011755+211320 contribute to measuring the Hubble Constant and the scale of the cosmos? Cosmology & Distance Ladder
CSS110130:011755+211320 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.
Could gravitational waves or neutrinos from CSS110130:011755+211320 be detected on Earth? Multi-Messenger Astronomy
No neutrino or gravitational-wave counterpart has been reported for CSS110130:011755+211320, 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.
How does CSS110130:011755+211320 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), the distance to CSS110130:011755+211320 is not established for a historical comparison (unclassified; no redshift or luminosity distance is published). While historical naked-eye supernovae occurred within our Milky Way or its immediate satellites, modern discoveries like CSS110130:011755+211320 allow astrophysicists to probe diverse galactic environments, metallicities, and stellar populations across the broader universe.
Can I see CSS110130:011755+211320 tonight with a backyard telescope or binoculars? Backyard Observation
Unknown — no measured brightness. CSS110130:011755+211320 was discovered 5768 days ago (2011/01/30), 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 CSS110130:011755+211320 pose any threat to Earth? Planetary Safety
Earth is in no danger from CSS110130:011755+211320. The astrophysical 'lethal kill zone' for a supernova to damage our ozone layer is roughly 50 to 100 light-years. This transient is far outside the solar neighbourhood: it was discovered by a wide-field survey at a magnitude only reachable for an extragalactic object, and any transient in our own galaxy within that radius would have appeared far brighter than the ~18th magnitude reported here. Its exact distance is unmeasured, but the detection brightness alone rules out any nearby threat.
Data sourced from IAU TNS, ALeRCE, WISeREP, and the sne.space. View All General Astrophysics FAQs →
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