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Supernova SN 185
Infrared images from NASA's Spitzer Space Telescope and WISE are combined with X-ray data from the Chandra X-ray Observatory and ESA's XMM-Newton Observatory in this image of RCW 86.
Event typeSupernova remnant, supernova Edit this on Wikidata
Type Ia?
Date7 December 185
ConstellationCircinus and Centaurus
Right ascension14h 43m
Declination−62° 30′
EpochJ2000
Galactic coordinatesG315.4−2.3
Distance2,800 pc (9,100 ly)[1]
RemnantShell
HostMilky Way
Notable featuresAncient records of SN 185 may be the earliest written description of a supernova.
Peak apparent magnitude"as much as −8"[2]
Other designationsSN 185, SNR G315.0-02.3, SNR G315.4-02.3, 1ES 1436-62.4, 1RXS J144254.3-622815, 3FHL J1443.0-6227e, AJG 27, 3A 1438-626, GPS 1438-624, MSH 14-6-03, 2FHL J1443.2-6221e
Preceded byNone known
Followed bySN 386
[edit on Wikidata]

SN 185 was a transient astronomical event observed in the year AD 185, likely a supernova. The transient occurred in the direction of Alpha Centauri, between the constellations Circinus and Centaurus, centered at RA 14h 43m Dec −62° 30′, in Circinus. This "guest star" was observed by Chinese astronomers in the Book of Later Han (後漢書),[3] and might have been recorded in Roman literature.[2] It remained visible in the night sky for eight months. This is believed to be the first supernova for which records exist.

History

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The Book of Later Han gives the following description:

In the 2nd year of the epoch Zhongping [中平], the 10th month, on the day Guihai [癸亥] [December 7, Year 185], a 'guest star' appeared in the middle of the Southern Gate [南門] [an asterism consisting of ε Centauri and α Centauri], The size was half a bamboo mat. It displayed various colors, both pleasing and otherwise.[4] It gradually lessened. In the 6th month of the succeeding year it disappeared.[5]

The gaseous shell RCW 86 is probably the supernova remnant of this event and has a relatively large angular size of roughly 45 arc minutes[1] (larger than the apparent size of the full moon, which varies from 29 to 34 arc minutes). The distance to RCW 86 is estimated to be 2,800 parsecs (9,100 light-years).[1] Recent X-ray studies show a good match for the expected age.[6]

Infrared observations from NASA's Spitzer Space Telescope and Wide-field Infrared Survey Explorer (WISE) reveal how the supernova occurred and how its shattered remains ultimately spread out to great distances. The findings show that the stellar explosion took place in a hollowed-out cavity, allowing material expelled by the star to travel much faster and farther than it would have otherwise.[7]

Differing modern interpretations of the Chinese records of the guest star have led to quite different suggestions for the astronomical mechanism behind the event, from a core-collapse supernova[7] to a distant, slow-moving comet[8] – with correspondingly wide-ranging estimates of its apparent visual magnitude (−8 to +4). The recent Chandra results suggest that it was most likely a Type Ia supernova (a type with consistent absolute magnitude),[7][9] and therefore similar to Tycho's Supernova (SN 1572), which had apparent magnitude −4 at a similar distance.

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See also

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References

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Revisions and contributorsEdit on WikipediaRead on Wikipedia

SN 185

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SN 185 was a Type Ia supernova that exploded approximately 8,000 light-years from Earth in 185 CE, observed by ancient Chinese astronomers as a bright "guest star" emerging on December 7 within the Southern Gate asterism near Alpha Centauri in the modern constellations of Centaurus and Circinus. The event was recorded in the Houhanshu as a scintillating, multicolored object about half a yan (roughly 0.4–1 degree) in apparent size, which faded gradually and remained visible for at least eight months until mid-186 CE. At its peak, the supernova's brightness was estimated at –7 to –8.8 magnitude, making it one of the most luminous celestial events recorded in antiquity and comparable to Mars in the night sky. As the earliest documented supernova in human history, SN 185 provides critical insights into the behavior of Type Ia explosions, which occur when a white dwarf in a binary system accretes sufficient mass from a companion star to trigger thermonuclear detonation. The resulting remnant, RCW 86, is a shell-like structure spanning about 45 arcminutes in angular size, expanding at a high velocity of approximately 70–120 km/s, consistent with its young age of around 1,800 years as seen from Earth. Multi-wavelength observations reveal RCW 86 emitting in optical, radio, X-ray, and gamma-ray bands, with X-ray spectra showing iron lines indicative of Type Ia nucleosynthesis and synchrotron emission from shock-accelerated cosmic rays interacting with the surrounding medium. The remnant's morphology suggests the supernova detonated within a wind-blown bubble carved by the progenitor system's mass loss, influencing its rapid expansion and low-density environment. Recent imaging, such as the 2023 Dark Energy Camera (DECam) mosaic on the Víctor M. Blanco 4-meter Telescope, has captured the full extent of RCW 86's filamentary structure, highlighting its irregular ring of glowing gas and dust while confirming its association with SN 185 through proper motion measurements. In 2025, SDSS-V Local Volume Mapper observations provided new insights into collisionless shocks in the remnant. This historical event underscores the value of ancient records in calibrating modern astrophysical models, as SN 185's light curve and spectrum—reconstructed from the remnant—align with standard Type Ia templates used as "standard candles" for measuring cosmic distances. Ongoing studies of RCW 86, including gamma-ray detections by instruments like Fermi-LAT, explore particle acceleration and the remnant's role in galactic cosmic ray production.

Historical Observations

Chinese Astronomical Records

The primary ancient documentation of SN 185 comes from Chinese astronomical annals, where it is described as a "guest star" (kexing) that appeared on December 7, 185 AD, within the Southern Gate asterism (Nanmen), corresponding to a position near Alpha Centauri. This event was recorded in the Hou Hanshu (Book of the Later Han), the official history of the Later Han dynasty (25–220 AD), compiled in the 5th century but drawing on contemporary court observations. The record notes the star's sudden emergence without any preceding tail or motion, distinguishing it from comets, which were typically described with brooms or directional movement in Chinese texts. The Hou Hanshu provides a detailed textual account: "In the second year of the Zhongping reign period, the tenth month, on a Guihai day (December 7, AD 185), a ‘guest star’ emerged within the Southern Gate... It seemed to be as large as half a yan, with scintillating, variegated colors, and it then grew smaller, until in the sixth month of the following year... it disappeared." This describes an initial brightness comparable to Mars, making it highly conspicuous in the southern sky, and a gradual fading over approximately eight months, with visibility ceasing around July 186 AD. No additional records from other Chinese annals, such as the Jinshu or Korean sources, corroborate this event, underscoring the Hou Hanshu as the sole primary source. In the context of during the , such guest stars were systematically observed by imperial court astronomers, who maintained detailed records as part of their duties to monitor celestial omens . These phenomena were interpreted through correlative cosmology, where appearances in specific asterisms like Nanmen—associated with southern regions and gates of the imperial palace—could signal political instability, military threats, or changes in the , though no explicit prognostic interpretation is attached to this particular record in the Hou Hanshu.

Roman and Other Accounts

Historical accounts of the supernova SN 185 from Roman sources are scarce and indirect, contrasting sharply with the detailed Chinese records. Two potential references appear in Western literature from the period. In the History of Herodian, written around 250 AD, a description notes: "There were certain portents which coincided with these events; some stars shone continuously by day, others became elongated and seemed to hang in the middle of the sky." This passage, dated uncertainly between 184 and 188 AD, may allude to the event during the reign of Emperor Commodus (180–192 AD), though the timing and specificity remain ambiguous, possibly conflating multiple celestial phenomena. Another possible mention occurs in the , a fourth-century collection, in the Vita Commodi: "Before the war of the deserters the heavens were ablaze." This account, drawing from earlier sources like or Marius Maximus, describes fiery skies as an , but its reliability is questioned due to the text's late composition and potential displacement of events. No direct Roman astronomical observations confirm the , reflecting the absence of systematic sky monitoring in the , unlike the imperial Chinese astronomical bureaus. The lack of detailed records extends to other non-Chinese civilizations, such as Indian astronomers, where no contemporary mentions of a guest star in 185 AD have been identified in surviving texts like the Surya Siddhanta or Jyotisha works. This scarcity may stem from cultural priorities, with Roman and Indian writings emphasizing omens or astrology over precise celestial catalogs for transient events. Additionally, the supernova's position in the southern constellation Centaurus, at a declination of approximately -62°, rendered it invisible from much of the Mediterranean world, including Italy and Gaul, where it would have appeared below the horizon. Visibility was marginal at best from southern outposts like Alexandria or Carthage, limiting opportunities for observation in northern latitudes. Overall, the historical reliability of these Western allusions is low, as they lack the positional and durational details found in Eastern documentation, underscoring the event's primary confirmation through Chinese records. Textual ambiguities, combined with the geographic constraints, explain why SN 185 was not widely noted in Roman or other Mediterranean sources, despite its brightness.

The Supernova Event

Visibility and Duration

The guest star associated with SN 185 first appeared on December 7, 185 CE, as documented in Chinese astronomical records from the imperial observatory at Lo-Yang. It was positioned in the southern sky between the constellations Centaurus and Circinus, near Alpha Centauri, within the Southern Gate asterism. The modern position of the remnant is at a declination of approximately -62 degrees, but due to precession, the historical coordinates in 185 CE corresponded to a higher declination (around -40° to -45°), allowing visibility from northern latitudes including China. At its peak, the supernova exhibited an estimated of -7 to -8, rendering it one of the brightest celestial objects visible to the , potentially observable even in twilight under clear conditions. It remained visible for approximately 8 months, gradually dimming without reported positional variability until fading by mid-186 CE. Historical accounts described it as a scintillating, multicolored object, features that aligned with a rather than a or nova.

Estimated Physical Characteristics

SN 185 is classified as a Type Ia supernova based on the chemical composition of its remnant, which shows an abundance of iron-group elements indicative of a thermonuclear detonation of a white dwarf, as well as the historical light curve derived from ancient records that matches the characteristic decline time of Type Ia events. X-ray observations reveal shocked ejecta rich in iron, a signature of the explosive nucleosynthesis in Type Ia supernovae, distinguishing it from core-collapse types that produce more oxygen and less iron. The peak luminosity of SN 185 is estimated at approximately 10910^9 solar luminosities (L⊙L_\odot), aligning with the standard of Type Ia supernovae, which serve as reliable distance indicators due to their consistent peak output. This value is inferred from the event's historical apparent and the distance to the remnant (about 2.5 kpc), combined with models of Type Ia light curves powered by . The progenitor system is believed to be a carbon-oxygen white dwarf in a binary configuration that accreted mass from a companion until reaching the Chandrasekhar limit of approximately 1.4 solar masses (M⊙M_\odot), triggering a thermonuclear runaway explosion. Evidence from hydrodynamic simulations of the remnant supports a single-degenerate scenario, where the white dwarf's wind carved a low-density cavity prior to detonation. The explosion released roughly 104410^{44} joules in kinetic energy, typical for Type Ia events, with the ejecta expanding at velocities exceeding 3000 km/s in parts of the remnant. The light curve was powered by the radioactive decay of nickel-56 (56^{56}Ni) produced in the explosion, decaying to cobalt-56 and then iron-56, providing the energy for the observed luminosity over months.

Supernova Remnant

Identification with RCW 86

The identification of the supernova remnant RCW 86 with the historical event SN 185 was first proposed in 1977 by astronomers David H. Clark and F. Richard Stephenson, based on the positional coincidence of the remnant with the recorded location of the 185 AD transient near the stars Alpha and Beta Centauri. This initial association relied on historical Chinese astronomical records placing the guest star in the southern sky region encompassing the modern-day remnant, which spans about 45 arcminutes in diameter. Confirmation of this link came in the early 2000s through advanced X-ray observations that revealed spectral signatures consistent with a Type Ia supernova explosion. High-resolution X-ray spectroscopy from instruments aboard Chandra and XMM-Newton detected prominent emission lines of intermediate-mass elements such as silicon (Si) and sulfur (S), which are characteristic ejecta from the thermonuclear detonation of a white dwarf star in a binary system—hallmarks of Type Ia events. These observations, detailed in studies from 2006 onward, provided chemical evidence aligning RCW 86 with SN 185, distinguishing it from core-collapse supernovae that produce more oxygen and heavier metals. The distance to RCW 86 has been estimated at approximately 2,500 parsecs (about 8,000 light-years) from Earth, determined through multiple methods including X-ray absorption by interstellar dust and gas along the line of sight, which indicates the column density of material intervening between the remnant and observer. Complementary distance constraints come from expansion parallax measurements, where proper motions of optical H-alpha filaments tracked over time yield a tangential expansion velocity when combined with the assumed distance, supporting the 2.5 kpc value. This distance enables calculation of the remnant's dynamical age, estimated at 1,800 to 2,000 years from modeling its expansion into a low-density cavity, consistent with the approximately 1,840 years since SN 185 (as of 2025). This resolves prior discrepancies where earlier expansion measurements suggested an age of 10,000 years or more due to underestimated shock speeds in the low-density circumstellar environment. The high-velocity shocks, inferred from non-thermal X-ray emission, indicate the supernova expanded into a pre-existing cavity, allowing faster dynamical evolution than typical interactions.

Morphology and Expansion History

RCW 86 exhibits a large shell-type morphology, spanning approximately 45 arcminutes in diameter, with irregular and tattered edges arising from interactions between the blast wave and the surrounding interstellar medium. Expansion measurements indicate shock velocities of 600–1500 km/s from Doppler shifts in optical emission lines and proper motions of Hα filaments corresponding to 700–2200 km/s (average ~1200 km/s at 2.5 kpc), with regional variations such as higher values (~2000 km/s) in the northeast. These are consistent with the dynamics of a young supernova remnant expanding into a low-density cavity. The remnant has evolved into the Sedov-Taylor phase in regions interacting with denser material, during which remains negligible and the shock front primarily sweeps up and compresses ambient interstellar gas, driving the overall expansion. Morphological asymmetries, such as the elongated filament in the northeast region, likely stem from an off-center explosion within a low-density cavity or inhomogeneous density distributions in the ambient medium.

Modern Astronomical Studies

Multi-Wavelength Observations

Multi-wavelength observations of the supernova remnant RCW 86 have revealed a complex structure shaped by interactions between the supernova ejecta and the surrounding interstellar medium, with emissions spanning the electromagnetic spectrum providing insights into the shock dynamics and particle populations. X-ray observations conducted with the Chandra X-ray Observatory and XMM-Newton telescope have identified hot plasma components indicative of shocked material, with temperatures reaching kT ≈ 1 keV in the high-temperature ejecta regions. Spectral analysis shows prominent emission lines from iron (Fe Kα at ~6.4 keV) and silicon (Si K), consistent with reverse-shocked Type Ia supernova ejecta enriched in these elements. Recent Imaging X-ray Polarimetry Explorer (IXPE) observations have measured polarized X-ray emission from RCW 86, revealing details of the magnetic field structure in the remnant's shocks. In the optical and infrared regimes, the Dark Energy Camera (DECam) on the Víctor M. Blanco 4-meter Telescope captured a 2023 image spanning approximately 45 arcminutes, depicting a tattered shell of glowing debris with prominent filaments outlining the remnant's structure and evidence of intervening dust lanes. Hα emission lines trace the shocked ionized gas in these filaments, highlighting regions of radiative cooling and interaction with dense clouds. Radio observations using the Australia Telescope Compact Array (ATCA) at frequencies around 1.4 GHz have mapped the remnant's shell morphology, revealing non-thermal synchrotron emission arising from relativistic electrons spiraling in the magnetic field at the shock front. The emission exhibits a smooth, radially oriented magnetic field configuration, supporting diffusive shock acceleration processes. Gamma-ray observations with the High Energy Stereoscopic System (H.E.S.S.) have detected TeV emission primarily from the remnant's shell, showing a strong spatial correlation with interstellar atomic gas and indicating hadronic interactions from cosmic rays accelerated at the shock. This TeV signal confirms RCW 86 as a site of efficient particle , with energies comparable to those in other young supernova remnants.

Scientific Significance and Debates

SN 185 is recognized as the oldest confirmed historical supernova, documented in ancient Chinese records from 185 CE, offering a critical benchmark for the light curves of Type Ia supernovae due to its reported visibility duration of approximately eight months, which aligns with the characteristic decline phase observed in modern Type Ia events. This historical data, combined with the identification of its remnant RCW 86, provides insights into the early evolutionary stages of Type Ia supernova remnants, including shell formation and interaction with circumstellar material in a wind-blown bubble environment. As a confirmed Type Ia explosion, SN 185 exemplifies the thermonuclear disruption of a white dwarf, serving as a reference for calibrating models of peak luminosity and spectral evolution in these events. Studies of RCW 86 have advanced research by demonstrating efficient particle acceleration at supernova shocks, with non-thermal emission indicating electrons energized to multi-keV levels and broader evidence suggesting protons can reach energies up to the PeV regime, consistent with Galactic origins. Observations reveal that pressure exceeds thermal gas pressure in parts of the remnant, underscoring the role of young Type Ia remnants like RCW 86 in injecting high-energy particles into the . A key debate surrounds the age of RCW 86, initially estimated at around 10,000 years based on its angular size and assumed expansion rates, but later refined to approximately 2,000 years through measurements and high-velocity detections that match the timing of SN 185. This revision relies on expansion velocities exceeding 500 km/s in certain regions, though uncertainties in distance—estimated between 0.7 and 2.5 kpc—continue to fuel discussions on the remnant's dynamical history and progenitor environment. The inclusion of SN 185 among the few reliably recorded Galactic supernovae bolsters estimates of the Milky Way's supernova rate at 2–3 events per century, informing nucleosynthesis models where Type Ia contributions dominate the production of iron-peak elements like nickel and iron. This rate, derived from historical events and remnant statistics, constrains the frequency of white dwarf disruptions and their impact on Galactic chemical enrichment.

References

  1. https://noirlab.edu/public/news/noirlab2307/
  2. https://www.raa-journal.org/issues/all/2006/v6n5/202203/P020220325535227510034.pdf
  3. https://chandra.harvard.edu/resources/flash/historic_supernovas.html
  4. https://iopscience.iop.org/article/10.1088/0004-637X/741/2/96
  5. https://arxiv.org/abs/2507.08257
  6. https://www.aanda.org/articles/aa/full_html/2012/09/aa19896-12/aa19896-12.html
  7. https://academic.oup.com/book/8331/chapter/153982895
  8. https://press.uchicago.edu/books/hoc/HOC_V2_B2/HOC_VOLUME2_Book2_chapter13.pdf
  9. https://www.giss.nasa.gov/pubs/docs/1977/1977_Stothers_st07810a.pdf
  10. https://www.scirp.org/journal/paperinformation?paperid=107638
  11. https://www.researchgate.net/publication/6071888_A_Revisit_to_the_Guest_Star_of_AD_185
  12. http://spider.seds.org/spider/Misc/sn0185.html
  13. https://www.nasa.gov/image-article/oldest-recorded-supernova/
  14. https://arxiv.org/abs/1108.1207
  15. https://arxiv.org/abs/1404.5434
  16. https://arxiv.org/abs/2411.09740
  17. https://arxiv.org/abs/2412.01766
  18. https://arxiv.org/pdf/astro-ph/9709117
  19. https://arxiv.org/abs/astro-ph/0607307
  20. https://iopscience.iop.org/article/10.1086/507628
  21. https://www.esa.int/Science_Exploration/Space_Science/New_evidence_links_stellar_remains_to_oldest_recorded_supernova
  22. https://arxiv.org/abs/1306.3994
  23. https://www.mpi-hd.mpg.de/HESS/pages/home/som/2016/02/
  24. https://academic.oup.com/mnras/article/441/4/3040/1203244
  25. http://adsabs.harvard.edu/full/1989ApJ...337..399C
  26. https://pos.sissa.it/482/044/
  27. https://noirlab.edu/public/images/noirlab2307a/
  28. https://ui.adsabs.harvard.edu/abs/2013MNRAS.435..910H/abstract
  29. https://www.researchgate.net/publication/231153867_The_Radio_Structure_of_the_Supernova_Remnant_G3154-23_MSH_14-63
  30. https://www.aanda.org/articles/aa/pdf/2003/14/aa2975.pdf
  31. https://arxiv.org/abs/1805.10647
  32. https://iopscience.iop.org/article/10.3847/1538-4357/ab108f
  33. https://ui.adsabs.harvard.edu/abs/1993ComAp..17..125V/abstract
  34. https://ui.adsabs.harvard.edu/abs/1994ApJS...92..487T/abstract
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