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'''SN 1999em''' was a well-observed<ref name=Elmhamdi_et_al_2003/> ] in the ] ],<ref name=SIMBAD/> which lies within the mostly southern ] of ]. Using a corrected version of the expanding photosphere method (EPM), the distance to the supernova is estimated as {{convert|11.5|±|1|Mpc|e6ly|order=flip|abbr=out|link=on}}.<ref name=Dessart_Hillier_2006/> This is in good agreement with the ] method, which yields a distance of {{convert|11.71|±|0.92|Mpc|e6ly|order=flip|abbr=out|link=on}}.<ref name=Leonard_et_al_2003/> '''SN 1999em''' was a well-observed<ref name=Elmhamdi_et_al_2003/> ] in the ] ],<ref name=SIMBAD/> which lies within the mostly southern ] of ]. It was discovered on October 29, 1999 at a ] of 13.3.<ref name=Li_1999/> Using a corrected version of the expanding photosphere method (EPM), the distance to the supernova is estimated as {{convert|11.5|±|1|Mpc|e6ly|order=flip|abbr=out|link=on}}.<ref name=Dessart_Hillier_2006/> This is in good agreement with the ] method, which yields a distance of {{convert|11.71|±|0.92|Mpc|e6ly|order=flip|abbr=out|link=on}}.<ref name=Leonard_et_al_2003/>


==Observations== ==Observations==
], plotted from data published by Galbany ''et al.'' (2016)<ref name="Galbany2016"/>]]
This supernova event was first detected by the ] from a ] frame taken October 29, 1999 with the ] (KAIT). The discovery was confirmed by the ] the same day. It showed an ] of 13.5. A KAIT image of the same area taken October 20th showed nothing at the position of this supernova.<ref name=Li_1999/> SN 1999em was positioned {{val|15.4|u=arcsecond}} west and {{val|17.0|u=arcsecond}} south of the NGC 1637 nucleus. A spectrum taken October 30 showed this to be a ] event. The expansion velocity of the photosphere was measured at {{val|10300|u=km/s|fmt=commas}}. Interstellar lines in the spectrum indicated the event may be partially obscured by ].<ref name=Jha_et_al_1999/> This supernova event was first detected by the ] from a ] frame taken October 29, 1999 with the ] (KAIT). The discovery was confirmed by the ] the same day. It showed an ] of 13.5. A KAIT image of the same area taken October 20th showed nothing at the position of this supernova.<ref name=Li_1999/> SN 1999em was positioned {{val|15.4|u=arcsecond}} west and {{val|17.0|u=arcsecond}} south of the NGC 1637 nucleus. A spectrum taken October 30 showed this to be a ] event. The early expansion velocity of the photosphere was measured at {{val|10300|u=km/s|fmt=commas}}. Interstellar lines in the spectrum indicated the event may be partially obscured by ].<ref name=Jha_et_al_1999/>


] was detected from this source on November 1–2 and 11–12 using the ]. The number of photons detected suggested a luminosity of {{val|1|e=38|u=erg/s}} for the source.<ref name=Fox_Lewin_1999/> A compact radio source at this position was detected on December 1 from the ] ].<ref name=Lacey_et_al_1999/> This was the first type II-p supernova to be detected at both X-ray and radio wavelengths.<ref name=Pooley_et_al_2002/> By now the target was identified as a type II-P supernova,<ref name=Lacey_et_al_1999/> based on the shape of the ] and spectral properties.<ref name=Leonard_et_al_2001/> ] measured between November 1999 and January 2000 showed an increasing level of ] at later dates. This implied asphericity toward the core of the explosion – meaning a deviation from spherical symmetry.<ref name=Wang_et_al_2000/> ] was detected from this source on November 1–2 and 11–12 using the ]. The number of photons detected suggested a luminosity of {{val|1|e=38|u=erg/s}} for the source.<ref name=Fox_Lewin_1999/> A compact radio source at this position was detected on December 1 from the ] ].<ref name=Lacey_et_al_1999/> This was the first type II-p supernova to be detected at both X-ray and radio wavelengths.<ref name=Pooley_et_al_2002/> By now the target was identified as a type II-P supernova,<ref name=Lacey_et_al_1999/> based on the shape of the ] and spectral properties.<ref name=Leonard_et_al_2001/> ] measured between November 1999 and January 2000 showed an increasing level of ] at later dates. This implied asphericity toward the core of the explosion – meaning a deviation from spherical symmetry.<ref name=Wang_et_al_2000/>


] observations showed that SN 1999em remained in its plateau phase for approximately 90&nbsp;days, indicating that the progenitor possessed a massive ] when the explosion occurred.<ref name=Leonard_et_al_2001/> The explosion date was estimated to be {{val|5.3|1.4|u=days}} before discovery.<ref name=Hamuy_et_al_2001/><ref name=Leonard_et_al_2001/> By day 161, the spectrum was dominated by ]s, indicating that the remnant was transitioning to the nebular phase.<ref name=Leonard_et_al_2001/> Evidence showed that dust formation began at around day 500. The exponential decay rate of the light curve tail was mainly powered by the ] of ] to ]. Ejecta mass is estimated at approximately {{val|10|to|11|u=Solar mass}} and the surviving ] has {{val|1.5|u=Solar mass}}.<ref name=Elmhamdi_et_al_2003/> ] observations showed that SN 1999em remained in its plateau phase for approximately 90&nbsp;days, indicating that the progenitor possessed a massive ] when the explosion occurred.<ref name=Leonard_et_al_2001/> The explosion date was estimated to be {{val|5.3|1.4|u=days}} before discovery.<ref name=Hamuy_et_al_2001/><ref name=Leonard_et_al_2001/> By day 161, the spectrum was dominated by ]s, indicating that the remnant was transitioning to the nebular phase.<ref name=Leonard_et_al_2001/> Evidence showed that dust formation began at around day 500. The exponential decay rate of the light curve tail was mainly powered by the ] of ] to ]. Ejecta mass is estimated at approximately {{val|10|to|11|ul=Solar mass}} and the surviving ] has {{val|1.5|u=Solar mass}}.<ref name=Elmhamdi_et_al_2003/>


The host galaxy is close enough that individual ]s can be resolved. However, no such object was detected at the position of the event.<ref name=Smartt_et_al_2002/> Supernova models indicate a progenitor mass in the range of {{val|11|to|13|ul=Solar mass}}, with near solar ] and an explosive energy of {{val|1.2|ul=foe}}.<ref name=You_et_al_2024/> This star had a radius of about {{val|120|to|150|ul=Solar radius}}.<ref name=Elmhamdi_et_al_2003/> Radio and X-ray emission indicate the progenitor was surrounded by clumpy or filamentary circumstellar material that was fed by a low ] rate of about {{val|2|e=-4|ul=Solar mass}}·yr<sup>−1</sup> with a wind velocity of {{val|10|u=km/s}}.<ref name=Pooley_et_al_2002/><ref name=Elmhamdi_et_al_2003/> The light curve for this event is nearly identical to that of ], suggesting they may have similar progenitor stars.<ref name=You_et_al_2024/> The host galaxy is close enough that individual ]s can be resolved. However, no such object was detected at the position of the event.<ref name=Smartt_et_al_2002/> Supernova models indicate a progenitor mass in the range of {{val|11|to|13|ul=Solar mass}}, with near solar ] and an explosive energy of {{val|1.2|ul=foe}}.<ref name=You_et_al_2024/> This star had a radius of about {{val|120|to|150|ul=Solar radius}}.<ref name=Elmhamdi_et_al_2003/> Radio and X-ray emission indicate the progenitor was surrounded by clumpy or filamentary circumstellar material that was fed by a low ] rate of about {{val|2|e=−4|u=Solar mass}}·yr<sup>−1</sup> with a wind velocity of {{val|10|u=km/s}}.<ref name=Pooley_et_al_2002/><ref name=Elmhamdi_et_al_2003/> The light curve for this event is nearly identical to that of ], suggesting they may have similar progenitor stars.<ref name=You_et_al_2024/>


== References == == References ==
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| editor-last=Green | editor-first=D. W. E. | editor-last=Green | editor-first=D. W. E.
| bibcode=1999IAUC.7296....2J }}</ref> | bibcode=1999IAUC.7296....2J }}</ref>

<ref name="Galbany2016">{{cite journal | last1=Galbany | first1=Lluís | last2=Hamuy | first2=Mario | last3=Phillips | first3=Mark M.
| last4=Suntzeff | first4=Nicholas B. | last5=Maza | first5=José | last6=de Jaeger | first6=Thomas
| last7=Moraga | first7=Tania | last8=González-Gaitán | first8=Santiago | last9=Krisciunas | first9=Kevin
| last10=Morrell | first10=Nidia I. | last11=homas-Osip | first11=Joanna | last12=Krzeminski | first12=Wojtek
| last13=González | first13=Luis | last14=Antezana | first14=Roberto | last15=Wishnjewski | first15=Marina
| last16=McCarthy | first16=Patrick | last17=Galaz | first17=Gaspar | last18=Green | first18=Elisabeth M.
| last19=Impey | first19=Chris | last20=Kim | first20=Yong-Cheol | last21=Kirhakos | first21=Sofia
| last22=Malkan | first22=Mathew A. | last23=Mulchaey | first23=John S. | last24=Phillips | first24=Andrew C.
| last25=Pizzella | first25=Alessandro | last26=Prosser | first26=Charles F. | last27=Schmidt | first27=Brian P.
| last28=Schommer | first28=Robert A. | last29=Sherry | first29=William | last30=Strolger | first30=Louis-Gregory
| last31=Wells | first31=Lisa A. | last32=Williger | first32=Gerard M.
| title=UBVRIz Light Curves of 51 Type II Supernovae | journal=The Astronomical Journal | date=February 2016
| volume=151 | issue=2 | page=33 | doi=10.3847/0004-6256/151/2/33 | doi-access=free | arxiv=1511.08402 | bibcode=2016AJ....151...33G
}}</ref>


<ref name=Fox_Lewin_1999>{{citation | postscript=. <ref name=Fox_Lewin_1999>{{citation | postscript=.
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| volume=970 | issue=2 | at=id. 145 | date=August 2024 | volume=970 | issue=2 | at=id. 145 | date=August 2024
| doi=10.3847/1538-4357/ad50c6 | doi=10.3847/1538-4357/ad50c6
| doi-access=free
| arxiv=2402.19260 | bibcode=2024ApJ...970..145Y }}</ref> | arxiv=2402.19260 | bibcode=2024ApJ...970..145Y }}</ref>


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| volume=338 | issue=4 | pages=939–956 | date=February 2003 | volume=338 | issue=4 | pages=939–956 | date=February 2003
| doi=10.1046/j.1365-8711.2003.06150.x | doi=10.1046/j.1365-8711.2003.06150.x
| doi-access=free
| arxiv=astro-ph/0209623 | bibcode=2003MNRAS.338..939E }}</ref> | arxiv=astro-ph/0209623 | bibcode=2003MNRAS.338..939E }}</ref>


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| journal=The Astrophysical Journal | journal=The Astrophysical Journal
| volume=902 | issue=2 | at=id. 95 | date=October 2020 | volume=902 | issue=2 | at=id. 95 | date=October 2020
| doi=10.3847/1538-4357/abb4e8 | arxiv=2008.09328 | doi=10.3847/1538-4357/abb4e8 | doi-access=free
| arxiv=2008.09328
| bibcode=2020ApJ...902...95L }} | bibcode=2020ApJ...902...95L }}
*{{citation | postscript=. *{{citation | postscript=.

Latest revision as of 07:29, 8 January 2025

Supernova event of October 1999 in the galaxy NGC 1637
SN 1999em
Event typeSupernova
Type II-P
InstrumentKatzman Automatic Imaging Telescope
ConstellationEridanus
Right ascension04 41 27.04
Declination−02° 51′ 45.2″
EpochJ2000
Distance38.2 ± 3.0 million light-years (11.71 ± 0.92 Mpc).
HostNGC 1637
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[edit on Wikidata]

SN 1999em was a well-observed type II-P supernova in the spiral galaxy NGC 1637, which lies within the mostly southern constellation of Eridanus. It was discovered on October 29, 1999 at a visual magnitude of 13.3. Using a corrected version of the expanding photosphere method (EPM), the distance to the supernova is estimated as 37.5 ± 3.3 million light-years (11.5 ± 1 Mpc). This is in good agreement with the Cepheid method, which yields a distance of 38.2 ± 3.0 million light-years (11.71 ± 0.92 Mpc).

Observations

Light curves in four photometric bands, plotted from data published by Galbany et al. (2016)

This supernova event was first detected by the Lick Observatory Supernova Search from a CCD frame taken October 29, 1999 with the Katzman Automatic Imaging Telescope (KAIT). The discovery was confirmed by the Beijing Astronomical Observatory the same day. It showed an apparent visual magnitude of 13.5. A KAIT image of the same area taken October 20th showed nothing at the position of this supernova. SN 1999em was positioned 15.4″ west and 17.0″ south of the NGC 1637 nucleus. A spectrum taken October 30 showed this to be a type II supernova event. The early expansion velocity of the photosphere was measured at 10,300 km/s. Interstellar lines in the spectrum indicated the event may be partially obscured by dust.

X-ray emission was detected from this source on November 1–2 and 11–12 using the Chandra X-ray Observatory. The number of photons detected suggested a luminosity of 1×10 erg/s for the source. A compact radio source at this position was detected on December 1 from the NRAO Very Large Array. This was the first type II-p supernova to be detected at both X-ray and radio wavelengths. By now the target was identified as a type II-P supernova, based on the shape of the light curves and spectral properties. Spectrapolarimetry measured between November 1999 and January 2000 showed an increasing level of polarization at later dates. This implied asphericity toward the core of the explosion – meaning a deviation from spherical symmetry.

Photometric observations showed that SN 1999em remained in its plateau phase for approximately 90 days, indicating that the progenitor possessed a massive hydrogen envelope when the explosion occurred. The explosion date was estimated to be 5.3±1.4 d before discovery. By day 161, the spectrum was dominated by emission lines, indicating that the remnant was transitioning to the nebular phase. Evidence showed that dust formation began at around day 500. The exponential decay rate of the light curve tail was mainly powered by the radioactive decay of Co to Fe. Ejecta mass is estimated at approximately 10 to 11 M☉ and the surviving neutron star has 1.5 M☉.

The host galaxy is close enough that individual bright supergiants can be resolved. However, no such object was detected at the position of the event. Supernova models indicate a progenitor mass in the range of 11 to 13 M☉, with near solar metallicity and an explosive energy of 1.2 foe. This star had a radius of about 120 to 150 R☉. Radio and X-ray emission indicate the progenitor was surrounded by clumpy or filamentary circumstellar material that was fed by a low stellar mass loss rate of about 2×10 M☉·yr with a wind velocity of 10 km/s. The light curve for this event is nearly identical to that of SN 1999gi, suggesting they may have similar progenitor stars.

References

  1. ^ Leonard, Douglas C.; et al. (September 2003), "The Cepheid Distance to NGC 1637: A Direct Test of the Expanding Photosphere Method Distance to SN 1999em", The Astrophysical Journal, 594 (1): 247–278, arXiv:astro-ph/0305259, Bibcode:2003ApJ...594..247L, doi:10.1086/376831.
  2. ^ Elmhamdi, Abouazza; et al. (February 2003), "Photometry and spectroscopy of the Type IIP SN 1999em from outburst to dust formation", Monthly Notice of the Royal Astronomical Society, 338 (4): 939–956, arXiv:astro-ph/0209623, Bibcode:2003MNRAS.338..939E, doi:10.1046/j.1365-8711.2003.06150.x.
  3. "SN 1999em", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2025-01-05.
  4. ^ Li, W. D. (October 1999), Green, D. W. E. (ed.), "Supernova 1999em in NGC 1637", IAU Circular, 7294: 1, Bibcode:1999IAUC.7294....1L.
  5. Dessart, L.; Hillier, D. J. (February 2006), "Quantitative spectroscopic analysis of and distance to SN1999em", Astronomy and Astrophysics, 447 (2): 691–707, arXiv:astro-ph/0510526, Bibcode:2006A&A...447..691D, doi:10.1051/0004-6361:20054044.
  6. Galbany, Lluís; Hamuy, Mario; Phillips, Mark M.; Suntzeff, Nicholas B.; Maza, José; de Jaeger, Thomas; Moraga, Tania; González-Gaitán, Santiago; Krisciunas, Kevin; Morrell, Nidia I.; homas-Osip, Joanna; Krzeminski, Wojtek; González, Luis; Antezana, Roberto; Wishnjewski, Marina; McCarthy, Patrick; Galaz, Gaspar; Green, Elisabeth M.; Impey, Chris; Kim, Yong-Cheol; Kirhakos, Sofia; Malkan, Mathew A.; Mulchaey, John S.; Phillips, Andrew C.; Pizzella, Alessandro; Prosser, Charles F.; Schmidt, Brian P.; Schommer, Robert A.; Sherry, William; Strolger, Louis-Gregory; Wells, Lisa A.; Williger, Gerard M. (February 2016). "UBVRIz Light Curves of 51 Type II Supernovae". The Astronomical Journal. 151 (2): 33. arXiv:1511.08402. Bibcode:2016AJ....151...33G. doi:10.3847/0004-6256/151/2/33.
  7. Jha, S.; et al. (October 1999), Green, D. W. E. (ed.), "Supernova 1999em in NGC 1637", IAU Circular, 7296: 2, Bibcode:1999IAUC.7296....2J.
  8. Fox, D. W.; Lewin, W. H. G. (November 1999), Marsden, B. G. (ed.), "Supernova 1999em in NGC 1637", IAU Circular, 7318: 1, Bibcode:1999IAUC.7318....1F.
  9. ^ Lacey, C. K.; et al. (December 1999), Green, D. W. E. (ed.), "Supernova 1999em in NGC 1637", IAU Circular, 7336: 2, Bibcode:1999IAUC.7336....2L.
  10. ^ Pooley, David; et al. (June 2002), "X-Ray, Optical, and Radio Observations of the Type II Supernovae 1999em and 1998S", The Astrophysical Journal, 572 (2): 932–943, Bibcode:2002ApJ...572..932P, doi:10.1086/340346.
  11. ^ Leonard, Douglas C.; et al. (June 2001), "Is It Round? Spectropolarimetry of the Type II-p Supernova 1999EM", The Astrophysical Journal, 553 (2): 861–885, arXiv:astro-ph/0009285, Bibcode:2001ApJ...553..861L, doi:10.1086/320959.
  12. Wang, L.; et al. (February 2000), Green, D. W. E. (ed.), "Supernova 1999em in NGC 1637", IAU Circular, 7355: 1, Bibcode:2000IAUC.7355....1W.
  13. Hamuy, Mario; et al. (September 2001), "The Distance to SN 1999em from the Expanding Photosphere Method", The Astrophysical Journal, 558 (2): 615–642, arXiv:astro-ph/0105006, Bibcode:2001ApJ...558..615H, doi:10.1086/322450.
  14. Smartt, Stephen J.; et al. (February 2002), "The Nature of the Progenitor of the Type II-P Supernova 1999em", The Astrophysical Journal, 565 (2): 1089–1100, arXiv:astro-ph/0107499, Bibcode:2002ApJ...565.1089S, doi:10.1086/324690.
  15. ^ You, Kai-An; et al. (August 2024), "Modeling the Progenitor Stars of Observed Type IIP Supernovae", The Astrophysical Journal, 970 (2), id. 145, arXiv:2402.19260, Bibcode:2024ApJ...970..145Y, doi:10.3847/1538-4357/ad50c6.

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