{{short description|Supernova/gamma-ray burst in the constellation Telescopium}} {{Use dmy dates|date=March 2025}} {{Infobox astronomical event | name = SN 1998bw | image = File:SN 1998bw.jpg | image_scale = 1.4 | caption =Occurred on the galaxy ESO 184-G82 | alt = | names = | event_type = supernova | class = Type Ic | start_time = 26 April 1998 | duration = | detected_by = | constellation = Telescopium | ra = {{RA|19|35|03.17}}<ref name=Barbon_et_al_2008/> | dec = {{DEC|−52|50|46.1}}<ref name=Barbon_et_al_2008/> | epoch = | gal = 344.99°, −27.72°<ref name=SIMBAD/> | distance = | redshift = | source = | remnant = | host = ESO 184-G82 | progenitor = | progenitor_type = | b-v = | notes = | peak = | energy = | website = | predecessor = | successor = | commons = | embedded = | onlysourced = }} '''SN 1998bw''' was a rare broad-lined Type Ic<ref name=Woosley_et_al_1999/> gamma ray burst supernova detected on 26 April 1998 in the {{nowrap|ESO 184-G82}} spiral galaxy, which some astronomers believe may be an example of a collapsar (hypernova).<ref name=grb980425/> The hypernova has been linked to {{nowrap|GRB 980425}}, which was detected on 25 April 1998, the first time a gamma-ray burst has been linked to a supernova.<ref name=Vreeswijk00/> The hypernova is approximately 140 million light years away, very close for a gamma ray burst source.<ref name=ESO9847/>
The region of the galaxy where the supernova occurred hosts stars 5-8 million years old and is relatively free from dust. A nearby region hosts multiple Wolf-Rayet stars less than 3 million years old, but it is unlikely that the supernova progenitor could be a runaway from that region. The implication is that the progenitor was a star that originally had a mass of {{solar mass|25-40}}, if it exploded as a single star at the end of its life.<ref name=kruhler/>
==Observations== [[File:SN1998bwLightCurve.png|thumb|left|Light curves in four photometric bands for SN 1998bw, plotted from data published by Clocchiatti et al. (2011)<ref name="Clocchiatti2011"/>]] On 25 April 1998, a gamma ray burst was detected by the BeppoSAX satellite and assigned the identifier GRB 980425. The event lasted for 30 seconds,<ref name=IAU_6884/> and was about average in terms of burst flux.<ref name=Wang_Wheeler_1998/> A check of images from the ESO New Technology Telescope showed a rapidly brightening point source within the error box of GRB 980425. It was located in the face-on spiral galaxy ESO 184-G82, in a spiral arm at an offset from the nucleus. This candidate supernova event lacked spectral lines of hydrogen, ruling out a normal core-collapse Type II supernova, and it was a missing line of silicon that indicated it is not a typical Type Ia supernova.<ref name=IAU_6895/>
A few weeks after full light, the spectrum of supernova SN 1998bw showed no clear indications of helium. This suggested the event be classed as a Type Ic supernova, although it showed some peculiarities compared to other supernovae of this type. The expansion velocity measured from calcium lines was measured as {{val|11700|u=km/s|fmt=commas}}, and {{val|9100|u=km/s|fmt=commas}} from silicon lines.<ref name=Patat_Piemonte_1998/> The maximum recorded expansion velocities reached {{val|3|e=4|u=km/s}}.<ref name=Patat_et_al_2001/> Energy emissions from the supernova showed polarization, which supported a core-collapse scenario with asymmetry.<ref name=Kay_et_al_1998/>
Radio measurements of the supernova showed that it was unusually luminous in this band. The data suggested a shock wave moving at a relativistic velocity, whereas most supernovae ejecta are non-relativistic.<ref name=Kulkarni_et_al_1998/> This was the first evidence found for a relativistic shock from a supernova.<ref name=Wieringa_et_al_1999/> The supernova light curves from radio to X-ray bands also indicated a blast wave that was highly relativistic. The data was consistent with a physical association between SN 1998bw and GRB 980425,<ref name=Iwamoto_1999/><ref name=Li_Chevalier_1999/> and supported the idea of a hypernova or collapsar event. This scenario results in the formation of a black hole from the collapse of a massive star.<ref name=Iwamoto_1999/><ref name=Woosley_MacFadyen_2000/> Spherically-symmetrical models failed to reproduce an event with this energy level, indicating a highly asymmetrical explosion that produced the gamma-ray burst from a relativistic jet.<ref name=Höflich_et_al_1999/> In this case, only a fraction of the progenitor's stellar mass was ejected, with the remainder collapsing to form a black hole.<ref name=Woosley_et_al_1999/>
The supernova transitioned to the nebular phase around 100 days after the explosion.<ref name=Meada_et_al_2006/> Expansion velocities remained very high compared to other core-collapse supernovae at similar phases.<ref name=Patat_et_al_2001/> The unusual spectrum observed during the nebular phase matched a model for a strongly aspherical explosion observed from near the direction of a relativistic jet.<ref name=Maeda_et_al_2002/><ref name=Meada_et_al_2001/> The radio emission from the supernova can best be explained by interaction between the relativistic shock and clumpy circumstellar medium previously ejected by a strong stellar wind.<ref name=Weiler_et_al_2001/> Observations from the Chandra X-ray Observatory in 2004 found X-ray emission that supported this scenario.<ref name=Waxman_2004/> It also lent support to the idea that the supernova and gamma-ray burst were the same event.<ref name=Kouveliotou_et_al_2004/>
===Environment=== Observations with the Hubble Space Telescope indicated that the host for the supernova event is a sub-luminous galaxy with a morphological classification of SBc. This indicates ESO 184-G82 is a barred spiral galaxy with loosely-wound spiral arms. The galaxy is undergoing strong star formation and the supernova occurred in an active star forming area that includes an H II region. This environment is fairly typical for Type II supernovae. The supernova afterglow was about a magnitude brighter than expected from a radioactive decay model, suggesting a contribution from a surrounding stellar cluster.<ref name=Fynbo_et_al_2000/>
The host galaxy appears morphologically disturbed, which suggests interaction from nearby galaxies. This could explain the amplified star forming process.<ref name=Fynbo_et_al_2000/> Six galaxies lie within the field of ESO 184-G82 but none of them have a matching redshift of 0.0087{{±|0.0006}}. Thus, it appears to be an isolated dwarf galaxy and another explanation is needed for the star formation.<ref name=Foley_et_al_2006/> A 2020 study with the Atacama Large Millimeter Array discovered the galaxy has a ring of dense neutral hydrogen, which includes clumps of gas. One of these clumps was the host of SN 1998bw. The presence of a ring indicates a past collision with a companion galaxy.<ref name=Arabsalmani_et_al_2020/>
==References== <references>
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<ref name=SIMBAD>{{cite simbad | title=SN 1998bw | access-date=2025-03-20 | postscript=. | mode = cs2 }}</ref>
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<ref name=ESO9847>{{cite web | title=A strange supernova with a gamma-ray burst | date=15 October 1998 | publisher=European Southern Observatory | url=https://www.eso.org/public/news/eso9847/ | accessdate=2015-11-14 }}</ref>
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<ref name=Kulkarni_et_al_1998>{{cite journal | title=Radio emission from the unusual supernova 1998bw and its association with the γ-ray burst of 25 April 1998 | display-authors=1 | last1=Kulkarni | first1=S. R. | last2=Frail | first2=D. A. | last3=Wieringa | first3=M. H. | last4=Ekers | first4=R. D. | last5=Sadler | first5=E. M. | last6=Wark | first6=R. M. | last7=Higdon | first7=J. L. | last8=Phinney | first8=E. S. | last9=Bloom | first9=J. S. | journal=Nature | volume=395 | issue=6703 | pages=663–669 | date=October 1998 | doi=10.1038/27139 | bibcode=1998Natur.395..663K }}</ref>
<ref name=Iwamoto_1999>{{cite journal | title=On the Radio-to-X-Ray Light Curves of SN 1998bw and GRB 980425 | last=Iwamoto | first=Koichi | journal=The Astrophysical Journal | volume=512 | issue=1 | pages=L47–L50 | date=February 1999 | doi=10.1086/311867 | arxiv=astro-ph/9810400 | bibcode=1999ApJ...512L..47I }}</ref>
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<ref name=Foley_et_al_2006>{{cite journal | title=The galaxies in the field of the nearby GRB 980425/SN 1998bw | last1=Foley | first1=S. | last2=Watson | first2=D. | last3=Gorosabel | first3=J. | last4=Fynbo | first4=J. P. U. | last5=Sollerman | first5=J. | last6=McGlynn | first6=S. | last7=McBreen | first7=B. | last8=Hjorth | first8=J. | display-authors=1 | journal=Astronomy and Astrophysics | volume=447 | issue=3 | date=March 2006 | pages=891–895 | doi=10.1051/0004-6361:20054382 | arxiv=astro-ph/0510813 | bibcode=2006A&A...447..891F }}</ref>
<ref name=Arabsalmani_et_al_2020>{{cite journal | title=Local starburst conditions and formation of GRB 980425/SN 1998bw within a collisional ring | last1=Arabsalmani | first1=M. | last2=Renaud | first2=F. | last3=Roychowdhury | first3=S. | last4=Arumugam | first4=V. | last5=Floc'h | first5=E. Le | last6=Bournaud | first6=F. | last7=Cormier | first7=D. | last8=Zwaan | first8=M. A. | last9=Christensen | first9=L. | last10=Pian | first10=E. | last11=Madden | first11=S. | last12=Levan | first12=A. | display-authors=1 | journal=The Astrophysical Journal | volume=899 | issue=2 | at=id. 165 | date=August 2020 | doi=10.3847/1538-4357/aba3c0 | doi-access=free | arxiv=2007.01317 | bibcode=2020ApJ...899..165A }}</ref>
</references>
==Further reading== {{Div col|small=yes}} *{{cite journal | title=Spatial coincidence between ultra-high energy cosmic rays and TeV gamma rays in the direction of GRB 980425/SN 1998bw | last=Mirabal | first=Nestor | journal=Research Notes of the AAS | volume=7 | issue=4 | at=id. 80 | date=April 2023 | doi=10.3847/2515-5172/acd006 | doi-access=free | arxiv=2305.01500 | bibcode=2023RNAAS...7...80M }} *{{cite journal | title=Radiative-transfer models for explosions from rotating and non-rotating single WC stars. Implications for SN 1998bw and LGRB/SNe | display-authors=1 | last1=Dessart | first1=Luc | last2=Hillier | first2=D. John | last3=Yoon | first3=Sung-Chul | last4=Waldman | first4=Roni | last5=Livne | first5=Eli | journal=Astronomy & Astrophysics | volume=603 | at=id. A51 | date=July 2017 | doi=10.1051/0004-6361/201730873 | arxiv=1703.08932 | bibcode=2017A&A...603A..51D }} *{{cite journal | title=The properties of the host galaxy and the immediate environment of GRB 980425/SN 1998bw from the multiwavelength spectral energy distribution | last1=Michałowski | first1=Michał J. | last2=Hjorth | first2=Jens | last3=Malesani | first3=Daniele | last4=Michałowski | first4=Tadeusz | last5=Castro Cerón | first5=José María | last6=Reinfrank | first6=Robert F. | last7=Garrett | first7=Michael A. | last8=Fynbo | first8=Johan P. U. | last9=Watson | first9=Darach J. | last10=Jørgensen | first10=Uffe G. | display-authors=1 | journal=The Astrophysical Journal | volume=693 | issue=1 | pages=347–354 | date=March 2009 | doi=10.1088/0004-637X/693/1/347 | arxiv=0809.0508 | bibcode=2009ApJ...693..347M }} *{{cite journal | title=IFU observations of the GRB 980425/SN 1998bw host galaxy: emission line ratios in GRB regions | last1=Christensen | first1=L. | last2=Vreeswijk | first2=P. M. | last3=Sollerman | first3=J. | last4=Thöne | first4=C. C. | last5=Le Floc'h | first5=E. | last6=Wiersema | first6=K. | display-authors=1 | journal=Astronomy and Astrophysics | volume=490 | issue=1 | pages=45–59 | date=October 2008 | doi=10.1051/0004-6361:200809896 | arxiv=0807.3554 | bibcode=2008A&A...490...45C }} *{{cite journal | title=Multidimensional simulations for early-phase spectra of aspherical hypernovae: SN 1998bw and off-axis hypernovae | last1=Tanaka | first1=Masaomi | last2=Maeda | first2=Keiichi | last3=Mazzali | first3=Paolo A. | last4=Nomoto | first4=Ken'ichi | display-authors=1 | journal=The Astrophysical Journal | volume=668 | issue=1 | pages=L19–L22 | date=October 2007 | doi=10.1086/522671 | arxiv=0708.3242 | bibcode=2007ApJ...668L..19T }} *{{cite journal | title=Optical emission from aspherical supernovae and the hypernova SN 1998bw | display-authors=1 | last1=Maeda | first1=Keiichi | last2=Mazzali | first2=Paolo A. | last3=Nomoto | first3=Ken'ichi | journal=The Astrophysical Journal | volume=645 | issue=2 | pages=1331–1344 | date=July 2006 | doi=10.1086/504581 | arxiv=astro-ph/0511389 | bibcode=2006ApJ...645.1331M }} *{{cite journal | title=Light curve and spectral models for the hypernova SN 1998BW associated with GRB 980425 | last1=Nakamura | first1=Takayoshi | last2=Mazzali | first2=Paolo A. | last3=Nomoto | first3=Ken'ichi | last4=Iwamoto | first4=Koichi | display-authors=1 | journal=The Astrophysical Journal | volume=550 | issue=2 | pages=991–999 | date=April 2001 | doi=10.1086/319784 | arxiv=astro-ph/0007010 | bibcode=2001ApJ...550..991N }} *{{cite journal | title=On the kinematics of GRB 980425 and its association with SN 1998BW | last=Salmonson | first=Jay D. | journal=The Astrophysical Journal | volume=546 | issue=1 | pages=L29–L31 | date=January 2001 | doi=10.1086/318063 | arxiv=astro-ph/0010123 | bibcode=2001ApJ...546L..29S }} *{{cite journal | title=Monte Carlo simulations of supernova light curves and the hypernova SN1998bw | last=Chugai | first=N. 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{{DEFAULTSORT:Sn 1998bw}} {{Supernovae}} {{Telescopium}}
Category:Hypernovae Category:Supernovae Category:Gamma-ray bursts 19980426 Category:Telescopium