TY - JOUR
T1 - Coronal lines and dust formation in SN 2005ip
T2 - Not the brightest, but the hottest type IIn supernova
AU - Smith, Nathan
AU - Silverman, Jeffrey M.
AU - Chornock, Ryan
AU - Filippenko, Alexei V.
AU - Wang, Xiaofeng
AU - Li, Weidong
AU - Ganeshalingam, Mohan
AU - Foley, Ryan J.
AU - Rex, Jacob
AU - Steele, Thea N.
N1 - Publisher Copyright:
© 2009 The American Astronomical Society. All rights reserved. Printed in the U.S.A.
PY - 2009/4/20
Y1 - 2009/4/20
N2 - We present optical photometry and spectroscopy of SN 2005ip for the first 3 yr after discovery, showing an underlying Type II-L supernova (SN) interacting with a steady wind to yield an unusual Type IIn spectrum. For the first ∼160 days, it had a fast linear decline from a modest peak absolute magnitude of about -17.4 (unfiltered), followed by a plateau at roughly -14.8 for more than 2 yr. Initially having a normal broad-lined spectrum superposed with sparse narrow lines from the photoionized circumstellar medium (CSM), it quickly developed signs of strong CSM interaction with a spectrum similar to that of SN 1988Z. As the underlying SN II-L faded, SN 2005ip exhibited a rich high-ionization spectrum with a dense forest of narrow coronal lines, unprecedented among SNe but reminiscent of some active galactic nuclei. The line-profile evolution of SN 2005ip confirms that dust formation caused its recently reported infrared excess, but these lines reveal that it is the first SN to show clear evidence for dust in both the fast SN ejecta and the slower postshock gas. SN 2005ip's complex spectrum confirms the origin of the strange blue continuum in SN 2006jc, which also had postshock dust formation. We suggest that SN 2005ip's late-time plateau and coronal spectrum result from rejuvenated CSM interaction between a sustained fast shock and a clumpy stellar wind, where X-rays escape through the optically thin interclump regions to heat the preshock CSM to coronal temperatures.
AB - We present optical photometry and spectroscopy of SN 2005ip for the first 3 yr after discovery, showing an underlying Type II-L supernova (SN) interacting with a steady wind to yield an unusual Type IIn spectrum. For the first ∼160 days, it had a fast linear decline from a modest peak absolute magnitude of about -17.4 (unfiltered), followed by a plateau at roughly -14.8 for more than 2 yr. Initially having a normal broad-lined spectrum superposed with sparse narrow lines from the photoionized circumstellar medium (CSM), it quickly developed signs of strong CSM interaction with a spectrum similar to that of SN 1988Z. As the underlying SN II-L faded, SN 2005ip exhibited a rich high-ionization spectrum with a dense forest of narrow coronal lines, unprecedented among SNe but reminiscent of some active galactic nuclei. The line-profile evolution of SN 2005ip confirms that dust formation caused its recently reported infrared excess, but these lines reveal that it is the first SN to show clear evidence for dust in both the fast SN ejecta and the slower postshock gas. SN 2005ip's complex spectrum confirms the origin of the strange blue continuum in SN 2006jc, which also had postshock dust formation. We suggest that SN 2005ip's late-time plateau and coronal spectrum result from rejuvenated CSM interaction between a sustained fast shock and a clumpy stellar wind, where X-rays escape through the optically thin interclump regions to heat the preshock CSM to coronal temperatures.
KW - Circumstellar matter
KW - Stars: mass loss
KW - Stars: winds, outflows
KW - Supernovae: individual (SN 2005ip)
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U2 - 10.1088/0004-637X/695/2/1334
DO - 10.1088/0004-637X/695/2/1334
M3 - Article
AN - SCOPUS:85021118009
SN - 0004-637X
VL - 695
SP - 1334
EP - 1350
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -