Imperial College London
Emeritus Professor Peter Meikle

Emeritus ProfessorPeterMeikle

Faculty of Natural Sciences, Department of Physics

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Contact

 

+44 (0)20 7594 7531p.meikle

 
 
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Location

 

Blackett LaboratorySouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@article{Pozzo:2006:10.1111/j.1365-2966.2006.10204.x,
author = {Pozzo, M and Meikle, WPS and Rayner, JT and Joseph, RD and Filippenko, AV and Foley, RJ and Li, W and Mattila, S and Sollerman, J},
doi = {10.1111/j.1365-2966.2006.10204.x},
journal = {Monthly Notices of the Royal Astronomical Society},
pages = {1169--1195},
title = {Optical and infrared observations of the Type IIPSN 2002hh from days 3 to 397},
url = {http://dx.doi.org/10.1111/j.1365-2966.2006.10204.x},
volume = {368},
year = {2006}
}
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RIS format (EndNote, RefMan)

TY  - JOUR
AB  - We present optical and infrared (IR) observations of the Type II SN 2002hh from 3 to 397 d after explosion. The optical spectroscopic (4–397 d) and photometric (3–278 d) data are complemented by spectroscopic (137–381 d) and photometric (137–314 d) data acquired at IR wavelengths. This is the first time L-band spectra have ever been successfully obtained for a supernova (SN) at a distance beyond the Local Group. The VRI light curves in the first 40 d reveal SN 2002hh to be an SN IIP (plateau) – the most common of all core-collapse SNe. SN 2002hh is one of the most highly extinguished SNe ever investigated. To provide a match between its early-time spectrum and a coeval spectrum of the Type IIP SN 1999em, as well as maintaining consistency with K I interstellar absorption, we invoke a two-component extinction model. One component is due to the combined effect of the interstellar medium (ISM) of our Milky Way Galaxy and the SN host galaxy, while the other component is due to a ‘dust pocket’ where the grains have a mean size smaller than in the ISM. The early-time optical light curves of SNe 1999em and 2002hh are generally well matched, as are the radioactive tails of these two SNe and SN 1987A. The late-time similarity of the SN 2002hh optical light curves to those of SN 1987A, together with measurements of the optical/IR luminosity and [Fe II] 1.257 μm emission indicate that 0.07 ± 0.02 M of 56Ni was ejected by SN 2002hh. However, during the nebular phase the HKL′ luminosities of SN 2002hh exhibit a growing excess with respect to those of SN 1987A. We attribute much of this excess to an IR-echo from a pre-existing, dusty circumstellar medium. Based on an IR-echo interpretation of the near-IR (NIR) excess, we deduce that the progenitor of SN 2002hh underwent recent mass-loss of ∼0.3 M. A detailed comparison of the late-time optical and NIR spectra of SNe 1987A and 2002hh is presented. While the overall im
AU  - Pozzo,M
AU  - Meikle,WPS
AU  - Rayner,JT
AU  - Joseph,RD
AU  - Filippenko,AV
AU  - Foley,RJ
AU  - Li,W
AU  - Mattila,S
AU  - Sollerman,J
DO  - 10.1111/j.1365-2966.2006.10204.x
EP  - 1195
PY  - 2006///
SN  - 0035-8711
SP  - 1169
TI  - Optical and infrared observations of the Type IIPSN 2002hh from days 3 to 397
T2  - Monthly Notices of the Royal Astronomical Society
UR  - http://dx.doi.org/10.1111/j.1365-2966.2006.10204.x
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000237353000018&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/56115
VL  - 368
ER  -
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