Photometry and Spectroscopy of the Type IIP SN 1999em from Outburst to Dust Formation

Details Photometry and Spectroscopy of the Type IIP SN 1999em from Outburst to Dust Formation Photometry and Spectroscopy of the Type IIP SN 1999em from Outburst to Dust Formation

2002-09-30

arxiv.org/abs/astro-ph/0209623v1

Mon.Not.Roy.Astron.Soc.338:939-956,2003

Astronomy and Astrophysics

Astrophysics

20 pages, 22 figures and 5 tables. To appear in MNRAS (accepted)

Scientific paper

10.1046/j.1365-8711.2003.06150.x

We present photometry and spectra of the type IIP SN1999em in NGC 1637 from several days after the outburst till day 642. An amount of $\approx 0.02 M_{\odot}$ of ejected $^{56}$Ni is inferred using the recovered bolometric light curve . The H$\alpha$ and He I 10830 \AA lines at the nebular epoch show that the distribution of the bulk of $^{56}$Ni can be represented approximately by a sphere of $^{56}$Ni with a velocity of 1500 km s$^{-1}$, which is shifted towards the far hemisphere by about 400 km s$^{-1}$. The fine structure of the H$\alpha$ at the photospheric epoch reminiscent of the "Bochum event" in SN 1987A is analysed . The late time spectra show a dramatic transformation of the [O I] 6300 \AA line profile between days 465 and 510, which we interpret as an effect of dust condensation during this period. Late time photometry supports the dust formation scenario after day 465. The [O I] line profile suggests that the dust occupies a sphere with velocity $\approx 800$ km s$^{-1}$ and optical depth $\gg10$. The plateau brightness and duration combined with the expansion velocity suggest a presupernova radius of $120-150 R_{\odot}$, ejecta mass of $10-11 M_{\odot}$ and explosion energy of $(0.5-1)\times10^{51}$ erg. The ejecta mass combined with the neutron star and a conservative assumption about mass loss implies the main sequence progenitor of $M_{\rm ms}\approx 12-14 M_{\odot}$. From the [O I] 6300,6364 \AA doublet luminosity we infer the oxygen mass to be a factor four lower than in SN 1987A which is consistent with the estimated SN 1999em progenitor mass . We note a "second-plateau" behaviour of the light curve after the main plateau at the beginning of the radioactive tail. This feature seems to be common to SNe IIP with low $^{56}$Ni mass.

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