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

By A. Elmhamdi, I. J. Danziger, N. Chugai, A. Pastorello, Massimo Turatto, E. Cappellaro, G. Altavilla, S. Benetti, Ferdinando Patat, M. Salvo. 2002

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We present photometry and spectra of the Type IIP supernova 1999em in NGC 1637 from several days after the outburst till day 642. The radioactive tail of the recovered bolometric light curve of SN 1999em indicates that the amount of the ejected 5 6 Ni is 0.02 M O .. The Ha and HeI 10 830-A lines at the nebular epoch show that the distribution of the bulk of 5 6 Ni can be represented approximately by a sphere of 5 6 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 Ha at the photospheric epoch reminiscent of the 'Bochum event' in SN 1987A is analysed in terms of two plausible models: bipolar 5 6 Ni jets and non-monotonic behaviour of the Ha optical depth combined with the one-sided 5 6 Ni ejection. The late-time spectra show a dramatic transformation of the [O I] 6300-A 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 800 km s - 1 and optical depth >> 10. The latter exceeds the optical depth of the dusty zone in SN 1987A by more than 10 times. Use is made of the Expanding Photosphere Method to estimate the distance and the explosion time, D 7.83 Mpc and t 0 ≃ 1999 October 24.5 UT, in accord with observational constraints on the explosion time and with other results of detailed studies of the method. The plateau brightness and duration combined with the expansion velocity suggest a pre-supernova radius of 120-150 R O ., ejecta mass of 10-11 M O . and explosion energy of (0.5-1) x 10 5 1 erg. The ejecta mass combined with the neutron star and a conservative assumption about mass loss implies the main sequence progenitor of M m s 12-14 M O .. The derived mass range is in agreement with the upper limit to the mass found using pre-supernova field images by Smartt et al. From the [OI] 6300, 6364 A 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 according to nucleosynthesis and stellar evolution theory. 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 5 6 Ni mass.

Subfields: Astronomy and Astrophysics

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1. S. Smartt
2. N. Smith
3. A. Filippenko
4. S. Valenti
5. J. Silverman
6. J. C. Wheeler
7. R. Chevalier
8. R. Foley

Citations in the corpus

• THE YELLOW SUPERGIANT PROGENITOR OF THE TYPE II SUPERNOVA 2011dh IN M51 (2011, background): “The distance and extinction of SN 1987A are from Suntzeff & Bouchet (1990); the explosion epoch and extinction of SN 1999em is from Elmhamdi et al. (2003), while its distance is taken from Leonard et al. (2003).”
• The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines (2013, background): “…and 56Ni masses)5 (Turatto et al. 1993; Schmidt et al. 1993; 5 Some objects in the “subluminous” class of Type IIP SNe (e.g. Benetti et al. 1994; Elmhamdi et al. 2003; Pozzo et al. 2006; Sahu et al. 2006; Quimby et al. 2007; Maguire et al. 2010; Andrews et al. 2011; Inserra et al. 2011; Roy…”
• The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling (2012, unknown): “The best existing datasets are for SN 1990E (Schmidt et al. 1993; Gomez & Lopez 1993; Benetti et al. 1994), SN 1999em (Leonard et al. 2002a; Elmhamdi et al. 2003), SN 1999gi (Leonard et al. 2002b), SN 2002hh (Pozzo et al. 2006), SN 2004dj (Chugai et al. 2005), SN 2004et (Sahu et al. 2006, M10), SN…”
• CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE (2014, methodology): “34Mend and56Ni mass are plotted against the steepness parameter S (see Elmhamdi et al. 2003 for more discussion on this topic), where we do not observe trends seen by previous authors.”
• Dust in the Early Universe: Dust Formation in the Ejecta of Population III Supernovae (2003, unknown): “Also, dust formation was confirmed in the ejecta of SN 1999em from the appearance of blueshifted line emissions, as observed in SN 1987A (Elmhamdi et al. 2003).”
• Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae (2009, methodology): “…only four IIP SNe for which extended photometric and spectral monitoring observations have been published; SN 1990E (Schmidt et al. 1993; Benetti et al. 1994), SN 1999em (Elmhamdi et al. 2003; Leonard et al. 2002a; Hamuy et al. 2001), SN 1999gi (Leonard et al. 2002b) and SN 2005cs (Pastorello etal.”
• SN 2008S: An electron-capture SN from a super-AGB progenitor? (2009, background): “In particular, it can attenuate the red wings of spectral lines, causing an apparent blue shift of the lineprofiles (Lucy et al. 1991; Danziger et al. 1991; Elmhamdi et al. 2003; Pozzo et al. 2004).”
• Young Core-Collapse Supernova Remnants and Their Supernovae (2004, background): “Late spectral observations of the Type IIP SN 1999em show a very centrally peaked H line, although the peak is redshifted by 400 km s 1 from the systemic velocity (Elmhamdi et al. 2003).”
• DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj (2009, methodology): “Finally we note that both Chugai et al. (2005) and Zhang et al. (2006) also used the V -light curve “steepness” method of Elmhamdi et al. (2003), which is insensitive to distance and extinction uncertainties.”
• Low‐luminosity Type II supernovae: spectroscopic and photometric evolution (2003, background): “This might be the case of SN 1999em (Baron et al. 2000; Leonard et al. 2002a; Pooley et al. 2002; Hamuy et al. 2001; Elmhamdi et al. 2003) for which recent Cepheid distance measurements Leonard et al. (2003) suggest that the host galaxy distance was previously underestimated and, consequently, the…”
• Nebular emission-line profiles of Type Ib/c supernovae - Probing the ejecta asphericity (2009, background): “This effect has been observed in some Type II SNe, for instance SNe 1987A and 1999em, more than one year after explosion (cf. e.g. Danziger et al. 1989, Lucy et al. 1989 and Elmhamdi et al. 2003).”
• Dust Formation and He II λ4686 Emission in the Dense Shell of the Peculiar Type Ib Supernova 2006jc (2007, background): “Two more-recent cases providing evidence for dust formation are SN 1999em (Elmhamdi et al. 2003) and SN 2003gd (Sugerman et al. 2006), although Meikle et al. (2007) found that the mass of dust formed in SN 2003gd was very small.”
• Dust formation and survival in supernova ejecta (2007, background): “Direct observational evidences for dust production have been collected only for a limited number of SNe, such as 1987A (Wooden et al. 1993) 1999em (Elmhamdi et al. 2003), and 2003gd (Sugerman et al. 2006).”
• SN 2005cs in M51 – II. Complete evolution in the optical and the near-infrared (2009, background): “The line velocities of these SNe are systematically smallerby a factor ∼ 2 (see Figure 12) with respect to the normal SN IIP 1999em (Hamuy et al. 2001; Leonard et al. 2002b; Elmhamdi et al. 2003a).”