Photometric and spectroscopic evolution of the Type IIP supernova SN 2004et

By Devendra Kumar Sahu, G. Anupama, S. Srividya, S. Muneer. 2006

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We present optical photometry and spectroscopy of the normal type IIP supernova SN2004A, which was discovered in the galaxy NGC 6207 on 2004 January 9.84UT. Early observations indicated that the supernova was discovered at about two weeks since explosion. We estimate the distance to NGC 6207 to be 20.35 \pm 4.5 Mpc using the Standard Candle method. Using this distance, we estimate the ejected nickel mass in the explosion to be 0.032 \pm 0.02M\odo\cdot. The plateau luminosity, its duration (about 80 days) and the expansion velocity of the supernova ejecta at the middle of the plateau indicate an explosion energy of 4.7 \pm 2.7 x 10^50 ergs and an ejected envelope mass of 7.2 \pm 2.2M\odot\cdot . The ejected envelope mass implies a main sequence mass of 10 2.5\pm M\odot\cdot for the progenitor.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0b555b27c25e5c98608e82e97e68499e7f327eb0

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Citations in the corpus

SN 2005cs in M51 – II. Complete evolution in the optical and the near-infrared (2009, unknown): “…SN 1999br (Hamuy 2003; Pastorello et al. 2004), SN 2004dj (Vinkó et al. 2006), SN 1999gi (Leonard et al. 2002a), SN 1999em (Hamuy et al. 2001; Leonard et al. 2002b; Elmhamdi et al. 2003a), SN 2003gd (Hendry et al. 2005), SN 2004et (Sahu et al. 2006; Kuntal et al. 2007), SN 1996W (Pastorello 2003).”
The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling (2012, methodology): “We adopt a distance of 5.5 Mpc for NGC 6946, as determined using the H i Tully-Fisher relation (Pierce 1994), and in agreement with the average value of several other distance determinations (Schmidt 1993; Schoniger & Sofue 1994; Karachentsev et al. 2000; Sahu et al. 2006).”
Discovery of the Dust-Enshrouded Progenitor of SN 2008S with Spitzer (2008, methodology): “The appearance of the type IIn SN 2008S in the nearby galaxy NGC 6946 (d ≃ 5.6 Mpc; Sahu et al. 2006) was fortuitous, since a massive stellar progenitor would be relatively easy to find.”
SN 2008S: An electron-capture SN from a super-AGB progenitor? (2009, methodology): “…± 0.6 28.92 ± 0.21 planetary nebulae luminosity function Herrmann et al. (2008) 5.7 ± 0.7 28.78 ± 0.40 EMP SN 1980K Schmidt et al. (1994) 5.7 ± 0.3 28.78 ± 0.11 SCM SN 2004et Sahu et al. (2006) of the EW changes in the Na I D lines, we carried out a quantitative statistical test, performing a…”
A NEW CLASS OF LUMINOUS TRANSIENTS AND A FIRST CENSUS OF THEIR MASSIVE STELLAR PROGENITORS (2008, unknown): “SN 2008S SN 2008S in NGC 6946 (D ≈ 5.6 Mpc; Sahu et al. 2006) was discovered February 1.79 UT (Arbour & Boles 2008).”
The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines (2013, methodology): “…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 et al. 2011; Tomasella et al. 2013), we…”
Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae (2009, methodology): “Sahu et al. (2006) found a56Ni mass of 0.062± 0.02 M⊙ and Misra et al. (2007) a 56Ni mass of 0.056± 0.016 M⊙ using this steepness method.”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, unknown): “062 ± 0.02 M⊙ (S method) (Sahu et al. 2006),0.068 ± 0.009 M⊙ (BL method) (Utrobin & Chugai 2009),0.06± 0.03M⊙ (BL method) and0.”
The search for failed supernovae with the Large Binocular Telescope: first candidates (2014, methodology): “NGC 6946 was determined using Botticella et al. (2009) for chip 2 and Sahu et al. (2006) for chip 1.”
Production of dust by massive stars at high redshift (2011, methodology): “…method direct confirmation of newly formed dust in the ejecta has been presented for some SNe, including SN 1987A (e.g., Danziger et al, 1989; Lucy et al, 1989), SN 1990I (e.g., Elmhamdi et al, 2004), SN 1999em (e.g., Elmhamdi et al, 2003), and SN 2004et (e.g., Sahu et al, 2006; Kotak et al, 2009).”