SN 2004aw: confirming diversity of Type Ic supernovae

By Stefan Taubenberger, A. Pastorello, P. Mazzali, S. Valenti, G. Pignata, D. Sauer, A. Arbey, O. Bärnbantner, S. Benetti, A. D. Valle and 17 more. 2006

155 citations recorded by the source corpus.

Optical and near-infrared (near-IR) observations of the Type Ic supernova (SN Ic) 2004aw are presented, obtained from -3 to +413 d with respect to the B-band maximum. The photometric evolution is characterized by a comparatively slow post-maximum decline of the light curves. The peaks in redder bands are significantly delayed relative to the bluer bands, the I-band maximum occurring 8.4 d later than that in B. With an absolute peak magnitude of -18.02 in the V band the SN can be considered fairly bright, but not exceptional. This also holds for the U through I bolometric light curve, where SN 2004aw has a position intermediate between SNe 2002ap and 1998bw. Spectroscopically SN 2004aw provides a link between a normal SN Ic like SN 19941 and the group of broad-lined SNe Ic. The spectral evolution is rather slow, with a spectrum at day +64 being still predominantly photospheric. The shape of the nebular [OI] λλ6300, 6364 line indicates a highly aspherical explosion. Helium cannot be unambiguously identified in the spectra, even in the near-IR. Using an analytical description of the light-curve peak we find that the total mass of the ejecta in SN 2004aw is 3.5-8.0 M ⊙ , significantly larger than that in SN 19941, although not as large as in SN 1998bw. The same model suggests that about 0.3 M ⊙ of 56 Ni has been synthesized in the explosion. No connection to a GRB can be firmly established.

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

View Paper: https://www.semanticscholar.org/paper/adaba423466e80bb21959fce724dac55a7c9a3dd

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In Astronomy and Astrophysics

1. S. Smartt
2. N. Smith
3. A. Filippenko
4. Ryan Chornock
5. Weidong Li
6. E. Berger
7. J. Silverman
8. R. Kirshner

In Electrical and Electronic Engineering

1. N. Smith
2. A. Filippenko
3. A. Gal-yam
4. S. Smartt
5. Ryan Chornock
6. J. Silverman
7. Weidong Li
8. S. Jha

In Nuclear and High Energy Physics

1. N. Smith
2. S. Smartt
3. A. Filippenko
4. A. Gal-yam
5. Weidong Li
6. Ryan Chornock
7. S. Jha
8. R. Kirshner

Citations in the corpus

• The Broad-lined Type Ic SN 2003jd (2007, methodology): “For SN 2004aw we have adopted the colour excess computed by Taubenberger et al. (2006), E(B − V ) = 0.37 mag, using the conservative relation between reddening and the EW of the interstellar Na i D lines (Turatto et al. 2003).”
• Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, result): “Explosion parameter estimates here were found to broadly agree with those in the literature where an analytical model was applied to the SN (e.g. Taubenberger et al. 2006, 2011; Soderberg et al. 2008; Valenti et al. 2008, 2011; Benetti et al. 2011; Drout et al. 2011; Pignata et al. 2011; Cano 2013;…”
• SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL (2013, background): “10 the comparison of the early time spectra with those of SN 2010gx (Pastorello et al. 2010), and the Type Ic SNe 1994I (Baron et al. 1996) and 2004aw (Taubenberger et al. 2006) highlights a difference in the line evolution between PTF11rks and other SL-SNe.”
• A new method for estimating the bolometric properties of Ibc supernovae (2013, background): “The decay times of 56Ni and 56Co, respectively, are τNi = 8.77 days (Taubenberger et al. 2006 and references therein) and τCo = 111.3 days (Martin 1987). τm is the effective diffusion time and determines the overall width of the bolometric light curve. τm is expressed in relation to the opacity κ…”
• FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109 (2008, background): “Comparison of the NIR spectra of proper SNe Ib 1999ex, 2001B, and 2008D with those of SNe Ic (see Taubenberger et al. 2006 and references therein) shows that all SNe display a strong feature at ∼1.04 µm but 4000 6000 8000 10000 Rest Wavelength (Å) −20 0 20 40 S ca le d f λ + C on st an t 08D,…”
• SN 2008ha: AN EXTREMELY LOW LUMINOSITY AND EXCEPTIONALLY LOW ENERGY SUPERNOVA (2009, background): “SN 2002ha does not have the second maximum in the NIR bands that is common to SNe Ia; however, there appears to be a shoulder in HK around 20–40 days after B-band maximum.”
• RAPIDLY EVOLVING AND LUMINOUS TRANSIENTS FROM PAN-STARRS1 (2014, unknown): “…Ia (Foley et al. 2013; Kasliwal et al. 2012; Perets et al. 2010), type Ib/Ic (Drout et al. 2011; Valenti et al. 2008; Campana et al. 2006; Taubenberger et al. 2006; Bersten et al. 2012; Olivares et al. 2012; Cobb et al. 2010; Valenti et al. 2012), type IIP/IIL (Arcavi et al. 2012;…”
• On the diversity of superluminous supernovae: ejected mass as the dominant factor (2015, unknown): “…et al. (2002) SN2002ap IcBL −16.49 Mazzali et al. (2002) Gal-Yam, Ofek & Shemmer (2002) SN2003jd IcBL −18.19 Valenti et al. (2008a) SN2004aw Ic −17.24 Taubenberger et al. (2006) SN2007gr Ic −16.36 Valenti et al. (2008b) SN2008D Ib −16.24 Soderberg et al. (2008), Modjaz et al. (2009) SN2009jf…”
• ULTRA-BRIGHT OPTICAL TRANSIENTS ARE LINKED WITH TYPE Ic SUPERNOVAE (2010, background): “The similarity with normal stripped-envelope SNe is even more evident in the comparison of the last spectrum of SN 2010gx (June 5) with spectra of the type Ic SNe 2003jd (Valenti et al. 2008a) and 2004aw (Taubenberger et al. 2006) obtained about 1 week after their B-band peaks.”
• Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey (2014, background): “This behaviour holds for both SNe Ib and Ic and has been noticed in several single-object papers (e.g., SN 2004aw, Taubenberger et al. 2006; SN 2007Y, Stritzinger et al. 2009; SN 1999ex Stritzinger et al. 2002; SN 2003jd Valenti et al. 2008; SN 2007gr Hunter et al. 2009; SN 2009bb Pignata et al.…”
• Determining the Type, Redshift, and Age of a Supernova Spectrum (2006, background): “A striking example is the nearby SN Ic SN 2004aw (Taubenberger et al. 2006), originally classified as an SN Ia by Benetti et al. (2004).”
• OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, background): “While Taubenberger et al. (2006) published their own spectra of this SN Ic, here we present 15 new CfA spectra, among which the earliest one at tVmax = −6 days was taken three days earlier than that in Taubenberger et al. SN 2004dk.”
• GROND—a 7-Channel Imager (2008, background): “…of X-ray heated binaries (Orosz & Bailyn 1997) (4) mapping of galaxies to study the stellar population; (5) multi-color light curves of supernovae (Taubenberger et al. 2006); (6) differentiate achromatic microlensing events (Paczynski 1986) from other variables with similar light curves; (7)…”
• Progenitors of Core-Collapse Supernovae (2009, background): “The LGRB related SNe (SN1998bw, SN2003dh, SN2003lw) have estimated ejecta masses of 8-13M⊙, while the energetic SN2004aw and SN2003jd (which lack detected LGRBs) were calculated at 3-5M⊙(Taubenberger et al. 2006, Mazzali et al. 2006b, Valenti et al. 2008).”
• DISCOVERY, PROGENITOR AND EARLY EVOLUTION OF A STRIPPED ENVELOPE SUPERNOVA iPTF13bvn (2013, methodology): “The 20581 Å doublet is often used to confirm the presence of He (Taubenberger et al. 2006; Marion et al. 2013).”