The Type Ic Hypernova SN 2002ap

By P. Mazzali, J. Deng, K. Maeda, K. Nomoto, H. Umeda, K. Hatano, K. Iwamoto, Y. Yoshii, Yukiyasu Kobayashi, T. Minezaki and 24 more. 2002

224 citations recorded by the source corpus.

Photometric and spectroscopic data of the energetic Type Ic supernova (SN) 2002ap are presented, and the properties of the SN are investigated through models of its spectral evolution and its light curve. The SN is spectroscopically similar to the "hypernova" SN 1997ef. However, its kinetic energy [~(4-10) × 1051 ergs] and the mass ejected (2.5-5 M☉) are smaller, resulting in a faster evolving light curve. The SN synthesized ~0.07 M☉ of 56Ni, and its peak luminosity was similar to that of normal SNe. Brightness alone should not be used to define a hypernova, whose defining character, namely very broad spectral features, is the result of high kinetic energy. The likely main-sequence mass of the progenitor star was 20-25 M☉, which is also lower than that of both hypernovae SN 1997ef and SN 1998bw. SN 2002ap appears to lie at the low-energy and low-mass end of the hypernova sequence as it is known so far. Observations of the nebular spectrum, which is expected to dominate by the summer of 2002, are necessary to confirm these values.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/457233b5cb8352cf2eb999b79cb1e365fb613458

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Citations in the corpus

• The Afterglow, Energetics, and Host Galaxy of the Short-Hard Gamma-Ray Burst 051221a (2006, background): “…measurements rule out 6 the presence of the brighter two SNe (1998bw and 1994I) while our limits are consistent with a faint SN2002ap-like event with a peak optical magnitude ofMV ∼> −17.2 (restframe) corresponding to a limit on the mass of synthesized Nickel of ∼< 0.07 M⊙ (Mazzali et al. 2002).”
• On the Rates of Gamma-Ray Bursts and Type Ib/c Supernovae (2006, unknown): “—(1) Mazzali et al. 2004; (2) Filippenko 1997; (3) Galama et al. 1998; (4) Hatano et al. 2001; (5) Mazzali et al. 2002; (6) Foley et al. 2003; (7) Filippenko et al. 2002; (8) Filippenko & Chornock 2003; (9) Stanek et al. 2003; (10) Hjorth et al. 2003; (11) Filippenko et al. 2003; (12) Matheson et…”
• The Supernova Gamma-Ray Burst Connection (2006, background): “Specific cases include Type Ic supernovae SN 1997ef, 1997dq (Mazzali et al., 2004) and SN 2002ap (Mazzali et al., 2002; Yoshii et al., 2003).”
• Observed and Physical Properties of Core-Collapse Supernovae (2002, background): “Although the definition of hypernova is ambiguous, if SN 1997ef and SN 2002ap are included in this category (Nomoto et al. 2000; Mazzali et al. 2002), then at least one SN II (1992am) also qualifies as a hypernova.”
• The Rates of Hypernovae and Gamma-Ray Bursts: Implications for Their Progenitors (2004, background): “…from the very bright and energetic SNe 1998bw (Iwamoto et al. 1998) and 2003dh (Mazzali et al. 2003), the moderately bright but very energetic SNe 1997ef (Mazzali et al. 2000) and 1997dq (Mazzali et al., in preparation), and the normally bright but over-energetic SN 2002ap (Mazzali et al. 2002).”
• A Two-Component Model for the Light Curves of Hypernovae (2003, methodology): “The spherical hydrodynamical models used to fit the early phases of SN 1998bw (Nakamura et al. 2001), SN 1997ef (Iwamoto et al. 2000; Mazzali et al. 2000), and SN 2002ap (Mazzali et al. 2002; Yoshii et al. 2003) do not reproduce well the later phase light curves.”
• The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, background): “SN 2002ap was extremely energetic and bore a striking spectroscopic similarity to the ‘hypernovae’ 1997ef and 1998bw (Gal-Yam, Ofek & Shemmer 2002; Mazzali et al. 2002).”
• On the diversity of superluminous supernovae: ejected mass as the dominant factor (2015, unknown): “…et al. (1995), Richmond et al. (1996) SN1998bw IcBLa −16.84 Patat et al. (2001) SN1999ex Ic −16.84 Stritzinger 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)…”
• The fast, luminous ultraviolet transient AT2018cow: extreme supernova, or disruption of a star by an intermediate-mass black hole? (2018, methodology): “We attempted to subtract the hot continuum to test this connection more rigorously, but the match is poor, being both too blue and too broad (Figure 11) compared to even the earliest spectra of SN1998bw or SN2002ap (Patat et al. 2001; Kinugasa et al. 2002), or of 10 We emphasize that the existence o”
• Observational and Physical Classification of Supernovae (2016, unknown): “The discovery of the nearby SN 2002ap (Gal-Yam et al. 2002; Mazzali et al. 2002; Foley et al. 2003) that was not associated with a GRB, further boosted the study of this class as a variant of SNe Ic, based on the strong spectroscopic resemblance (Fig.”
• Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “…2006aj is less energetic (E51 ∼ 2) and its progenitor mass is smaller (∼20 M ) (Mazzali et al. 2006), whereas SN 2010bf may be as energetic as E51 ∼ 10 (Bufano et al. 2012) Other non-GRB “hypernovae” have been recognized, such as SN 1997ef (Iwamoto et al. 2000) and SN 2002ap (Mazzali et al. 2002).”
• Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329 (2003, background): “The similarities of the GRB 030329 supernova to SN 1998bw are striking, while the match to other “hypernovae” such as SN 1997ef (Iwamoto et al. 2000) and SN 2002ap (Mazzali et al. 2002) is not as good.”
• Circumstellar Emission from Type Ib and Ic Supernovae (2006, background): “The broadline character of the optical spectrum of SN 1998bw, with velocities up to 60,000 km s 1, led to the view that SNe Ib/c with such broad lines were likely to be related to GRBs, including SN 2002ap (Mazzali et al. 2002).”
• SN 2004aw: confirming diversity of Type Ic supernovae (2006, background): “…= −17.35 mag (Sharina et al. c© 2006 RAS, MNRAS 000, 1–22 1996; Foley et al. 2003; Yoshii et al. 2003, µ = 29.46 mag, E(B − V ) = 0.09 mag), and with MV = −17.14 mag, the BL-SN 1997ef is not very luminous either (Garnavich et al. 1997a,b,c; Mazzali et al. 2002, µ = 33.54 mag, E(B − V ) = 0.04 mag).”
• Observed Fractions of Core-Collapse Supernova Types and Initial Masses of their Single and Binary Progenitor Stars (2010, background): “…arise from only moderately massive stars, D ow nloaded from https://academ ic.oup.com /m nras/article-abstract/412/3/1522/1049969 by guest on 15 M arch 2020 based on the ejecta mass estimates and progenitor limits (Iwamoto et al. 1994; Mazzali et al. 2002; Sauer et al. 2006; Crockett et al. 2007).”
• The Type Ic Hypernova SN 2003dh/GRB 030329 (2003, background): “…the spectrum of SN 1997ef obtained on 1998 January 1 (dotted line), and our synthetic spectrum (thick dashed line). flux to the AG is justified by the fact that because of lineblanketing Type Ib/c SNe, like SNe Ia, always show a flux deficiency to the blue of∼3600 (e.g., Mazzali et al. 2002).”
• SN 2003lw and GRB 031203: A Bright Supernova for a Faint Gamma-Ray Burst (2004, unknown): “2 of Mazzali et al., 2002).”
• Long γ-Ray Bursts and Type Ic Core-Collapse Supernovae Have Similar Locations in Hosts (2007, background): “While some broad-lined SN Ic are exceptionally luminous, there are examples, such as SN 2002ap (E ∼ (4-10) ×1051 ergs), which match best with a low-energy model (Mazzali et al. 2002).”