A Study of the Type II-Plateau Supernova 1999gi and the Distance to its Host Galaxy, NGC 3184

By D. Leonard, A. Filippenko, Weidong Li, Thomas Matheson, R. Kirshner, Ryan Chornock, S. V. Dyk, P. Berlind, M. Calkins, P. Challis and 3 more. 2002

146 citations recorded by the source corpus.

We present optical spectra and photometry sampling the first 6 months after discovery of supernova (SN) 1999gi in NGC 3184. SN 1999gi is shown to be a Type II-plateau event with a photometric plateau lasting until about 100 days after discovery. Using the expanding photosphere method (EPM), we derive a distance to SN 1999gi of 11.1 Mpc and an explosion date of 1999 December 5.8, or 4.1 days prior to discovery. This distance is consistent with a Tully-Fisher distance recently derived to NGC 3184 (D ≈ 11.59 Mpc), but it is somewhat closer than the Cepheid distances recently derived to two galaxies that have generally been assumed to be associated with the group containing NGC 3184 (NGC 3319, D = 13.30 ± 0.55 Mpc, and NGC 3198, D = 13.80 ± 0.51 Mpc). From many lines of evidence, we conclude that SN 1999gi is only minimally reddened. A comparison between the color of SN 1999gi at early times and that of an infinitely hot blackbody restricts the reddening to E(B-V) < 0.45 mag, while a comparison between the color evolution of SN 1999gi and the well-observed (and extensively modeled) Type II-P SN 1999em implies an even more restrictive upper reddening limit of E(B-V) < 0.3 mag. A variety of other, independent reddening estimates are consistent with these upper limits and yield a probable reddening of E(B-V) = 0.21 ± 0.09 mag. We reconsider the upper mass limit (9 M⊙) recently placed on the progenitor star of SN 1999gi by Smartt et al. in light of these results. Following the same procedures, but using the new data presented here, we arrive at a less restrictive upper mass limit of 15 M⊙ for the progenitor. The increased upper limit results mainly from the larger distance derived through the EPM than was assumed by the Smartt et al. analyses, which relied on less precise (and less recent) distance measurements to NGC 3184. Finally, we confirm the existence of "complicated" P Cygni line profiles in early-time and later photospheric-phase spectra of SN 1999gi. These features, first identified by Baron et al. in spectra of SN 1999em as high-velocity absorptions, in addition to the "normal" lower velocity component, are here verified to be true P Cygni profiles consisting of both an absorption trough and an emission peak at early times. In the earliest spectrum, taken less than a day after discovery, the features extend out to nearly -30,000 km s-1, indicating the existence of very high velocity material in the outer envelope of SN 1999gi.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4d576e62508a0f2ecdf46b8f1fa2796886640fa9

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In Astronomy and Astrophysics

1. S. Smartt
2. N. Smith
3. Stan Woosley
4. A. Filippenko
5. S. Valenti
6. D. Kasen
7. E. Berger
8. Alexander Heger

In Nuclear and High Energy Physics

1. S. Smartt
2. Stan Woosley
3. Alexander Heger
4. J. C. Wheeler
5. S. Valenti
6. A. Gal-yam
7. D. Kasen
8. A. Filippenko

Citations in the corpus

• 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…”
• Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae (2009, methodology): “Figure 21 shows the photospheric velocity estimated from the Scii (6246 Å) line of SN 2004et compared with the velocities for three other type IIP SNe, SN 1999br (Pastorello et al. 2004),SN 1999em (Leonard et al. 2002a) and SN 2005cs (Pastorello et al. Figure 15.”
• 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).”
• The Carnegie Supernova Project: The Low‐Redshift Survey (2005, methodology): “…for measuring luminosity distances employing the Expanding Photosphere Method (Eastman et al. 1996; Schmidt et al. 1994; Hamuy et al. 2001; Leonard et al. 2002; Dessart & Hillier 2005) or the Standardized Candle Method (Hamuy & Pinto 2002), thereby providing an independent check on the…”
• The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling (2012, unknown): “…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 2005cs (e.g. Pastorello…”
• Photometric and spectroscopic evolution of the Type IIP supernova SN 2004et (2006, methodology): “…V light curve of SN 2004et with those of other SNe IIP, namely, SN 1999em (Hamuy et al. 2001; Leonard et al. 2002a; Elmhamdi et al. 2003b), SN 1999gi (Leonard et al. 2002b), SN 1997D (Benetti et al. 2001 and references therein), SN 1990E (Schmidt et al. 1993) and SN 1987A (Hamuy et al. 1988).”
• PAIR INSTABILITY SUPERNOVAE: LIGHT CURVES, SPECTRA, AND SHOCK BREAKOUT (2011, methodology): “…R-band light curves of representative PI SN models with observations of a typical Type Ia supernova (SN 2001el, Krisciunas et al. 2003), a typical Type IIP supernova (SN 1999em, Leonard et al. 2002), and SN 2006gy, one of the most the luminous core-collapse SNe discovered (Smith et al. 2006).”
• Spectropolarimetry of Supernovae (2008, methodology): “…(24) Leonard et al. (2001); Wang et al. (2001); (25) unpublished; (26) Wang et al. (2003a); (27) Maund et al. (2007c); (28) Kawabata et al. (2002), Leonard et al. (2002), Wang et al. (2003); (29) Wang et al. (2004), Kawabata et al. unpublished; (30) Kawabata et al. (2003); (31) Chornock &…”
• On the Progenitor of SN 2005gl and the Nature of Type IIn Supernovae (2006, methodology): “We follow Leonard et al. (2002) in quantifying this observation as follows.”
• The diversity of Type II supernova versus the similarity in their progenitors (2016, unknown): “2015; Gall et al. 2015; Pastorello et al. 2009; Inserra et al. 2013; Leonard et al. 2002a).”