Table 4
Parameters of the explosion sites of the 1987A-like SNe.
| SN | Host galaxy | Type1 | μ 2 | AB,MW | M B | d /r25 |
P04 | P04 corr. |
|
|
||||||||
| 1909A | NGC 5457 | SABc | 29.343 | 0.037 | –21.01 | 1.119 | 8.59 | 8.3010 |
| 1982F | NGC 4490 | SBcd | 29.92 | 0.093 | –20.25 | 0.23 | 8.53 | 8.6011 |
| 1987A | LMC | SBm | 18.504 | 0.324 | –18.02 | – | 8.31 | – |
| 1998A | IC 2627 | SABc | 32.19 | 0.518 | –20.03 | 0.66 | 8.51 | 8.41 |
| 1998bt | A132541-2646 | – | 36.415 | 0.244 | –13.25 | – | 7.98 | – |
| 2000cb | IC 1158 | SABc | 32.686 | 0.491 | –19.34 | 0.93 | 8.46 | 8.24 |
| NOOS-005 | 2MASX J05553978-6855381 | S | 35.46 | 0.6568 | –20.01 | 1.26 | 8.51 | 8.17 |
| 2004em | IC 1303 | Sc | 34.07 | 0.466 | –19.73 | 0.96 | 8.49 | 8.26 |
| 2005ci | NGC 5682 | Sb | 32.73 | 0.141 | –18.07 | 0.66 | 8.36 | 8.26 |
| 2006V | UGC 6510 | SABc | 34.367 | 0.125 | –20.97 | 1.31 | 8.59 | 8.22 |
| 2006au | UGC 11057 | Sc | 33.387 | 0.742 | –20.64 | 0.90 | 8.56 | 8.36 |
| 2009E | NGC 4141 | SBc | 32.38 | 0.086 | –17.75 | 0.68 | 8.33 | 8.22 |
Notes. In Col. 3 we report the morphologic types of the host galaxies, in Cols. 4 and 5 the adopted distance moduli and Galactic extinctions from Schlegel et al. (1998), in Col. 6 the B-band absolute magnitudes of the galaxies, in Col. 7 the ratios between the deprojected position of the SN and r25 computed following Hakobyan et al. (2009), in Col. 8 the oxygen abundances from Pilyugin’s relation (computed at 0.4r25, Pilyugin et al. 2004), in Col. 9 the corrected oxygen abundances from Pilyugin’s relation computed at the deprojected SN distance.
Unless otherwise specified, distance moduli are computed from HyperLeda’s vVir, adopting H0 = 72 km s-1 Mpc-1.
Distance computed from the tip of the red giant branch (TRGB, Rizzi et al. 2007). Cepheid distances are found to be too sensitive to metallicity. The metallicity correction is even more crucial in the case of NGC 5457 where inner metal-poor and outer metal-rich cepheids give uncorrected distance moduli that may differ by 0.3−0.4 mag (Saha et al. 2006).
For LMC we adopted a cepheid distance, well consistent with that derived from the TRGB (Sakai et al. 2004; Rizzi et al. 2007).
SN 1998bt was discovered in the course of the Mount Stromlo Abell cluster supernova search (Germany et al. 2004). Unfortunately, no spectroscopic classification exists for this SN. According to Germany et al. (2004), there is a very faint host galaxy at the position of SN 1998bt, but no spectrum was ever obtained of this galaxy. We assume that the galaxy hosting SN 1998bt belongs to a cluster monitored by the search whose average redshift is z = 0.046.
Average EPM distance from Table 4.1 of Hamuy (2001).
Distance as in Taddia et al. (2011), but obtained adopting an Hubble Constant H0 = 72 km s-1 Mpc-1.
This galaxy is behind LMC, so the extinction reported here includes both Galaxy and LMC contributions (see text for references).
Computed using the position angle provided by Jarrett et al. (2003).
Other sources give 12 + log(O/H) ≈ 7.7−7.8 at the position of SN 1909A (Kennicutt et al. 2003; Pilyugin et al. 2004; Bresolin 2007).
An alternative estimate from Pilyugin & Thuan (2007) gives 12 + log(O/H) = 8.35.
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