EDP Sciences
Free Access
Issue
A&A
Volume 580, August 2015
Article Number A131
Number of page(s) 34
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201525989
Published online 19 August 2015

Online material

Table 1

Sample and basic data of 63 (38 SNe IIn, 6 SNe Ibn, 1 SN Ia-CSM, 18 SN IMs) CSI SN host galaxies.

Table 2

Log of the photometric and spectroscopic observations at the Nordic Optical Telescope with ALFOSC.

Table 3

Deprojected and normalized distance from the host center and line ratios for the H ii regions with observed spectrum.

Table 5

Apparent (u/U,B,V,R/r/unf.,I/i) peak magnitudes, galactic and host extinction for the SNe IIn, Ibn, and Ia-CSM of our sample.

Table 6

Absolute (U/u,B,V,R/r/unf.,I/i) peak magnitudes for the SNe IIn, Ibn, and Ia-CSM of our sample.

Table 7

Wind velocity and mass-loss rate for a subsample of CSI SNe (IIn, Ibn, Ia-CSM).

thumbnail Fig. 4

BPT diagram for each H ii region that we spectroscopically observed. Above the dashed line (Kauffmann et al. 2003, see Sect. 4) the line fluxes are AGN contaminated and we rejected those spectra from our metallicity study. Most of the spectra fall in the star-forming part of the BPT diagram, below the dashed line. The symbols marked with black edges indicate that the ratio between [O iiiλ5007] and Hβ is an upper limit. All the line ratios are reported in Table 3.

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thumbnail Fig. 5

Metallicity gradients of ten SN IIn host galaxies observed with the NOT+ALFOSC. Symbols and lines as in the bottom panel of Fig. 2. Black open squares with arrows correspond to upper limits. The gradients of the hosts of SNe 2006jd and 2005ip are not shown, as we could not measure the flux from bright H ii regions. Instead, we used literature data. For the host of SN 1995N, whose gradient is not shown, we only have one measurement and we did not assume any gradient, as it is an irregular and interacting galaxy.

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thumbnail Fig. 6

Metallicity gradients of five SN Ibn and one SN Ia-CSM host galaxies observed with the NOT+ALFOSC. Symbols and lines as in the bottom panel of Fig. 2.

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thumbnail Fig. 7

Metallicity gradients of twelve SN IM host galaxies observed with the NOT+ALFOSC. Symbols and lines as in the bottom panel of Fig. 2. We label the gradient “P04" when we use the one measured by Pilyugin et al. (2004), and “P04" when we assumed the average P04 gradient. The data of the hosts of V1 and OT2005 are not shown as we do not determine or adopt a gradient for them, but we only measured the metallicity of one H ii region close the SN location.

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thumbnail Fig. 11

Absolute peak magnitudes for SNe IIn and Ibn against the metallicity at the SN position. Triangles are upper limits.

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thumbnail Fig. 12

Top left panel: mass-loss rates of SNe IIn versus local metallicity measurements. Triangles are upper limits. Above 10-3M yr-1, the mass-loss rates appear to be higher at higher metallicity. The power-law (PL) dependence on metallicity (α = 0.69 e.g., Vink 2011) of the line-driven mass-loss rates is shown with a black segment and is consistent with the data. SNe IIn-L (98S-like) typically show lower mass-loss rates than long-lasting SN IIn (88Z-like). Top right panel: mass-loss rate CDFs for metal-poor and metal-rich SNe IIn, shown to better highlight that at higher metallicities the mass-loss rates tend to be higher. Two different metallicity cuts are shown, at log(O/H) + 12 = 8.3 and 8.5. Bottom left panel: wind velocities of SNe IIn and SNe Ibn versus local metallicities. Triangles are upper limits. The PL dependence on metallicity (α= 0.12 (e.g., Kudritzki 2002) of the line-driven wind velocities rates is shown with a black segment, and is consistent with the data. SNe IIn-L (98S-like) typically show higher wind velocities than long-lasting SN IIn (88Z-like). Bottom right panel: wind-velocity CDFs, for metal-poor and metal-rich SNe IIn, shown to better highlight that at higher metallicities the wind velocities tend to be slightly higher. Two different metallicity cuts are shown, at log(O/H) + 12 = 8.3 and 8.5.

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thumbnail Fig. 13

Left-hand panel: metallicity CDFs for CSI SNe showing and not showing MIR dust emission at late epochs (Fox et al. 2011). These CDFs do not show any statistically significant difference. Right-hand panel: CDFs of the peak absolute r/R/unf. band magnitudes for the same CSI SNe showing and not showing MIR dust emission at late epochs. These CDFs show that SNe with MIR dust emission tend to be brighter at peak.

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thumbnail Fig. 14

Top panel: SN IM peak absolute magnitudes (from Smith et al. 2011a) versus local metallicity. Central panel: absolute magnitude of SN IM progenitors (from Smith et al. 2011a) versus local metallicities. Triangles are lower limits. With the exception of SN 1961V and of those events where we have limits poorer than 12 mag, at lower metallicity the luminosity seems to be higher. Bottom panel: difference between each peak outburst and the corresponding progenitor magnitude versus metallicity is shown. Triangles are lower limits. The data suggest larger ΔM at larger metallicity. Red corresponds to R/unf. bands, blue to B band, green to V band, magenta to I band, brown to NIR, orange to R/V.

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© ESO, 2015

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