Table 2
SN sites observed with SINFONI.
| SN (type) | BrγEW (Å) | CO EW (Å) | BrγEW age (Myr) | CO EW age (Myr) | HαEW age (Myr) |
|---|---|---|---|---|---|
| 1970A (II) | 4.6 ± 1.5 | Not detected |  |
– | 7.18 |
| 1985P (IIP) | Not detected | Not detected | – | – | Not detected |
| 1992ba (IIP) | Not detected | Not detected | – | – |  |
| 1997X (Ic) | 3.2 ± 2.7 | − 13.4 ± 5.8 |  |
>7.54 |  |
| 1999br (IIP) | Not detected | Not detected | – | – |  |
| 2000ew (Ic) | Not detected | Not detected | – | – |  |
| 2004dg (IIP) + 2012P (IIb) | 91.2 ± 5.2 | Not detected |  |
– |  |
| 2009dq (IIb) | 7.9 ± 0.7 | − 12.9 ± 2.3 |  |
>7.70 |  |
| 2012A (IIP) | Not detected | Not detected | – | – |  |
| 2012au (Ib) | Not detected | Not detected | – | – |  |
| 1923A (II) | 8.2 ± 3.0 | − 16.1 ± 3.8 |  |
>7.85 | – |
Notes. CO EW is presented with a negative value to indicate that it is measured from absorption line. The SN 1923A explosion site at NGC 5236 was observed with SINFONI, but not included in the main optical sample for analysis. SNe 2004dg and 2012P occurred very close together within ~2′′, on the sameH II region. The flag “not detected” indicates that the line is not observed at the SN position within 3σ.
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