2013A&A...558A.143T


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:51:15

2013A&A...558A.143T - Astronomy and Astrophysics, volume 558A, 143-143 (2013/10-1)

A metallicity study of 1987A-like supernova host galaxies.

TADDIA F., SOLLERMAN J., RAZZA A., GAFTON E., PASTORELLO A., FRANSSON C., STRITZINGER M.D., LELOUDAS G. and ERGON M.

Abstract (from CDS):

The origin of the blue supergiant (BSG) progenitor of Supernova (SN) 1987A has long been debated, along with the role that its sub-solar metallicity played. We now have a sample of SN 1987A-like events that arise from the rare core collapse (CC) of massive (∼20M) and compact (≲100R) BSGs. The metallicity of the explosion sites of the known BSG SNe is investigated, as well as the association of BSG SNe to star-forming regions. Both indirect and direct metallicity measurements of 13 BSG SN host galaxies are presented, and compared to those of other CC SN types. Indirect measurements are based on the known luminosity-metallicity relation and on published metallicity gradients of spiral galaxies. In order to provide direct metallicity measurements based on strong line diagnostics, we obtained spectra of each BSG SN host galaxy both at the exact SN explosion sites and at the positions of other HII regions. We also observed these hosts with narrow Hα and broad R-band filters in order to produce continuum-subtracted Hα images. This allows us to measure the degree of association between BSG SNe and star-forming regions, and to compare it to that of other SN types. BSG SNe are found to explode either in low-luminosity galaxies or at large distances from the nuclei of luminous hosts. Therefore, their indirectly measured metallicities are typically lower than those of SNe IIP and Ibc. This result is confirmed by the direct metallicity estimates, which show slightly sub-solar oxygen abundances (12+log(O/H)∼8.3-8.4dex) for the local environments of BSG SNe, similar to that of the Large Magellanic Cloud (LMC), where SN 1987A exploded. However, we also note that two objects of our sample (SNe 1998A and 2004em) were found at near solar metallicity. SNe IIb have a metallicity distribution similar to that of our BSG SNe. Finally, we find that the degree of association to star-forming regions is similar among BSG SNe, SNe IIP and IIn. Our results suggest that LMC metal abundances play a role in the formation of some 1987A-like SNe. This would naturally fit in a single star scenario for the progenitors. However, the existence of two events at nearly solar metallicity suggests that also other channels, e.g. binarity, contribute to produce BSG SNe.

Abstract Copyright:

Journal keyword(s): supernovae: general - stars: evolution - galaxies: abundances

Simbad objects: 33

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Number of rows : 33

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SN 2005db SN* 00 41 26.79 +25 29 51.6     17.3     SNIIn 25 1
2 SN 2004ek SN* 01 09 58.51 +32 22 47.7     17.1     SNII 19 1
3 UGC 724 GiG 01 09 59.4026726823 +32 22 06.409141075   14.0       ~ 55 0
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
5 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4485 2
6 2MASX J05553978-6855381 Lev 05 55 39.781 -68 55 38.17   16.16   15.58   ~ 4 0
7 CXOU J095546.6+694037 HXB 09 55 46.6554840699 +69 40 37.878213478           SNIIP 42 1
8 SN 1998A SN* 11 09 50.33 -23 43 43.1       17.0   SNIIpec 47 1
9 SN 1994R SN* 11 09 51.32 -23 43 34.7     16     SNII 9 1
10 IC 2627 EmG 11 09 53.3869919103 -23 43 33.174011728   12.67   11.36 11.9 ~ 98 0
11 SN 2010gx SN* 11 25 46.71 -08 49 41.4           SNIc 129 1
12 SN 2006V SN* 11 31 30.01 -02 17 52.2     18.0     SNII 28 1
13 UGC 6510 G 11 31 32.0801974768 -02 18 33.136716649   14.0       ~ 43 0
14 NGC 4141 G 12 09 47.3107821922 +58 50 57.257545305   14.5       ~ 58 0
15 SN 2009E SN* 12 09 49.56 +58 50 50.3           ~ 42 1
16 NGC 4485 GiP 12 30 31.113 +41 42 04.22 12.10 12.42 11.93 11.93   ~ 253 2
17 NGC 4490 GiP 12 30 36.368 +41 38 37.07 10.03 10.22 9.79     ~ 525 3
18 SN 1982F SN* 12 30 38 +41 38.0   16.2       SNIIP 38 1
19 SN 2008ax SN* 12 30 40.80 +41 38 16.1   23.6 23.5 14.1 22.6 SNIIb 207 1
20 SN 1998bt SN* 13 25 41.93 -26 46 55.7     19.7     ~ 7 1
21 Anon J132541-2646 G 13 25 41.93 -26 46 55.7           ~ 2 0
22 SN 1909A SN* 14 02 03.17 +54 28 05.9   13.5 13.50     SNIIP: 52 1
23 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 2546 2
24 NGC 5630 G 14 27 36.581 +41 15 28.14   13.6       ~ 91 0
25 SN 2005dp SN* 14 27 36.62 +41 15 15.0     16.0     SNII 20 1
26 SN 2005ci SN* 14 34 44.88 +48 40 19.8     18.5     SNII 28 1
27 NGC 5682 GiP 14 34 44.963 +48 40 12.93   15.1       ~ 83 0
28 SN 2000cb SN* 16 01 32.15 +01 42 23.0     18.0     SNII 47 1
29 IC 1158 G 16 01 34.072 +01 42 28.19   13.2   13.3 12.9 ~ 73 0
30 SN 2006au SN* 17 57 13.56 +12 11 03.2     17.2     SNII 21 1
31 UGC 11057 G 17 57 14.934 +12 10 46.32   13.8       ~ 39 0
32 IC 1303 GiG 19 31 30.051 +35 52 35.82   15.0       ~ 33 0
33 SN 2004em SN* 19 31 31.11 +35 52 15.7     17.5     SNII 16 1

    Equat.    Gal    SGal    Ecl

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2020.07.14-18:51:15

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