J/MNRAS/444/2428 Disturbance levels of SNe host galaxies (Hakobyan+, 2014)
Supernovae and their host galaxies.
II. The relative frequencies of supernovae types in spirals.
Hakobyan A.A., Nazaryan T.A., Adibekyan V.Z., Petrosian A.R., Aramyan L.S.,
Kunth D., Mamon G.A., de Lapparent V., Bertin E., Gomes J.M., Turatto M.
<Mon. Not. R. Astron. Soc., 444, 2428-2441 (2014)>
=2014MNRAS.444.2428H 2014MNRAS.444.2428H
ADC_Keywords: Supernovae ; Galaxies, optical ; Galaxies, peculiar
Keywords: supernovae: general - galaxies: active - galaxies: interactions -
galaxies: spiral - galaxies: stellar content
Abstract:
We present an analysis of the relative frequencies of different
supernova (SN) types in spirals with various morphologies and in
barred or unbarred galaxies. We use a well-defined and homogeneous
sample of spiral host galaxies of 692 SNe from the Sloan Digital Sky
Survey in different stages of galaxy-galaxy interaction and activity
classes of nucleus. We propose that the underlying mechanisms shaping
the number ratios of SNe types can be interpreted within the framework
of interaction-induced star formation, in addition to the known
relations between morphologies and stellar populations. We find a
strong trend in behaviour of the NIa/NCC ratio depending
on host morphology, such that early spirals include more Type Ia SNe.
The NIbc/NII ratio is higher in a broad bin of early-type
hosts. The NIa/NCC ratio is nearly constant when changing
from normal, perturbed to interacting galaxies, then declines in
merging galaxies, whereas it jumps to the highest value in
post-merging/remnant galaxies. In contrast, the NIbc/NII
ratio jumps to the highest value in merging galaxies and slightly
declines in post-merging/remnant subsample. The interpretation is that
the star formation rates and morphologies of galaxies, which are
strongly affected in the final stages of interaction, have an impact
on the number ratios of SNe types. The NIa/NCC (NIbc/NII)
ratio increases (decreases) from star-forming to active galactic
nuclei (AGN) classes of galaxies. These variations are consistent with
the scenario of an interaction-triggered starburst evolving into AGN
during the later stages of interaction, accompanied with the change of
star formation and transformation of the galaxy morphology into an
earlier type.
Description:
The full table of disturbance levels for 608 individual host galaxies
of SNe. We define for all 608 hosts their level of morphological
disturbance with the possible presence of signs of interactions and
mergers.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 32 608 Disturbance levels of 608 individual host galaxies
--------------------------------------------------------------------------------
See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/PASP/117/773 : Classifications of SN host galaxies. III (van den Bergh+ 2005)
J/A+A/544/A81 : Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)
http://www.sdss.org : SDSS Home Page
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Hgal SN host galaxy identification (1)
21- 32 A12 --- Dlev Disturbance level of SN host galaxy (2)
--------------------------------------------------------------------------------
Note (1): JHHMMSS.ss+DDMMSS.s for SDSS JHHMMSS.ss+DDMMSS.s
Note (2): We define four categories of SN host disturbances as:
normal = hosts without any visible disturbance in their morphological
structure
perturbed = hosts with visible morphological disturbance, but without long
tidal arms, bridges, or destruction of spiral patterns
interacting = hosts with obvious signs of galaxy-galaxy interaction
merging = hosts with evidence of an ongoing merging process;
see e.g. Lambas et al., 2012A&A...539A..45L 2012A&A...539A..45L
p-merg./rem. = post-merging/remnant, single galaxies that exhibit signs of a
past interaction, with a strong or already relaxed
disturbance, see e.g. Ellison et al., 2013MNRAS.435.3627E 2013MNRAS.435.3627E and
Lotz et al., 2008MNRAS.391.1137L 2008MNRAS.391.1137L, respectively
--------------------------------------------------------------------------------
Acknowledgements:
Artur Hakobyan, hakobyan(at)bao.sci.am
References:
Hakobyan et al., Paper I 2012A&A...544A..81H 2012A&A...544A..81H, Cat. J/A+A/544/A81
(End) Artur Hakobyan [BAO], Patricia Vannier [CDS] 23-Apr-2015