J/MNRAS/471/1390 Properties of 102 SNe and their 100 hosts (Hakobyan+, 2017)
Supernovae and their host galaxies.
V. The vertical distribution of supernovae in disc galaxies.
Hakobyan A.A., Barkhudaryan L.V., Karapetyan A.G., Mamon G.A., Kunth D.,
Adibekyan V., Aramyan L.S., Petrosian A.R., Turatto M.
<Mon. Not. R. Astron. Soc. 471, 1390 (2017)>
=2017MNRAS.471.1390H 2017MNRAS.471.1390H (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Galaxies, optical ; Galaxy catalogs ;
Morphology ; Positional data ; Surveys
Keywords: supernovae: general - Galaxy: disc - galaxies: spiral -
galaxies: stellar content - galaxies: structure
Abstract:
We present an analysis of the height distributions of the different
types of supernovae (SNe) from the plane of their host galaxies. We
use a well-defined sample of 102 nearby SNe appearing inside
high-inclined (i≥85°), morphologically non-disturbed S0-Sd host
galaxies from the Sloan Digital Sky Survey. For the first time, we
show that in all the subsamples of spirals, the vertical distribution
of core-collapse (CC) SNe is about twice closer to the plane of the
host disc than the distribution of SNe Ia. In Sb-Sc hosts, the
exponential scale height of CC SNe is consistent with those of the
younger stellar population in the Milky Way (MW) thin disc, while the
scale height of SNe Ia is consistent with those of the old population
in the MW thick disc. We show that the ratio of scale lengths to scale
heights of the distribution of CC SNe is consistent with those of the
resolved young stars with ages from ∼10 up to ∼100Myr in nearby
edge-on galaxies and the unresolved stellar population of
extragalactic thin discs. The corresponding ratio for SNe Ia is
consistent with the same ratios of the two populations of resolved
stars with ages from a few 100Myr up to a few Gyr and from a few Gyr
up to ∼10Gyr, as well as with the unresolved population of the thick
disc. These results can be explained considering the age-scale height
relation of the distribution of stellar population and the mean age
difference between Type Ia and CC SNe progenitors.
Description:
The full database of 102 individual SNe (SN designation, type,
equatorial coordinates, V and U) and their 100 host galaxies (galaxy
SDSS designation, distance, morphological type and corrected g-band
D25).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 92 102 Properties of 102 SNe and their 100 hosts
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/A+A/544/A81 : Supernovae and their hosts in SDSS DR8 (Hakobyan+, 2012)
J/MNRAS/444/2428 : Disturbance levels of SNe host galaxies (Hakobyan+, 2014)
J/MNRAS/456/2848 : Properties of 500 SNe and their 419 hosts (Hakobyan+, 2016)
J/MNRAS/459/3130 : Lists of arm and interarm supernovae (Aramyan+, 2016)
http://www.sdss.org : SDSS Home Page
Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- SN Supernova (SN) designation
8- 13 A6 --- Type SN type (from spectroscopy)
14 A1 --- n_Type [*] Note on SN type (1)
15 A1 --- u_Type [:] Uncertainty flag on SN type
17- 26 F10.6 deg RAdeg Right ascension (J2000) of SN
28- 36 F9.6 deg DEdeg Declination (J2000) of SN
38- 43 F6.2 arcsec Vcoor The V coordinate of SN along the minor axis
of host galaxy
45- 51 F7.2 arcsec Ucoor The U coordinate of SN along the major axis
of host galaxy
53- 71 A19 --- Gal SN host galaxy identification (2)
73- 79 F7.3 Mpc Dist Host galaxy distance
81- 84 A4 --- MType Host galaxy morphological type
85 A1 --- u_MType [:?] Uncertainty flag on morphology (3)
87- 92 F6.2 arcsec Diam Host galaxy diameter (4)
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Note (1): For SN 1962A, SN type has been inferred from the light curve
and marked by "*".
Note (2): JHHMMSS.ss+DDMMSS.s for SDSS JHHMMSS.ss+DDMMSS.s
An alternative name is mentioned when SDSS identification was not
possible to obtain.
Note (3): Uncertainties in host galaxy morphological type are marked by ":"
and "?" (highly uncertain).
Note (4): Corrected major axis in arcsec (isophotal level of 25mag/arcsec2
in the SDSS g-band) of the host galaxy.
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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
Hakobyan et al., Paper II 2014MNRAS.444.2428H 2014MNRAS.444.2428H, Cat. J/MNRAS/444/2428
Hakobyan et al., Paper III 2016MNRAS.456.2848H 2016MNRAS.456.2848H, Cat. J/MNRAS/456/2848
Aramyan et al., Paper IV 2016MNRAS.459.3130A 2016MNRAS.459.3130A, Cat. J/MNRAS/459/3130
(End) Artur Hakobyan [BAO], Patricia Vannier [CDS] 15-Sep-2017