J/A+A/580/A131 Circumstellar-interacting supernovae (Taddia+, 2015)
Metallicity at the explosion sites of interacting transients.
Taddia F., Sollerman J., Fremling C., Pastorello A., Leloudas G.,
Fransson C., Nyholm A., Stritzinger M.D., Ergon M., Roy R., Migotto K.
<Astron. Astrophys., 580, A131-131 (2015)>
=2015A&A...580A.131T 2015A&A...580A.131T (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Morphology ; Photometry, UBVRI ; Abundances
Keywords: supernovae: general - stars: evolution - galaxies: abundances -
circumstellar matter - stars: winds, outflows
Abstract:
Some circumstellar-interacting (CSI) supernovae (SNe) are produced by
the explosions of massive stars that have lost mass shortly before the
SN explosion. There is evidence that the precursors of some SNe IIn
were luminous blue variable (LBV) stars. For a small number of CSI
SNe, outbursts have been observed before the SN explosion. Eruptive
events of massive stars are named SN impostors (SN IMs) and whether
they herald a forthcoming SN or not is still unclear. The large
variety of observational properties of CSI SNe suggests the existence
of other progenitors, such as red supergiant (RSG) stars with
superwinds. Furthermore, the role of metallicity in the mass loss of
CSI SN progenitors is still largely unexplored. Our goal is to gain
insight into the nature of the progenitor stars of CSI SNe by studying
their environments, in particular the metallicity at their locations.
We obtain metallicity measurements at the location of 60 transients
(including SNe IIn, SNe Ibn, and SN IMs) via emission-line diagnostic
on optical spectra obtained at the Nordic Optical Telescope and
through public archives. Metallicity values from the literature
complement our sample. We compare the metallicity distributions among
the different CSI SN subtypes, and to those of other core-collapse SN
types. We also search for possible correlations between metallicity
and CSI SN observational properties. We find that SN IMs tend to occur
in environments with lower metallicity than those of SNe IIn. Among
SNe IIn, SN IIn-L(1998S-like) SNe show higher metallicities, similar
to those of SNe IIL/P, whereas long-lasting SNe IIn (1988Z-like) show
lower metallicities, similar to those of SN IMs. The metallicity
distribution of SNe IIn can be reproduced by combining the metallicity
distributions of SN IMs (which may be produced by major outbursts of
massive stars like LBVs) and SNe IIP (produced by RSGs). The same
applies to the distributions of the normalized cumulative rank (NCR)
values, which quantifies the SN association to HII regions. For SNe
IIn, we find larger mass-loss rates and higher CSM velocities at
higher metallicities. The luminosity increment in the optical bands
during SN IM outbursts tend to be larger at higher metallicity,
whereas the SN IM quiescent optical luminosities tend to be lower. The
difference in metallicity between SNe IIn and SN IMs indicates that
LBVs are only one of the progenitor channels for SNe IIn, with
1988Z-like and 1998S-like SNe possibly arising from LBVs and RSGs,
respectively. Finally, even though line-driven winds likely do not
primarily drive the late mass-loss of CSI SN progenitors, metallicity
has some impact on the observational properties of these transients.
Description:
In Table 1 we report the list of 60 transients included in our sample.
Thirty-five of them are SNe IIn, six are SNe Ibn, one is a SN Ia-CSM,
18 are SN IMs (if we also count SN 2009ip in the SN IMs, then we have
19 of these transients).
With the NOT, long-slit spectra were obtained for the host galaxies of
13 SNe IIn, five SNe Ibn, one SN Ia-CSM, and 16 SN IMs (the derived
metallicity for SN 2007sv was published in Tartaglia et al.
2015MNRAS.447..117T 2015MNRAS.447..117T). The host galaxies observed at the NOT are marked
with the letter "o" in the third column of Table 1. With the NOT, we
also obtained broad-band R and narrow-band Hα images for the SNe
IIn (except for SN 1995G) and Ibn. We complemented our observed sample
with host galaxies whose metallicities (at the center of the galaxy or
at the SN position) were already available in the literature (marked
with the letter "l" in the third column of Table 1) or whose spectra
were available in public archives (marked with the letter "a" in the
third column of Table 1).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 160 60 Sample and basic data of 63 (38 SNe IIn,
6 SNe Ibn, 1 SN Ia-CSM, 18 SN IMs)
CSI SN host galaxies
table2.dat 77 35 Log of the photometric and spectroscopic
observations at the Nordic Optical Telescope
with ALFOSC
table3.dat 33 141 Deprojected and normalized distance from the
host center and line ratios for the HII regions
with observed spectrum
table5.dat 156 42 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
table6.dat 61 42 Absolute (U/u,B,V,R/r/unf.,I/i) peak magnitudes
for the SNe IIn, Ibn, and Ia-CSM of our sample
table7.dat 86 29 Wind velocity and mass-loss rate for a
subsample of CSI SNe (IIn, Ibn, Ia-CSM).
refs.dat 70 56 References
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- SN SN name
10- 19 A10 --- Type SN type
26- 28 A3 --- Source [ola/ ] Data source (1)
30- 56 A27 --- Host Host galaxy
58- 65 F8.6 --- z Redshift
67- 68 I2 h RAh SN right ascension (J2000)
70- 71 I2 min RAm SN right ascension (J2000)
73- 77 F5.2 s RAs SN right ascension (J2000)
79 A1 --- DE- SN declination sign (J2000)
80- 81 I2 deg DEd SN declination (J2000)
83- 84 I2 arcmin DEm SN declination (J2000)
86- 89 F4.1 arcsec DEs SN declination (J2000)
91- 92 I2 h RAHh Host galaxy right ascension (J2000)
94- 95 I2 min RAHm Host galaxy right ascension (J2000)
97-101 F5.2 s RAHs Host galaxy right ascension (J2000)
103 A1 --- DEH- Host galaxy declination sign (J2000)
104-105 I2 deg DEHd Host galaxy declination (J2000)
107-108 I2 arcmin DEHm Host galaxy declination (J2000)
110-113 F4.1 arcsec DEHs Host galaxy declination (J2000)
115-121 F7.4 arcmin 2a ?=- Major axis
123-129 F7.4 arcmin 2b ?=- Minor axis
131-134 F4.1 --- ttype ?=- t-type (2)
135 A1 --- l_ttype [h] h: from Hyperleda
137-139 I3 deg PA ?=- Position angle
141-147 A7 --- r2a Reference for a and b axis (3)
149-155 A7 --- rPA Reference for PA (3)
157-160 F4.2 --- rSN/R25 ?=- Radius ratio
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Note (1): Data sources as follows:
o = observed
l = literature
a = archive
Note (2): The t-type is obtained from the ASC.
Note (3): References as follows:
NED = B band (de Vaucouleurs et al., 1991, Cat. VII/155/)
NED(B) = B band (Palomar survey)
NED(R) = r band (SDSS)
NED(IR) = K band (2MASS)
NED(Be) = B band (ESO survey)
HYP = Hyperleda
H97 = Hagen et al., 1997A&A...324L..29H 1997A&A...324L..29H
ASI = Asiago Supernova Catalogue,
https://heasarc.gsfc.nasa.gov/W3Browse/all/asiagosn.html
NED = From NED
SIM(IR) = From Simbad
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- SN SN name
9- 18 A10 --- Type SN type
25- 38 A14 --- Galaxy Galaxy name
41 A1 --- Phot1 Photometry filter
43- 48 A6 --- Int1 Integration time for Phot1 filter (s)
50- 56 A7 --- Phot2 Photometry filter
58- 62 A5 --- Int2 Integration time for Phot2 filter (s)
64- 77 A14 --- IntSp Spectroscopy integration time (s) (1)
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Note (1): Spectroscopic observations were performed with Slit 1.0 +Grism #4.
We could not image the host galaxies of the SN IMs because during the
observational campaign of April 2014 several nights were lost due to bad
weather, and we decided to spend the remaining nights doing spectroscopy.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- SN SN name
11- 15 F5.3 --- r/R25 ? Deprojected and normalized distance
from the host center
16- 17 A2 --- n_r/R25 [** SN] Note on r/R25 (1)
19 A1 --- l_log(FNII/FHa) Upper limit flag on log(FNII/FHa)
20- 25 F6.3 [-] log(FNII/FHa) Line ratio F([NII]6584)/F(Hα)
27 A1 --- l_log(FOIII/FHb) Upper limit flag on log(FOIII/FHb)
28- 33 F6.3 [-] log(FOIII/FHb) Line ratio F([OIII]5007)/F(Hβ)
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Note (1): Notes as follows:
** = Excluded from the metallicity analysis after spectral classification
with the BPT diagram.
SN = No Deprojected and normalized distance
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- SN SN name
10- 19 A10 --- Type SN type
25 A1 --- l_Umax Limit flag on Umax
26- 32 F7.4 mag Umax ?=- Apparent U peak magnitude
34- 37 F4.2 mag e_Umax ? rms uncertainty on Umax
40 A1 --- n_Umax [u] u: u magnitude
43 A1 --- l_Bmax Limit flag on Bmax
44- 50 F7.4 mag Bmax ?=- Apparent B peak magnitude
52- 55 F4.2 mag e_Bmax ? rms uncertainty on Bmax
59 A1 --- l_Vmax Limit flag on Vmax
60- 66 F7.4 mag Vmax ?=- Apparent V peak magnitude
68- 71 F4.2 mag e_Vmax ? rms uncertainty on Vmax
74 A1 --- l_Rmax Limit flag on Rmax
75- 79 F5.2 mag Rmax ?=- Apparent R peak magnitude
81- 84 F4.2 mag e_Rmax ? rms uncertainty on Rmax
87 A1 --- n_Rmax [ur] r: r magnitude; u: unf magnitude
91 A1 --- l_Imax Limit flag on Imax
92- 97 F6.3 mag Imax ?=- Apparent I peak magnitude
99-102 F4.2 mag e_Imax ? rms uncertainty on Imax
105 A1 --- n_Imax [i] i: imax magnitude
108-112 F5.3 mag AV(MW) Galactic extinction
116-120 F5.3 mag AV(h) ?=- Host extinction
124-156 A33 --- Ref References (1)
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Note (1): Reference number into parenthesis in refs.dat file.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- SN SN name
10- 19 A10 --- Type SN type
21 A1 --- l_U/uMax Limit flag on U/uMax
22- 27 F6.2 mag U/uMax ?=- Absolute U or u peak magnitude
29 A1 --- l_BMax Limit flag on BMax
30- 35 F6.2 mag BMax ?=- Absolute B peak magnitude
37 A1 --- l_VMax Limit flag on VMax
38- 43 F6.2 mag VMax ?=- Absolute V peak magnitude
46 A1 --- l_R/r/unfMax Limit flag on R/r/unfMax
47- 53 F7.3 mag R/r/unfMax ? Absolute R, r or unf peak magnitude
55 A1 --- l_I/iMax Limit flag on I/iMax
56- 61 F6.2 mag I/iMax ?=- Absolute I or i peak magnitude
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- SN SN name
10- 19 A10 --- Type SN type
25 A1 --- l_Vw Limit flag on Vw
26- 29 I4 km/s Vw Wind velocity
30 A1 --- --- [-]
31- 34 I4 km/s Vwu ? Upper value of Vw when interval
37- 40 I4 km/s e_Vw ? rms uncertainty on Vw
42 A1 --- l_dM/dt Limit flag on dM/dt
43- 48 F6.4 Msun/yr dM/dt ?=- Mass-loss rate
49 A1 --- --- [-]
50- 55 F6.4 Msun/yr dM/dtu ? Upper value of dM/dt when interval
57- 62 F6.4 Msun/yr e_dM/dt ? rms uncertainty on dM/dt
65- 86 A22 --- Ref References and notes (1)
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Note (1): * for SN 1998S: Fassia et al. (2000MNRAS.318.1093F 2000MNRAS.318.1093F) report a
mass-loss rate of 2x10-5M_☉/yr for the outer CSM and 3x10-3M_☉/yr
for the inner CSM. The value reported by Anupama et al. (2001A&A...367..506A 2001A&A...367..506A)
is in the middle of this range.
Reference number into parenthesis in refs.dat file.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 41 A18 --- Aut Author's name
43- 70 A28 --- Com Comments
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 03-Nov-2015