J/ApJ/845/85 Absorption velocities for 21 super-luminous SNe Ic (Liu+, 2017)
Analyzing the largest spectroscopic data set of hydrogen-poor super-luminous
supernovae.
Liu Y.-Q., Modjaz M., Bianco F.B.
<Astrophys. J., 845, 85-85 (2017)>
=2017ApJ...845...85L 2017ApJ...845...85L (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Redshifts ; Spectroscopy
Keywords: methods: data analysis; supernovae: general;
supernovae: individual: (ASASSN-15lh, SN 2011kl, SN 2007bi)
Abstract:
Super-luminous supernovae (SLSNe) are tremendously luminous explosions
whose power sources and progenitors are highly debated. Broad-lined
SNe Ic (SNe Ic-bl) are the only type of SNe that are connected with
long-duration gamma-ray bursts (GRBs). Studying the spectral
similarity and difference between the populations of hydrogen-poor
SLSNe (SLSNe Ic) and of hydrogen-poor stripped-envelope core-collapse
SNe, in particular SNe Ic and SNe Ic-bl, can provide crucial
observations to test predictions of theories based on various power
source models and progenitor models. In this paper, we collected all
of the published optical spectra of 32 SLSNe Ic, 21 SNe Ic-bl, as well
as 17 SNe Ic, quantified their spectral features, constructed average
spectra, and compared them in a systematic way using new tools we have
developed. We find that SLSNe Ic and SNe Ic-bl, including those
connected with GRBs, have comparable widths for their spectral
features and average absorption velocities at all phases. Thus, our
findings strengthen the connection between SLSNe Ic and GRBs. In
particular, SLSNe Ic have average FeIIλ5169 absorption
velocities of -15000±2600km/s at 10 days after peak, which are
higher than those of SNe Ic by ∼7000km/s on average. SLSNe Ic also
have significantly broader FeIIλ5169 lines than SNe Ic.
Moreover, we find that such high absorption and width velocities of
SLSNe Ic may be hard to explain with the interaction model, and none
of the 13 SLSNe Ic with measured absorption velocities spanning over
10 days has a convincing flat velocity evolution, which is
inconsistent with the magnetar model in one dimension. Lastly, we
compare SN 2011kl, the first SN connected with an ultra-long GRB, with
the mean spectrum of SLSNe Ic and of SNe Ic-bl.
Description:
We have collected the spectra of all available super-luminous
supernovae (SLSNe) Ic that have a date of maximum light published
before April of 2016. These SLSNe Ic were mainly discovered and
observed by the All-Sky Automated Survey for Supernovae (ASAS-SN), the
Catalina Real-Time Transient Survey, the Dark Energy Survey (DES), the
Hubble Space Telescope Cluster Supernova Survey, the Pan-STARRS1
Medium Deep Survey (PS1), the Public ESO Spectroscopic Survey of
Transient Objects (PESSTO), the Intermediate Palomar Transient Factory
(iPTF) as well as the Palomar Transient Factory (PTF), and the
Supernova Legacy Survey (SNLS). See table 1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 138 32 Spectral sample of super-luminous supernovae
(SLSNe) Ic
table2.dat 46 72 Measured absorption velocities
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/ApJ/690/1358 : Spectra of unusual optical transient SCP 06F6 (Barbary+, 2009)
J/ApJ/702/226 : Swift/UVOT panchromatic obs. of SN 2008D (Modjaz+, 2009)
J/ApJ/741/97 : Light curves of Ibc supernovae (Drout+, 2011)
J/ApJ/759/107 : Core-collapse SNe and host galaxies (Kelly+, 2012)
J/MNRAS/437/656 : SN PS1-11ap light curves (McCrum+, 2014)
J/ApJ/785/37 : Type Ic SN 2010mb optical photometry (Ben-Ami+, 2014)
J/ApJ/788/154 : Palomar Transient Factory SNe IIn photometry (Ofek+, 2014)
J/ApJS/213/19 : Optical and near-IR light curves of 64 SNe (Bianco+, 2014)
J/ApJ/793/38 : Palomar Transient Factory photometric obs. (Arcavi+, 2014)
J/ApJ/797/24 : Imaging observations of iPTF 13ajg (Vreeswijk+, 2014)
J/A+A/574/A60 : Light curve templates of SNe Ib/c from SDSS (Taddia+, 2015)
J/ApJ/819/35 : Light curves of four transients from PTF+SNLS (Arcavi+, 2016)
J/MNRAS/458/84 : Host galaxies of Superluminous Supernovae (Angus+, 2016)
J/ApJ/827/90 : Spectroscopy of SNe Ib, IIb and Ic (Liu+, 2016)
J/ApJ/828/3 : Swift obs. of the superluminous SNI ASASSN-15lh (Brown+, 2016)
J/ApJ/830/13 : Host-galaxy NUV-NIR data of superluminous SNe (Perley+, 2016)
J/ApJ/832/108 : Spectral properties of Type Ic + Ic-bl SNe (Modjaz+, 2016)
J/ApJ/836/25 : Swift UVOT light curves of ASASSN-15lh (Margutti+, 2017)
http://www.weizmann.ac.il/astrophysics/wiserep : WISeREP home page
http://zenodo.org/record/826368#.WsOW3eaYM-g : Added data products
for this paper
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Name Supernova Name
25- 26 A2 --- f_Name Flag on Name (1)
28- 44 A17 --- OName Other names, comma separated
46- 51 F6.4 --- zsp [0.09/1.6] Spectroscopic Redshift
53-118 A66 d Phases Phase(s) of spectra, comma separated (2)
120-133 A14 --- Filt Light curve (LC) filters (3)
135-138 A4 --- Ref References (4)
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Note (1): Flags on individual SN as follows:
* = Whether this is a SN or tidal disruption event is still debated;
** = This is the only SLSN that was discovered in connection with an
ultra-long GRB.
Note (2): Phases are in the rest-frame with respect to maximum light and
rounded to the nearest whole day. The number in parentheses is the
number of spectra with phases larger than 90 days after the date of
maximum light, which we include for completeness, but do not analyze
here. The references for the date of maximum light are the same as
references in the last column.
Note (3): Light curve (LC) filters are used to determine dates of maximum
light in references in the last column. The LC filters without
parentheses are in the observed-frame, while those in parentheses are in
the rest-frame. The latter is either converted to rest frame in this
paper or taken from the references in the last column. For PS1-10ky and
PS1-10awh The authors set a date of maximum light based on LCs on g, r,
i, z, y-filters. Thus, the date of maximum light is a rough estimate,
not a true measurement.
Note (4): References. References are only for the SN spectra, not for the SN
discovery. Reference as follows:
1 = Barbary et al. (2009, J/ApJ/690/1358)
2 = Chen et al. (2017A&A...602A...9C 2017A&A...602A...9C)
3 = Chomiuk et al. (2011ApJ...743..114C 2011ApJ...743..114C)
4 = Dong et al. (2016Sci...351..257D 2016Sci...351..257D)
5 = Gal-Yam et al. (2009Natur.462..624G 2009Natur.462..624G)
6 = Greiner et al. (2015Natur.523..189G 2015Natur.523..189G)
7 = Howell et al. (2013ApJ...779...98H 2013ApJ...779...98H)
8 = Inserra et al. (2013ApJ...770..128I 2013ApJ...770..128I)
9 = Leloudas et al. (2012A&A...541A.129L 2012A&A...541A.129L)
10 = Lunnan et al. (2013ApJ...771...97L 2013ApJ...771...97L)
11 = McCrum et al. (2014, J/MNRAS/437/656)
12 = Nicholl et al. (2013Natur.502..346N 2013Natur.502..346N)
13 = Nicholl et al. (2014MNRAS.444.2096N 2014MNRAS.444.2096N)
14 = Nicholl et al. (2015ApJ...807L..18N 2015ApJ...807L..18N)
15 = Nicholl et al. (2016ApJ...826...39N 2016ApJ...826...39N)
16 = Quimby et al. (2007ApJ...668L..99Q 2007ApJ...668L..99Q)
17 = Quimby et al. (2011Natur.474..487Q 2011Natur.474..487Q)
18 = Papadopoulos et al. (2015MNRAS.449.1215P 2015MNRAS.449.1215P)
19 = Smith et al. (2016ApJ...818L...8S 2016ApJ...818L...8S)
20 = Vreeswijk et al. (2014, J/ApJ/797/24)
21 = Yan et al. (2015ApJ...814..108Y 2015ApJ...814..108Y)
22 = Young et al. (2010A&A...512A..70Y 2010A&A...512A..70Y)
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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- 23 A23 --- Name SN Name
25- 27 I3 d Phase [-28/68] Phase, with respect to maximum light (1)
29- 34 I6 km/s vabs [-22300/-3970] FeIIλ5169 absorption
velocity (2)
37- 40 I4 km/s E_vabs [268/5930] Positive uncertainty on vabs
43- 46 I4 km/s e_vabs [148/6070] Negative uncertainty on vabs
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Note (1): Phases are in the rest-frame with respect to maximum light and
rounded to the nearest whole day.
Note (2): Velocities at phases less than 10 days after max may not be
accurate, since the feature may have been contaminated by FeIII (see
section 3.1.1. for discussion) and are not included in our subsequent
analysis, but are provided here for completeness.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-Apr-2018