J/MNRAS/482/1545 Berkeley sample of stripped-envelope SNe (Shivvers+, 2019)
The Berkeley sample of stripped-envelope supernovae.
Shivvers I., Filippenko A.V., Silverman J.M., Zheng W., Foley R.J.,
Chornock R., Barth A.J., Cenko S.B., Clubb K.I., Fox O.D.,
Ganeshalingam M., Graham M.L., Kelly P.L., Kleiser I.K.W., Leonard D.C.,
Li W., Matheson T., Mauerhan J.C., Modjaz M., Serduke F.J.D., Shields J.C.,
Steele T.N., Swift B.J., Wong D.S., Yuk H.
<Mon. Not. R. Astron. Soc., 482, 1545-1556 (2019)>
=2019MNRAS.482.1545S 2019MNRAS.482.1545S (SIMBAD/NED BibCode)
ADC_Keywords: Spectroscopy ; Supernovae
Keywords: techniques: spectroscopic - astronomical data bases: miscellaneous -
stars: massive - supernovae: general
Abstract:
We present the complete sample of stripped-envelope supernova (SN)
spectra observed by the Lick Observatory Supernova Search (LOSS)
collaboration over the last three decades: 888 spectra of 302 SNe, 652
published here for the first time, with 384 spectra (of 92 SNe) having
photometrically determined phases. After correcting for redshift and
Milky Way dust reddening and reevaluating the spectroscopic
classifications for each SN, we construct mean spectra of the three
major spectral subtypes (Types IIb, Ib, and Ic) binned by phase. We
compare measures of line strengths and widths made from this sample to
the results of previous efforts, confirming that OIλ7774
absorption is stronger and found at higher velocity in Type Ic SNe
than in Types Ib or IIb SNe in the first ∼30 days after peak
brightness, though the widths of nebular emission lines are consistent
across subtypes. We also highlight newly available observations for a
few rare subpopulations of interest.
Description:
Our data include observations obtained with a variety of instruments
mounted on the telescopes at Lick and Keck Observatories: the UV
Schmidt spectrograph (1987-1992; Miller & Stone 1987, Lick Observatory
Techical Reports . p. 48) and the Kast Double Spectrograph (since
1992; Miller & Stone 1993, Lick Observatory Techical Reports. p. 66)
on the Shane 3m telescope, and the Low Resolution Imaging Spectrometer
(LRIS; Oke et al. 1995PASP..107..375O 1995PASP..107..375O), the Echellette Spectrograph
and Imager (ESI; Sheinis et al. 2002PASP..114..851S 2002PASP..114..851S), and the DEep
Imaging Multi-Object Spectrograph (DEIMOS; Faber et al.
2003SPIE.4841.1657F 2003SPIE.4841.1657F), on the two Keck 10m telescopes. Taking advantage
of a few nights on the Shane 3m every lunar cycle, augmented by
occasional nights with one of the Keck telescopes, our group strives
to maintain a steady cadence of observations for all of the SNe we
study - Silverman et al. (2012MNRAS.425.1789S 2012MNRAS.425.1789S, Cat. J/MNRAS/425/1789)
describe our observing strategies in more detail. For the sample of
spectra presented here, we calculate a typical (median) time lag of
14.8d between successive observations of any given SN.
Table 2 presents the sample of SNe included in this data release, our
adopted classifications and dates of peak brightness (if available),
and the values we used to perform redshift and dust-reddening
corrections. Table 3 provides a description of the spectra included in
our sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 88 317 The SNe in our sample
table3.dat 99 888 The spectra presented in this paper
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See also:
J/MNRAS/425/1789 : Berkeley supernova Ia program. I. (Silverman+, 2012)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Supernova name
15- 33 A19 --- Type Supernova type
35- 58 A24 --- Host Supernova host galaxy
60- 67 F8.5 --- z Values used to perform redshift corrections
69- 73 F5.3 mag E(B-V) Values used to perform Milky Way
dust-reddening corrections
75- 81 F7.1 d tpeak ? Modified Julian Date of peak brightness
83- 85 F3.1 d e_tpeak ? Error on tpeak
87- 88 I2 --- Nspectra Number of spectra
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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- 13 A13 --- Name Supernova name (1)
15- 33 A19 --- Type Supernova type
35- 48 A14 "Y:M:D" Date UT Date of observation
50- 55 F6.1 d Phase ? Phase, days relative to peak brightness,
if date of peak is constrained
57- 59 F3.1 d e_Phase ? Error on Phase
61- 83 A23 --- Inst Instrument
85- 88 I4 0.1nm wvlmin Wavelenght range (minimum)
90- 94 I5 0.1nm wvlmax Wavelenght range (maximum)
96- 99 A4 0.1nm Res Estimated average resolution across the
spectrum
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Note (1): SN 1985F's historical spectrum was observed under unique conditions -
we exclude from our analyses below but we include it here for
completeness.
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 28-Jun-2022