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Table A.1.

Sample of 61 ordinary type Ic-BL SNe and 13 GRB-SNe used for velocity measurements, showing the event name, SN type, redshift (z), explosion time (texp) and its uncertainty (Δtexp), the number of spectra in the sample, and the data source.

Event name SN Type* z texp [UTC]† Δtexp [days] Num. Spectra‡ Sources
GRB980425-SN1998bw GRB-SN 0.008499 1998-04-25T21:49:11 29 (5) 1, 2, WISeREP1, GRBSNWebtool2
GRB030329-SN2003dh GRB-SN 0.1685 2003-03-29T11:37:14 16 (0) 3, 4, WISeREP, GRBSNWebtool
GRB060218-SN2006aj GRB-SN 0.033023 2006-02-18T03:34:31 34 (3) 5, 6, 7, 8, WISeREP, GRBSNWebtool, GRBNASASwift3
GRB100316D-SN2010bh GRB-SN 0.0593 2010-03-16T12:44:50 16 (0) 9, WISeREP, GRBSNWebtool, GRBNASASwift
GRB101219B-SN2010ma GRB-SN 0.55185 2010-12-19T16:27:53 6 (0) 10, WISeREP, GRBSNWebtool, GRBNASASwift
GRB120422A-SN2012bz GRB-SN 0.283 2012-04-22T07:12:03 13 (0) 11, WISeREP, GRBSNWebtool, GRBNASASwift
GRB130702A-SN2013dx GRB-SN 0.15 2013-07-02T00:05:23 29 (0) 12, 13, 14, 15, WISeREP, GRBSNWebtool
GRB161219B-SN2016jca GRB-SN 0.1475 2016-12-19T18:48:39 3 (0) WISeREP, GRBSNWebtool, GRBNASASwift
GRB171010A-SN2017htp GRB-SN 0.328 2017-10-10T19:00:50 5 (0) 16, WISeREP, GRBSNWebtool
GRB171205A-SN2017iuk GRB-SN 0.0368 2017-12-05T07:20:43 26 (0) WISeREP, GRBSNWebtool, GRBNASASwift
GRB180728A-SN2018fip GRB-SN 0.117 2018-07-28T17:29:00 14 (0) ESO Archive, GRBNASASwift
GRB190829A-AT2019oyw GRB-SN 0.0785 2019-08-29T19:56:44 10 (0) WISeREP, GRBSNWebtool, GRBNASASwift
SN2020bvc GRB-SN 0.025235 2020-02-03T16:04:48 14 (0) 17, WISeREP, GRBSNWebtool
1997ef Ic-BL 0.011805 1997-11-20T00:00:00 38 (7) 5, 18, 19, WISeREP
1997dq Ic-BL 0.003196 1997-09-29T00:00:00 15 (5) 5, 18, 20, WISeREP
1998ey Ic-BL 0.016 1998-12-02T15:37:26 2.0 6 (0) 21, WISeREP
2002bl Ic-BL 0.016 2002-02-22T10:48:00 8.4 4 (0) 22, 23, WISeREP
2002ap Ic-BL 0.002108 2002-01-27T00:00:00 2.0 43 (12) 5, 24, 25, 26, WISeREP
2003bg Ic-BL/IIba 0.004403 2003-02-25T00:00:00 14 (6) 27, 28, WISeREP
2003jd Ic-BL 0.01886 2003-10-20T12:00:00 4.5 29 (4) 5, 22, 29, WISeREP
2005da Ic-BL 0.01501 2005-07-16T08:38:24 2.0 4 (0) 5, 22, 30, WISeREP
2006nx Ic-BL 0.137 2006-11-11T05:02:24 0.71 3 (0) 31, WISeREP
2007ce Ic-BL 0.046 2007-04-10T02:24:00 5.2 11 (0) 5, 22, 32, WISeREP
2007ru Ic-BL 0.015464 2007-11-25T12:00:00 3.0 5 (0) 5, 22, 33, WISeREP
2007I Ic-BL 0.021638 2007-01-12T10:33:36 2.0 7 (3) 5, 22, 34, WISeREP
2007D Ic/Ic-BLb 0.023146 2007-01-05T07:12:00 0.3 4 (0) 5, 22, 35, 36, WISeREP
2008ew Ic/Ic-BLc 0.02026 2008-08-08T05:16:48 2.0 4 (0) 22, 37, WISeREP, SNID4
2009bb Ic-BL (pec.)d 0.0104 2009-03-19T02:24:00 0.6 28 (2) 38, 39, WISeREP
2009dr Ic-BL 0.199 2009-04-15T06:00:00 2.0 6 (1) 40, WISeREP
2009ca Ic-BL/SLSNe 0.0957 2009-03-25T08:38:24 3.35 4 (0) 38, 41, WISeREP
PTF10vgv Ic-BL 0.015 2010-09-13T23:16:48 2.0 10 (3) 13, 42, WISeREP
2010ah Ic-BL 0.0498 2010-02-21T00:00:00 4 (0) 13, 43, 44, WISeREP
PTF10ysd Ic-BL 0.0963 2010-09-25T12:00:00 2.0 3 (0) 13, WISeREP
PTF10xem Ic-BL 0.0567 2010-09-22T03:36:00 2.0 5 (2) 13, WISeREP
PTF10tqv Ic-BL 0.0795 2010-08-14T04:04:48 2.0 3 (0) 13, WISeREP
PTF10qts Ic-BL 0.0907 2010-08-03T14:24:00 2.0 13 (2) 13, 45, WISeREP
PTF10gvb Ic/Ic-BLf 0.098 2010-04-29T14:24:00 2.0 6 (0) 13, 46, WISeREP
PTF10aavz Ic-BL 0.062 2010-11-07T11:31:12 2.0 4 (1) 13, WISeREP
2010ay Ic-BL 0.0671 2010-02-21T07:12:00 1.3 3 (0) 22, 47, 48, WISeREP
PTF11qcj Ic-BL 0.028 2011-10-08T12:00:00 6 (1) 49, WISeREP
PTF12gzk Ic/Ic-BLg 0.01377 2012-07-23T07:12:00 0.6 55 (12) 22, 50, 51, WISeREP
PTF12as Ic-BL 0.033 2011-12-25T12:14:24 2.0 3 (1) 13, WISeREP
2012ap Ic-BL (pec.)h 0.01224 2012-02-07T17:02:23 2.5 15 (4) 52, 53, WISeREP
2012aa Ic-BL/SLSNi 0.0799 2011-12-26T12:00:00 10.0 4 (1) 22, 54, WISeREP
OGLE-2013-SN-134 Ic/Ic-BLj 0.039 2013-12-08T07:29:48 2.0 2 (0) 55, WISeREP, SNID
iPTF13ebw Ic-BL 0.069 2013-11-15T17:02:24 2.0 6 (0) 12, 13, WISeREP
2013bn Ic-BL 0.054 2013-04-03T23:02:24 2.0 5 (0) 13, 22, WISeREP
LSQ14bef Ic-BL 0.05 2014-04-20T00:00:00 2.0 1 (0) 56, WISeREP
2014cp Ic-BL 0.016164 2014-06-23T00:00:00 10 (6) 50, 57, WISeREP
2014ad Ic-BL 0.005 2014-03-08T12:00:00 3.0 31 (5) 58, WISeREP
iPTF14gaq Ic-BL 0.0826 2014-09-19T17:02:24 2.0 3 (0) 13, WISeREP
iPTF14dby Ic-BL 0.074 2014-06-19T13:55:12 2.0 4 (1) 13, WISeREP
iPTF15eov Ic-BL 0.0535 2015-12-02T05:16:48 2.0 17 (0) 13, WISeREP
iPTF15dqg Ic-BL 0.065 2015-11-02T05:31:12 2.0 4 (0) 13, WISeREP
iPTF15dld Ic-BL 0.047 2015-10-03T00:00:00 1.0 6 (0) 59, WISeREP
2016gox Ic-BL 0.042 2016-09-10T02:09:36 2.0 4 (0) 13, WISeREP
2016P Ic/Ic-BLk 0.0146 2016-01-16T00:00:00 2.0 19 (1) 60, 61, WISeREP
2016ilj Ic-BL 0.039711 2016-11-08T18:00:00 2.0 3 (0) 13, WISeREP
2016coi Ic-BL (pec.)l 0.0036 2016-05-23T21:36:00 1.5 100 (26) 62, 63, WISeREP
2017dgk Ic/Ic-BLm 0.065 2017-04-21T22:31:42 2.0 2 (0) 64, WISeREP, SNID
2017ens Ic-BL/IInn 0.1086 2017-06-03T19:12:00 1.5 17 (14) 65, WISeREP
2017ifh Ic-BL 0.039 2017-10-30T00:15:50 7.5 5 (0) 61, WISeREP
2017fwm Ic-BL 0.016 2017-07-26T18:37:26 0.2 6 (0) WISeREP, SNID
2017dio Ic-BL/IIno 0.037 2017-04-14T06:00:00 0.25 15 (0) 66, 67, WISeREP
2017dcc Ic-BL 0.0245 2017-04-12T11:45:38 3.96 9 (2) 68, WISeREP
2017cw Ic-BL 0.093 2016-12-29T21:36:00 2.0 3 (0) 13, WISeREP
2018kqr Ic-BL 0.045 2018-12-06T12:07:19 3.0 2 (0) 69, WISeREP, SNID
2018gsk Ic-BL 0.0116 2018-09-15T15:15:50 2.0 13 (1) 70, WISeREP, SNID
2018gju Ic-BL 0.05 2018-09-13T12:30:14 2.0 1 (0) 71, WISeREP, SNID
2018giu Ic-BL 0.026 2018-09-13T21:23:45 1.5 7 (0) 72, WISeREP, SNID
2018gep Ic-BL (pec.)p 0.033 2018-09-09T02:24:00 0.95 7 (0) 73, WISeREP
2018cbz Ic-BL 0.0223 2018-05-29T08:54:14 2.0 6 (0) 61, 74, WISeREP
2020abdw Ic/Ic-BLq 0.0327790007 2020-11-21T06:02:28 4.0 3 (0) 75, WISeREP, SNID
2022crr Ic-BL 0.0188 2022-02-08T06:11:31 0.94 3 (0) WISeREP, SNID

Notes.

(*)

For cases where the SN type is ambiguous, the most-likely and second-most likely types are shown. Refer to the lettered footnotes for further information.

(†)

In some instances, Δtexp was not known for an SN, while for the GRB-SNe texp is taken from the GRB trigger time, meaning that the uncertainty is just a few seconds.

(‡)

The total number of spectra for each SN is shown in this column, with the number in brackets indicates the number of these spectra that show evidence of emission/nebular features.

(1)

WISeREP indicates that some of the spectra for this event, along with redshift information, was collected from WISeREP https://www.wiserep.org/

(2)

GRBSNWebtool indicates that some of the spectra for this burst were collected from the GRBSN webtool https://grbsn.watchertelescope.ie

(3)

GRBNASASwift indicates that the redshift and explosion times of a GRB-SN was sourced from https://swift.gsfc.nasa.gov/archive/grb_table/.

(4)

SNID indicates that this SN was classified by the authors using the SNID tool (Blondin & Tonry 2007).

(a)

SN2003bg is suggested by (Hamuy et al. 2009) to be a type IIb hypernova, because the late time nebular spectra look somewhat like a type Ib/c SN (lacking hydrogen). However, (Soderberg et al. 2006) suggest it started as a type Ic-BL SN before evolving to a type II SN before becoming a type Ib/c SN. This SN is also radio loud and X-ray luminous (Soderberg et al. 2006).

(b)

SN2007D Possible transition object between a type Ic SN and a type Ic-BL SN. It has clear type Ic-BL SN broad features. However, the velocities are much lower than typical type Ic-BL SNe (Wang et al. 2019). Additionally it has produced significantly more Ni than type Ic/Ic-BL SNe.

(c)

SN2008ew was classified for this publication using SNID. Both type Ic SN templates and type Ic-BL SN templates provide reasonable fits.

(d)

SN2009bb is an engine-driven type Ic-BL SN with strong radio emission (Pignata et al. 2011). A choked jet scenario has been proposed for this SN (Margutti et al. 2014).

(e)

SN2009ca was initially claimed as a type Ic-BL SN by Taddia et al. (2019). However, more recent analysis by Stritzinger et al. (2023) suggested it may be a SLSN.

(f)

PTF10gvb was initially claimed as a type Ic-BL SN by Taddia et al. (2019). However, analysis by Quimby et al. (2018) suggested it may be a SLSN.

(g)

PTF12gzk has high velocities, similar to type GRB-SNe (Modjaz et al. 2016). However, its spectra show narrow more consistent with type Ic SNe (Ben-Ami et al. 2012). Radio indicates relativistic material (Horesh et al. 2013).

(h)

SN2012ap is an engine-driven type Ic-BL SN with evidence of a relativistic outflow observed in radio (Chakraborti et al. 2015); Milisa.2015.

(i)

SN2012aa has a luminosity second bump in the late time optical light curve that suggest it is intermediate between type Ic-BL SN and SLSN(Roy et al. 2016). Spectroscopically it appears similar to a type Ic-BL SN such as SN2007gr and SN2006aj(Roy et al. 2016).

(j)

OGLE-2013-SN-134 was classified for this publication using SNID. It appears to show good fits to type Ic SNe and type Ic-BL SNe. However, this classification is based on a single spectrum.

(k)

SN2016P is transitions from a type Ic-BL SN at early times (Gangopadhyay et al. 2020)), but later on becomes more like a type Ic SN (Prentice et al. 2019).

(l)

SN2016coi is a peculiar type Ic-BL SN in that it exhibits a helium feature early in its evolution, indicating that it is not fully stripped (Terreran et al. 2019); Prentice.2018. This SN has similar radio and X-ray emission to engine-driven SNe such as SN2009bb and SN2012ap(Terreran et al. 2019).

(m)

SN2017dgk was classified for this publication using SNID. It appears to show good fits to type Ic SNe and type Ic-BL SNe. However, this classification is based on a single spectrum.

(n)

SN2017ens undergoes a transition from a type Ic-BL SN to a type IIn SN, and is impacted by CSM interaction (Chen et al. 2018). As such, we only obtained velocities from the first ∼1 month of spectra, and only one Fe II measurement was made. There is also some evidence that this SN is a SLSN (Margutti et al. 2023).

(o)

SN2017dio undergoes a transition from a type Ic-BL SN to a type IIn SN at around 18 days, and is impacted by CSM interaction (Kuncarayakti et al. 2018). As such, we only obtained velocities from the first ∼15 days of spectra.

(p)

SN2018gep is similar to fast-blue optical transients in terms of its rise time and its initial very blue continuum (Pritchard et al. 2021).

(q)

SN2020abdw was classified for this publication using SNID. Although there was a similar template type Ia SN, the better fits visually are for type Ic/Ic-BL SNe, with most being type Ic-BL SNe. Notably it matches PTF12gzk which is a type Ic/Ic-BL SN.

References. (1) Patat et al. (2001); (2) Pian et al. (1999); (3) Kosugi et al. (2004); (4) Matheson et al. (2003); (5) Modjaz et al. (2014); (6) Sonbas et al. (2008); (7) Pian et al. (2006); (8) Modjaz et al. (2006); (9) Bufano et al. (2012); (10) Sparre et al. (2011); (11) Melandri et al. (2012); (12) Schulze et al. (2021); (13) Taddia et al. (2019); (14) Volnova et al. (2017) (15) D’Elia et al. (2015); (16) Bright et al. (2019); (17) Ho et al. (2020); (18) Matheson et al. (2001); (19) Mazzali et al. (2000); (20) Mazzali et al. (2004); (21) Arbour & Schwartz (1998), (22) Shivvers et al. (2019); (23) Armstrong (2002); (24) Foley et al. (2003); (25) Chornock et al. (2013); (26) Gal-Yam et al. (2002); (27) Hamuy et al. (2009); (28) Mazzali et al. (2009); (29) Valenti et al. (2008); (30) Lee & Li (2005); (31) Taddia et al. (2015); (32) Gomez et al. (2022); (33) Sahu et al. (2009); (34) Lee & Li (2007); (35) Wang et al. (2019); (36) Drout et al. (2011); (37) Griffith et al. (2008); (38) Stritzinger et al. (2023); (39) Pignata et al. (2011); (40) Quimby et al. (2009); (41) Taddia et al. (2018); (42) Corsi et al. (2012); (43) Mazzali et al. (2013); (44) Corsi et al. (2011); (45) Walker et al. (2014); (46) Quimby et al. (2018); (47) Sanders et al. (2012a); (48) Sanders et al. (2012b); (49) Corsi et al. (2014); (50) Childress et al. (2016); (51) Ben-Ami et al. (2012); (52) Liu et al. (2015); (53) Milisavljevic et al. (2015); (54) Roy et al. (2016); (55) Wyrzykowski et al. (2013); (56) Polshaw et al. (2014); (57) Zheng et al. (2022); (58) Sahu et al. (2018); (59) Pian et al. (2017); (60) Gangopadhyay et al. (2020); (61) Prentice et al. (2019); (62) Terreran et al. (2019); (63) Prentice et al. (2018); (64) Gutierrez et al. (2017); (65) Chen et al. (2018); (66) Shi et al. (2024); (67) Kuncarayakti et al. (2018); (68) Tonry et al. (2017); (69) De et al. (2020); (70) Tonry et al. (2018d); (71) Tonry et al. (2018c); (72) Tonry et al. (2018b); (73) Pritchard et al. (2021); (74) Tonry et al. (2018a); (75) De (2020).

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