public survey. It was saved on Jun 30 by AMPEL, and reported to TNS the same
day (Nordin et al., 2020). It was saved again on July 3 by the BTS survey.
SEDM and LT spectra were obtained as part of BTS. The LT spectrum on July 13
led to the Type IIn classification and measurement of $z=0.074$ (Perley et
al., 2020a). Further inspection as part of this paper reclassified it as Type
II.

###  A.20 AT 2020aexw / ZTF20abmocba

AT 2020aexw was discovered by ZTF, first detected on 2020 July 18 at
$r=20.52\pm 0.21\,$mag as part of ZUDS. It was saved on July 19 by AMPEL and
on July 26 by the rapidly evolving transients program. LT follow-up imaging
was acquired. A NOT spectrum was attempted but not successful. A DBSP spectrum
was obtained on Aug 12 resulting in a redshift measurement from very strong
emission lines.

###  A.21 AT 2020yqt / ZTF20abummyz / PS20ksm

AT 2020yqt was discovered by Pan-STARRS1 on 2020 Aug 22 and reported to TNS on
2020 November 1 (Chambers et al., 2020). It was first detected as part of the
ZTF 1DC survey on 2020 Aug 19 at $r=19.95\pm 0.17\,$mag, and saved by a
scanner on Aug 20 as part of a filter for rapidly evolving transients. The
host galaxy had an SDSS spectrum which classified it as a starburst, with a
redshift $z=0.09855\pm 0.00001$. Due to the fast evolution, we triggered a
Gemini ToO program (PI: A. Miller) and obtained a spectrum on Aug 25 that was
primarily featureless. Subsequent spectra with P200 and LRIS did not show
obvious supernova features and were dominated by host-galaxy light.

###  A.22 SN 2020rsc / ZTF20aburywx / ATLAS20xxj

SN 2020rsc was first detected on 2020 Aug 19 as part of the public survey at
$g=19.58\pm 0.17\,$mag, and reported to TNS that day by the ALeRCE broker
(Forster et al., 2020d). It was also detected that night as part of the
Caltech 1DC survey. It was first saved on 2020 Aug 20 by a filter for rapidly
evolving transients. The next day, it was noted that it was already fading,
and a Gemini ToO program was triggered. The Gemini spectrum on Aug 22 showed
He I at 8000 $\rm km$ $\rm s^{-1}$. On 2020 Aug 22 the source passed the CLU
filter. An additional spectrum with MMT+Binospec was obtained on Aug 24, and a
GTC spectrum was obtained on Aug 25. Swift was triggered and observed on Aug
26, and the VLA was triggered on September 2 with the observation taking place
on September 9. A final Keck spectrum on September 15 led to the Type IIb
classification.

###  A.23 SN2020vyv / ZTF20acigusw / ATLAS20bdhi / PS20kra

SN 2020vyv was first detected in the ZTF public survey on 2020 October 12 at
$r=19.17\pm 0.10\,$mag. It was saved the same day by AMPEL and the BTS survey,
and reported to TNS (Fremling, 2020). It was classified as a Type II SN with a
Keck/LRIS spectrum on 2020-10-14 (Siebert et al., 2020b).

###  A.24 SN 2020xlt / ZTF20aclfmwn

SN 2020xlt was first detected on 2020 October 19 in public-survey data at
$r=19.93\pm 0.22$, and was reported to TNS that day by ALeRCE (Forster et al.,
2020e). It was also detected that night as part of the Caltech 1DC survey, and
the next night as part of the high-cadence partnership survey. It was saved on
October 19 as part of AMPEL (Nordin et al., 2019e) and the infant supernova
program, and SEDM was triggered: the spectrum was featureless. Despite the
proximity to a bright extended galaxy, the redshift was unknown. The transient
was noted to be fading on October 22, and on October 26 it passed a filter for
rapidly evolving transients, leading to a GTC+OSIRIS spectrum on 2020 October
30 that enabled the redshift measurement of $z=0.0389$ and the classification
as a Type IIb.

##  Appendix B Photometric evolution of individual events

Here we provide light curves for the events not shown in the main text.

Figure 20: Light curves for gold-sample events whose light curves were not
shown in the main text. In panels with H-poor SNe we show the Type Ibc
template from Drout et al. (2011) for reference. In the Type II and Type IIb
panels we show the $V$-band light curve of SN 1993J (Schmidt et al., 1993) for
reference. Figure 21: Light curves for the silver sample. For reference, in
each panel we show the Type Ibc template from Drout et al. (2011). Upper
limits are shown with triangles. Upper limits are connected to detections by
dashed lines. Figure 22: ZTF P48 $g$\- and $r$-band light curves for the
bronze sample. Upper limits are shown with triangles, and non-detections are
connected to detections by dashed lines.

##  Appendix C Log of Optical Spectra

Here we provide the full log of optical spectra, some of which were obtained
from TNS. We do not report observations for objects with extensive
spectroscopic observations previously presented in the literature: AT 2018cow
(Perley et al., 2019), SN 2018gep (Ho et al., 2019a), SN 2019dge (Yao et al.,
2020), and SN 2020oi.

Table 15: Log of spectroscopic observations of objects presented in this
paper. Phase given with respect to the observed maximum of the $g$-band light
curve.

Name | UT Date | Target | Phase | Telescope + Instrument
---|---|---|---|---
SN 2018ghd | 20180914 | Transient | $-2$ | P60+SEDM
SN 2018ghd | 20180916 | Transient | $0$ | P60+SEDM
SN 2018ghd | 20180921 | Transient | $4$ | P60+SEDM
SN 2018ghd | 20181110 | Transient | $54$ | Keck1+LRIS
SN 2018ghd | 20190105 | Transient | $110$ | Keck1+LRIS
AT 2018lug | 20180913 | Transient | $0$ | P200+DBSP
AT 2018lug | 20190104 | Host | $112$ | Keck1+LRIS
SN 2018gjx | 20180918 | Transient | $0$ | P60+SEDM
SN 2018gjx | 20180918 | Transient | $0$ | EFOSC2+NTT [1]
SN 2018gjx | 20180919 | Transient | $0$ | P60+SEDM
SN 2018gjx | 20181012 | Transient | $23$ | P60+SEDM
SN 2018gjx | 20181016 | Transient | $27$ | NOT+ALFOSC
SN 2018gjx | 20181110 | Transient | $52$ | Keck1+LRIS
SN 2018gjx | 20181130 | Transient | $72$ | TNG+DOLORES
SN 2018gjx | 20190105 | Transient | $108$ | Keck1+LRIS
SN 2018gjx | 20190706 | Transient | $290$ | Keck1+LRIS
SN 2019aajs | 20190227 | Transient | $-1$ | LT+SPRAT
SN 2019aajs | 20190302 | Transient | $1$ | LT+SPRAT
SN 2019aajs | 20190304 | Transient | $3$ | NOT+ALFOSC
SN 2019aajs | 20190315 | Transient | $14$ | NOT+ALFOSC
SN 2019aajs | 20190406 | Transient | $36$ | Keck1+LRIS
SN 2019deh | 20190410 | Transient | $-4$ | P60+SEDM
SN 2019deh | 20190410 | Transient | $-4$ | LT+SPRAT
SN 2019deh | 20190411 | Transient | $-3$ | LT+SPRAT
SN 2019deh | 20190412 | Transient | $-2$ | LT+SPRAT
SN 2019deh | 20190414 | Transient | $0$ | LT+SPRAT
SN 2019deh | 20190415 | Transient | $0$ | P60+SEDM
SN 2019deh | 20190423 | Transient | $8$ | NOT+ALFOSC
SN 2019deh | 20190423 | Transient | $8$ | P60+SEDM
SN 2019deh | 20190424 | Transient | $9$ | P200+DBSP
SN 2019deh | 20190428 | Transient | $13$ | P60+SEDM
SN 2019deh | 20190511 | Transient | $26$ | NOT+ALFOSC
AT 2019esf | 20190504 | Transient | $-2$ | P60+SEDM
AT 2019esf | 20200218 | Host | $287$ | Keck1+LRIS
AT 2019kyw | 20190709 | Transient | $-3$ | P60+SEDM
AT 2019kyw | 20190801 | Transient | $19$ | P200+DBSP
AT 2019kyw | 20190809 | Transient | $27$ | P200+DBSP
SN 2019myn | 20190813 | Transient | $1$ | P60+SEDM
SN 2019myn | 20190831 | Transient | $19$ | Keck1+LRIS
SN 2019php | 20190907 | Transient | $2$ | P200+DBSP
SN 2019php | 20190924 | Transient | $19$ | Keck1+LRIS
SN 2019qav | 20190911 | Transient | $-2$ | P60+SEDM
SN 2019qav | 20190924 | Transient | $10$ | Keck1+LRIS
SN 2019qav | 20190928 | Transient | $14$ | Keck1+LRIS
SN 2019qav | 20191027 | Transient | $43$ | Keck1+LRIS
SN 2019rii | 20191003 | Transient | $1$ | P200+DBSP
SN 2019rii | 20191027 | Transient | $25$ | Keck1+LRIS
SN 2019rta | 20191004 | Transient | $0$ | P60+SEDM
SN 2019rta | 20191005 | Transient | $1$ | P200+DBSP
SN 2019rta | 20191015 | Transient | $11$ | P60+SEDM
SN 2019rta | 20191027 | Transient | $23$ | Keck1+LRIS
SN 2020ano | 20200125 | Transient | $1$ | P60+SEDM
SN 2020ano | 20200129 | Transient | $5$ | Gemini+GMOS
SN 2020ano | 20200214 | Transient | $21$ | P200+DBSP
SN 2020ano | 20200218 | Transient | $25$ | Keck1+LRIS
AT 2020bdh | 20200213 | Transient | $16$ | EFOSC2+NTT [2]
AT 2020bdh | 20200226 | Transient | $29$ | P200+DBSP
AT 2020bot | 20200202 | Transient | $0$ | P200+DBSP
AT 2020bot | 20200203 | Transient | $1$ | Gemini+GMOS
SN 2020ikq | 20200429 | Transient | $-3$ | P60+SEDM
SN 2020ikq | 20200503 | Transient | $0$ | P60+SEDM
SN 2020ikq | 20200510 | Transient | $7$ | LT+SPRAT
SN 2020ikq | 20200511 | Transient | $8$ | P60+SEDM
SN 2020ikq | 20200515 | Transient | $12$ | NOT+ALFOSC
SN 2020ikq | 20200517 | Transient | $14$ | P60+SEDM
SN 2020jmb | 20200511 | Transient | $-1$ | P60+SEDM
SN 2020jmb | 20200516 | Transient | $3$ | LT+SPRAT
SN 2020jmb | 20200523 | Transient | $10$ | P60+SEDM
SN 2020jmb | 20200528 | Transient | $15$ | P200+DBSP
SN 2020jji | 20200511 | Transient | $0$ | P60+SEDM
SN 2020jji | 20200527 | Transient | $16$ | P200+DBSP
AT 2020kfw | 20200528 | Transient | $5$ | P200+DBSP
SN 2020ntt | 20200713 | Transient | $9$ | LT+SPRAT
SN 2020ntt | 20200715 | Transient | $11$ | P60+SEDM
AT 2020aexw | 20200812 | Host | $21$ | P200+DBSP
AT 2020yqt | 20200825 | Transient | $5$ | Gemini+GMOS
AT 2020yqt | 20200829 | Transient | $9$ | P200+DBSP
AT 2020yqt | 20200920 | Transient | $31$ | Keck1+LRIS
SN 2020rsc | 20200822 | Transient | $-2$ | Gemini+GMOS
SN 2020rsc | 20200824 | Transient | $0$ | MMT
SN 2020rsc | 20200825 | Transient | $0$ | GTC+OSIRIS
SN 2020rsc | 20200915 | Transient | $21$ | Keck1+LRIS
AT 2020xnd | 20201019 | Transient | $4$ | Keck1+LRIS
AT 2020xnd | 20201021 | Transient | $6$ | Keck1+LRIS
SN 2020vyv | 20201014 | Transient | $1$ | Keck1+LRIS [3]
SN 2020xlt | 20201028 | Transient | $8$ | P60+SEDM
SN 2020xlt | 20201030 | Transient | $10$ | GTC+OSIRIS

[1] Gromadzki et al. (2018), [2] Smith et al. (2020b), [3] Siebert et al.
(2020b)

##  Appendix D Spectroscopic evolution of individual events

In this section we plot the full set of spectra for each object in the gold
sample.

Figure 23: Spectroscopic evolution for gold-sample objects. Raw spectra are
shown in light grey, and smoothed spectra are overlaid in black.

Figure 24: Spectroscopic evolution for gold-sample objects. Raw spectra are
shown in light grey, and smoothed spectra are overlaid in black.

Figure 25: Spectroscopic evolution for gold-sample objects. Raw spectra are
shown in light grey, and smoothed spectra are overlaid in black.

Figure 26: Spectroscopic evolution for gold-sample objects. Raw spectra are
shown in light grey, and smoothed spectra are overlaid in black.

##  Appendix E Host Galaxy Properties

In this section we provide additional details and figures for the host-galaxy
properties described in Section 4. We model the spectral energy distributions
(SEDs) with the software package cigale (Code Investigating GALaxy Evolution;
Burgarella et al., 2005; Noll et al., 2009; Boquien et al., 2019). We adopt
the Bruzual & Charlot (2003) simple stellar population model to compute the
stellar emission and the Chabrier (2003) initial mass function. Furthermore,
we assume a linear-exponential star-formation history [functional form
$t\times\exp\left(-t/\tau\right)$, where $t$ is the age of the SFH episode and
$\tau$ is the $e$-folding timescale]. To calculate the nebular emission from
the ionised gas in H II regions, we fix the cigale ionisation parameter log
$\text{U}_{\text{ion}}$ as $-2$. We use a modified Calzetti et al. (2000)
starburst attenuation curve to model the dust attenuation. Dust emission was
included via the Dale et al. (2014) dust templates. More details on the models
used can be found in Boquien et al. (2019). We generate 24385536 models and
choose the best-fit SED using Bayesian inference. In Figure 27 we show the
best-fit SED for the host galaxy of AT 2020yqt as an example.

Table 16:  The models and fitting parameters used for cigale Galaxy attributes |  Brief description
---|---
SFH |  SFR $\propto$ $\frac{t}{\tau^{2}}$ $exp(-t/\tau)$
|  $\tau=250,500,1000,2000,4000,6000,8000$ Myr
|  Age $t=250,500,1000,2000,4000,8000,12000$ Myr
SSPs models |  BC03 (Bruzual & Charlot, 2003) $+$ Chabrier IMF (Chabrier, 2003)
|  Stellar metallicity = 0.0004, 0.004, 0.008, 0.02 $Z_{\odot}$
Dust Attenuation |  Modified power law curves (Calzetti et al., 2000) \+ differential reddening of stars according to age
|  $E(B-V)_{\rm young}$ = 0.0, 0.2, 0.3, 0.5, 0.8, 1.0, 1.5, 2.0, 3.0
|  $E(B-V)_{\rm old}$ = 0.3, 0.50, 1.0
|  ${\rm UV-bump~{}wavelength}=217.5~{}{\rm nm}$
|  ${\rm UV-bump~{}amplitude}=0.0,1.0,2.0,3.0$
|  ${\rm powerlaw~{}slope}=-0.13,-0.2,-0.5$
Dust emission |  Dust templates of Dale et al. (2014) $+$ Energy Balance
|  AGN fraction = 0
|  alpha = 1.0, 1.5, 2.0, 2.5
Nebular |  $\log U_{\rm ion}=$ -2.0
|  emission line width = 300.0 km/s
Table 17: Summary of the host galaxy SED modelling Object | $\chi^{2}/{\rm n.o.f.}$ |  $M_{B}$ (mag) | $\log\,M/M_{\odot}$ | $\log\,{\rm SFR}/\left(M_{\odot}\,{\rm yr}^{-1}\right)$ | $\log{\rm Age}/{\rm yr}$ | $E(B-V)\,({\rm mag})$
---|---|---|---|---|---|---
Gold sample
ZTF18aakuewf | 2.10/9 | -18.57 | $9.47^{+0.15}_{-0.10}$ | $-0.48^{+0.09}_{-0.08}$ | $9.91^{+0.12}_{-0.19}$ | $0.25^{+0.06}_{-0.03}$
ZTF18abcfcoo | 56.74/24 | -18.46 | $9.59^{+0.06}_{-0.12}$ | $-0.19^{+0.10}_{-0.13}$ | $9.93^{+0.10}_{-0.15}$ | $0.25^{+0.07}_{-0.04}$
ZTF18abfcmjw | 0.61/14 | -16.19 | $8.65^{+0.12}_{-0.14}$ | $-1.22^{+0.28}_{-0.23}$ | $9.89^{+0.13}_{-0.21}$ | $0.31^{+0.15}_{-0.08}$
ZTF18abukavn | 9.85/19 | -16.59 | $8.45^{+0.09}_{-0.08}$ | $-1.08^{+0.04}_{-0.07}$ | $9.81^{+0.18}_{-0.19}$ | $0.25^{+0.06}_{-0.03}$
ZTF18abvkmgw | 2.09/15 | -19.23 | $10.30^{+0.12}_{-0.13}$ | $0.37^{+0.32}_{-0.20}$ | $9.89^{+0.13}_{-0.23}$ | $0.58^{+0.43}_{-0.24}$
ZTF18abwkrbl | 3.11/16 | -19.58 | $10.19^{+0.08}_{-0.13}$ | $0.42^{+0.15}_{-0.14}$ | $9.91^{+0.12}_{-0.21}$ | $0.28^{+0.12}_{-0.06}$
ZTF19aakssbm | 1.55/9 | -17.76 | $9.64^{+0.17}_{-0.14}$ | $-0.61^{+0.22}_{-0.49}$ | $9.94^{+0.09}_{-0.13}$ | $0.28^{+0.11}_{-0.06}$
ZTF19aapfmki | 5.75/17 | -20.94 | $10.72^{+0.05}_{-0.07}$ | $0.89^{+0.07}_{-0.12}$ | $9.95^{+0.09}_{-0.12}$ | $0.25^{+0.06}_{-0.03}$
ZTF19abobxik | 5.43/14 | -18.32 | $9.42^{+0.13}_{-0.10}$ | $-0.54^{+0.06}_{-0.08}$ | $9.90^{+0.13}_{-0.19}$ | $0.25^{+0.06}_{-0.03}$
ZTF19abuvqgw | 1.27/3 | -12.66 | $6.51^{+0.56}_{-0.39}$ | $-2.21^{+0.37}_{-0.34}$ | $8.94^{+0.80}_{-0.38}$ | $0.37^{+0.58}_{-0.13}$
ZTF19abyjzvd | 14.49/18 | -19.83 | $9.87^{+0.20}_{-0.16}$ | $0.60^{+0.21}_{-0.25}$ | $9.66^{+0.22}_{-0.50}$ | $0.25^{+0.08}_{-0.04}$
ZTF19acayojs | 4.23/10 | -19.81 | $10.27^{+0.18}_{-0.31}$ | $0.67^{+0.37}_{-0.20}$ | $9.84^{+0.17}_{-0.63}$ | $0.28^{+0.15}_{-0.06}$
ZTF19accjfgv | 10.75/11 | -18.50 | $9.43^{+0.20}_{-0.18}$ | $0.01^{+0.29}_{-0.22}$ | $9.72^{+0.24}_{-0.55}$ | $0.33^{+0.19}_{-0.10}$
ZTF20aaelulu | 1.22/10 | -21.82 | $10.90^{+0.23}_{-0.14}$ | $1.46^{+0.22}_{-0.41}$ | $9.75^{+0.23}_{-0.52}$ | $0.43^{+0.49}_{-0.15}$
ZTF20aahfqpm | 0.64/7 | -19.52 | $9.57^{+0.19}_{-0.21}$ | $0.54^{+0.45}_{-0.25}$ | $9.23^{+0.55}_{-0.49}$ | $0.32^{+0.26}_{-0.09}$
ZTF20aaxhzhc | 8.57/16 | -18.02 | $9.25^{+0.07}_{-0.31}$ | $-0.53^{+0.31}_{-0.07}$ | $9.91^{+0.12}_{-0.49}$ | $0.25^{+0.06}_{-0.03}$
ZTF20aayrobw | 5.93/13 | -17.38 | $8.77^{+0.16}_{-0.15}$ | $-0.70^{+0.11}_{-0.09}$ | $9.78^{+0.20}_{-0.41}$ | $0.26^{+0.08}_{-0.04}$
ZTF20aazchcq | 1.00/14 | -18.53 | $9.49^{+0.20}_{-0.15}$ | $-0.24^{+0.19}_{-0.32}$ | $9.86^{+0.15}_{-0.21}$ | $0.25^{+0.08}_{-0.04}$
ZTF20abjbgjj | 4.73/13 | -17.98 | $9.16^{+0.24}_{-0.22}$ | $-0.19^{+0.37}_{-0.33}$ | $9.68^{+0.27}_{-0.62}$ | $0.34^{+0.26}_{-0.10}$
ZTF20aburywx | 9.05/14 | -19.46 | $10.15^{+0.13}_{-0.14}$ | $0.41^{+0.18}_{-0.21}$ | $9.88^{+0.14}_{-0.25}$ | $0.32^{+0.15}_{-0.09}$
ZTF20acigusw | 4.68/18 | -19.48 | $9.86^{+0.15}_{-0.15}$ | $0.46^{+0.20}_{-0.12}$ | $9.74^{+0.23}_{-0.50}$ | $0.26^{+0.11}_{-0.05}$
ZTF20aclfmwn | 6.18/11 | -20.65 | $10.70^{+0.09}_{-0.12}$ | $0.70^{+0.16}_{-0.16}$ | $9.93^{+0.10}_{-0.15}$ | $0.26^{+0.09}_{-0.04}$
Silver sample
ZTF18abvkwla | 19.49/14 | -19.34 | $9.32^{+0.16}_{-0.21}$ | $0.31^{+0.10}_{-0.10}$ | $9.29^{+0.22}_{-0.32}$ | $0.25^{+0.06}_{-0.03}$
ZTF19aatoboa | 23.53/17 | -19.65 | $9.91^{+0.18}_{-0.15}$ | $0.42^{+0.20}_{-0.16}$ | $9.78^{+0.21}_{-0.50}$ | $0.29^{+0.11}_{-0.06}$
ZTF19abfarpa | 4.10/11 | -17.56 | $8.76^{+0.18}_{-0.18}$ | $-0.64^{+0.33}_{-0.18}$ | $9.70^{+0.25}_{-0.56}$ | $0.28^{+0.11}_{-0.06}$
ZTF20aaivtof | 2.95/11 | -18.38 | $8.93^{+0.20}_{-0.27}$ | $-0.08^{+0.14}_{-0.41}$ | $9.22^{+0.64}_{-0.32}$ | $0.25^{+0.06}_{-0.03}$
ZTF20aakypiu | 10.77/17 | -21.28 | $11.67^{+0.04}_{-0.12}$ | $0.41^{+0.92}_{-0.10}$ | $9.78^{+0.09}_{-0.12}$ | $0.29^{+0.53}_{-0.07}$
ZTF20ababxjv | 2.96/15 | -19.66 | $10.31^{+0.17}_{-0.22}$ | $0.61^{+0.33}_{-0.25}$ | $9.84^{+0.17}_{-0.50}$ | $0.42^{+0.51}_{-0.16}$
ZTF20abmocba | 10.15/16 | -19.48 | $9.86^{+0.12}_{-0.38}$ | $0.18^{+0.36}_{-0.05}$ | $9.90^{+0.12}_{-0.66}$ | $0.26^{+0.11}_{-0.05}$
ZTF20abummyz | 7.74/16 | -20.01 | $10.04^{+0.17}_{-0.20}$ | $0.98^{+0.27}_{-0.26}$ | $9.26^{+0.55}_{-0.36}$ | $0.42^{+0.48}_{-0.14}$
ZTF20acigmel | 4.62/3 | -15.62 | $7.23^{+0.25}_{-0.19}$ | $-1.12^{+0.16}_{-0.15}$ | $8.71^{+0.35}_{-0.22}$ | $0.27^{+0.11}_{-0.05}$
Figure 27: The SED of ZTF20abummyz’s host galaxy (empty circles) from the UV
to mid-IR. The solid black line shows the best-fitting model of the SED. The
SED model consists of a stellar component (yellow curve), a contribution
ionised gas, e.g., star-forming regions (green curve) and emission from heated
dust (red curve) at $>30,000$ Å. The photometry predicted by the best-fit
model is shown by the red circles. The blue curve represents the stellar
component corrected for host attenuation.

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