TY - JOUR
T1 - The double-peaked type Ic Supernova 2019cad: another SN 2005bf-like object
AU - Gutiérrez, C. P.
AU - Bersten, M. C.
AU - Orellana, M.
AU - Pastorello, A.
AU - Ertini, K.
AU - Folatelli, G.
AU - Pignata, G.
AU - Anderson, J. P.
AU - Smartt, S.
AU - Sullivan, M.
AU - Pursiainen, M.
AU - Inserra, C.
AU - Elias-Rosa, N.
AU - Fraser, M.
AU - Kankare, E.
AU - Stritzinger, M.
AU - Burke, J.
AU - Frohmaier, C.
AU - Galbany, L.
AU - Hiramatsu, D.
AU - Howell, D. A.
AU - Kuncarayakti, H.
AU - Mattila, S.
AU - Müller-Bravo, T.
AU - Pellegrino, C.
AU - Smith, M.
PY - 2021
Y1 - 2021
N2 - Abstract
We present the
photometric and spectroscopic evolution of supernova (SN) 2019cad during
the first ∼100 days from explosion. Based on the light curve
morphology, we find that SN 2019cad resembles the double-peaked type
Ib/c SN 2005bf and the type Ic PTF11mnb. Unlike those two objects,
SN 2019cad also shows the initial peak in the redder bands. Inspection
of the g −band light curve indicates the initial peak is reached in ∼8 days, while the r
band peak occurred ∼15 days post-explosion. A second and more prominent
peak is reached in all bands at ∼45 days past explosion, followed by a
fast decline from ∼60 days. During the first 30 days, the spectra of
SN 2019cad show the typical features of a type Ic SN, however, after
40 days, a blue continuum with prominent lines of Si ii λ6355 and C ii
λ6580 is observed again. Comparing the bolometric light curve to
hydrodynamical models, we find that SN 2019cad is consistent with a
pre-SN mass of 11 M⊙, and an explosion energy of 3.5× 1051 erg. The light curve morphology can be reproduced either by a double-peaked 56Ni distribution with an external component of 0.041 M⊙, and an internal component of 0.3 M⊙ or a double-peaked 56Ni distribution plus magnetar model (P ∼11 ms and B ∼ 26 × 1014 G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the 56Ni model would require extreme values, while the magnetar model would still be feasible.
AB - Abstract
We present the
photometric and spectroscopic evolution of supernova (SN) 2019cad during
the first ∼100 days from explosion. Based on the light curve
morphology, we find that SN 2019cad resembles the double-peaked type
Ib/c SN 2005bf and the type Ic PTF11mnb. Unlike those two objects,
SN 2019cad also shows the initial peak in the redder bands. Inspection
of the g −band light curve indicates the initial peak is reached in ∼8 days, while the r
band peak occurred ∼15 days post-explosion. A second and more prominent
peak is reached in all bands at ∼45 days past explosion, followed by a
fast decline from ∼60 days. During the first 30 days, the spectra of
SN 2019cad show the typical features of a type Ic SN, however, after
40 days, a blue continuum with prominent lines of Si ii λ6355 and C ii
λ6580 is observed again. Comparing the bolometric light curve to
hydrodynamical models, we find that SN 2019cad is consistent with a
pre-SN mass of 11 M⊙, and an explosion energy of 3.5× 1051 erg. The light curve morphology can be reproduced either by a double-peaked 56Ni distribution with an external component of 0.041 M⊙, and an internal component of 0.3 M⊙ or a double-peaked 56Ni distribution plus magnetar model (P ∼11 ms and B ∼ 26 × 1014 G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the 56Ni model would require extreme values, while the magnetar model would still be feasible.
KW - Supernovae
KW - General AS supernovae
KW - Individual: SN 2019cad
U2 - 10.1093/mnras/stab1009
DO - 10.1093/mnras/stab1009
M3 - Journal article
SN - 0035-8711
VL - 504
SP - 4907
EP - 4922
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -