The double-peaked type Ic Supernova 2019cad: another SN 2005bf-like object. (arXiv:2104.03723v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gutierrez_C/0/1/0/all/0/1">C. P. Gutiérrez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bersten_M/0/1/0/all/0/1">M. C. Bersten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orellana_M/0/1/0/all/0/1">M. Orellana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pastorello_A/0/1/0/all/0/1">A. Pastorello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ertini_K/0/1/0/all/0/1">K. Ertini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Folatelli_G/0/1/0/all/0/1">G. Folatelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pignata_G/0/1/0/all/0/1">G. Pignata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_J/0/1/0/all/0/1">J. P. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smartt_S/0/1/0/all/0/1">S. Smartt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sullivan_M/0/1/0/all/0/1">M. Sullivan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pursiainen_M/0/1/0/all/0/1">M. Pursiainen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inserra_C/0/1/0/all/0/1">C. Inserra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elias_Rosa_N/0/1/0/all/0/1">N. Elias-Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fraser_M/0/1/0/all/0/1">M. Fraser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kankare_E/0/1/0/all/0/1">E. Kankare</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stritzinger_M/0/1/0/all/0/1">M. Stritzinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_J/0/1/0/all/0/1">J. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frohmaier_C/0/1/0/all/0/1">C. Frohmaier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">L. Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hiramatsu_D/0/1/0/all/0/1">D. Hiramatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howell_D/0/1/0/all/0/1">D. A. Howell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuncarayakti_H/0/1/0/all/0/1">H. Kuncarayakti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mattila_S/0/1/0/all/0/1">S. Mattila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muller_Bravo_T/0/1/0/all/0/1">T. Müller-Bravo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pellegrino_C/0/1/0/all/0/1">C. Pellegrino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_M/0/1/0/all/0/1">M. Smith</a>
We present the photometric and spectroscopic evolution of supernova (SN)
2019cad during the first $sim100$ 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 $sim8$ days, while the r band
peak occurred $sim15$ days post-explosion. A second and more prominent peak is
reached in all bands at $sim45$ days past explosion, followed by and fast
decline from $sim60$ 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 ${lambda}6355$ and C II
${lambda}6580$ 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$_{odot}$, and an explosion energy of $3.5times 10^{51}$ erg. The
light curve morphology can be reproduced either by a double-peaked $^{56}$Ni
distribution with an external component of 0.041 M$_{odot}$ and an internal
component of 0.3 M$_{odot}$ or a double-peaked $^{56}$Ni distribution plus
magnetar model (P $sim11$ ms and B $sim26times 10^{14}$ G). If SN 2019cad
were to suffer from significant host reddening (which cannot be ruled out), the
$^{56}$Ni model would require extreme values, while the magnetar model would
still be feasible.
We present the photometric and spectroscopic evolution of supernova (SN)
2019cad during the first $sim100$ 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 $sim8$ days, while the r band
peak occurred $sim15$ days post-explosion. A second and more prominent peak is
reached in all bands at $sim45$ days past explosion, followed by and fast
decline from $sim60$ 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 ${lambda}6355$ and C II
${lambda}6580$ 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$_{odot}$, and an explosion energy of $3.5times 10^{51}$ erg. The
light curve morphology can be reproduced either by a double-peaked $^{56}$Ni
distribution with an external component of 0.041 M$_{odot}$ and an internal
component of 0.3 M$_{odot}$ or a double-peaked $^{56}$Ni distribution plus
magnetar model (P $sim11$ ms and B $sim26times 10^{14}$ G). If SN 2019cad
were to suffer from significant host reddening (which cannot be ruled out), the
$^{56}$Ni model would require extreme values, while the magnetar model would
still be feasible.
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