Interacting SN Light Curves(More observations, less simulations)SN2017gmr; Andrews+19

Type I
Interacting…maybe?

Type II SNe; See Moriya’s talk yesterday

D. Sand (Arizona) 

aFeb 22, 2023

Type Ia SN: Early Light Curves Shed Lighton Progenitor & Explosion

Type Ia SN: Early Light Curves Shed Lighton Progenitor & Explosion - All expected features that deviate from a smooth early rise occur on<2-ish day time scales.
- Need early discovery *and* multi-band follow-up on <1 day time scales
to sample these features.

Type Ia SN: Early Light Curves Shed Lighton Progenitor & Explosion

Kasen 2010 - All expected features that deviate from a smooth early rise occur on<2-ish day time scales.
- Need early discovery *and* multi-band follow-up on <1 day time scales
to sample these features.

Type Ia SN: Early Light Curves Shed Lighton Progenitor & Explosion‘Normal’ SNe Ia-Multi-band photometry is essential for testing of models. U-band!

SN2021aefx NGC 1566; D=18 Mpc

Hosseinzadeh+22

No light curve model can perfectly explain the early light curve ofSN2021aefx. Early Swift data does not match expectations fromshocks from a companion star, etc.
See also Ashall+22

SN2017cbv

Same story — early light curve can be explained by shock interaction
with companion star, but not in UV. Fe-line blanketing?

SN2019yvq
Strong initial UV pulse — closer toexpectations for single degenerate case
02es-like. Underluminous, Ti II in spectra
Single degenerate light curve ts wel.

.

lfi

Miller+20; Siebert+20; Burke+21

SN2017cbv
With companion interaction, you also expect Halpha/helium at latetimes…but we don’t see it. (Sand et al. 2018)

If truethenButH is seen at late times in a handful ofunderluminous SN Ia-Generally not enough mass to be strippedhydrogen from a companion star
-Could be some kind of CSM from anova-like eruption in the past?
-What fraction of underluminous SN Ia
have H at late times? <15% (Sand+19)

Elias-Rosa+19
Kollmeier+19

ZTF Early Light Curves
Deckers et al. 2022

-Six out of 30 nearby SN Ia have an
early excess. ~20% of sample-Four were ‘blue’ and two were ‘red’.

-Concluded some mix of CSM
interaction and either singledegenerate/nickel clumps.

Las Cumbres/DLT40 Early SN Ia Light Curve Sample
Burke et al. 2022.

.

fi-Nine SN Ia with extremely early discovery and immediate mult-band followup. A high S/N, multi-band complement to similar ZTF samples-All t uniformly with Kasen+10 model of shock interaction with nondegenerate companion star-Three of nine systems show early excess, in agreement with expectations
from the model.

Las Cumbres/DLT40 Early SN Ia Light Curve Sample
Burke et al. 2022.

.

fi-Nine SN Ia with extremely early discovery and immediate mult-band followup. A high S/N, multi-band complement to similar ZTF samples-All t uniformly with Kasen+10 model of shock interaction with nondegenerate companion star-Three of nine systems show early excess, in agreement with expectations
from the model.

Las Cumbres/DLT40 Early SN Ia Light Curve Sample
Burke et al. 2022

Kasen 2010.

.

fi-Nine SN Ia with extremely early discovery and immediate mult-band followup. A high S/N, multi-band complement to similar ZTF samples-All t uniformly with Kasen+10 model of shock interaction with nondegenerate companion star-Three of nine systems show early excess, in agreement with expectations
from the model.

Core Collapse SNe Just some very early light curve + spectroscopy examples

Core Collapse SNeJust some very early light curve + spectroscopy examples
SN2017gmrAndrews+19). 

?

fl-A ‘mini-bump’ in the U&B light curve over ~2 days,reminiscent of Moriya’s talk yesterday-No ash on same time scale, except maybe a Halphaline with FWHM~50 km/s (RSG wind?
-Very broad feature at 4500A-LSST won’t do this. Most surveys would struggle.

Core Collapse SNeJust some very early light curve + spectroscopy examples
SN2017gmrMoriya+18

Andrews+19). 

?

fl-A ‘mini-bump’ in the U&B light curve over ~2 days,reminiscent of Moriya’s talk yesterday-No ash on same time scale, except maybe a Halphaline with FWHM~50 km/s (RSG wind?
-Very broad feature at 4500A-LSST won’t do this. Most surveys would struggle.

Core Collapse SNeJust some very early light curve + spectroscopy examples
SN2018cuffi.

) ?

fl-Modeled with SNEC (Morozova+15) with steady state wind-0.06 M_sun/yr for 14 months (a lot-No ash at all, even with a spectrum at +1.7 days. Consistent with con ned
CSM from light curve modeling-Argues for *both* high cadence light curves and spectra.

Core Collapse SNeJust some very early light curve + spectroscopy examples
SN2021yja

Hosseinzadeh+22 fi

fl-Again, no ash features, but a ‘ledge’. But amongst the most luminous in theUV. Again, suggestive of con ned CSM as described by Luc earlier

Core Collapse SNeJust some very early light curve + spectroscopy examples
SN2021yja 

-Light curve modeling suggests 15 M_sun progenitor, high mass loss rate (0.18
M_sun/yr), but compact (Kozyreva+22).

Summar-Early, high cadence and multi-band light curves set strong constraints oncompanion shocking in SN Ia-High quality early light curve data of nearby CC SNe can also constrain
mass loss history, especially in conjunction with spectra and multiwavelength analyses-Do not forget high cadence, good quality spectra as well.

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y21