Interacting supernovae at cosmological distances
Takashi Moriya
National Astronomical Observatory of Japan

High-redshift SNe IIn from CFHT

Cooke et al. (2009)

High-redshift SNe IIn from CFHT

Cooke et al. (2009)

Subaru high-redshift SN survey•

Subaru/Hyper Suprime-Cam (HSC)
Prime Focus

Subaru TelescopeSubaru high-redshift SN survey•

Subaru/Hyper Suprime-Cam (HSC)• Field of View = 1.75 deg2

Subaru high-redshift SN survey

Yasuda et al. (2019)

Subaru high-redshift SN survey
We have been observing a 1.75 deg2 eld for more than 5 seasons

Moriya et al. (2021)fi•

High-redshift SN discovery from Subaru/HSC•

a SLSN at z = 2.4•

some more high-redshift SLSNe discovered
No long-lasting PISN candidates discovered•

Moriya et al. (2019a)

Long-lasting supernovae

Moriya et al. (2021)

HSC16aayt at z = 0.68

Moriya et al. (2021)

HSC16aayt at z = 0.68

Moriya et al. (2019b)

HSC16aayt at z = 0.68

Moriya et al. (2019b)

HSC19edgb at z ~ 0.23?

HSC19edge at z = 0.33

Going further away•

deep and wide transient surveys in NIR needed to discover more distant SNe
2020s are a golden age of wide- eld NIR astronomy!

EuclidESA, 2023 (July!)fi•RomanNASA, 2026-

Euclid mission
main target: cosmology with weak lensing & galaxy clustering• 15000 deg2 wide eld + 40 deg2 deep eld

fiScaramella et al. (2021)fi•

Euclid ltersfiScaramella et al. (2021)

Euclid Deep Field observation plan

(Euclid Deep Field North)(Euclid Deep Field South)+ some higher
cadenceobservations forcalibrations(Euclid Deep Field Fornax)

each visit reach VIS = 25.5 mag & Y = J = H = 24.0 mag

Moriya et al. (2022a)

A Type IIn model•

44-2243.5-2143-20UBV
R
I

absolute Vega magnitude-1

log bolometric luminosity (erg s )•ejecta: 10 Msun, 5e51 erg
CSM: 0.1 Msun/yr, 100 km/s, up to 1e16 cm

42.5
42
41.5
41-19-18-17-16

40.5-15

40-14
050

100
days after explosion

150

200

050

100
days after explosion

150200Light curves
z=12221VISYJH

22.5VISYJH222323.5

AB magnitude

apparent AB magnitude

peak magnitude2424.52324252525.5
26050

100

150
200250days in observer frame

300

350

400

260

123redshift456

Discovering PISNe with the Euclid Deep Survey

PISN model fromKasen et al. (2011)

Moriya et al. (2022a)

Discovering PISNe with the Euclid Deep Survey

Moriya et al. (2022a)

Roman•fi•

cosmology mission including Type Ia SN cosmology• 2-year time domain survey is guaranteed• plan to use F129, F158, F183
Roman broad-band lters
25% is open for general observers• we can submit proposals
redder lter than Euclid• Roman can go higher redshiftsfi•

PISN light curves with the Roman lters

PISN model fromKasen et al. (2011)

Roman can discover PISNe beyond z = 6=> constraining massive star properties at the epoch of reionizationfiMoriya et al. (2022b)

Roman light curvesz = 1025

peak magnitude
21

F158
F183
F213

2226

23
apparent AB magnitude

apparent AB magnitude

F158
F183
F213

272824252627282929300100200300
400
days in observer frame

500

600

3002468redshift

10121416

Robertson et al. (2015)

High-redshift PISN from Roman••••

F158 = 27.0 mag & F213 = 26.5 mag limits
10 deg2
5 year survey period
PISN rate based on the SFR density and Saltpeter IMF~ 20 PISNe at z > 6 from Roman!
Moriya et al. (2022b)

Summary•

SNe IIn detected up to z ~ 2.4 with optical transient surveys• long-lasting transients in optical surveys are good SN IIn candidates•

Euclid (launch in July 2023) can detect SNe IIn up to z ~ 4• cadence is not optimal•

Roman (launch in 2026) can detect SNe IIn up to z ~ 13