Environments of SNe
including interacting SNe

Hanin KUNCARAYAKTI (≈ kun-čå-rå-yak-ti)
University of Turku, Finland

1Motivation: SN-progenitor connection•

Do observations match theoretical predictions?

•

What about interacting SNe?

2

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Georgy+2009
Heger+2003

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

SN “environment”
Not the circumstellar surroundings, but stellar populations•

Ranging from the whole galaxy (~kpc) toimmediate surroundings (~pc)•

In a star cluster, σv = few km/s (e.g. Bastian &Goodwin 2006) —> few pc/Myr•

Assumption: SN environment isrepresentative of progenitor’s birthplace•

Progenitor age (initial mass), metallicity,… production of certain SN types as afunction of env•= 15 pc

But beware of caveats
3

SN 2004dj

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Direct detections•

Pre-SN archival images, mostly HST

Pre-explosion•

Constrains initial progenitor mass throughphotometry, HRD•

Mostly SN II progenitors —> RSG ~ 8-20 M⊙•

Several SN IIb: yellow supergiants•

SN Ib/c: a few definitive detections?
•

SN

After

Fainter than typical WR stars, or in binaries (seetalk by Yoon, week I)
4

Smartt (2015)

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Drawbacks of direct detections(see also talk by Fraser, week I)• Resolution (distance) limited• Not all SNe have pre-explosion data; difficult to increase statistics• Existing data may not be good enough (only in 1-2 bands,

crowding/ambiguity, shallow…)

3212

J. R. Maund et al.

• Ideally, should be accompanied with confirmation of progenitor

disappearance• Metallicity? Extinction?
• Relies on star’s luminosity and color (evolutionary status) very

shortly before the explosion
SN 2009kr

5

Maund et al. 2015: progenitor candidate survived the SN

Figure 5. Pre-explosion WFPC2 and late-time ACS F555W and F814W observations of the site of SN 2009kr. The difference between
both filters, is shown in the right-hand panels of each row. Positive residuals in the difference image correspond to sources that are brighimage.

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Resolved (HST) photometry of SN local stellar
populations+ numerous otherauthors

Van Dyk+1999

Maund 2017, 2018

Ic

II
Ib
IIb

Resolved stellar populations of historic SNe and remnants:•
Diaz-Rodriguez, Murphy, Williams, Jennings+

6

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Pixel statistics/NCR•••

Fruchter+2006, James& Anderson 2006

CCSNe

Rank pixels bybrightness, normalize,
get value at SN position
GRB

Compare normalized
cumulative rank pixel
values (NCR) ofdifferent SN types
Brighter pixels
7MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

H! pixel statistics

Habergham+2014

Brighter H! pixels
8

Also see Ransome+2023

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Pixel statistics — SN vs massive stars•

Kangas+2017•

NCR of resolved stars in LMC and M33

9MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Main sequence

Evolved stars

Kangas+2017•

As expected: younger (~ more massive) stars are more associated to SF•

Compare this to SNe!

10

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

IIP

IIL

IIb

Ib

Ic

Kangas+201711

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

IIP

IIL

IIb

Ib

Ic

IIn

Kangas+2017

SN IIn ≠ LBV
12

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Explosion site spectroscopy•

Age indicator: e.g. H! EW

Ic
Ib
Ib/c

Leloudas+11

13

HK+18bMIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Explosion site spectroscopy•

Metallicity is somewhat scale-dependent, but comparison between populations should be (mostly) OK•

Proxy: host Z —> integrated, nuclear, Z gradient

Broad-lined Ic are moremetal-poor than Ic.
Necessary for GRB
production?

14

Modjaz+2011

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

IFU spectroscopy•

Spatial & spectral information in one go•

SN site + host galaxy (if large IFU)•

Better localization of SN parent stellar population,
can probe variations in the vicinity & context
within the host•

Metallicity information, also age

Kuncarayakti+2013aKrühler+2017

15

Christensen+2008; Stanishev+2012; Kuncarayakti+2013ab, 2018;
Rigault+2013; Galbany+2014, 2016ab, 2018; Krühler+2017; Cikota+2017;
Izzo+2017, 2018; Lyman+2018, 2020; Schady+2019; Sun+2021…

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Kuncarayakti+2018b, d < 40 Mpc (200 pc/“ scale)
YO
UN

ME
GE
R

TA
LR

•

Ic youngest, IIn oldest•

No significant metallicity differences in CCSNe•

Single+binary progenitors for SESNe

IC
H

Low-Z tail in SN II and Ic

16

vs. Georgy+09
rotating single-starMIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Galbany+2018

Stellar population age, SN II vs. others

Ic

•

•

SN Ic: youngest, high-Z
and SFRIIn

Two IIn populations?
Young and old.
17

Ib

IIb

Ibc

Ia

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Ganss+2022, <30 Mpc

Galbany+2018•

Targeted/untargeted:different trends
18

Low-Z tail in SN II and Ic

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

SN populations in luminous IR galaxies (LIRGs)

Kankare+2021
19

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Part II

20

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

IIn/Ibn environments

21
Impostors are more metal-poor than IIn/Ibn

Taddia+2015

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Taddia+2015

22•

IIn-L (98S-like): higher Z•

88Z-like (long-lasting) and IIn-P(94W-like): lower Z, like impostors

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Taddia+201523

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

cutoff(cf. next talk by Moriya!)

Taddia+201524

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Fraser+2013: 2009ip

Fransson+22

Smith+2022

25

Brennan+2022: 2016jbu

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

SNe II in low-luminosity hosts
Gutiérrez+18

Also see talk by Beasor, week II

26

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments•

2015bs, type II (Anderson, Dessart, Gutiérrez+2018)•

Host Mr ~ -12.2 mag (faintest)•~0.1 Zsun•

Progenitor 17-25 Msun?

27

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Ibn hosts
Pastorello+2015c:• Ibn hosts are almost all spirals• Z plays marginal role
Schulze+2021

28

Kool+2021

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

PS1-12sk(Sanders+2013)

28 kpcHosseinzadeh+2019(See Griffin’s talk on Fri)29

starStarburst99[3]progenitor. Thepopulation
minimumage
agesdata.
from Starburst99 remove this progenitor• Equivalent– Goodthroughseeing stellar
allows wind
for recognitionof structures
down to few hundred
parsecs. width (EW) of H↵ emission line was also used withand helium
before turning
into a Wolf-Rayetlower
masses,closer to 13SNe
M . — Hanin Kuncarayakti: Environments
MIAPbPInteractingThe
ratiodataof Wolf-Rayetstars
Ibn doesusing
not add
up so there• Raw
was reduced
andandcombinedthe standard
pipelines. Datacube
wascorrectedforatmosphericeffects.
– Starburst99 does not include binary system and it underestimates the age, but is still a useful tool for rough estimations.
A type Ia supernova is produced by an old stellar system and the surroundin• Final datacube is a mosaic of four pointings, total IFU FoV of 2’x2’ with a–spectral
range thespanningfromnm to 935
EW describes
strengthof 475an emission
linenmin relation to
the accompanying
continuum
spectra.
results
support this view.
Supernova
candidate AT2016cnz was never classid evolvestoresemble
type
Ib
in
later
times.
The
understandingisand a resolution of 0.2”/pixel.
suggestsa typeII supernovaage
withlow massprogenitor.
– EW can be used as an age indicator as H↵ emissions declinewiththe populationas amassive
stars
producing the
WeWe
hav
ha
hrough stellar wind and the helium beneath reveals itself shortly
These
resultssuggest that progenitors to the Ibn and IIb supernovae inthis caionizing
photonshavedied. SNSN(a)(a)
The
host
galaxy
NGC
2466
and
the
observed
locations.
(b)
H↵H↵
map
ofof
the
galaxy.
emerginThe
hostgalaxy
NGC
2466
and
the
observed
locations.
(b)
map
the
galaxy.
emerg
Wolf-Rayet stars. In these kind of binary systems the stars interact with each oprogeniproge• Ionization parameter, which indicates the ratio of hydrogen ionizing
and neutral
was measured
withsimilara ratiotypesof of stars
ter from photons
stellar surfaces.
The gas,phenomenon
produces
wit
constraiH↵ and [SII]6717Å+6731Å[4].
constrmedia as with massive stars but at lower initial masses.
• Metallicities, the amount of elements heavier than helium, Supernova
were calculated forType
SNe and the galaxy
using the N2 andS2ASASSN-14dd
Age (Myrs)
Metallicity(log(Omation can be observed
simultaneously
allowing
detailed
analysisSN2016iye
indexes. N2 uses the ratio of H↵ and [NII]6584Å emission lines and additionally S2 uses the [SII] doublet[5][6].

SN Ibn host IFU analysis: (some) progenitors are not that massive

55

White lightroscopy

Ack
Ack

Starburst99 BPASSv2.1
N2
ASASSN-14dd Ibn
7.5
31.6
8.52± 0.05
The
com
The
c
SN2016iye
IIb
6.25
31.6
8.47± 0.01 8.5
Ia galaxy, which
6.35 implies relatively
79.4 old
8.49±
The observed core-collapse supernovae are not in luminous star SN2003gh
forming regions in thisage 0.01 8.7
and low mass for their progenitors. It is possible to miss smaller
star forming regionsat this distance,
low ionization
AT2016cnz
Cand.
7.01 but the20.0
8.48± 0.02 8.4

ate of the art IFU that can collect separate spectra for each pixel

4 Results

AT2016cnz

ors and their enviroments; the whole galaxy can be studied with

Refe
Re

SN2003gh

three hours with a seeing of 0.8”-1.5”.
ion light-years. At this distance the scale is 0.362 kpc/”.
o few hundred parsecs.
pipelines. Datacube was corrected for atmospheric effects.
V of 2’x2’ with a spectral range spanning from 475 nm to 935 nm

parameters supports the view of older ages[Figure 2]. Wolf-Rayet stars have a maximum lifetime of 5 Myrs and a minimum
Robe
1.
Rob
mass of 25 M at solar metallicities[7]. Observed metallicitiesTableare 1:
sub-solar
so theinages
have toandbe theeven
smaller
for a 14dd
singlecomes1.
Supernovae
the galaxy
criticalvalues.
from a s
star progenitor. The minimum ages from Starburst99 remove thisoutright
andpointing
the BPASS
ageolderfittingotherprogenitor
SNe with typethe EWmethodto theageimpliesof this Ibn progenito
2. 2.
EldridEldlower masses, closer to 13 M .
A type Ia supernova is produced by an old stellar system and the surrounding enviroment is not directly linked with it. The
3. 3.
Leith
Lei
results support this view. Supernova candidate AT2016cnz was never classified spectroscopically, but the BPASS age fitting
5 kpc
1'
4. 4.
Diaz,
Dia
suggests a type II supernova with a low mass progenitor.
We havepresented
resultsof a study
on asystems
supernova
using
These results suggest that progenitors to the Ibn and IIb supernovae
in thiscase arethein fact
interacting
binaryand host
not galaxy
5.
Marin
5.
Ma
(a) The host galaxy NGC 2466 and the observed SN locations. (b) H↵ mapofthegalaxy.
emerging
view
that
type
Ibn
and
IIb
supernovae
arealso
producedininteract
Wolf-Rayet stars. In these kind of binary systems the stars interact with each other through Roche lobe overflow, expelling matprogenitor.
The thestrength
MUSE asstripped
an instrumentwith addition of6.spectra
ter from stellar surfaces. The phenomenon produces similar typesof stars withouterofenvelopes
and circumstellar
Dopit
6.
Dop
constraining
supernova
progenitorsinsituations
where
the
progenitor
stars
cmedia as with massive stars but at lower initial masses.

5 SummaryH-alphaSN2016iye

ASASSN-14dd(c)(c)
S2S2
metallicity
map
ofof
the
galaxy.
Radialdependence
ofof (d)H↵
EW
map,
highervaluesindicatestronger
H↵H↵
and
thus
metallicity
mapthegalaxy.
Radialdependence
(d)
H↵
EW
map,
highervaluesindicatestrongerandthusSupernovaType
Age (Myrs)
Metallicity(log(O/H)+12)
metallicity
isyoungerstellarpopulations
metallicity
evident.
youngerstellarpopulations
Starburst99 BPASSv2.1
N2
S2• isevident.

Host: 1 Ibn, 1 IIb, 1 Ia, 1 unk. inAcknowledgments
13 yrsASASSN-14dd Ibn
7.5
31.6
Figure1: 1:
Different
maps
constructed
from
the
IFU
datacube
FigureDifferent
maps
constructed
from
the
IFU
datacube
SN2016iye
IIb
6.25
31.6
Ia
6.35
79.4
• SN2003gh
AT2016cnz
Cand.
7.01
20.0

AT2016cnz•

s. (b) H↵ map of the galaxy.

8.52±
The0.05
computer resourcesof the Finnish IT Center for Science (CSC) and the F
8.47± 0.01 8.53± 0.02
8.49± 0.01 8.75± 0.03
8.48± 0.02 8.46± 0.03

SN not associated with a strongReferences
HII region

SN2003gh

1'

7. 7.
Crow
Cro

5 kpc

1. Roberto, C. F. & Abilio, M. 2005, MNRAS, 358, 363

Table 1: Supernovae in the galaxy and the critical values. 14dd comesfrom aJ.stellar
population
an PASA,older age
2. Eldridge,
J. & Stanway,
E. R.with2017,
34, thanE058theother SNe with the
EW methodpointing M⊙
to the older
age of this Ibn progenitor.
Possiblyfrom
10-20
progenitor
3. Leitherer, C & Schaerer, D 1999, ApJS, 123, 3

4. Diaz, A. I., & Terlevich, E. 1991, MNRAS, 253,
245 Kravtsov,
Timo

5 Summary
5. Marino, R. A. & Rosales-Ortega, F. F. 2013,
A&A,thesis,
559, 12 U. Turku
MSc(Also see Dessart,
Hillier,HK,
2022)
We have presented the results of a study on a supernova host galaxy using integral field spectroscopy. Results support the
30IIb supernovae are also produced
6. Dopita,
M.A. & binary
Kewley,systems
L.J., 2016,
Astrophys
Space
Sci,
361,
61
(now
ESO
emerging view that type Ibn andin interacting
insteadof justby a atsinglestar Chile)(aMIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Icn hosts

SESNe
USSNe
2019hgp; Gal-Yam+2021

SF hosts; but we know only a handful of Icn so far(See Pellegrino’s talk on Thu)

31

Pellegrino+2022

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Davis+2022
32

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Ic with CSM•••(Also see talk by Sollerman
on Thu)2010mb (Ben-Ami+2014; see Gal-Yam’s talk on week II)•

slow, broad LC, variable narrow [O I], pPISN candidate•

SF host, ~0.5 Zsun, 0.32 Msun/yr SFR (~LMC-like?)2017dio (HK+2018a)•

Ic -> IIn, slow rise (80d)•unresolved host, fainter (Mg ~ -15 mag) than SMC

Cf. iPTF14hls(Arcavi+2017):
SMC-like, 0.4-0.9 Zsun,
3e8 Msun

2017ens (Chen+2018)•(Super) luminous IcBL -> IIn•

Host Mg ~ -16.5 mag, Z ~ 0.3 Zsun
33

Also 2015bs, earlier slides

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

87A-like SNe

Taddia+2013

34

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

SLSN hosts

Leloudas+1535

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments••

H-poor:•Stifled SLSN-I production >0.4 Zsun•

Cut > 1e10 Msun

H-rich: diverse

Chen+16
Schulze+18

Kangas+22

Also see works by Lunnan+, Angus+, Howell+, Perley+…

36

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

FBOT hosts••

SF hosts
Mild preference for high sSFR, low-Z

37

Wiseman+20

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

The Pasture

Lyman+2020
AT2018cow

38

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Lyman+2020
39

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments(See also Dan Perley’stalk, week II)

Sun+2023

40

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

Summary•

Typically SNe Ic arise from higher mass and metallicity populations•

No significant differences in metallicity for other SN subclasses, except for SLSNe, LGRB

•

•

•

Hybrid envelope stripping? Cf. Fang, Maeda, HK+19 nebular spec•

Relation between mass loss/CSM with environments…?

Interactors:•

IIn from both old and young populations; similar to SN II env on average•

Ibn? Icn?

Some curious oddballs: associations with low-luminosity (~ low-Z); *cherry-picking, of course•

But for decades we’ve been used to large, bright galaxies, high-Z — do we understand low-Z?
41

MIAPbP Interacting SNe — Hanin Kuncarayakti: Environments

42