Nature’s

Early interaction with C/O

Gal-Yam et al. 2014, NatureI. Arcavi

Avishay Gal-Yam
Department of Particle Physics and Astrophysics
Weizmann Institute of ScienceOutline• SN 2010mb – PPISN?
• SN 2022oqm• One slide regarding SN 2019hgp (Icn)

SN 2010mb (Ben-Ami et al. 2014)• Long-lasting (600d) type Ic SN• Powered by interaction at late times

SN 2010mb (Ben-Ami et al. 2014)• Long-lasting (600d) type Ic SN• Powered by interaction at late times

SN 2010mb (Ben-Ami et al. 2014)• Long-lasting (600d) type Ic SN• Powered by interaction at late times• Narrow O emission lines (OIII 5007
and OI 5577) powered by theinteraction

SN 2010mb (Ben-Ami et al. 2014)• Long-lasting (600d) type Ic SN• Powered by interaction at late times• Narrow O emission lines (OIII 5007
and OI 5577) powered by theinteraction

SN 2010mb (Ben-Ami et al. 2014)• Long-lasting (600d) type Ic SN• Powered by interaction at late times• Narrow O emission lines (OIII 5007
and OI 5577) powered by theinteraction• Can be decomposed into 56Ni +interaction

SN 2010mb (Ben-Ami et al. 2014)• Long-lasting (600d) type Ic SN• Powered by interaction at late times• Narrow O emission lines (OIII 5007
and OI 5577) powered by theinteraction• Can be decomposed into 56Ni +interaction• Requires high CSM mass (~3 solar)
and high ejecta mass (>10 solar)• Suggests PPISNSN 2022oqm (Irani et al. 2014)• A modern event with nicer data, early
UV bumpSN 2022oqm (Irani et al. 2014)• A modern event with nicer data, early
UV bumpSN 2022oqm (Irani et al. 2014)• A modern event with nicer data, early
UV bump• Very early spectrum – highly ionizedC/O (we correct erroneous ID of He II
in PTF14gqr = 2014ft)• Velocities are slow (5000 km/s) earlyon and fast (>10000 km/s) later:
Seeing (thin) CSM and then SNphotosphereSN 2022oqm (Irani et al. 2014)• A modern event with nicer data, early
UV bump• Very early spectrum – highly ionizedC/O (we correct erroneous ID of He II
in PTF14gqr = 2014ft)• Velocities are slow (5000 km/s) earlyon and fast (>10000 km/s) later:
Seeing (thin) CSM and then SNphotosphere• Obvious transformation at day 2

20000km/s

SN 2022oqm (Irani et al. 2014)• A modern event with nicer data, early
UV bump• Very early spectrum – highly ionizedC/O (we correct erroneous ID of He II
in PTF14gqr = 2014ft)• Velocities are slow (5000 km/s) earlyon and fast (>10000 km/s) later:
Seeing (thin) CSM and then SN
photosphere• Obvious transformation at day 2• CSM+shock cooling +0.12 solar massof 56Ni• Nebular at 60days and Ca-rich at latetime; Massive star or WD?

CSM
Shockcooling56NiType Icn (Garching: 4 years later)
3#10 -15Type II-P (~solar)
Type IIb (H-depleted wind)Type Ibn (He wind)Type Ic (He depleted wind)Type Ic (C/O/Ne wind)

O VI
2.5

He II

H,
2

Scaled F 6 [erg/s/cm 2 /Ang]

Growing list of objects:
SN 2019hgp
SN 2021csp (Perley et al.)
SN 2021ckj, SN 2019jc (Pellegrino et al.)
SN 2022ann (Davis et al.)

He II

C II

N IV

1.5

He I
He I He I C II

C III + He II
1C IV
C III
[Ne III] [O III]
C III

0.5

Tomorrow: Type Icn: WR explosions?

03500

4000

4500

5000

5500

6000

Rest wavelength [Ang]

6500

7000

7500

8000

SN 2019hgp• Very fast evolving SN

SN 2019hgp• Very fast evolving SN• Unique early spectrum: C,O,Ne; no
H; No strong features from He

SN 2019hgp• Very fast evolving SN• Unique early spectrum: C,O,Ne; no
H; No strong features from He

SN 2019hgp• Very fast evolving SN• Unique early spectrum: C,O,Ne; no
H; No strong features from He

SN 2019hgp• Very fast evolving SN• Unique early spectrum: C,O,Ne; no
H; No strong features from He• C/O explosion within an extended
C/O wind; evolving into a Ic SN

SN 2019hgp• Very fast evolving SN• Unique early spectrum: C,O,Ne; noH; No strong features from He• C/O explosion within an extended
C/O wind; evolving into a Ic SN• Can be explained by SB in a windfollowing interaction with a CSM

SN 2019hgp• Very fast evolving SN• Unique early spectrum: C,O,Ne; noH; No strong features from He• C/O explosion within an extended
C/O wind; evolving into a Ic SN• Can be explained by SB in a windfollowing interaction with a CSM

SN 2019hgp• Very fast evolving SN• Unique early spectrum: C,O,Ne; noH; No strong features from He• C/O explosion within an extended
C/O wind; evolving into a Ic SN• Can be explained by SB in a windfollowing interaction with a CSM

Meanwhile, in Israel…

Sagi Ben-Ami, Eran Ofek (PIs) and the WIS observatory team

ULTRASATULTRASAT

Thanks