1. The Caltech Core-Collapse Program (CCCP)
Avishay Gal-Yam
The Benoziyo Center for Astrophysics,
Weizmann Institute off Science, Israel

2. CCCP executive committee
CCCP Team
CCCP executive committee
Avishay Gal-Yam (PI)
Brad Cenko Dave Sand
Derek Fox Dae-Sik Moon
Doug Leonard Alicia Soderberg

3. Outline The CCCP Project Motivations Type II SNe Limitations
Future prospects and PTF

4. The CCCP: A large observational program designed to:
Observe a well-defined complete sample of core-collapse SNe: every young (<30 days after last non-detection at discovery) core-collapse (via spectroscopy or phototyping) SN, above 18.5 mag, visible from Palomar
Collect homogeneous optical photometry (P60), multi-epoch spectroscopy (P200, Keck), IR SEDs (P200)
Characterize the CC SN population
Test viability of SNe II-P for cosmology
Provide well studied sample of Ib/c SNe as comparison for high-z GRB studies
Support other SN studies at Caltech and in general

5. CCCP – First Results 50 SNe observed
SN 2004dh
II-P
SN 2004fc II
SN 2005Y
SN 2005bf
Ib/c
SN 2004dk Ib
SN 2004fe Ic
SN 2005Z
SN 2005bp
SN 2004dn
SN 2004ff
SN 2005aa
SN 2005bw
SN 2004dr
SN 2004fx
SN 2005ab
SN 2005bx
IIn
SN 2004du
SN 2004ge
SN 2005ad
SN 2005by
SN 2004eb
IIb
SN 2004gq
SN 2005an
SN 2005ci
SN 2004ek
SN 2004gt
SN 2005ap
SN 2005cl
SN 2004em
SN 2004gv
SN 2005ar
SN 2005cp
SN 2004er
SN 2005E
SN 2005au
SN 2005cs
SN 2004et
SN 2005H
SN 2005ay
SNF0630
Quest_SN1
SN 2005O
SN 2005az
SN 2005db
SN 2004ex
SN 2005U
SN 2005ba
SN 2005dp
Total 49 36 13
SN 2005ds
Additional CCCP would-be’s:
SN 2004gk
SN 2004gy
50 SNe observed
>5000 photometric points, >200 spectra, ~150 IR points
Main observing phase complete. Reference and calibrations in progress

6. Motivations (1): Constraining SN models
Red
Supergiant
Blue
Late W-R
(C, O)
Early W-R
(He, N)
Massive
Binaries
Luminous
Variables
SN 1987A
(faint, slow)
Type II-P
Type IIL/IIb
(little H)
Type Ic (He)
GRB/XRF
Type Ib
(H, He)
Type IIn
(dense CSM)
Initial conditions: stars
Theory
Observations
End product: supernova
Observations
Model

7. From Observations to Explosion Physics: the Progenitor – SN Map
Red
Supergiant
Type II-P
0.5’’ a b c
1997
2005
2007
Gal-Yam & Leonard 2008
Blue
Supergiant
SN 1987A
(faint, slow)
Type IIn
(dense CSM)
LBV
( Car)
SN 2005gl
Gal-Yam et al. 2007, 2008
Late W-R
(WN)
Type IIL/IIb
(little H)
Early W-R
(WC/WO)
Type Ib
(H, He)
Massive
Binaries
Type Ic (He)
Data from Van Dyk, Li, Filippenko et al.; Smartt, Hendry, Maund et al.; Gal-Yam & CCCP et al.

8. Motivations (2): Rates (esp. at high-z)
Typical properties (peak mag, color curve) of CC SNe a major missing ingredient (starting with Dahlen et al. 1999, Sullivan et al. 2000, up to Weidong Li’s talk)
Need to: classify SNe
Convert counts to rates

9. What’s missing on the SN side?
Self consistent classification
Typical properties (and their dispersion) for each class
Relative fractions

10. Why not a catalog sample?
In a sample of SNe Ib/c from the literature:
SN 1991D: “The exceptionally bright Type Ib supernova 1991D” (Benetti et al. 2002)
SN 1992ar: “The Luminous Type Ic Supernova 1992ar at z=0.145” (Clocchiatti et al. 2002)
SN 1997ef: “A hypernova model for the peculiar type Ic supernova 1997ef” (Nomoto et al. 1999)
And similar others, including SN 1999as, among the brightest SN ever (6/13 obviously biased)

11. 22 SNe II from CCCP (extended):
Do SNe spectroscopically similar to SN 1999em (II-P prototype) always have a plateau
Are supernovae not similar to 1999em always non-plateau?
What do SNe IIn look like

12. Guessing game (1) SN 2005an:

13. Guessing game (2) SN 2005au:

14. Classical II-Ps:

15. Peculiar II-Ps

16. SN 2004ek: a peculiar SN II

17. SN 2004cs, SN 2004ex: type IIb

18. Type IIn

19. A Look at Type II SNe 22 events with good data 12(14)(15)(18) II-P
Photo type
Spec type
Reference/comments
SN 2004A P
II-P
Hendry et al. 2006
SN 2004cs L
IIb
Rajala et al. 2005
SN 2004dh
Nugent et al. 2006
SN 2004dr II
SN 2004du
SN 2004ek
pec
SN 2004em
P-pec
SN 2004er
SN 2004et
Li et al. 2005
SN 2004ex
Gal-Yam et al. 2007
SN 2004fc
SN 2004fx
Hamuy et al. 2006
SN2005an
II (similar to 99em)
(preliminary, 1 of 3 spectra)
SN2005au
IIb (weak)
(preliminary, 1 of 4 spectra)
SN2005ay
Tsvetkov et al. 2006; Gal-Yam et al. 2008; Bufano et al. 2008
SN 2005ba
(preliminary, 1 of 2 spectra)
SN 2005bw
SN 2005ci
SN 2005cl
“P”
IIn
SN 2005cp
SN 2005cs
Li et al. 2006; Pastorello et al. 2006; Tsvetkov et al …
SN 2005db
A Look at Type II SNe
22 events with good data
12(14)(15)(18) II-P
2/3 IIb (and counting)
4 II-L (inc. 2 IIb)
3 IIn

20. Some conclusions:
Both light curve and multi-epoch spectroscopy are essential
SNe II-P appear to constitute a large fraction of SNe II and core-collapse events in total (~50%)
BTW, f(8<M<15 / 8<M<150) = 57% (for Salpeter IMF)
SNe II-L appear to exist (photo-L, spectroscopically non b/n) but are rare
CCCP was too small! You really need x10 more of the same

21. The population of SNe Ib/c
Gal-Yam et al. 2006
Soderberg et al. in prep.

22. Cosmology with SNe II-P
Nugent et al. 2006; Leonard+ in prep

23. CCCP data also used in: Rajala et al. 2005 (phototyping)
Gal-Yam et al (the progenitor of SN 2004gt)
Nugent et al (II-P)
Leonard et al (spectropolarimetry of SN 2004dj, Nature)
Hendry et al (the progenitor of type II-P SN 2004A)
Gal-Yam et al. 2007, 2008 (progenitor of SN 2005gl

24. What Next? Phase I: reference frames, calibration
Phase II: taking advantage of this well-defined sample of SNe to study:
Environment (high resolution imaging with Keck-LGS, HST)
H imaging (where possible) to measure distances to HII regions
Local metallicity from nearby HII regions (high resolution spectroscopy)

25. What is missing?
CCCP is dominated by KAIT-discovered objects, and is therefore limited to the bright-galaxy population
At high-z, low mass, high SFR galaxies will be important
Core-collapse SNe in small galaxies ARE DIFFERENT
Need a “blind” survey

26. Core Collapse Supernovae: something new?
Most nearby SNe are found in targeted searches of luminous galaxies
Blind surveys find new types of supernovae in faint hosts. New SNe?
Pilot projects (SNF) give interesting clues …
PTF will provide 75(10) CC SNe in hosts with <LMC(<SMC) metallicities

27. The PTF
There is nothing like searching, if you want to find something.
You usually find something, if you search,
but it is not always quite the something you were after.
Thorin Oakenshild

28. Thanks!

29. SN 2004dr: a type II-L SN