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

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

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

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

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

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

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.

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

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

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)

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

Guessing game (1) SN 2005an:

Guessing game (2) SN 2005au:

Classical II-Ps:

Peculiar II-Ps

SN 2004ek: a peculiar SN II

SN 2004cs, SN 2004ex: type IIb

Type IIn

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. 2006 … 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

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

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

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

CCCP data also used in: Rajala et al. 2005 (phototyping) Gal-Yam et al. 2005 (the progenitor of SN 2004gt) Nugent et al. 2006 (II-P) Leonard et al. 2006 (spectropolarimetry of SN 2004dj, Nature) Hendry et al. 2006 (the progenitor of type II-P SN 2004A) Gal-Yam et al. 2007, 2008 (progenitor of SN 2005gl

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)

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

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

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

Thanks!

SN 2004dr: a type II-L SN