The Caltech Core Collapse Program CCCP Avishay Gal-Yam

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

CCCP executive committee CCCP Team 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 corecollapse SNe: every young (<30 days after last nondetection at discovery) core-collapse (via spectroscopy or phototyping) SN, above 18. 5 mag, visible from Palomar Collect homogeneous optical photometry (P 60), multiepoch spectroscopy (P 200, Keck), IR SEDs (P 200) 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

SN 2004 dh SN 2004 dk SN 2004 dn CCCP – First Results II-P SN 2004 fc II SN 2005 Y II SN 2005 bf Ib/c Ib SN 2004 fe Ic SN 2005 Z II SN 2005 bp II Ic SN 2004 ff Ic SN 2005 aa II SN 2005 bw II II SN 2005 bx IIn • 50 II SN observed 2005 ab SNe 2004 fx II SN SN 2004 dr II SN 2004 ge Ic SN 2005 ad II SN 2005 by • >5000 photometric points, >200 SN 2004 eb IIb SN spectra, 2004 gq Ib/c SNpoints. II SN 2005 ci ~150 IR 2005 an II SN 2004 ek IIn SN 2004 du II SN 2004 gt Ic SN 2005 ap II SN 2005 cl • Main observing SN 2005 ar complete. phase Ib SN 2005 cp II SN 2004 gv Ib/c Reference and calibrations. SN 2005 cs in SN 2004 er II SN 2005 E Ib SN 2005 au II SN 2004 et II-P SN 2005 H II SN 2005 ay II SNF 0630 progress SN 2004 em II IIn II II Quest_SN 1 II SN 2005 O Ib SN 2005 az Ib SN 2005 db IIn SN 2004 ex IIb SN 2005 U II SN 2005 ba II SN 2005 dp II Total 49 II 36 Ib/c 13 SN 2005 ds II SN 2004 gk Ic SN 2004 gy II Additional CCCP would-be’s:

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

From Observations to Explosion Physics: the Progenitor – SN Map Red Supergiant Type II-P Blue Supergiant SN 1987 A (faint, slow) LBV ( Car) Late W-R 1997 (WN) Early W-R (WC/WO) Massive Binaries Type IIn (dense CSM) SN 2005 gl Gal-Yam et al. 2007, 2008 Gal-Yam & Leonard 2008 Type IIL/IIb a 2005 0. 5’’ b 2007 (little H) c Type Ib (H, He) 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 1991 D: “The exceptionally bright Type Ib supernova 1991 D” (Benetti et al. 2002) SN 1992 ar: “The Luminous Type Ic Supernova 1992 ar at z=0. 145” (Clocchiatti et al. 2002) SN 1997 ef: “A hypernova model for the peculiar type Ic supernova 1997 ef” (Nomoto et al. 1999) And similar others, including SN 1999 as, among the brightest SN ever (6/13 obviously biased)

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

Guessing game (1) SN 2005 an:

Guessing game (2) SN 2005 au:

Classical II-Ps:

Peculiar II-Ps

SN 2004 ek: a peculiar SN II

SN 2004 cs, SN 2004 ex: type IIb

Type IIn

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

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

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 2004 gt) • Nugent et al. 2006 (II-P) • Leonard et al. 2006 (spectropolarimetry of SN 2004 dj, Nature) • Hendry et al. 2006 (the progenitor of type II-P SN 2004 A) • Gal-Yam et al. 2007, 2008 (progenitor of SN 2005 gl

What Next? Phase I: reference frames, calibration Phase II: taking advantage of this welldefined 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

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 2004 dr: a type II-L SN