Improving the Low-Redshift Foundations: Results from the Lick Observatory Supernova Search (LOSS) Alex Filippenko Department of Astronomy University of California, Berkeley (Main collaborators: W. Li, J. Leaman, M. Ganeshalingam) May 7, 2008

Previous ESSENCE Hubble Diagram 60 SNe Ia, Wood-Vasey et al. (2007)

Preliminary Current ESSENCE Hubble Diagram 156 SNe Ia, Wood-Vasey et al. (2008, in prep.)

30 inch (0.76 m) mirror Lick Observatory; Katzman Automatic Imaging Telescope Funded by NSF, the Sylvia & Jim Katzman Foundation, the TABASGO Foundation, AutoScope Corp., Sun Microsystems, Hewlett- Packard Co., the University of California (Berkeley and Santa Cruz), and NASA. (Laurie Hatch)

Weidong Li

SN 2001en Cosmic ray New image Template Difference (after much processing) Undergraduate students examine the SN candidates that were found automatically. NGC 523

LOSS SNe, m < 19 mag when discovered

, 1.5 million obs LOSS Cadence: 2-12 days Observation interval (days) NoofobsNoofobs a. 200 gal: every 2 days b. 5,000 gal: every 5 days c. 10,000 gal: every 10 days

LOSS results: follow-up efforts Prompt alerts to ~80 astronomers/SN observers CfA Supernova program (Kirshner et al.) Carnegie SN Program (Freedman, Phillips, et al.) Follow up with our own telescope network 10-20% of time Photometry; calibration 6-9 nights/mon Calibration; photometry 3 nights/mon spectroscopy Occasional spectroscopy KAITLick 1-mLick 3-mKeck I/II 10-m

SN 1998dh (Type Ia) Age: -6 days Maximum +26 days +47 days +102 days

Mohan Ganeshalingam

Template subtraction; SN photometry (Automatic pipeline)

SN Ia

SN II

Preliminary results on SNe Ia (Ganeshalingam et al. 2008, in prep.)

A V (mag)  Hubble type, E  Sd/Irr SNe Ia

(before correction)

SNe Ia (MLCS2k2)

(KAIT + Jha et al. 2007)

Bulk Flows from SN Ia (Riess et al. 1995, 1997)

SN Ia 1998dh before/after SN 1998de before/after

(Leonard et al. 2005, ApJ, 632, 450)

Chornock et al SYNOW model with 11 ions ( Fe II, Fe III, Si II, S II, Ca II, Mg II, O I, Ni II, Co II, Ti II, C III ) V phot =5000 km/sec SN 2005hk (Chornock et al. 2006)

CSP Observations of SN 2005hk (Phillips) HJHJ No secondary maximum in IR. Strength of the secondary maximum correlated with the amount of mixing of 56 Ni in the ejecta (Kasen 2006). The absence of secondary maximum suggests complete mixing of 56 Ni.

Supernova Rates Cappellaro et al (C99 hereafter) *5 surveys (1 visual, 4 photographic plates) *137 SNe in about 10 4 galaxies *B-band luminosity normalization * SN rate as a function of SN type (Ia, Ib/c, II) and host morphology (E/S0, Sa/b, Sbc/d, Irr) Mannucci et al (M05 hereafter) Same database as C99 K-band luminosity normalization SNr versus galaxy color (B-K) Benchmark for z = 0 SN rate:

Jesse Jesse Leaman

LOSS SN rates ( ): Leaman, Li, & AVF (2008, in prep.) 844 SNe observed (600 LOSS discoveries & 240 independent confirmations) SNe used* in the SN rate calculation for a given normalization technique and SN type: Filter| Ia | Ib/c | II | ? | Total B K B&K *Only SNe for which we have all host-galaxy information were included

Units 1 SNu = 1 SN / (100 yr) / (10 10 L Sun ) (SNuB, SNuK for B and K bands) 1 SNuM = 1 SN / (100 yr) / (10 10 M Sun )

SN Ia rate proportional to (1) SFR [prompt] and (2) galaxy mass [extended] (confirms Mannucci et al. 2004, 2005, Scannapieco & Bildsten 2005, Neill et al. 2006, Sullivan et al. 2006)

(Dahlen, Strolger, & Riess 2008 compilation and new high-z results; dashed line = best 1- component model with delay time 3.4 Gyr.) LOSS rate = Volume SN Ia rate versus redshift

Katzman Automatic Imaging Telescope (KAIT) (Laurie Hatch)