The Lick Observatory Supernova Search (LOSS) and Follow-up Program Alex Filippenko Department of Astronomy University of California, Berkeley (with W. Li, S. Jha, J. Leaman, M. Ganeshalingam, et al.)

Caprielle Corona Nikole Filippenko

03W-01a, total eclipse

the Katzman Automatic Imaging Telescope; 0.75 m, at Lick Observatory Fully robotic observations Fully automatic image processing Humans verify SNe Monitor many galaxies Maintain small interval

Weidong Li (UCB)

2. No. of images per night 700  1300 images/night 3. Interval distribution 1. No. of galaxies monitored: 14,000  7,500 (06/2004) Observation interval (days) Number of observations 2001  2003 After Jun 2004

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

SN 2001en Cosmic ray New image Template Difference (after much processing) Undergraduate students confirm, and find the trickier ones, by eye. (Auto- observe some candidates.) NGC 523

KAIT Supernova Search & Analysis Team, May 2005

LOSS SNe, m < 19 mag at time of discovery Year N(SN) Total nearby SNe, m < 19 mag LOSS SNe

755 SNe in the galaxies monitored by LOSS during (67%) discovered by LOSS. 716 have SN type and host-galaxy redshift. Can study rates, systematics, etc.

Supernova rate (Leaman, Li, AF 2006) E S Sa Sab Sb Sbc Sc Ir Gal. TypeIaIb/cIIN(gal) Total: 566 SNe in 13,000 galaxies Previous: 137 SNe in 4,000 galaxies (5 combined searches: visual & photographic) Cappellaro et al. 1999

Jesse Jesse Leaman

All SNe (716) Luminosity function of SNe a) Discovery mag; peak mag from light curve b) Monte Carlo completeness simulation of our search We have unfiltered light curves for all 716 SNe from the galaxy monitoring data! N(SN type, Gal type, L) Discovery mag

A network of SN observers Prompt alerts to 70 astronomers/SN observers Carnegie Supernova Program (CSP), CfA group, Caltech Core-Collapse Program (CCCP), CTIO group, ESO group, etc. Follow-up with our own telescopes 10-20% of time Photometry calibration 2-3 nights/mon Calibration photometry 3 nights/mon spectroscopy Occasional spectroscopy KAITLick 1-mLick 3-mKeck I/II 10-m

Filtered photometry database Some Good Great Total SN Ia SN II SN Ibc Total: 278 (As of Dec 19, 2005)

KAIT BVRI follow-up of bright SNe Ia; data reduced by hand (labor intensive!) B V R I

Mohan Ganeshalingam

Sample light curves from LOSS photometry pipeline (1)

Sample light curves from LOSS photometry pipeline (2)

For details, see Li, Filippenko, Chornock, & Jha 2003b, PASP, 115, 844 Respond automatically to GRB alerts. Interrupt KAIT’s normal observations; take a pre-arranged sequence of images. Reach 19 th mag within 60 s of alerts. Unfiltered obs.; now V, I, unfiltered.

GRB KAIT2

GRB KAIT3

(Li, Filippenko, Chornock, & Jha 2003a) Obs. started at t = 105s 18 data points in 10 min One of the 2 GRBs (through 2002) with reverse-shock emission detected

Nearby SNe Ia: Physics and progenitors Li et al in prep U B V R I High-quality data for modeling Also observed by HST, Swift SN subclasses/statistics: progenitors 91T-like: only in spiral galaxies 91bg-like: prefer E galaxies Normal: in all kinds of galaxies Peculiar/bizarre SNe Ia (Jha et al. 2006, in press) 2002cx

SN 2002cx- like: a new subclass of SN Ia… but we really don’t know what produces them!

Nearby SNe Ia: Cepheid distances SN Ia HST Calibration team (Saha et al.) 11 observed, 2 were ideal calibrators Subset analyzed by the HST H0 Key project (Freedman et al.) Recent efforts led by Riess et al. (2005) 2 ideal calibrators observed. 2 more are being observed (1995al; 2002fk). H0 = 73 ± 4 ± 5 km s -1 Mpc -1

Si Correcting for Intrinsic Variations and Dust shape of the light curve lets us read the label on our cosmic light bulb measuring colors lets us correct for attenuation of the light by dust

Si MLCS2k2 light curve fits SN 1999cp and SN 2002cr, both in NGC 5468 μ = ± 0.07 mag μ = ± 0.10 mag KAIT BVRI photometry

Si Correcting for Intrinsic Variations and Dust

Going with the Flows (Jha et al. 2006)

Nearby SNe Ia: Anchor for Hubble diagram

A Hubble Bubble? a 6% difference in the expansion rate at a radius of 300 million light years statistical signifcance is 3σ, but robust with subsamples, other distance techniques Jha, Riess, & Kirshner (2006)

a real local void? K-corrections? photometric offset? –new data vs. Calán/Tololo? –morphology/extinction? a potentially huge systematic ➔ test with more nearby objects! A Hubble Bubble?

Systematic Effects These are now beginning to dominate statistical uncertainties in studies like ESSENCE, SNLS, etc. Will be completely overwhelming for SNAP/JDEM, LSST, etc. Need to understand effects of metallicity, progenitor evolution, dust, demographics… The NEARBY samples are crucial!

SN 2004dj (SN II-P) in NGC 2403 Spectropol- arimetric study (Doug Leonard, AF, et al.; mostly Lick 3-m); Nature, 23 March issue

SN II-P

Polarization of SN 2004dj

SN 2002ap (Ic-pec): Leonard+ 03

Conclusions for core-collapse SNe The deeper we peer into the heart of the explosion, the greater the asphericity (Wang, Wheeler, et al. also discovered this). In Type II-plateau events, the asphericity at early times is cloaked by a thick hydrogen envelope. > Implies an intrinsically aspherical explosion mechanism!

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

Conclusions, SNe Ia All are intrinsically polarized. Continuum pol.: suggests minor-to-major axis ratio of ~0.9 if viewed equator-on (Höflich 1991 models). Line pol.: suggests partial obscuration of the photosphere by clumpy, newly synthesized intermediate-mass elements. High-velocity SNe Ia have the strongest line pol.: clumps have greater optical depth than in normal SNe Ia. High EWs. More of the C and O fused to IMEs.