The Lick Observatory Supernova Search (LOSS) and Follow-up ProgramAlex FilippenkoDepartment of AstronomyUniversity 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)

No. of images per night 7001300 images/night3. Interval distribution1. No. of galaxies monitored:14,000 7,500 (06/2004)Observation interval (days)Number of observations20012003After Jun 2004

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

SN 2001enCosmic rayNew imageTemplateDifference (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 discoveryYear N(SN)

1998 20 40 38 68 82 95 83 82Total nearby SNe, m < 19 magLOSS SNehttp://astron.berkeley.edu/~bait/kait.html

755 SNe in the galaxies monitored by LOSS during 1998-2005.508 (67%) discovered by LOSS.716 have SN type and host-galaxy redshift.Can study rates, systematics, etc.

Supernova rate (Leaman, Li, AF 2006) E 1049 30 0 0 S0 2566 17 2 9 Sa 962 13 6 15 Sab 728 14 5 15 Sb 1777 47 15 53 Sbc 1237 21 20 36 Sc 1771 32 28 61 Ir 2618 10 7 13 Gal. Type IaIb/cII N(gal)Total: 566 SNe in 13,000 galaxiesPrevious: 137 SNe in 4,000 galaxies(5 combined searches: visual & photographic) Cappellaro et al. 1999

JesseJesse Leaman

All SNe (716)Luminosity function of SNeDiscovery mag; peak mag from light curveMonte Carlo completeness simulation of our searchWe 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 observersPrompt alerts to 70 astronomers/SN observersCarnegie Supernova Program (CSP), CfA group, Caltech Core-Collapse Program (CCCP), CTIO group, ESO group, etc.Follow-up with our own telescopes10-20% of time Photometry calibration2-3 nights/mon Calibration photometry3 nights/monspectroscopyOccasionalspectroscopyKAITLick 1-mLick 3-mKeck I/II 10-m

Filtered photometry databaseSome Good Great TotalSN Ia 59 21 95 175SN II 27 24 31 82SN Ibc 4 5 12 21Total: 278(As of Dec 19, 2005)

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

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 KAITs normal observations; take a pre-arranged sequence of images. Reach 19th mag within 60 s of alerts. Unfiltered obs.; now V, I, unfiltered.

GRB 020211 KAIT2

GRB 021212 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. 2006 in prepUBVRIHigh-quality data for modelingAlso observedby HST, Swift SN subclasses/statistics: progenitors91T-like: only in spiral galaxies91bg-like: prefer E galaxiesNormal: in all kinds of galaxiesPeculiar/bizarre SNe Ia (Jha et al. 2006, in press)2002cx

SN 2002cx-like: a new subclass of SN Iabut we really dont know what produces them!

Nearby SNe Ia: Cepheid distancesSN 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

SiCorrecting for Intrinsic Variations and Dustshape 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

SiMLCS2k2 light curve fitsSN 1999cp and SN 2002cr, both in NGC 5468 = 33.46 0.07 mag = 33.49 0.10 mag KAIT BVRI photometry

SiCorrecting 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 yearsstatistical signifcance is 3,but robust with subsamples, other distance techniquesJha, Riess, & Kirshner (2006)

a real local void?K-corrections?photometric offset?new data vs. Caln/Tololo?morphology/extinction?Jha, Riess, & Kirshner (2006)a potentially huge systematic test with more nearby objects!A Hubble Bubble?

Systematic EffectsThese 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, demographicsThe 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 SNeThe 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 IaAll are intrinsically polarized.Continuum pol.: suggests minor-to-major axis ratio of ~0.9 if viewed equator-on (Hflich 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.

AF-03W-01a (Credit: Jay Pasachoff)weidong.jpgLoss in numbersAF-03W-138-r (rotated 90 deg).May 6, 2005 group photo of KAIT SN searchers (but some missing: Katsuki, Harish Khandrika, Brian Beutler (gone?), Matthew Moore; new ones like Prakash? And one other -- look up)Mohan Ganeshalingam, Brandon Swift, Sung Park, Jayme Burkett, Nick Ponticello (new), John Graham, Harrison Pugh (Berkeley High School student).SN ratesSN followup statistics09/24/04 UT Lick Research trip -- Brandon Swift and Mohan GaneshalingamAF-03W-121AF-03W-122.

These objects have different Delta and extinction!!

after correcting for expansion

still some surprises in the nearby sample...a local void? or indications of systematic error?strong implications for distant objects

Zehavi et al 1998 found a void signature (but they used omega_m=1 cosmology which enhanced significance)6 +/- 2 percent difference in H0 within and beyond 7500 km/smakes a huge difference in precision cosmologyreal (but not confirmed in TF or FP distances, and would be unexpectedly large in LSS)photometric offset (confirmed in Jose Luis distances with updated dm15)