Improving the Low-Redshift Foundations: Results from the Lick Observatory Supernova

Search (LOSS)

Alex FilippenkoDepartment of AstronomyUniversity of California, Berkeley

(Main collaborators: W. Li, J. Leaman, M. Ganeshalingam)

May 7, 2008

Previous ESSENCE Hubble Diagram

60 SNe Ia, 2002-2005

Wood-Vasey et al. (2007)

Preliminary Current ESSENCE Hubble Diagram

156 SNe Ia, 2002-2007

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

2001 - 2007, 1.5 million obs

LOSS Cadence: 2-12 days

Observation interval (days)

No

of

obs

a. 200 gal: every 2 daysb. 5,000 gal: every 5 daysc. 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

Occasionalspectroscopy

KAIT Lick 1-m Lick 3-m Keck I/II 10-m

SN 1998dh(Type Ia)

Age: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.)

AV (mag)

2.0

1.5

1.0

0.5

0.0

2.0

1.0

0.0

-1.0

Hubble type, E Sd/Irr

SNe Ia

SNe Ia

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

Chornock et al. 2006

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)

Vphot=5000 km/sec

SN 2005hk (Chornock et al. 2006)

CSP Observations of SN 2005hk (Phillips)

H

J

• No secondary maximum in IR.

• Strength of the secondary maximum correlated with the amount of mixing of 56Ni in the ejecta (Kasen 2006).

• The absence of secondary maximum suggests complete mixing of 56Ni.

Supernova RatesSupernova Rates

Cappellaro et al. 1999 (C99 hereafter)*5 surveys (1 visual, 4 photographic plates)*137 SNe in about 104 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. 2005 (M05 hereafter)•Same database as C99•K-band luminosity normalization•SNr versus galaxy color (B-K)

Benchmark for z = 0 SN rate:

JesseJesse Leaman

LOSS SN rates (1998-LOSS SN rates (1998-2006): 2006): Leaman, Li, & AVF (2008, Leaman, Li, & AVF (2008,

in prep.)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 | ? | TotalB 247 97 284 14 642K 235 93 274 13 615 B&K 227 87 265 12 591*Only SNe for which we have all host-galaxy information were included

Units•1 SNu = 1 SN / (100 yr) / (1010 LSun)

(SNuB, SNuK for B and K bands)

•1 SNuM = 1 SN / (100 yr) / (1010 MSun)

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)