2. 1885 -- 1949: 0-6 1950 -- 1980: 20 1980 -- 1990: 30 1991 -- 1996: 70 1997 -- 2000: 180 2001 -- 2003: 300 affordable CCD camera Commercial 14”--32” tel Computer + automation High-z SN search Reasons: SNe/year

3. Current active nearby SN searches LOSS 336 SNe (1998-2003) UC Berkeley SN factory  83 SNe (2002-2003) LBL Puckett 67 SNe (1998-2003) Amateur Boles 57 SNe (1997-2003) Amateur Armstrong 46 SNe (1998-2003) Amateur Evans 41 SNe (1981-2003) Amateur  Currently operation on hold

4. Scientific Goals of LOSS Monitor a well-defined galaxy sample Find lots of SNe and find them young Do photometric followups for many SNe Detailed log files for everyday observation GRB followup New

5. 30 inch (0.75 m) mirror Lick Observatory, Mt. Hamilton, near San Jose, CA Funded by NSF, the Sylvia & Jim Katzman Foundation, AutoScope Corp., Sun Microsystems, Hewlett- Packard Co., the University of California (Berkeley and Santa Cruz), and NASA.

6. 30 inch R-C telescope, f/8.2 Laser optical encoders Compact and light-weight Precise secondary maneuver 20 slot filter wheel Apogee AP7 camera, 6.8’ FOV, 0.8”/pix Off-axis guiding Automatic weatherstation TelescopeSecondaryCamerasWeatherstation Step motors Guider Apogee filterwheel

7. workstation HETE-2 pc1pc2pc3 GCN Berkeley Lick Obs. KAIT 90 miles Fully robotic obs Hardware control Obs schedule and control SN search schedule SN search image processing GRB response

8. Program to respond to GRB alerts promptly Interrupt KAIT and take a pre-arranged sequence of images Reaching 19 th mag within 60s of alerts Unfiltered obs  will use filters System Obs. Obs started at t=105s after burst 18 data points in the first 10 minutes One of the best early GRB light curves One of the few GRBs with reverse shock emission detected GRB 021211 GRB 020813 A mix of automatic and manually remote obs Slow early-time power-law decline index

12. (Li, Filippenko, Chornock, & Jha 2003)

13. Swift

14. 2.No. of images per night 20s  19 th mag 110 img/hr 700-1300 img/night Interval distribution t < 10 days (80%) Most SNe are discovered young!!! 1. No. of galaxies monitored: 19,000

15. 3. No. of SN discoveries Year LOSS SNe 1998 20 1999 40 2000 38 2001 68 2002 82 2003 95 95? Oh, No!

17. 10% -- 20% of the KAIT time ~40% of LOSS SNe: some photometry ~25% of LOSS SNe: good photometry Daily around max, every 2-7 days after max 196 SNe observed as of Nov 10,2003. Distribution of SN followup Some Good Great Total SN Ia 48 14 70 132 SN II 10 21 25 56 SN Ibc 1 1 6 8 Total: 196 Why not Ib/c?? 1. rare 2. tough When? We are working on them.

18. (SN Ia) Li et al. 2001

19. (SN II-P) Leonard et al. 2002

20. W. Li, A. V. Filippenko, E. Gates et al. 2001, PASP, 113, 1178 M. Modjaz, W. Li, A. V. Filippenko et al. 2001, PASP,113, 308 W. C. G. Ho, S. D. Van Dyk, C. Y. Peng et al. 2001, PASP, 113, 1349 W. Li, A. V. Filippenko, S. D. Van Dyk et al. 2002, PASP, 114, 403 W. Li, A. V. Filippenko, R. Chornock et al. 2003, PASP, 115, 453 A. G. Riess, A. V. Filippenko, W. Li et al. 1999, AJ, 118, 2675 W. Li, A. V. Filippenko, A. G. Riess et al. 2001, ApJ, 546, 719 W. Li, A. V. Filippenko, A. G. Riess et al. 2001, ApJ, 546, 734 T. Matheson, A. V. Filippenko, R. Chornock et al. 2000, AJ, 119, 2303 T. Matheson, A. V. Filippenko, W. Li et al. 2001, AJ, 121, 1648 R. Foley, M. Papenkova, B. Swift et al. 2003, PASP, 115, 1220 S. D. Van Dyk, C. Y. Peng, J. Y. King et al. 2000, PASP, 112, 1532 D. C. Leonard, A. V. Filippenko, W. Li et al. 2002, AJ, 124, 2490 D. C. Leonard, A. V. Filippenko, E. L. Gates et al. 2002, PASP, 114, 35 D. C. Leonard, A. V. Filippenko, R. Chornock, W. Li 2002, AJ, 124, 2506 S. D. Van Dyk, W. Li, A. V. Filippenko 2003, PASP, 115, 1289 S. van den Bergh, W. Li, A. V. Filippenko 2002, PASP, 114, 820 S. Van den Bergh, W. Li, A. V. Filippenko 2003, PASP, 115, 1280 SN Ia photometry SN Ia statistics SN Ib/c SN II SN rates GRB W. Li, A. V. Filippenko, R. Chornock, S. Jha 2003, ApJ, 586, L9 W. Li, A. V. Filippenko, R. chornock, S. Jha 2003, PASP, 115, 844

21. 1.A stable nearby SN search engine 2.In collaboration with CfA, CSP: more followup 3.Publish existing photometry database: SNe Ia: correlation, H0, local flow SNe II : correlation, EPM SNe Ibc: correlation, SN/GRB connection 4.SN rate, statistics 5.GRB followup in the Swift era

22. KAIT is conducting the world’s most successful search for very nearby SNe, and has yielded interesting results on the statistics and photometric properties of SNe and GRB optical afterglows. We have shown that good science can be done with a small telescope when correctly engineered and programmed.