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The Lick Observatory Supernova Search (LOSS) and Follow-up Program

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. KAIT,.

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The Lick Observatory Supernova Search (LOSS) and Follow-up Program

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  1. 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.)

  2. Caprielle Corona Nikole Filippenko

  3. 03W-01a, total eclipse

  4. KAIT, 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

  5. Weidong Li (UCB)

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

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

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

  9. KAIT Supernova Search & Analysis Team, May 2005

  10. LOSS SNe, m < 19 mag at time of discovery • Year N(SN) • 1998 20 • 40 • 38 • 68 • 82 • 95 • 83 • 82 Total nearby SNe, m < 19 mag LOSS SNe http://astron.berkeley.edu/~bait/kait.html

  11. 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.

  12. Supernova rate (Leaman, Li, AF 2006) Gal. Type N(gal) Ia Ib/c II 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 Total: 566 SNe in 13,000 galaxies Previous: 137 SNe in 4,000 galaxies (5 combined searches: visual & photographic) Cappellaro et al. 1999

  13. Jesse Leaman Jesse

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

  15. 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 KAIT Lick 1-m Lick 3-m Keck I/II 10-m 10-20% of time Photometry calibration 2-3 nights/mon Calibration photometry 3 nights/mon spectroscopy Occasional spectroscopy

  16. Filtered photometry database Some Good Great Total SN Ia59 2195 175 SN II27 2431 82 SN Ibc4 512 21 Total: 278 (As of Dec 19, 2005)

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

  18. Mohan Ganeshalingam

  19. Sample light curves from LOSS photometry pipeline (1)

  20. Sample light curves from LOSS photometry pipeline (2)

  21. KAIT GRB Program • 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 19th mag within 60 s of alerts. • Unfiltered obs.; now V, I, unfiltered.

  22. GRB 020211 KAIT2

  23. GRB 021212 KAIT3

  24. (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

  25. Nearby SNe Ia: Physics and progenitors High-quality data for modeling 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 Li et al. 2006 inprep (Jha et al. 2006, in press) I 2002cx R V B Also observed by HST, Swift U

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

  27. 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

  28. 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

  29. MLCS2k2 light curve fits KAIT BVRI photometry Si μ = 33.46 ± 0.07 mag μ = 33.49 ± 0.10 mag SN 1999cp and SN 2002cr, both in NGC 5468

  30. Correcting for Intrinsic Variations and Dust Si

  31. Going with the Flows (Jha et al. 2006)

  32. Nearby SNe Ia: Anchor for Hubble diagram

  33. 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)

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

  35. 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!

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

  37. SN II-P

  38. Polarization of SN 2004dj

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

  40. 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!

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

  42. 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.

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