Improving the Low-Redshift Foundations: Results from the Lick Observatory Supernova Search (LOSS)
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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
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Previous ESSENCE Hubble Diagram
60 SNe Ia, 2002-2005
Wood-Vasey et al. (2007)
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Preliminary Current ESSENCE Hubble Diagram
156 SNe Ia, 2002-2007
Wood-Vasey et al. (2008, in prep.)
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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)
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Weidong Li
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SN 2001en
Cosmic ray
New image Template
Difference (after much processing)
Undergraduate students examine the SN candidates that were found automatically.
NGC 523
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LOSS SNe, m < 19 mag when discovered
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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
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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
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SN 1998dh(Type Ia)
Age:Age: -6 days
Maximum
+26 days
+47 days
+102 days
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Mohan Ganeshalingam
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Template subtraction; SN photometry
(Automatic pipeline)
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SN Ia
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SN II
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Preliminary results on SNe
Ia(Ganeshalingam et al. 2008, in prep.)
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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
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SNe Ia
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SNe Ia
(before correction)
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SNe Ia
(MLCS2k2)
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(KAIT + Jha et al. 2007)
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Bulk Flows from SN Ia (Riess et al. 1995, 1997)
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SN Ia 1998dh before/after
SN 1998de before/after
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(Leonard et al. 2005, ApJ, 632, 450)(Leonard et al. 2005, ApJ, 632, 450)
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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)
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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.
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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:
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JesseJesse Leaman
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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
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Units•1 SNu = 1 SN / (100 yr) / (1010 LSun)
(SNuB, SNuK for B and K bands)
•1 SNuM = 1 SN / (100 yr) / (1010 MSun)
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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)
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(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
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Katzman Automatic Imaging Telescope (KAIT)
(Laurie Hatch)