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Supernova Cosmology
Robert P. KirshnerEntering 7th decade
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Thank you!PH.D. STUDENTS
Peter N. Kupferman I've lost track-- he was at JPL. The Aerospace Corporation.
William P. Blair, Astrophysicist and Research Professor, Johns Hopkins University
Bradley C. Whitmore, Astronomer, Space Telescope Science Institute
Robert A. Fesen, Professor of Astronomy, Dartmouth College
Eliot Malumuth, Research Scientist, Goddard Space Flight Center
J. Ward Moody, Professor of Astronomy, Brigham Young University
Michael V. Newberry, software entrepreneur, Tucson, Arizona
Ronald Eastman, Lawrence Livermore National Laboratory (retired)
R. Chris Smith, Director, Cerro Tololo Inter-American Observatory
Brian P. Schmidt, Professorial Fellow, Australian National University
Jason Pun, Assistant Professor, Hong Kong Institute of Science and Technology
Adam G. Riess, Professor, Johns Hopkins & Space Telescope Science Institute
Huan Lin, Scientist, Experimental Astrophysics, Fermi National Accelerator Lab
Saurabh Jha, Assistant Professor, Rutgers University
Maryam Modjaz, Miller Fellow, University of California, Berkeley
Malcolm Hicken, McKinsey, Houston
Ashley Ruiter SAO Predoc Munich
Andy Friedman 2010
Kaisey Mandel 2010
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More!UNDERGRADUATES
Alicia Soderberg, Clay Fellow, CfA
Patrick Kelly grad student at Stanford Quincy House
Matt George Berkeley grad student Quincy House
Peter Williams Berkeley grad student Quincy House
Jenny Graves finishing Ph.D. at Santa Cruz Senior thesis
Kuenley Chu postdoc with Richard Ellis at Caltech A-35 Head TF
Nancy Levenson Associate Director, Gemini Observatory,Senior Thesis A-35
Jon Morse NASA Headquarters Senior thesis
Marc Kuchner NASA Goddard Senior thesis
OWN CATEGORY: Peter Challis, staff member HCO
POSTDOCS
Ian Wilson (lives in Australia-- I think he may teach at a high school)
Stuart Schurmann, (I have no idea where he is!)
Alan Uomoto (Carnegie)
Eric Schlegel (UT San Antonio),
Bruno Leibundgut (ESO),
David Jeffery (UNLV),
Pilar Ruiz-Lapuente (Barcelona),
Peter Hoelfich (Florida)
Peter Garnavich (Notre Dame)
Tom Matheson (NOAO)
Stephane Blondin (ESO)
Michael Wood-Vasey (Pittsburgh)
Ryan Foley, Clay Fellow (CfA)
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Fritz Zwicky at work
Courtesy of the Archives, California Institute of Technology
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Courtesy of the Archives,
California Institute of Technology
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Charlie Kowal
At work in theengine room
Note the imagingtechnology of 1968!
Photo courtesy Caltech Public Relations Archives
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Kowal (1968)
! Had distances good to~30% from SN I
Speculated that individualmeasurements might begood to 5-10%
“It may even be possible to
measure the second-orderterm in the redshift-magnitude relation whenlight curves becomeavailable for very distantsupernovae.”
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Bev Oke1928-2004
Photo courtesy
Caltech Public
Relations Archives
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Giant Electronic Cameras
100’s =>1000 Megapixels
Palomar Transit Factory
Photo courtesy Photo courtesy Mansi KasliwalMansi Kasliwal
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A gigapixel camera
to make your eyes light up!
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Brian Schmidt explains to his thesis advisorhow easy it is to subtract images
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Searching by Subtractionunskilled and therefore inexpensive labor
under careful supervision--computers!
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CfA Supernova Group(Also manufactured in
supernovae)
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Spectra
Similar at a given age, but notidentical
SNID: Blondin & Tonry (2007)
Fe seen at late times
Matheson et al. (2008)
787 spectra of 55 SN Ia in
http://www.cfa.harvard.edu/supernova/SNarchive.html
2211 spectra of 413 SN Ia --Blondin
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Multiband LightCurves for brightsupernovae
CfA1 Riess (22)CfA2 Jha (44)CfA3 Hicken (185)each ~world’stotal at the time
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Curiously, in 2008, the
biggest statistical error
in SN cosmology was
due to the small size of
the low-z sample!
This has now been
remedied by the CfA3
sample
Hicken et al. ApJ 700,
331 (2009) July 20
185 Type I Light Curves
Hicken et al. ApJ 700,
1097 (2009) August 1
Improved Dark Energy
Constraints
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Kowal (1968)
! Had distances good to~30% from SN I
!Speculated that individualmeasurements might begood to 5-10%
“It may even be possible to
measure the second-orderterm in the redshift-magnitude relation whenlight curves becomeavailable for very distantsupernovae.”
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Low Redshift and High
Low:
CfA3 (Hicken) +CfA2 (Jha) +
CfA1 (Riess) +Calan-Tololo
High:
ESSENCE
SNLS
Higher-Z
From the Union dataset (Kowalski 2008)
To the Constitution (amore perfect Union!)
Hicken (2009)
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Kowal (1968)
! Had distances good to~30% from SN I
!Speculated that individualmeasurements might begood to 5-10%
!“It may even be possible
to measure the second-order term in the redshift-magnitude relation whenlight curves becomeavailable for very distantsupernovae.”
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Pretty goodconcordance
SN orthogonal to CMB,good fit with baryonoscillation constraints
!DE = 0.72 +/- 0.02
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From Kowalski
astro-ph 0804.4142
Based on Low z:
Calan-Tololo + CfA
1 +CfA2 + SCP
ESSENCE + SNLS
+ Higher-Z
w = -0.94 +/-0.1
+/- 0.1 (sys)
Does not include
CfA3 (150 @ 0)
Sloan (300+ @ z=
0.1)
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Malcolm Hicken:squeezer of contours!
Where do we go from here?
Not much to be gained justfrom larger samples--needmore precisely measuredones, better selected
samples, and SN that are notaffected by dust! (Biggersamples to be sliced morefinely!)
Sloan-immanent
SNF
Carnegie- See Folatelli poster
PTF
Pan-STARRS
Also, need results thatdepend less on the light
curve fitter!
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Einstein &de Sitterbanish "
in 1931
Theydidn’t justset "=0
Theyexcluded
it fromtheirformalism!
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High-Z Team:
Riess et al. (1998)
Supernova
Cosmology Project:
Perlmutter et al.
(1999)
Einstein astonished!
But Lemaitre would
not have been. Hethought " might drive
the expansion Hubble
observed. His 1934
paper treats the
cosmological constant
as vacuum energy!
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Georges Lemaitre“The evolution of the world can be compared to
a display of fireworks that has just ended:
some few red wisps, ashes, and smoke.
Standing on a well-chilled cinder, we see the
slow fading of the suns, and we try to recall the
vanished brilliance of the origin of the worlds.”
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Georges Lemaitre“Everything happens as though the energy in
vacuo would be different from zero…weassociate a pressure p = -#c2 to the density of
energy #c2 of vacuum. This is essentially the
meaning of the cosmological constant $.”
PNAS 20, 12 (1934)
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" as the
source of
cosmicexpansion:DeSitter in
1930
Thanks to Jim Peebles
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Putting " on the Right
Hand Side
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The biggest uncertainties now are The biggest uncertainties now are systematicsystematicerrorserrors and the worst of these come from dust and the worst of these come from dust
(Conley et al. 2007; Sullivan talk)(Conley et al. 2007; Sullivan talk)
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Blank Presentation
Robert P. Kirshner
Theory by Dan Kasen (2006)- expect smallest variancein the IR: Pioneering work by Krisciunas & CTIO groupshows this is actually true!
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PAIRITEL (former 2MASS)
revived by Josh Bloom
(See Andy Friedman’s poster)
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J, H, Ks image from PAIRITEL
Make the measurements in the infrared!Make the measurements in the infrared!
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Michael Wood-
Vasey
Andy
Friedman
Wood-Vasey et
al. ApJ 689,
377 (2008)
NIR data only
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Next Step:
Better templates and BayeSNinference : Kaisey Mandel
ApJ (accepted) arxiv:0908.0536
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Life imitates art: facts mirror theory
H-band (1.6 microns) works best
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Training and Prediction
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Why not include IR + Optical?
Get better distances & learn aboutproperties of the dust by usingobservations over the range from B(0.4 µ) to K (2.2µ)
We want to know the ratio ofabsorption to color change (wemeasure colors but want to know
absorption)
Milky Way dust Rv = 3.1 =Av/ E(B-V),
but the hints are that SN dust is notthe same (Rv = 1.7 !)
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Dust properties for CfA3
(see Kaisey’s poster)
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The Payoff
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The Payoff
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PAIRITEL
Current sample ~40
Andy’s Thesis ~80-100
(See Andy’s poster)
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Only in space!Rest frame IR measurements of z~1 supernovae are not
possible from the ground (CSP was aiming at I-band, andthis was very difficult)
Go as far into the IR as technically feasible!Go as far into the IR as technically feasible!
Sky is very bright in NIR: >100x brighter than in space
Sky is not transparent in NIR: absorption due to water isvery strong and extremely variable
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JDEM
Joint Dark
Energy Mission
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ACRONYMAdvanced Cosmic Robotic Orbiting
New Year’s Mashup
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ACRONYMAAdvanceddvanced CCosmologicalosmological R Roboticobotic
OObjectbject
NNot ot YYet a et a MMissionission
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Z
W
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