Determining the Nature of Dark Energy: The Latest Results from ESSENCE and the Future of Observational Cosmology Michael Wood-Vasey Harvard-Smithsonian Center for Astrophysics 2008 February 26 LCOGT/KITP
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Determining the Nature of Dark Energy:
The Latest Results from ESSENCE and the
Future of Observational Cosmology
Michael Wood-VaseyHarvard-Smithsonian Center for Astrophysics
2008 February 26LCOGT/KITP
Baryons4%
Dark Energy73%
Dark Matter23%
c.f. Astier06, Spergel06, Eisenstein05, Perlmutter99, Riess98
Arable Land3%
Ocean70%
Other Land27%
Food and Agriculture Organization of the United Nations
What is Dark Energy?
Courtesy of David Weinberg
Three philosophically distinct possibilities...
A “classical” cosmological constant, as envisioned by Einstein, residing in the gravitational sector.
A “Vacuum energy” effect, arising from quantum fluctuations in the vacuum, acting as a “source” term
Departure from GR on cosmological length scales
Regardless, it’s evidence of new fundamental physics!
The Basic Question:
Is a cosmological constant model consistent with our observations of
the Universe?
The ESSENCE Survey Determine w to 10% or w!=-1
6-year project on CTIO 4m telescope in Chile; 12 sq. deg.
Wide-field images in 2 bands
Same-night detection of SNe
Spectroscopy
Keck, VLT, Gemini, Magellan
Goal is 200 SNeIa, 0.2<z<0.8
Data and SNeIa public real-time
ESSENCE Survey TeamClaudio Aguilera CTIO/NOAO Bruno Leibundgut ESO
Andy Becker Univ. of Washington Weidong Li UC Berkeley
Josh Blackman ANU/Stromlo/SSO Thomas Matheson NOAO
Stéphane Blondin Harvard/CfA Gajus Miknaitis Fermilab
Peter Challis Harvard/CfA Gautham Narayan Harvard University
Ryan Foley UC Berkeley Jose Prieto OSU
Alejandro Clocchiatti Univ. Católica de Chile Armin Rest NOAO/CTIO
Ricardo Covarrubias Univ. of Washington Adam Riess STScI/JHU
Tamara Davis Dark Cosmology Center Brian Schmidt ANU/Stromlo/SSO
Alex Filippenko UC Berkeley Chris Smith CTIO/NOAO
Arti Garg Harvard University Jesper Sollerman Stockholm Obs.
Peter Garnavich Notre Dame University Jason Spyromilio ESO
Malcolm Hicken Harvard University Christopher Stubbs Harvard University
Saurabh Jha SLAC/KIPAC Nicholas Suntzeff Texas A&M
Robert Kirshner Harvard/CfA John Tonry Univ. of Hawaii/IfA
Kevin Krisciunas Texas A&M Michael Wood-Vasey Harvard/CfA
R
I
Reference New Difference
2005 2006 Sep Oct
Nov Dec
Time
ESSENCE Spectra
Matheson et al. (2005)
One-parameter family
(Supernova Cosmology Project, Kim et al)
Color
Rate of decline
Peak brightness
One-parameter family
(Supernova Cosmology Project, Kim et al)
Color
Rate of decline
Peak brightness
σ ~ 0.13 mag
Apparent Brightness
z=0.48
−1.0 −0.5 0.0 0.5 1.0color
0
20
40
60
#/0.
10 b
in
nearbyESSENCE
SNLS
−1.0 −0.5 0.0 0.5 1.0color
0
20
40
60
#/0.
10 b
in
nearbyESSENCE
SNLS
SALT2 (Guy07)
All good nearby SNeIa Only z>0.015
−3 −2 −1 0 1 2 3 AV
0
20
40
60
#/0.
30 b
in
nearbyESSENCE
SNLSprior
−3 −2 −1 0 1 2 3 AV
0
20
40
60
#/0.
30 b
in
nearbyESSENCE
SNLSprior
MLCS2k2 (Jha07) flatnegav
Only z>0.015All good nearby SNeIa
−1.0 −0.5 0.0 0.5 1.0color
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
SNLSESSENCEnearby
−1.0 −0.5 0.0 0.5 1.0 color
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
SNLSESSENCEnearby
SALT2, beta=0
Luminosity vs. Color
All good nearby SNeIa
SALT2, beta=1.77 (Guy07)
−1.0 −0.5 0.0 0.5 1.0 color
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
SNLSESSENCEnearby
−1.0 −0.5 0.0 0.5 1.0color
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
SNLSESSENCEnearby
Corrected Luminosity vs. Color
−3 −2 −1 0 1 2 3 AV
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
nearbyESSENCE
SNLS
−3 −2 −1 0 1 2 3 AV
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
nearbyESSENCE
SNLS
Anti-Corrected Luminosity vs. Color
MLCS2k2 flatnegavbeta=0, R_V=3.1
−3 −2 −1 0 1 2 3 AV
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
nearbyESSENCE
SNLS
MLCS2k2 flatnegavbeta=-0.9, R_V=3.1
−3 −2 −1 0 1 2 3 AV
−3
−2
−1
0
1
2
3
Δµ
[m
ag]
nearbyESSENCE
SNLS
Corrected Luminosity vs. Color
ESSENCE Hubble Diagram
0.01 0.10 1.0034363840424446
µ
(ΩM, ΩΛ) = (0.27, 0.73)(ΩM, ΩΛ) = (0.3, 0.0)(ΩM, ΩΛ) = (1.0, 0.0)
0.01 0.10 1.00Redshift
−1.5−1.0
−0.5
0.0
0.5
1.01.5
Δµ
ESSENCEnearby
Wood-Vasey et al., 2007, ApJ, 666, 694
see alsoMiknaitis et al.,
2007, ApJ, 666, 674
Davis et al.,2007, ApJ, 666, 716
0.0 0.2 0.4 0.6 0.8 1.0ΩM
-2.0
-1.5
-1.0
-0.5
0.0w
SNeIaBAO
SNeIa+BAO
w=-1.05 +- 0.11 +- 0.13
ESSENCE
Flat,constant-w
578 PERLMUTTER ET AL. Vol. 517
FIG. 7.ÈBest-!t con!dence regions in the plane for our primary)M
-)"analysis, !t C. The 68%, 90%, 95%, and 99% statistical con!dence regionsin the plane are shown, after integrating the four-dimensional !t)
MÈ)"over and a. (See footnote 11 for a link to the table of this two-M
Bdimensional probability distribution.) See Fig. 5e for limits on the smallshifts in these contours due to identi!ed systematic uncertainties. Note thatthe spatial curvature of the universeÈopen, Ñat, or closedÈis not determi-native of the future of the universeÏs expansion, indicated by the near-horizontal solid line. In cosmologies above this near-horizontal line theuniverse will expand forever, while below this line the expansion of theuniverse will eventually come to a halt and recollapse. This line is not quitehorizontal, because at very high mass density there is a region where themass density can bring the expansion to a halt before the scale of theuniverse is big enough that the mass density is dilute with respect to thecosmological constant energy density. The upper-left shaded region,labeled ““ no big bang,ÏÏ represents ““ bouncing universe ÏÏ cosmologies withno big bang in the past (see Carroll et al. 1992). The lower right shadedregion corresponds to a universe that is younger than the oldest heavyelements (Schramm 1990) for any value of km s~1 Mpc~1.H0 º 50
on that day : the distribution, abundances, excitations, andvelocities of the elements that the photons encounter as theyleave the expanding photosphere all imprint on the spectra.So far, the high-redshift supernovae that have been studiedhave light-curve shapes just like those of low-redshift super-novae (see Goldhaber et al. 1999), and their spectra showthe same features on the same day of the light curve as theirlow-redshift counterparts having comparable light-curvewidth. This is true all the way out to the z \ 0.83 limit of thecurrent sample (Perlmutter et al. 1998b). We take this as astrong indication that the physical parameters of the super-nova explosions are not evolving signi!cantly over this timespan.
Theoretically, evolutionary e†ects might be caused bychanges in progenitor populations or environments. For
example, lower metallicity and more massive SN Ia-progenitor binary systems should be found in youngerstellar populations. For the redshifts that we are consider-ing, z \ 0.85, the change in average progenitor masses maybe small (Ruiz-Lapuente, Canal, & Burkert 1997 ; Ruiz-Lapuente 1998). However, such progenitor mass di†erencesor di†erences in typical progenitor metallicity are expectedto lead to di†erences in the !nal C/O ratio in the explodingwhite dwarf and hence a†ect the energetics of the explosion.The primary concern here would be if this changed thezero-point of the width-luminosity relation. We can look forsuch changes by comparing light curve rise times betweenlow- and high-redshift supernova samples, since this is asensitive indicator of explosion energetics. Preliminary indi-cations suggest that no signi!cant rise-time change is seen,with an upper limit of day for our sample (see forth-[1coming high-redshift studies of Goldhaber et al. 1999 andNugent et al. 1998 and low-redshift bounds from Vacca &Leibundgut 1996, Leibundgut et al. 1996b, and Marvin &Perlmutter 1989). This tight a constraint on rise-timechange would theoretically limit the zero-point change toless than D0.1 mag (see Nugent et al. 1995 ; Ho" Ñich,Wheeler, & Thielemann 1998).
A change in typical C/O ratio can also a†ect the ignitiondensity of the explosion and the propagation characteristicsof the burning front. Such changes would be expected toappear as di†erences in light-curve timescales before andafter maximum & Khokhlov 1996). Preliminary(Ho" Ñichindications of consistency between such low- and high-redshift light-curve timescales suggest that this is probablynot a major e†ect for our supernova samples (Goldhaber etal. 1999).
Changes in typical progenitor metallicity should alsodirectly cause some di†erences in SN Ia spectral features
et al. 1998). Spectral di†erences big enough to(Ho" Ñicha†ect the B- and V -band light curves (see, e.g., the extrememixing models presented in Fig. 9 of et al. 1998)Ho" Ñichshould be clearly visible for the best signal-to-noise ratiospectra we have obtained for our distant supernovae, yetthey are not seen (Filippenko et al. 1998 ; Hook et al. 1998).The consistency of slopes in the light-curve width-luminosity relation for the low- and high-redshift super-novae can also constrain the possibility of a strongmetallicity e†ect of the type that et al. (1998)Ho" Ñichdescribes.
An additional concern might be that even small changesin spectral features with metallicity could in turn a†ect thecalculations of K-corrections and reddening corrections.This e†ect, too, is very small, less than 0.01 mag, for photo-metric observations of SNe Ia conducted in the rest-frame Bor V bands (see Figs. 8 and 10 of et al. 1998), as isHo" Ñichthe case for almost all of our supernovae. (Only two of oursupernovae have primary observations that are sensitive tothe rest-frame U band, where the magnitude can change byD0.05 mag, and these are the two supernovae with thelowest weights in our !ts, as shown by the error bars of Fig.2. In general the I-band observations, which are mostlysensitive to the rest-frame B band, provide the primary lightcurve at redshifts above 0.7.)
The above analyses constrain only the e†ect ofprogenitor-environment evolution on SN Ia intrinsic lumi-nosity ; however, the extinction of the supernova light couldalso be a†ected, if the amount or character of the dustevolves, e.g., with host galaxy age. In ° 4.1, we limited the
Perlmutter et al. (1999, ApJ)Riess et al. (1998, AJ)0.0 0.5 1.0 1.5 2.0 2.5
!M
-1
0
1
2
3!
"
68.3
%95
.4%
95.4%
99.7
%
99.7
%
99.7
%No
Big B
ang
!tot =1
Expands to Infinity
Recollapses !"=0
Open
Closed
Accelerating
Decelerating
q0=0
q0=-0.5
q0=0.5
^
MLCS
0.0 0.5 1.0 1.5 2.0 2.5
!M
-1
0
1
2
3
!"
68.3%
95.4
%
95.4%
99.7
%
99.7
%
99.7
%No
Big B
ang
!tot =1
Expands to Infinity
Recollapses !"=0
Open
Closed
Accelerating
Decelerating
q0=0
q0=-0.5
q0=0.5
^
#m15(B)
No. 3, 1998 EVIDENCE FOR AN ACCELERATING UNIVERSE 1023
FIG. 6.ÈJoint con!dence intervals for from SNe Ia. The solid()M
, )")contours are results from the MLCS method applied to well-observed SNeIa light curves together with the snapshot method et al.(Riess 1998b)applied to incomplete SNe Ia light curves. The dotted contours are for thesame objects excluding the unclassi!ed SN 1997ck (z \ 0.97). Regions rep-resenting speci!c cosmological scenarios are illustrated. Contours areclosed by their intersection with the line )
M\ 0.
The normalized PDF comes from dividing this relativePDF by its sum over all possible states,
p(H0, )m, )" o l0)
\ exp ([s2/2)/~== dH0 /~== d)" /0= exp ([s2/2)d)
M, (10)
neglecting the unphysical regions. The most likely values forthe cosmological parameters and preferred regions ofparameter space are located where is mini-equation (4)mized or, alternately, is maximized.equation (10)
The Hubble constants as derived from the MLCSmethod, 65.2 ^ 1.3 km s~1 Mpc~1, and from the template-!tting approach, 63.8 ^ 1.3 km s~1 Mpc~1, are extremelyrobust and attest to the consistency of the methods. Thesedeterminations include only the statistical component oferror resulting from the point-to-point variance of the mea-sured Hubble Ñow and do not include any uncertainty inthe absolute magnitude of SN Ia. From three photoelec-trically observed SNe Ia, SN 1972E, SN 1981B, and SN1990N (Saha et al. the SN Ia absolute magni-1994, 1997),tude was calibrated from observations of Cepheids in thehost galaxies. The calibration of the SN Ia magnitude fromonly three objects adds an additional 5% uncertainty to theHubble constant, independent of the uncertainty in the zeropoint of the distance scale. The uncertainty in the Cepheid
distance scale adds an uncertainty of D10% to the derivedHubble constant & Walker(Feast 1987 ; Kochanek 1997 ;
& Freedman A realistic determination of theMadore 1998).Hubble constant from SNe Ia would give 65 ^ 7 km s~1Mpc~1, with the uncertainty dominated by the systematicuncertainties in the calibration of the SN Ia absolute magni-tude. These determinations of the Hubble constant employthe Cepheid distance scale of & FreedmanMadore (1991),which uses a distance modulus to the Large MagellanicCloud (LMC) of 18.50 mag. Parallax measurements by theHipparcos satellite indicate that the LMC distance could begreater, and hence our inferred Hubble constant smaller, by5% to 10% though not all agree with the inter-(Reid 1997),pretation of these parallaxes & Freedman(Madore 1998).All subsequent indications in this paper for the cosmo-logical parameters and are independent of the value)
M)"for the Hubble constant or the calibration of the SN Ia
absolute magnitude.Indications for and independent from can be)
M)", H0,
found by reducing our three-dimensional PDF to twodimensions. A joint con!dence region for and is)
M)"derived from our three-dimensional likelihood space
p()M
, )" o l0) \P~=
=p()
M, )", H0 o l0)dH0 . (11)
FIG. 7.ÈJoint con!dence intervals for from SNe Ia. The solid()M
, )")contours are results from the template-!tting method applied to well-observed SNe Ia light curves together with the snapshot method et(Riessal. applied to incomplete SNe Ia light curves. The dotted contours1998b)are for the same objects excluding the unclassi!ed SN 1997ck (z \ 0.97).Regions representing speci!c cosmological scenarios are illustrated. Con-tours are closed by their intersection with the line )
M\ 0.
0.0 0.5 1.0 1.5 2.0!M
0.0
0.5
1.0
1.5
2.0!
"ESSENCE+SNLS+gold
(!M,!") = (0.27,0.73)!Total=1
SNe Ia alone require >0
at 99.995% conf.
What To Do?
Think carefully
Different samples
Different splits of color vs. extinction
Understand dust in other galaxies
Understand any evolution of dust vs. redshift
ESSENCE SNeIa From All 6 Years
~200 SNeIa2007
2002
2006
2003
2004
2005
Previous ESSENCE Hubble Diagram
0.2 0.4 0.6 0.8 1.0 1.2Redshift
14
16
18
20
22
24
26 µ
(mag
)
(ΩM, ΩΛ) = (1.0, 0.0)(ΩM, ΩΛ) = (0.3, 0.0)
(ΩM, ΩΛ) = (0.27, 0.73)
nearbyESSENCESNLS
0.2 0.4 0.6 0.8 1.0 1.2Redshift
14
16
18
20
22
24
26 µ
(mag
)
(ΩM, ΩΛ) = (1.0, 0.0)(ΩM, ΩΛ) = (0.3, 0.0)
(ΩM, ΩΛ) = (0.27, 0.73)
nearbyESSENCESNLS
Preliminary Current ESSENCE Hubble Diagram
Summary & Future The State of LCDM is Strong
Tackle Extinction vs. Intrinsic Color
UV - Optical - NIR data
More nearby SNeIa: +300 from KAIT, CSP, CfA
SDSS-II, ESSENCE, SNLS joint analysis
Pan-STARRS1, Dark Energy Survey, LSST
JDEM with supernovae
ESSENCE Status Summary
Flat Universe model with a cosmological constant works fine.
w=-1.05 +- 0.11 (stat) +- 0.13 (sys)
Final ESSENCE results: due in 2008
Double sample
Improve systematics
Reach goal: w to 10%
Future of Probing the Nature of Dark Energy
SN cosmology tests
Gravitational lensing
Galaxy cluster abundances
Baryon oscillations
Particle physics experiments
Tests of gravity on all scales
signal!
Pan-STARRS
7 square degree field
1.8m effective aperture
24th magnitude in 300 sec
1 TB / night
Real-time analysis
Will find 10,000s of SNe!
Lensing shear map
Panoramic Survey Telescope & Rapid Response System
http://pan-starrs.ifa.hawaii.edu/
Medium-Deep SurveyPS1 PSDC-230-002-00
Figure 3: Celesitial sphere in Mercator projection showing extinction map from WMAP. The proposed Medium Deep
Fields are marked as black boxes, the white circle is one of the stellar transit fields, and the white square is M31. The
black line at -30 degrees Declination shows the southern limit of the PS1 Steradian Survey pointing centers.
Figure 4: Left: Outside view of the celestial sky tesselated into 6252 fields. Of these fields, 5464 have boresight centers
degrees Declination. Center, the 3 degree field of view of PS1 with an inscribed hexagon of 5.84 square degrees.
Right, the twenty percent overlap from a single tesselation due to the circular field of view.
PS1 MCS 12 September 25, 2006
Medium-Deep SurveyPS1 PSDC-230-002-00
Figure 3: Celesitial sphere in Mercator projection showing extinction map from WMAP. The proposed Medium Deep
Fields are marked as black boxes, the white circle is one of the stellar transit fields, and the white square is M31. The
black line at -30 degrees Declination shows the southern limit of the PS1 Steradian Survey pointing centers.
Figure 4: Left: Outside view of the celestial sky tesselated into 6252 fields. Of these fields, 5464 have boresight centers
degrees Declination. Center, the 3 degree field of view of PS1 with an inscribed hexagon of 5.84 square degrees.
Right, the twenty percent overlap from a single tesselation due to the circular field of view.
PS1 MCS 12 September 25, 2006
LSST
10 square degree field
6.5m effective aperture
24th magnitude in 20 sec
20 TB / night
Real-time analysis
Will find millions of SNe!
Lensing, BAO, Clusters
Large Synoptic Survey Telescope
Strongly Lensed SNeIa
100,000s of high-z SNeIa 0.1-1% should be strongly lensed
Multiply-imaged SNeIa time-delay with known magnification Measure H0
improve complementary cosmological constraints
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LSST Supernova LSST Supernova
CosmologyCosmologyL. Wang (LBNL), P. Pinto (U Arizona), H. Zhan (UC Davis)
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precision probes – Type Ia SNe, BAO, and weak lensing –
LSST will be a powerful tool for studying the properties of
dark energy and its evolution.
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In its normal survey mode, LSST will discover more than 280,000 Type Ia supernovae (SNe Ia) per year across the visible sky to a redshift of ~0.8. With a deep, pointed search in three 10-deg2
fields, it will discover and closely monitor 30,000 SNe annually to a redshift of z ~1.2. Using these SNe for cosmology will rely upon spectroscopic follow-up capabilities and upon novel methods
of deducing photometric redshifts from multi-band supernova light curves. This poster provides a sample of how LSST SNe Ia will be used as cosmological probes. A primary goal will be to
detect systematics affecting the supernova cosmology program and, at the same time, to constrain cosmological parameters. This will be feasible because LSST's extremely large sample size
allows for multiple parameter fits which can self-calibrate systematics in ways not accessible to current surveys. The systematic relations deduced from these SNe will be helpful for current and
future space-based projects targeting SNe at even higher redshifts. Such large samples will also enable discoveries of SNe Ia affected by foreground gravitational lensing. We explore the use of
LSST's SNe in constraining the behavior of dark energy and show how their combination with baryonic oscillation investigations will make LSST a particularly powerful experiment to this end.
Finally, we show how the distribution of so many well-observed SNe across the sky will constrain the angular variation of cosmological parameters.
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Oguri & Kawano (2003, MNRAS)
LSST Opens up the Skies
Data will be immediately publicly available
Allow all colleges and institutions to do research with big telescopes
Will change the nature of research
LSST Dark Energy
Supernovae
Weak Lensing
Baryon Oscillations
Galaxy Clusters
LSST & Supernovae LSST will find millions of supernovae
Hundreds of thousands well-studied z < 1.2
Tens of thousands z < 0.3
Opportunity for SN science on a new level
Cosmology and Dark Energy
Supernovae qua supernovae
SNe trace structure
Rates: star-formation, galaxy environments
New brilliant ideas . . .
0.0 0.2 0.4 0.6 0.8 1.0ΩM
-2.0
-1.5
-1.0
-0.5
0.0w
SNeIaBAO
SNeIa+BAO
w=-1.05 +- 0.11 +- 0.13
ESSENCE
Flat,constant-w
0.0 0.2 0.4 0.6 0.8 1.0ΩM
-2.0
-1.5
-1.0
-0.5
0.0w
SNeIaBAO
SNeIa+BAO
w=-1.05 +- 0.11 +- 0.13
ESSENCE
Flat,constant-w
LSST SN Ia (M, w)
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LSST Supernova LSST Supernova
CosmologyCosmologyL. Wang (LBNL), P. Pinto (U Arizona), H. Zhan (UC Davis)
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precision probes – Type Ia SNe, BAO, and weak lensing –
LSST will be a powerful tool for studying the properties of
dark energy and its evolution.
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In its normal survey mode, LSST will discover more than 280,000 Type Ia supernovae (SNe Ia) per year across the visible sky to a redshift of ~0.8. With a deep, pointed search in three 10-deg2
fields, it will discover and closely monitor 30,000 SNe annually to a redshift of z ~1.2. Using these SNe for cosmology will rely upon spectroscopic follow-up capabilities and upon novel methods
of deducing photometric redshifts from multi-band supernova light curves. This poster provides a sample of how LSST SNe Ia will be used as cosmological probes. A primary goal will be to
detect systematics affecting the supernova cosmology program and, at the same time, to constrain cosmological parameters. This will be feasible because LSST's extremely large sample size
allows for multiple parameter fits which can self-calibrate systematics in ways not accessible to current surveys. The systematic relations deduced from these SNe will be helpful for current and
future space-based projects targeting SNe at even higher redshifts. Such large samples will also enable discoveries of SNe Ia affected by foreground gravitational lensing. We explore the use of
LSST's SNe in constraining the behavior of dark energy and show how their combination with baryonic oscillation investigations will make LSST a particularly powerful experiment to this end.
Finally, we show how the distribution of so many well-observed SNe across the sky will constrain the angular variation of cosmological parameters.
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Future of Cosmology Luminosity Distance
SNeIa: SNAP; PanSTARRS, LSST GRBs?
Angular Diameter Distance Large Scale Structure
Baryon Acoustic Oscillations Lensing/Shear
Cosmic Microwave Background Planck
Gravity LIGO, LISA
Summary
The accelerating Universe poses a significant challenge to theory, experiment and observation.
The current data are consistent with a “simple” w = − 1, = 1
Upcoming projects have great potentialto yield new insights into dark energy
MDS survey
SN Ia Colors It’s been hard to disentangle intrinsic SN Ia colors
from reddening due to dust
Do SNeIa have an intrinsic color-luminosity relationship?
MV = c E(B-V)
Dust extinction has the equivalent through RV
MV = AV = RV E(B-V)
SNeIa in NIR
SNeIa are more standard in near infrared
Krisciunas seminal work 2000-2004 w/ 17 SNeIa
Recent confirmation: Wood-Vasey 2007
New homogeneous sample from PAIRITEL
Doubled sample of SNeIa
PAIRITEL: SN 2006D
SN 2006DSN 2006D
30”30”
NE
S 3S 3
S 1S 1
S 2S 2
12
14
16
18
20
mH
PAIRITEL SNeIaliterature SNeIa
(!M, !L, h0) = (0.23, 0.77, 0.72)MH = -19.19
1000 10000Velocity [km/s; CMB+Virgo]
-1.0
-0.5
0.0
0.5
1.0
mH -
(MH+µ"
CDM)
RMS = 0.41 #2
$ = 1.56
%z = 150 km/s , %µ = 0.10 mag
Optical Hubble Diagram
H-band Hubble Diagram
12
14
16
18
20
mH
PAIRITEL SNeIaliterature SNeIa
(!M, !L, h0) = (0.23, 0.77, 0.72)MH = -17.98
1000 10000Velocity [km/s; CMB+Virgo]
-1.0
-0.5
0.0
0.5
1.0
mH -
(MH+µ"
CDM)
RMS = 0.15 mag
#z = 150 km/s
No Trends in Residuals
0.0 0.5 1.0 1.5 2.0 2.5 !2 / DoF
-2
-1
0
1
2
mH -
(MH+µ"
CDM)
PAIRITEL SNeIaliterature SNeIa
0 5 10 15 20 25# H-band Observations
-0.4 -0.2 0.0 0.2 0.4 !
-2
-1
0
1
2
mH -
(MH+µ"
CDM)
PAIRITEL SNeIaliterature SNeIa
0.01 0.10 1.00 10.00 AV
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