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Surveying the Accelerating Universe with Supernovae

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Surveying the Accelerating Universe with Supernovae Surveying the Accelerating Universe with Supernovae Saurabh W. Jha Georgia Tech School of Physics Colloquium March 5, 2012 HST color composite of SN 2008A in NGC 634 from McCully et al. (in prep.) “Surveying” the Universe: Measuring Astronomical Distances the cosmological distance ladder Leavitt (1912): 100th anniversary! Cepheid variable stars yield precise distances Hubble’s Law Hubble (1929) measured distances using bright stars in other galaxies and average galaxy properties measuredthe cosmological galaxy redshifts distance with ladder spectroscopy, using the Doppler shift of atomic spectral lines Hubble’s Law Hubble (1929) wrong units! measured distances using bright stars in other galaxies and average galaxy properties measuredthe cosmological galaxy redshifts distance with ladder spectroscopy, using the Doppler shift of atomic spectral lines Hubble’s Law theHubble’s cosmological Law is a consequence distance ladder of the expansion of the Universe v = H0 d History and Future of the Expansion History and Future of the Expansion if the expansion were uniform, we could extrapolate backwards to get the age of the Universe: t0 = 1/H0 FLRW Cosmography general relativity + cosmological principle (homogeneity, isotropy) dr2 ds2 = c2 dt2 a(t)2 + r2 dθ2 + r2 sin2 θ dφ2 − 1 kr2 − a(t) scale factor k describes spatial curvature ≡ a λem 1 photons: ds2 =0 = = ⇒ a0 λobs 1+z FLRW Cosmography general relativity + cosmological principle (homogeneity, isotropy) dr2 ds2 = c2 dt2 a(t)2 + r2 dθ2 + r2 sin2 θ dφ2 − 1 kr2 − a(t) scale factor k describes spatial curvature ≡ a λem 1 photons: ds2 =0 = = ⇒ a0 λobs 1+z kinematic description of scale factor evolution a˙ aa¨ H q ... ≡ a ≡−a˙ 2 Taylor expand a(t) around t0: H 0, q 0, j 0, s 0, ... FLRW Cosmography general relativity + cosmological principle (homogeneity, isotropy) dr2 ds2 = c2 dt2 a(t)2 + r2 dθ2 + r2 sin2 θ dφ2 − 1 kr2 − a(t) scale factor k describes spatial curvature ≡ a λem 1 photons: ds2 =0 = = ⇒ a0 λobs 1+z kinematic description of scale factor evolution a˙ aa¨ H q ... ≡ a ≡−a˙ 2 Taylor expand a(t) around t0: H 0, q 0, j 0, s 0, ... L f = 2 4πdL FLRW Cosmography general relativity + cosmological principle (homogeneity, isotropy) dr2 ds2 = c2 dt2 a(t)2 + r2 dθ2 + r2 sin2 θ dφ2 − 1 kr2 − a(t) scale factor k describes spatial curvature ≡ a λem 1 photons: ds2 =0 = = ⇒ a0 λobs 1+z kinematic description of scale factor evolution a˙ aa¨ H q ... ≡ a ≡−a˙ 2 Taylor expand a(t) around t0: H 0, q 0, j 0, s 0, ... intrinsic luminosity L f = 2 measuredflux 4πdL FLRW Cosmography general relativity + cosmological principle (homogeneity, isotropy) dr2 ds2 = c2 dt2 a(t)2 + r2 dθ2 + r2 sin2 θ dφ2 − 1 kr2 − a(t) scale factor k describes spatial curvature ≡ a λem 1 photons: ds2 =0 = = ⇒ a0 λobs 1+z kinematic description of scale factor evolution a˙ aa¨ H q ... ≡ a ≡−a˙ 2 Taylor expand a(t) around t0: H 0, q 0, j 0, s 0, ... intrinsic luminosity L z du f = dL(z)=c(1 + z) (k = 0) measured 4πd2 H(u) flux L 0 History and Future of the Expansion a/a0 =1/(1 + z) d /c ∼ L FLRW Cosmography connecting kinematics and dynamics a Universe full of perfect fluids, with equations of state: P = w ρ c2 w equation of state parameter i i i ≡ 2 ρ (1 + z)3(1+wi) a˙ i ∝ ρi a¨ 2 a ∝ (ρi +3Pi/c )= ρi(1 + 3wi) a ∝− − FLRW Cosmography connecting kinematics and dynamics a Universe full of perfect fluids, with equations of state: P = w ρ c2 w equation of state parameter i i i ≡ 2 ρ (1 + z)3(1+wi) a˙ i ∝ ρi a¨ 2 a ∝ (ρi +3Pi/c )= ρi(1 + 3wi) a ∝− − w density acceleration a(t) matter 3 2/3 0 ρM (1 + z) ρM t (normal/dark) ∝ ∝− ∝ 4 1/2 radiation +⅓ ρ (1 + z) 2ρR t R ∝ ∝− ∝ cosmological Ht −1 ρΛ = const +2ρΛ e constant ∝ ∝ History and Future of the Expansion a/a0 =1/(1 + z) different pasts and futures depend on gravity and the contents of the Universe d /c ∼ L History and Future of the Expansion a/a0 =1/(1 + z) different pasts and futures depend on gravity and the contents of the Universe d /c ∼ L redshift yields the cosmic scale factor distance tells the time, but we need a good distance indicator Type Ia SN 1998bu in M96 March 14, 1997 Type Ia SN 1998bu in M96 March 14, 1997 May 18, 1998 Type Ia SN 1998bu in M96 one star in this galaxy becomes as bright as 10 billion stars! March 14, 1997 May 18, 1998 SN 1998bu maximum light spectrum intermediate mass elements are fused from C and O during the explosion ejecta travels at ~10,000 km/s Fe Si Fe Ca S Si ThermonuclearThe progenitor o(Typef a Type Ia)Ia s uSupernovaepernova . .which spills gas onto the Two normal stars The more massive secondary star, causing are in a binary pair. star becomes a giant. it to expand and become engulfed. The secondary, lighter star The common envelope is and the core of the giant star ejected, while the separation The remaining core of spiral-in within a common between the core and the the giant collapses and envelope. secondary star decreases. becomes a white dwarf. The aging companion The white dwarf's mass ...causing the companion star starts swelling, spilling increases until it reaches a star to be ejected away. gas onto the white dwarf. critical mass and explodes... the cosmological distance ladder a complicated and uncertain story, but we observe them to be very homogeneous Some “Nearby” SN Ia Light Curves SN 1998bu in M 96 SN 2001V in NGC 3987 the groundbreaking work: Calán/Tololo SN Survey 1996AJ....112.2391H shape of the light curve lets us read the label on our cosmic light bulb measuring colors lets us correct for Phillips et al. (1993); Hamuy et al. (1996) attenuation of the light by dust SN Ia are calibrated candles: luminosity correlated with light-curve decline rate (Phillips relation) multicolor templates constrain dust Krisciunas et al. (2006) MLCS2k2 Jha, Riess, & Kirshner (2007) MLCS2k2 light curve fits KAIT BVRI photometry Ganeshalingam et al. (2009, in prep) Si μ = 33.46 ± 0.07 mag μ = 33.49 ± 0.10 mag MLCS2k2 light curve fits KAIT BVRI photometry Ganeshalingam et al. (2009, in prep) Si μ = 33.46 ± 0.07 mag μ = 33.49 ± 0.10 mag SN 1999cp and SN 2002cr, both in NGC 5468 Correcting for Intrinsic Variations and Dust Si Correcting for Intrinsic Variations and Dust Si empirical validation that the method works! Hubble’s Law extended v = H0d 7 Si Hubble’s Law extended v = H0d 7 our latest results from the HubbleSi Space Telescope: -1 -1 H0 = 73.8 ± 2.4 km s Mpc (Riess et al. 2011) History and Future of the Expansion a/a0 =1/(1 + z) different pasts and futures depend on gravity and the contents of the Universe d /c ∼ L History and Future of the Expansion a/a0 =1/(1 + z) different pasts and futures depend on gravity and the contents of the Universe “nearby” supernovae d /c ∼ L to see these curves diverge, we need to look farther back in time: distant (high-redshift) type Ia supernovae Finding Distant Supernovae ESSENCE Survey ! 5 year project on 4m telescope at CTIO in Chile ! Started in 2002/3. 30 half-nights ! Wide field images in RI bands, 32 fields, every 4 nights, 11 "-deg ! Same-night detection of SNe ! Spectroscopy ! Magellan, Keck, Gemini telescopes ! Goal is ~200 SNe, 0.2<z<0.7 ! Distances to 2% in !z=0.1 bins CTIO 4m Image Subtraction (High-z Supernova Team) 10 A Distant Type Ia Supernova, z = 1.3 The Mighty Aphrodite ACS z-band 1 orbit 2002 August 01 The Mighty Aphrodite ACS z-band 1 orbit 2002 September 22 The Mighty Aphrodite ACS z-band 1 orbit 2002 October 01 The Mighty Aphrodite ACS z-band 1 orbit 2002 October 05 The Mighty Aphrodite ACS z-band 1 orbit 2002 October 10 The Mighty Aphrodite ACS z-band 1 orbit 2002 October 20 The Mighty Aphrodite ACS z-band 1 orbit 2002 October 30 The Mighty Aphrodite ACS z-band 1 orbit 2002 October 31 The Mighty Aphrodite ACS z-band 1 orbit 2002 November 17 The Mighty Aphrodite ACS z-band 1 orbit 2002 November 25 High-Z SN Search Team Supernova Cosmology Project Riess et al. (1998) Perlmutter et al. (1999) High-Z SN Search Team Supernova Cosmology Project Riess et al. (1998) Perlmutter et al. (1999) 2011 Nobel Prize in Physics from the New York Times York the New from THE ASTRONOMICAL JOURNAL, 116:1009È1038, 1998 September ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. Adam Riess Saul Perlmutter Brian Schmidt OBSERVATIONAL EVIDENCE FROM SUPERNOVAE FOR AN ACCELERATING UNIVERSE AND A COSMOLOGICAL CONSTANT THE ASTRONOMICAL JOURNAL, 116:1009È1038, 1998 September ADAM G.RIESS,1 A(LEXEI1998. TheV.F AmericanILIPPENKO Astronomical,1 PETER Society.CHALLIS All,2 rightsALEJANDRO reserved. PrintedCLOCCHIATTI in U.S.A. ,3 ALAN DIERCKS,4 PETER M.GARNAVICH,2 RON L.GILLILAND,5 CRAIG J.HOGAN,4 SAURABH JHA,2 ROBERT P. KIRSHNER,2 B.LEIBUNDGUT,6 M. M.PHILLIPS,7 DAVID REISS,4 BRIAN P.SCHMIDT,8,9 ROBERT A. SCHOMMER,7 R. CHRIS SMITH,7,10 J.SPYROMILIO,6 CHRISTOPHER STUBBS,4 NICHOLAS B. SUNTZEFF,7 AND JOHN TONRY11 Received 1998 March 13; revised 1998 May 6 OBSERVATIONAL EVIDENCE FROM SUPERNOVAE FOR AN ACCELERATING UNIVERSE AND A COSMOLOGICAL CONSTANT ABSTRACT We present spectral and photometric observations of 10 Type Ia supernovae (SNe Ia) in the redshift range 0.16 ¹ z ¹ 0.62.
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