Hubble Symposium 5 May 04
BVIBVI SN1a are standardizable candles: Bright = slow Dim = fast One parameter yields 10% luminosity distances SNIa Similarity and Diversity
Hubble Symposium 5 May 04 Luminosity Distance and Cosmological Parameters (Impress the ignorant) (See what’s going on)
Hubble Symposium 5 May 04 Z (m-M) / / / (speculative!) Luminosity Distances: 0.5 < z < 1.5 Z=0.5 Z=1.0 Z=1.5
Hubble Symposium 5 May 04 SNIa – Results in 1998
Hubble Symposium 5 May 04 SNIa - Results in 2003
Hubble Symposium 5 May 04 2dF: M h = 0.2 ± 0.03 KP: h = 0.72 ± 0.08 Constraints on M, , and w
Hubble Symposium 5 May 04 Higher z with ACS and GOODS 5 z-band epochs, spaced by 45 days, simultaneous v,i band, 120 tiles CDFS=08/02-02/03 HDFN=11/02-05/03 (Adam Riess, PI)
Hubble Symposium 5 May ak (1.57) 2002fz (0.839) 2003aj (1.4) 2002ga (0.988) 2002kb (0.474) 2002fv (~1.0) 2002lg (0.61) 2002fw (1.3) 2002hs (0.388) 2002hp (1.3) 2002hq (0.74) 2002kd (0.735) 2002fx (~1.8) 2003al (0.91) 2002ke (0.578) 2002kc (0.214) 2002hr (0.526) 2002fy (0.88) 2002ht (?) CDFS 2003dz (0.48) 2003er (0.63) 2003be (0.64) 2003dx (0.46) 2003bb (0.89) 2003bc (0.51) 2003ew (0.66) 2003eu (0.76) 2003ba (0.47) 2002kh (0.71) 2003et (0.83) 2003en (0.54) 2003es (0.968) 2003en (0.54) 2003dy (1.37) 2003ea (0.89) Vilas (0.86) 2003eb (0.92) 2003bd (0.67) 2003eq (0.85) 2002kl (0.39) 2003az (1.27) 2002ki (1.14) HDFN
Hubble Symposium 5 May 04 Aphrodite: ACS Delivers! Aphrodite (z=1.3) ACS grism spectrum NICMOS F110W ACS F850lp viz
Hubble Symposium 5 May 04 Images Subtractions discovery Thoth: Hidden by its Host red, elliptical host z=1.3
Hubble Symposium 5 May 04 Gilgamesh z=1.6 ACS f850lp NICMOS F110W F160W discovery~+10 days ~+20 days
Hubble Symposium 5 May 04 HST: Crucial for z > 1! Ground-based z=1.06 z=1.20 HST+ACS: z=1.30
Hubble Symposium 5 May 04 The New SN Ia Hubble Diagram 97ff 6 of the 7 highest redshift SNIa
Hubble Symposium 5 May 04 The Cosmic Acceleration Persists
Hubble Symposium 5 May 04 … and the Contours for Shrink.
Hubble Symposium 5 May 04 The Nature of Dark Energy isWhat is this stuff??? Three clues: –Quantity (flat?) –Quality w (-1?) –Constancy dw/dt (0?) w w present acceleration past deceleration
Hubble Symposium 5 May 04 SNIa Progenitors and Gestation Dahlen et al. 2004Strolger et al Still a big mystery!
Hubble Symposium 5 May 04 Progress on Dark Energy using SNIa Essential for –w 0, w’ constraints –Progess in systematics: Host galaxies Colors (rest frame UV) SNxx contamination Spectra Evolution –Progenitors and IC’s Want >10,000, need 1000 Wide field, optical colors Essential for –w 0, w’ constraints –Immunity to systematics Want 300, need 30 Use z, J, H, and grism Challenge is improving search efficiency z > 1 HST only z < 1 Ground based z d 1
Hubble Symposium 5 May 04 Ground-based Searches Project Start - End GPixHarvestClrsSampling Essence CTIO 4m per yr 2 2 week campaign CFHTLS CFHT 3.6m per yr 3 2 week campaign Pan-STARRS Telescope # per mo 5 Every 4 days Pan-STARRS per mo 5 Every 4 days
Hubble Symposium 5 May 04 SNIa Distances without Redshifts Barris et al. 2004
Hubble Symposium 5 May 04 SNIa Distances without Redshifts Barris et al. 2004
Hubble Symposium 5 May 04 The Near Future with HST 270 Orbits in Cycle 13 P.I. Riess (STScI) PANS: Probing Acceleration Now with Supernovae “Importance of Supernovae at z > 1.5 to Probe Dark Energy” Linder and Huterer 2003
Hubble Symposium 5 May 04 The Nature of Dark Energy, II Cosmological Constant –Consistent with the observations at 1- –All theorists hate it –PANS will make life very interesting for theorists! w
Hubble Symposium 5 May 04 Hubble Ultra-Wide-Field Imager Performance: –90 min 2 = 8 x ACS, same sensitivity –Expect 1 SNIa per pointing per orbit –efficient, continuous search possible HUFI (90 arcmin 2 ) Pick Off Mirror M3 M1 Corrector Mechanism Filter Mechanism Shutter Mechanism CCD Heat Pipes M1 Calibration Door Mechanism
Hubble Symposium 5 May 04 Three Futures No servicing; HST dies in 2008 –Our ~30 SNIa at z>1 remain a legacy for next 10 years of ground based observation (restricted to z<1) – ( DE, w 0, w’) = (0.1, 0.3, 0.8) HST sleeps in 2007; RM1 in 2009; WFC3 installed –Search CDF and HDF with WF3 / IR. Find SNIa at 1.3 < z < 2.0 at a rate of one per 10 – 20 orbits? ACS parallels? JWST??? – ( DE, w 0, w’) = (0.05, 0.2, 0.4) RM2 in 2012 to prove robotics technology for NASA –HUFI-red finds SNIa at 1.0 < z < 1.8 at a rate of 1 – 2 per orbit, IR light curves from WF3 and JWST, redshifts from JWST – ( DE, w 0, w’) = (0.05, 0.1, 0.2)
Hubble Symposium 5 May 04 JDEM/SNAP? ~ SDSS ESSENCE C F H T L HST/PANS Kait/SN Factory Phase Space of Supernova Dark Energy Surveys Current Published SNe Panstars/LSST?
Hubble Symposium 5 May 04 Supernova Systematics Uninteresting (avoidable) –Photometry error (0.03 0.01) –UV SEDs (0.05 0.00) –Poor LC coverage (0.04 0.00) –Host extinction (0.06 0.03) Interesting (intrinsic) –SN1a: progenitor, initial conditions, trigger (z) –Host extinction and properties (z) –Gravitational lensing (z) –Transparency of IGM (z)
Hubble Symposium 5 May 04 Hoeflich et al. Niemeyer et al. Turbulent flame consuming a white dwarf Luminosity-decline rate Spectra Theoretical Models for SNIa
Hubble Symposium 5 May 04 What Causes the Diversity? Progenitors may have different –Mass (luminosity ~ 56 Ni mass) –Metallicity (Z n 56 Ni ) –Age ( 22 Ne sedimentation?) –Binary companion (???) –Mass transfer mechanism (???) Explosion may have different –Trigger mechanism (???) –Propagation (deflagration/detonation, “weather”, etc) Good news: –Chandresekhar mass and NSE make explosions quite uniform (~50% and 1 parameter gets us to ~20%) Bad news: –Plenty of room for unknown systematics at the 2% level
Hubble Symposium 5 May 04 Z = 0.5 Offsets from Empty Universe
Hubble Symposium 5 May 04 Z = 1.5 Offsets from Empty Universe
Hubble Symposium 5 May 04 Z (m-M) / SNIa at z = 0.5
Hubble Symposium 5 May 04 Z (m-M) / SNIa at z = 1.0
Hubble Symposium 5 May 04 Z (m-M) / (speculative!) SNIa at z = 1.5
Hubble Symposium 5 May 04 Z (m-M) / / SNIa at 0.5 < z < 1.0
Hubble Symposium 5 May 04 z v b i SN Ia SN II Color Selection: An example b v i z SN Ia UV deficit
Hubble Symposium 5 May 04 Color Discrimination
Hubble Symposium 5 May 04 SN Ia Spectra at High-z ACS indicates Ca 3750 A See Riess et al 2003, astro-ph , and Blakeslee et al 2003, ApJ #1 #2 #3
Hubble Symposium 5 May 04 Expansion Kinematics (How Long Has This Been Going On?) z~ , ~5 GYR ago present acceleration past deceleration
Hubble Symposium 5 May 04 SNIa Progenitors and Gestation Strolger et al SNIa appear to sleep for 4 Gyr before explosion!
Hubble Symposium 5 May 04 Fall 2001 Continuous Search Barris et al. 2004
Hubble Symposium 5 May 04 Distance and Redshift from SNIa Photometry Alone Barris et al. 2004
Hubble Symposium 5 May 04 Pan-STARRS Reference Mission ModePSYAreaCad.SSB/grizY SS NEO 1.1d 0.2b 7000 h/d/ m SS KBO 1.0d 0.2b 33 hdm y Var. 0.8d 0.8b min 3 1.3d 2.5b 33 14d Med. Deep 0.6d 0.9b 12004d Ultra Deep 0.5d 0.7b 284d limit (AB) Total int. (min)
Hubble Symposium 5 May 04 Science with Pan-STARRS Moving Object Science –NEO – Near Earth Object threat –OSS/MBO – Main Belt and Other Solar System science –KBO – Kuiper Belt Objects –SOL – Solar Neighborhood (parallaxes and proper motions) Static and Invariable Object Science –WL – Weak Lensing –LSS – Large Scale Structure –LSB – Low Surface Brightness and dwarf galaxies –SPH – Spheroid formation –EGGS – Extragalactic and Galactic Stellar science Transient and Variable Object Science –AGN – Active Galactic Nuclei –SNE – Supernovae –GRB – Gamma Ray Bursts and afterglows –EXO – Exoplanets (from occulation) –YSO – Young Stellar Objects –VAR – Variability Science (especially stars) TGBN (Things that go Bump in the Night)