hubble symposium 5 may 04. bvibvi sn1a are standardizable candles: bright = slow dim = fast one...

Hubble Symposium 5 May 04


B

V

I

SN1a arestandardizablecandles:

Bright = slow Dim = fast

One parameteryields 10%luminosity distances

SNIa Similarity and Diversity


Luminosity Distance and Cosmological Parameters

(Impress the ignorant)

(See what’s going on)


Z (m-M)

0.5 0.13 +/- 0.05

1.0 0.00 +/- 0.08

1.5 -0.10 +/- 0.10

(speculative!)

Luminosity Distances: 0.5 < z < 1.5

Z=0.5Z=1.

0

Z=1.

5


SNIa – Results in 1998


SNIa - Results in 2003


2dF: Mh = 0.2 ± 0.03KP: h = 0.72 ± 0.08

Constraints on M, , and w


Higher z with ACS and GOODS

5 z-band epochs, spaced by 45 days, simultaneous v,i band, 120 tilesCDFS=08/02-02/03 HDFN=11/02-05/03

(Adam Riess, PI)


2003ak(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


Aphrodite: ACS Delivers!Aphrodite (z=1.3)

ACS grism spectrum

NICMOS F110W

ACS F850lp

viz


Images

Subtractions

discoveryThoth: Hidden by its Host

red, ellipticalhost

z=1.3


Gilgamesh z=1.6

ACSf850lp

NICMOSF110W

F160W

discovery ~+10 days ~+20 days


HST: Crucial for z > 1!

Ground-based

z=1.06

z=1.20

HST+ACS: z=1.30


The New SN Ia Hubble Diagram

97ff6 of the 7 highest redshift SNIa


The Cosmic Acceleration Persists


… and the Contours for Shrink.


The Nature of Dark Energy

• What isis this stuff???• Three clues:

– Quantity (flat?)– Quality w (-1?)– Constancy dw/dt (0?)

w w

present acceleration

past

dec

eler

atio

n


SNIa Progenitors and Gestation

Dahlen et al. 2004 Strolger et al. 2004

Still a big mystery!


Progress on Dark Energy using SNIa

• Essential for – w0, 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– w0, w’ constraints

– Immunity to systematics

• Want 300, need 30• Use z, J, H, and grism• Challenge is improving

search efficiency

z > 1HST only

z < 1Ground based

z

d

1


Ground-based Searches

ProjectStart - End

GPix Harvest Clrs Sampling

Essence

CTIO 4m2001 - 2005

0.0640

per yr2

2 week

campaign

CFHTLS

CFHT 3.6m2003 - 2008

0.4200

per yr3

2 week

campaign

Pan-STARRS Telescope #1

2006 - 2007

1100

per mo5

Every 4 days

Pan-STARRS 2007 - 41000

per mo5

Every 4 days


SNIa Distances without Redshifts

Barris et al. 2004


The Near Future with HST

270 Orbits in Cycle 13P.I. Riess (STScI)

PANS: Probing Acceleration Now with Supernovae

“Importance of Supernovae at z > 1.5 to Probe Dark Energy”

Linder and Huterer 2003


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 Ultra-Wide-Field Imager

• Performance:– 90 min2 = 8 x ACS, same

sensitivity– Expect 1 SNIa per

pointing per orbit– efficient, continuous

search possible

HUFI(90 arcmin2)

FOV Footprint at CCD FPA

-40

-30

-20

-10

0

10

20

30

40

-110 -100 -90 -80 -70 -60 -50 -40 -30 -20 -10 0 10 20 30 40 50 60 70 80 90 100 110

X image (mm)

y i

ma

ge

(m

m)

FOV at CCD CCD 1

CCD 2 CCD 3

4 K x 4 K CCD (3 each)

90 square arcminute FOV

hstfullfd.14,11/14/01, p. 44

Pick Off Mirror

M3

M1 Corrector Mechanism

Filter Mechanism

Shutter Mechanism

CCD Heat Pipes

M1

Calibration Door Mechanism


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, w0, 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, w0, 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, w0, w’) = (0.05, 0.1, 0.2)


JDEM/SNAP? ~2015-2020SDSSESSENCE

C F H T L

HST/PANS

Kait/SNFactory

Phase Space of Supernova Dark Energy Surveys

Current Published SNe

Panstars/LSST?


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 04Hoeflich et al.Niemeyer et al.

Turbulent flame consuming a white dwarf

Luminosity-decline rate

Spectra

Theoretical Models for SNIa


What Causes the Diversity?

• Progenitors may have different– Mass (luminosity ~ 56Ni mass)– Metallicity (Z n 56Ni )– Age (22Ne 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


Z = 0.5

Offsets from Empty Universe


Z = 1.5

Offsets from Empty Universe


Z (m-M)

0.5 0.13 +/- 0.05

SNIa at z = 0.5


Z (m-M)

1.0 0.00 +/- 0.08

SNIa at z = 1.0


Z (m-M)

1.5 -0.10 +/- 0.10

(speculative!)

SNIa at z = 1.5


Z (m-M)

0.5 0.13 +/- 0.05

1.0 0.00 +/- 0.08

SNIa at 0.5 < z < 1.0


zv

b

i

SN Ia

SN II

Color Selection: An example

b v i z

SN Ia UV deficit


Color Discrimination


SN Ia Spectraat

High-zACS

ACS ACS

ACS ACS ACS

indicates Ca II @ 3750 A

See Riess et al 2003, astro-ph 0308185,and Blakeslee et al 2003, ApJ

#1#2#3


Expansion Kinematics(How Long Has This Been Going On?)

z~0.3-0.6,~5 GYR ago

present acceleration

past

dec

eler

atio

n


SNIa Progenitors and Gestation

Strolger et al. 2004

SNIa appear to sleep for 4 Gyr before explosion!


Fall 2001 Continuous Search

Barris et al. 2004


Distance and Redshift from SNIa Photometry Alone

Barris et al. 2004


Pan-STARRS Reference MissionMode PSY Area Cad. SS B/g r i z Y

SSNEO

1.1d 0.2b

7000h/d/m

27.5 300

SSKBO

1.0d 0.2b

3 hdmy

26.5 60

Var.0.8d 0.8b

1334 min

29.422000

28.87400

28.74400

25.14400

3 1.3d 2.5b

3 14d 26.1 30

25.8 30

25.6 60

24.1 20

22.5 30

Med. Deep

0.6d 0.9b

1200 4d 27.3 271

27.2 460

27.51200

25.21900

24.2 600

Ultra Deep

0.5d 0.7b

28 4d 29.310000

29.218000

28.26300

27.26700

26.226000

5-5- limit (AB) limit (AB)

Total int. (min)Total int. (min)


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)

hubble symposium 5 may 04. bvibvi sn1a are standardizable candles: bright = slow dim = fast one...

Documents

hubble symposium

w slide

days slide

hdfn slide

diversity slide

deceleration slide

pi slide

aphrodite z