Accurate Measurement of the Hubble Constante with Type Ia

Accurate Measurement of the Hubble Constante with Type Ia

Accurate Measurement of the Hubble
Constante with Type Ia Supernovae
11-Kosmologietag 2016, Bielefeld University
28th of April 2016
Mickael RIGAULT
Cosmology using Type Ia Supernovae
Ωm = 0.295
ΩΛ = 0.705
µ( z
;
z
(
µ
2 hL S
H0
;
2 hL S
H0
)
w
,
⌦
i
N
Ωm = 1
ΩΛ = 0
)
i
N
Betoule et al. 2014
Mickael RIGAULT
2
Cosmology using Type Ia Supernovae, w & H0
Ωm = 0.295
ΩΛ = 0.705
µ( z
;
z
(
µ
Mickael RIGAULT
2 hL S
H0
)
i
N
;
SNe I
a
2 hL S
H0
)
w
,
⌦
i
N
Ωm = 1
ΩΛ = 0
Betoule et al. 2014
B
CM
3
Cosmology using Type Ia Supernovae, w & H0
Ωm = 0.295
ΩΛ = 0.705
;
z
µ(
2 hL S
H0
)
i
N
µ( z
;
2 hL S
H0
)
w
,
⌦
i
N
Ωm = 1
ΩΛ = 0
To get H0: Need an independent
measurement of the average
SN Ia Luminosity
Betoule et al. 2014
Mickael RIGAULT
4
Independent SNe Ia distance measurements
Cepheids: Young stars having a
pulsation-luminosity relation
)
⟩
N
S
L
⟨
;
f(d
Riess et al. (2009)
H0 = 72.5 ± 2.5 km s-1 Mpc-1
( 3% ; Ri e ss e t a l 2 011 ; E f st a t hi o u 2 01 4)
Mickael RIGAULT
5
The Hubble Constant in Cosmology
Planck 2015 — Cosmological Results
Test our understanding of the
cosmology (ΛCDM)
Change the model, change H0
z~1000
THE MODEL
CONSTRAINS H0
z~0
H0 = 67.8 ± 0.9 km s-1 Mpc-1
— mo de l d e p e ndent , ΛC D M —
Mickael RIGAULT
6
Tension In the Standard Model of Cosmology
~2.5σ
Indirect
(z~1000 ; ΛCDM)
Mickael RIGAULT
iou
ath
Efs
t
20
15
et
a
l. 2
01
4
New physics or Systematic errors ?
Direct
z~0 ; SNe Ia
7
Astrophysical Bias in Cosmology
Mickael RIGAULT
SN2011fe
8
The Local Perspective
GLOBAL
Hα map
Rigault et al. (2013)
LOCALE
Star forming
Environments
—
Young stars
Spiral, Star forming
Galaxies
Passive
Environnements
—
Old(er) stars
Mickael RIGAULT
9
Astrophysical Bias in Cosmology (>4σ)
Standardized SN Luminosity
Rigault et al. 2013, 2015
Rigault et al. in prep.
CNRS 01-07
Older
Younger
Age of surrounding stars
10
Independant SNe Ia distance measurements
Cepheids: Young stars having a
pulsation-luminosity relation
BIASED SAMPLE
)
⟩
SNe Ia having Cepheid distance
N
S
L
⟨
;
measurements are all
from
d
(
f
Star Forming Regions
Riess et al. (2009)
H0 = 72.5 ± 2.5 km s-1 Mpc-1
( 3% ; Ri e ss e t a l 2 011 ; E f st a t hi o u 2 01 4)
Mickael RIGAULT
11
Correct Astrophysics for Accurate Cosmology (H0)
Tension in the Standard model of Cosmology
~2.5σ
~1σ
Mickael RIGAULT
Indirect
Direct
(z~1000 ; ΛCDM)
z~0 ; SNe Ia
12
Correct Astrophysics for Accurate Cosmology (w)
50% Young
50% Old
90% Young 10% Old
PREDICTION
z)
(
N
LS
(z)
L SN
i
µ( z
;
N
2 hL S
H0
w)
,
⌦
Galaxies are more Star Forming
at Higher Redshift
i)
;
z
(
µ
2 hL SN
H0
Could impact w by a few %
Mickael RIGAULT
13
Correct Astrophysics for Accurate Cosmology
Access Better Standard Candles
– Confirmed par Kelly et al. (2014) –
« Youngs »
The LSST Science Book: “[…] Without
understanding the physical origins of this
dispersion, and whether it has systematic
effects that depend on redshift, we will not
be able to use the full statistical power of
the tens to hundreds of thousands of
SNe Ia that LSST will find. ” (p. 395).
Strong Reduction of the
Systematic Uncertainties
Mickael RIGAULT
14
Understand the Origin of the Dependencies
HST Project GO14163 (PI: Rigault) first measurements of:
-
The amount of dust along the line of sight
-
The age of the surrounding stars
UV + OPTICAL DATA
Break the Degeneracy
OPTICAL DATA (5 SDSS POINTS)
age & dust features are degenerated
Rigault GO14163
UV
CNRS 01-07
Optique
15
Understand the Origin of the Dependencies
~30 targets already, ~70 expected
u
g
r
i
z
f225W (UV)
PTF10zdt
CNRS 01-07
Rigault GO14163
16
Ne w G e ne r a t i o n o f Sur veys
ZTF 2017/2020: ~2000 SNe Ia (z<0.1)
M. RIGAULT
Humboldt Universität zu Berlin — 8th of December 2015
Star Formation Bias and Mass-step
The SF-bias explains the mass-step
THE FRACTION OF YOUNG STARS
IS GREAT IN LOW-MASS GALAXIES
On average, SNe Ia should be
brighter in high-mass hosts
M. RIGAULT
IPNL — 2015
20
Star Formation Bias and Mass-step
The SF-bias explains the mass-step
THE FRACTION OF YOUNG STARS
IS HIGHER IN LOW-MASS GALAXIES
THE FRACTION OF YOUNG STARS
IS HIGHER AT HIGHER REDSHIFT
M. RIGAULT
IPNL — 2015
21
SF-bias vs. Mass Step — Childress’ Model
Childress et al. 2014
M. RIGAULT
IPNL — 2015
22
SF-bias vs. Mass Step — Childress’ Model
Childress et al. 2014
Accurate model that confirms our prediction
M. RIGAULT
IPNL — 2015
23
Formation Stellaire — Hα vs. UV
Salim et al. 2007
Hα ⇔ UV ⇔ Étoiles
massives
Temps de vie des étoiles ∝ masse-2.5
S’il y a du Hα, il y a des jeunes étoiles
Mickael RIGAULT
25
Signal Hα Local
1 — extrait le
signal galactique
2 — ajuster les
propriétés physiques
CNRS 01-08
Mickael RIGAULT
26
Local FUV of Cepheid-SNe
Mickael RIGAULT
27
La Constante de Hubble
Tester le modèle de concordance — SNe Ia: mesure directe
MESURE DIRECTE DE H0
LE MODÈLE
CONTRAINT H0
i)
;
z
(
µ
2 hL SN
H0
µ( z
;
2 hL S
H0
i
N
w)
,
⌦
+ Céphéides SN →⟨ LSN⟩
SH0ES (Riess et al. 09)
Betoule et al. 2014
Planck 2015 — Résultats Cosmologiques
Mickael RIGAULT
28
La constante de Hubble et le CMB
outils: map.gsfc.nasa.gov/resources/camb_tool
H0 = 84 km s-1 Mpc-1
Mickael RIGAULT
29
Local Analyses at high-z
HST — CANDELS
z=1.1
Hemmati et al. (2014)
Densité stellaire
Mickael RIGAULT
Age
Extinction
Formation stellaire
30