Correcting for peculiar velocities of Type Ia Supernovae ... · P.-F. Leget,´ M. V. Pruzhinskaya,...
Transcript of Correcting for peculiar velocities of Type Ia Supernovae ... · P.-F. Leget,´ M. V. Pruzhinskaya,...
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Introduction Data Results Conclusions
Correcting for peculiar velocities ofType Ia Supernovae in galaxy clusters
P.-F. Leget, M. V. Pruzhinskaya, A. Ciulli, E. Gangler, Ph. Gris,L.-P. Says + SNFACTORY collaboration
Lomonosov Moscow State University, Sternberg Astronomical Institute
November 14, 2017
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Introduction Data Results Conclusions
Introduction
DataNearby Supernova Factory dataHost clusters dataRedshift measurement
ResultsImpact on the Hubble diagramPhysical properties of SNe Ia and their hosts in galaxy clusters
Conclusions
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Introduction Data Results Conclusions
Cosmology with SN IaSN Ia are standardizable candles
I ΩΛ = 0.705± 0.034 (Betoule et al. 2014)
I “luminosity distance-redshift” relationI standardization of SN Ia (Rust 1974, 1975; Pskovskii 1977, 1984;
Phillips 1993; Phillips et al. 1999; Riess et al. 1996; Perlmutter et al.1997, 1999; Wang et al. 2003; Guy et al. 2005, 2007; Jha et al. 2007)
M = MB − αX1 + βC
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Introduction Data Results Conclusions
Cosmology with SN IaPeculiar velocities
(from A. Ciulli)
I Is the uncertainty in the redshift negligible?(1 + zobs) = (1 + zc)(1 + zd)
I For low and intermediate redshifts (z < 0.2):I to remove all SNe with z < 0.015 from the Hubble diagram & to
add a 300–400 km/s peculiar velocity dispersion as z uncertainty(Astier et al. 2006; Wood-Vasey et al. 2007; Amanullahet al. 2010; Union 2.1)
I velocity maps of the nearby Universe (150 km/s, Hudson et al.2004; Conley et al. 2011; Betoule et al. 2014; JLA)
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Introduction Data Results Conclusions
Coma cluster
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σV = 1038 km/s(Colless & Dunn 1996)σm = 5σV
cz ln 10
Standard methods totake into accountpeculiar velocities cannot be applied forgalaxy clusters!
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Introduction Data Results Conclusions
SN Ia in clusters
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µ Doppler shift
Hubble lawTrue SN Ia redshiftObserved SN Ia redshift
zobs
num
bero
fgal
axie
s
Doppler shift
cluster redshift histogram
zc
∆µ
Doppler shift
Virgo, Fornax:Blakeslee et al. 1999;Radburn-Smith et al. 2004For SNe:Feindt et al. 2013; Dhawan et al.2017
How to estimate better theimpact of peculiar velocities onthe redshift measurements?
I to match the host galaxies of SNe Ia with known clusters of galaxiesI to use the host cluster redshift instead of the host galaxy redshift
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Introduction Data Results Conclusions
Nearby Supernova Factory data
I 145 SN Ia (CABALLOv2, 2004 – 2009; Aldering et al. 2002)I The sample contains the objects with good final references and
properly measured light-curve parameters, including quality cutssuggested by Guy et al. (2010).
I m∗B, X1, and C are estimated with the SALT2.4 lightcurve fitter(Guy et al. 2007, Betoule et al. 2014).
0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4Redshift
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Num
bero
fSN
e JLA
NearbySDSSSNLSHSTSNF
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Introduction Data Results Conclusions
Galaxy clusters
Methods for identifying the clusters:I over-density regions on the imagesI red sequence methodI diffuse X-ray emissionI Sunyaev-Zel’dovich effect
SIMBAD databaseI only clusters of galaxies
(exclude groups of galaxies)I d < 2.5 MpcI ∆z < 0.015
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Introduction Data Results Conclusions
Redshift calculation
σV ' 10R200H(z)→ zcler = σV√
Ngal
Simbad query
Galaxy cluster list
R200 query
SDSS DR13 query
SNF host
Literature query
yes
no
zcl, zcl,err
request
output
computation
for all
per cluster
R lit200
tttttttttttt
Rv200
tttttttttttt
Galaxy list in cluster area
Estimation of R200
R200 =
Ngal>10
Ngal<10 R200 = 1.1 Mpc
Ngal>Npaper
else
Biweight
Keep literature value
Remove duplicates
R200 =
final result
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Introduction Data Results Conclusions
Final matching
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I d < R200
I |zhost − zcl| < 3σVc
I + X-ray→ 11 SNe
0.00 0.02 0.04 0.06 0.08 0.10z
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log(
L50
0[e
rgs−
1 ])
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σ V[k
ms−
1 ]Xavier et al. 2013 (1.5 Mpc, σV = 500 km s−1);Dilday et al. 2010 (1.0 Mpc h−1, ∆z = 0.015)
Red sequence
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g−
r
SN2009hi PTF09foz SNF20060609-002
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2 SNF20080612-003
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SNF20061020-000
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SN2007nq
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Introduction Data Results Conclusions
X-ray emission (ROSAT)
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SNF20080731-000 SN2007nq
ZwCl 1742+3306 A0119
Host clusters data. Ensemble cluster
0 1 2 3 4 5
r/R200
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v/σV
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g−r
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Hubble diagram
χ2 =∑(
µi(MB, α, β)− µthi
σtoti
)2
(1)
µ = m∗b −MB + αX1 − βC (2)
µ th = 5 log10 dL−5, dL =c
H0(1+zh)
∫ zc
0
dz′c√ΩΛ + Ωm(1 + z′c)3
(3)
σ toti
2= σ 2
LCi+ σ 2
z + σ 2int (4)
zc =
z cl
c
z hostc
σz =
5√
z cl 2err
z cl ln(10), if inside a galaxy cluster
5√
z host 2err +0.0012
z host ln(10), otherwise
(5)14/18
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Introduction Data Results Conclusions
Hubble diagram
wRMS = 0.137m (without correction); wRMS = 0.130m (with correction); p = 5.9× 10−4
wRMS = 0.130m (inside clusters); wRMS = 0.151m (outside clusters); p = 3.8× 10−1
0.01 0.02 0.03 0.04 0.05 0.06 0.07 0.08 0.09zc
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∆µ
SNe Ia inside clusters, before correctionSNe Ia inside clusters, after correctionSNe Ia outside clusters
0.002 0.004 0.006 0.008
zc
−2.0
−1.6
−1.2
−0.8
∆µ
SN2006X
wRMS=0.151±0.010 magwRMS=0.137±0.036 magwRMS=0.130±0.038 mag
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Introduction Data Results Conclusions
The environment of SN Ia
The influence of the environmental effects on the SN Ia intrinsicluminosity was proved in many works:
I host galaxy morphology and stellar population age (Hamuy et al.1995,1996,2000; Riess et al. 1999; Sullivan 2003; Hicken et al. 2009;Pruzhinskaya et al. 2011; Hill et al. 2016; Henne et al. 2017)
I galocentric distance (Sullivan et al. 2003; Hill et al. 2016)I star-formation rate (Sullivan et al. 2006; Neill et al. 2009; Lampeitl
et al. 2010; Sullivan et al. 2010; Smith et al. 2012; Johansson 2013)I local star-formation rate (1-3 kpc; Rigault et al. 2013; Roman et al.,
arXiv:1706.07697)I stellar mass of host galaxy (Kelly et al. 2010; Sullivan et al. 2010;
Johansson 2013)I host metallicity (Gallagher et al. 2005,2008; Howell et al. 2009)
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Physical properties of SNe Ia in clusters
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Host morphology:I E/S0 (4), Spirals (7)
Highest correction:
I X1 ' 0I blue galaxiesI high local sSFRI smaller Mstellar
I r/R200 ' 0.7
−3 −2 −1 0 1X1
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−0.1 0.0 0.1 0.2C
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−15−14−13−12−11−10 −9log(LsSFR)
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9 10 11 12log(Mstellar)
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E S0 Sab Sb Sbc ScMorphology
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c|∆z|
[100
0km
s−1 ]
−0.4 −0.3 −0.2 −0.1 0.0RS residuals
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14.0 14.5 15.0log(M200)
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-13
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log(
LsS
FR)
Conclusions
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I We studied how the peculiar velocities of SNe Ia in galaxy clustersaffect the redshift measurements by matching 145 SNFACTORY
supernovae with known clusters of galaxies.I The applied technique allowed to decrease the spread on the Hubble
diagram. For the SNe in clusters wRMS is improved from 0.137m to0.130m with p-value = 5.9× 10−4.
I The described effect influences the distance measurements in thenearby Universe (z < 0.1) and has to be taken into account in futurecosmological surveys.
I The difference in SN light curve parameters inside and outside theclusters could be fruitful avenue of investigation for futurecosmological analysis.
Thanks for the attention!