Cosmology from Type II Supernovae

Mario Hamuy – Thomas de Jaeger – Lluis Galbany – Santiago GonzálezDepartamento de Astronomía – FCFM -- Universidad de Chile

Millennium Institute of Astrophysics

Future and Science of Gemini 2015, Toronto, June 16 2015

Improvement in precision between 1998-2014 !

60 Type Ia SupernovaePerlmutter et al. 1998

Riess et al. 1998

740 Type Ia SupernovaeBetoule et al. 2014

JLA SNe = low-z + SDSS II + SNLS + HSTBetoule et al. 2014

740 SNe:

118 low-z (Calán/Tololo; CfA, CSP)374 SDSS II (3 years, Sako et al. 2014)239 SNLS (3 years, Conley et al. 2011)9 HST (Riess et al 2007)

0.15-0.20mag

Improvement in precision between 1998-2014 !

60 Type Ia SupernovaePerlmutter et al. 1998

Riess et al. 1998

740 Type Ia SupernovaeBetoule et al. 2014

What causes acceleration? Dark energy, P=ωε ?

Cosmological constant, P=-ε , ω = -1 ?

With increasingly larger samplessystematic errors become critical

Alternative methods?

Type II Supernova light curves(Anderson et al. 2014)

GREAT

DIVERSITY

Velocity Curve(Hamuy & Pinto 2002)

Simple Approach

The luminosities of Type II

supernovae can be standardized

Luminosity-Velocity Relation(Hamuy & Pinto 2002)

The Standardized Candle Method (SCM)(Hamuy & Pinto 2002)

0.39 mag

The Standardized Candle Method (SCM)(Olivares et al. 2010)

0.31 mag

Luminosity-Velocity RelationObservations match Theory!

Kasen & Woosley 2009

0.27 mag

The Standardized Candle Method Revisited(Carnegie Supernova Program, de Jaeger et al. 2015)

� 2004-2009

� z=0.01-0.05

� Filters: ugri + BVYJHK

� Optical spectroscopy

� 54 Supernovae

The Standardized Candle Method Revisited(Carnegie Supernova Program, de Jaeger et al. 2015)

The Standardized Candle Method Revisited(Carnegie Supernova Program, de Jaeger et al. 2015)

The Luminosity-Velocity Relation Revisited(Carnegie Supernova Program, Gutiérrez et al. 2015)

The Standardized Candle Method Revisited(Carnegie Supernova Program, de Jaeger et al. 2015)

r-band

The Standardized Candle Method Revisited(Carnegie Supernova Program, de Jaeger et al. 2015)

J-band

The Standardized Candle Method (SCM)(Hamuy 2004)

0.38 mag

The Standardized Candle Method (SCM)(Nugent et al. 2006)

0.26 mag

The Standardized Candle Method (SCM)(Poznanski et al. 2009)

0.25 mag

The Standardized Candle Method (SCM)(D´Andrea et al. 2010)

0.29 mag

redshift

The Standardized Candle Method (SCM)(Poznanski et al. 2010)

0.25 mag

The Standardized Candle Method (SCM)(Maguire et al. 2010)

0.15 mag

So far so good, but what if we didn´t have spectroscopic information?

Can we come up with a method solely based on photometry?

The Photometric Candle Method (PCM)

Type II Supernova light curves(Anderson, et al. 2014)

time

brightness

s2

s3

Mmax

Mend

MtailPd

OPTd

s1

Trise

defined in Anderson et al. 2014

time

brightness

s2

s1

s3

Mmax

Mend

MtailPd

OPTd

Real data:

SN 2008m

The Photometric Candle Method(Carnegie Supernova Program, de Jaeger et al. 2015)

Anderson et al. 2014

HUBBLE FLOW cz>3000 km s-1

The Photometric Candle Method(Carnegie Supernova Program, de Jaeger et al. 2015)

( ) ZP+cz=βCαs+m 5log2 −

PCA of type II SN light curves

116 SNe II V-band LC from A14

Temporal reference (X reference)

Magnitude units (Y units)

Standardization

5 different options: TEXP, TMAX, TPT, TTRANS, TEND

MABS, MAPP

MXXX-MXXX,MAX, MABS-MABS,MAX + MABS,MAX MAPP-MAPP,MAX + MAPP,MAX

dMXXX, dMABS + dMABS,MAX, dMAPP + dMAPP,MAX

8 different options:

3 options: no, stddev, stddev/sqrt(N)

24 matrices per tREF120 DIFFERENT MATRICES

MW ext and time dilation correction

Normalization: mmax

Reference: Texp4 eigenvectors (templates)

Fitted LC

From an initial sample of 32 SNe with RMS= 0.7, we

achieved a RMS in the standardized magnitudes of 0.35

Only using a correction in one band

Further reduction is expected including a color term

PCA-standardized magnitudes

Cosmology from Type II SupernovaeConclusions

Precision of Type Ia supernovae: 0.15 mag (7% in distance)

Precision of SCM : 0.25 mag (12% in distance)

Precision of PCM: 0.35-0.42 mag (20% in distance)

Cosmology from Type II SupernovaeThe Next Steps

Expand the sample to high-z SNe:

Dark Energy Survey (DES) supernovae

Gemini-S + Magellan spectroscopic followup

Cosmology from Type II Supernovae in the 2020´s

LSST � Millions of Type SNe up to z=0.6 with a cadence of 15 days� Independent route for cosmological parameters via PCM

LSST + Gemini-S � Even better route for cosmology via SCM !

Type II SNe

2025