spectroscopic survey for the early-type host galaxies of type ia...

K-GMT 중대형 망원경 사용자 워크숍 2017. 03. 03. (Fri)

Spectroscopic Survey for the Early-type Host Galaxies of

Type Ia Supernovae

강이정1

김영로1, 이창희2, 이영욱1

1연세대학교, 2한국천문연구원

K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)

IntroductionType Ia Supernova & the accelerating Universe

Type Ia Supernovae (SNe Ia)

- The good distance indicator

: High peak luminosity

: Most homogeneous class of SNe

(Perlmutter et al. 1997)

cosmological parameter

The cosmological parameter space

- Combination of results from

1) Type Ia Supernovae

2) Cosmic Microwave Background (CMB)

3) Baryonic Acoustic Oscillation (BAO)Riess et al. (1998)

Suzuki et al. (2011)


IntroductionHubble Residual of SNe Ia & Properties of Host Galaxies

Hicken et al. (2009)

Hu

bb

le R

esi

du

al (

Mag

)

Host Galaxy Morphology

Fainter

Brighter

Sullivan et al. (2010)

Fainter

Brighter

Hu

bb

le R

esi

du

al (

Mag

)

log M

The Basic Assumption of SNe Ia cosmology

“Effective Standardizable Candle”

: Peak brightness – Light-curve shape relation

After the light curve correction,

is the look-back time evolution negligible…??

Hubble Residual of SNe Ia & Properties of Hosts

1. Morphological dependency

The early-type galaxies host brighter SNe Ia

(ΔHR ~ 0.16 mag., Hicken et al. 2009)

2. Mass dependency

More massive galaxies host brighter SNe Ia

(ΔHR ~ 0.08 mag., Sullivan et al. 2010)

Hubble Residual ≣ μSN – μz (μ : distance modulus)

the origin of dependency?

“the properties of stellar population?”


Yonsei Nearby Supernovae Evolution Investigation

1) Construction of SNe Ia Catalogue

: Light curve fitting with SNANA

(Y.-L. Kim et al, in prep.)

2) Properties of Early-Type Host Galaxy (ETG)

: Stellar Population Analysis with spectra

(Age, Metallicity, etc.)

Why the Early-Type Host Galaxies?

1) Absorption lines w/ stellar population models

: The best and most reliable method for

age/metallicity determination

2) the Full diversity of SNe la

: Host both Faint & Bright SNe Ia

3) More homogeneous age of stellar populations

4) No (or only little) effect of dust extinction

Project YONSEIYOnsei Nearby Supernova Evolution Investigation


Observations for SNe Ia Host galaxies

- List of SNe Ia Sample

: YONSEI SN Catalogue (Y.-L. Kim, in prep.)

- Morphological classification

: E-S0 in NASA Extragalactic Database (NED)

Telescope & Instrument setup- Telescope : LCO Ireene du Pont 2.5m

- Instrument : Boller & Chiven (B & C) spectrograph

- Size of slit : 1.5’’ x 271’’ (long-slit)

- Resolution : ~ 7 Å/FWHM

- Wavelength coverage : 3800-7200 Å

- Total 6 observing runs (2011-2014)

I. Evidence for Downsizing among ETG HostsLong-slit spectroscopy using 2.5m telescope

Ireene du Pont 2.5m telescope

Early-type HostGalaxies of SNe Ia

(DSS image)

Total 68 nearby (0.01 < z < 0.06) early-type host galaxies

(27 ETG hosts observed in the southern hemisphere)

mass and properties of SNe Ia ETG hosts

+ : the position of SN Ia


I. Evidence for Downsizing among ETG HostsDetermination of Stellar Population Age & Metallicities

Reduction of Long-slit Spectra

with IRAF

Weak Emission correction

: GANDALF(Sarzi + 2006)

Line Measurement: lick_ew in EZ_age(Graves & Schiavon 2008)

Velocity dispersion (σv), Hβ,

Data Reduction & Analyses

0.01 < z < 0.06 11 < B < 18 Hβ

Old

Metal Poor

Metal Rich

Young YEPS

Fully-calibrated spectra of NGC 4493

Determination of Age & Metallicities


I. Evidence for Downsizing among ETG HostsCorrelation between velocity dispersion & stellar population age of host galaxies

Age ∝ σv1.56 Age ∝ σv2.45

Age ∝ σv2.54 Age ∝ σv2.11

Significance of Non-zero slope:3.3σ

Significance

: 4.0σ

The posterior distribution of slope from Markov ChainMonte Carlos (MCMC) analysis

Significance

: 4.1σ

Significance

: 4.1σ

For the first time in the host galaxies studies : a significant (~ 3.9 σ) correlation between mass and age (Age ∝ σv

2.17)No correlation between metallicities and velocity dispersion


II. Age of Host Galaxies & Hubble Residual of SNe IaLong-slit spectroscopy using MMT 6.5m

Total 68 nearby host galaxies

(0.01 < z < 0.06)

27 in southern hemisphere

+ ~ 40 new hosts observed

in the northern hemisphere

(Overlapped : 6 galaxies)

PAPER I

Early-type Host Galaxies of Type Ia Supernovae. I. Evidence for Downsizing

Kang, Y., Kim, Y.-L., Lim, D., Chung, C., & Lee, Y.-W.2016, ApJS, 223, 7

Host Galaxies :Mass

Host Galaxies :Age

SNe Ia : Hubble Residual

Significant (~3.9σ) correlation

more massive galaxy: ∼6 Gyr older

More massive hosts : ~0.1 mag brighter SNe Ia

10 Gyr older host galaxies →~ 0.16 mag brighter SNe Ia

(PAPER II : Kang et al., in prep.)

We need more direct investigation!Pop. Age vs. HR

origin of the host mass and HR correlation a population age effect?

More host sample in the northern hemisphere

“Downsizing”


Telescope & Instrument setup

- Telescope : MMT 6.5 m Telescope

- Instrument : Blue Channel Spectrograph

- Size of slit : 1.5 x 180 ’’ (long-slit)

- Resolution : ~ 8 Å/FWHM

- Wavelength coverage : 3400 - 8000 Å

- Total 3 Observing runs

: including 1 night from K-GMT Science Program

(Prop. ID : mmt_2014_00002, PI: Y.-L. Lee)

- 2014-2015 : 29 hosts

- 2016 : 15 hosts

II. Age of Host Galaxies & Hubble Residual of SNe IaObservation & Analyses

Hβ

Old

Young

Metal Poor

Metal RichMMT 6.5m

YEPS

Fully-calibrated spectra of NGC 2258

Determination of Age & Metallicities


Stellar Population Age of Host Galaxies vs. Hubble Residual of SNe Ia

II. Age of Host Galaxies & Hubble Residual of SNe IaPreliminary results

If confirmed, implies the luminosity evolution of SNe Ia

plays a major role in the systematic uncertainties of the cosmology

*Hubble Residual : SALT2 Light curve fitter (Jha et al. 2007)

Hubble

Res

idual

(m

ag)

Age (Gyr)

Hubble

Res

idual

(m

ag)

Age (Gyr)


Passive host galaxies beyond z > 0.05

- Obtaining more ETG/Passive sample at higher z ( > 0.05)

- The pre-stage for high-z SNe Ia host survey

- Passive host galaxies (0.05 < z < 0.5) of SNe Ia samples

a) SDSS-II Survey (Frieman et al. 2008; Sako et al. 2008)

b) Pan-STARR1 Survey (PS1, Rest et al. 2014)

c) SuperNova Legacy Survey 3(SNLS3, Guy et al. 2010)

Observations

A) MMT 6.5 m telescope Blue Channel Spectrograph (BCS)

Prop. ID : MMT-2014-00002 (PI: Y.-W. Lee)

: 2 galaxies, 1 night

B) Gemini 8.1m telescope GMOS-N&S

Prop. ID : GS-2015B-Q-41 (PI: Y.-W. Lee)

: 2 galaxies, 2 of 6 hour (due to the bad weather)

Prop. ID : GN-2016A-Q-51 (PI: Y.-W. Lee)

: 3 galaxies, 8 hour

III. Observations for Passive host galaxies beyond z > 0.05MMT 6.5m & Gemini 8.1m from K-GMT SCIENCE PROGRAM

Gemini 8.1m

Rest et al. 2014


III. Observations for Passive host galaxies beyond z > 0.05 Flux-Calibrated Spectra of Passive Host Galaxies

SDSS-II SN 2MASX J14564322+0919361z ~ 0.08

MMT/BCS

+

SN 2005fh

SDSS-II SN 2MASXJ2317297.3+0025473z ~ 0.119

+PS1-10jp

PS1 SN SDSS J141718.46+535841.5z ~ 0.387

MMT/BCSGMOS-S

GMOS-N

SNLS SN SDSS J100047.40+015908.5z ~ 0.45


“Evolution-free and dust-free” dark energy test at high-z

- Including Passive SNe Ia host galaxies in 0.5 < z < 1.0

- Comparing old pop. of low-z host & young pop. high-z host

- Hδ, Hγ, Fe lines (4000-7000Å in rest frame) → GMT/GMACS long-slit mode

“Evolution-free & Dust-free” dark energy test in Giant Magellan Telescope Era

참조 : K-GMT 과학백서 2015

“GMT를이용한 Ia 초신성의광도진화연구와이를통한암흑에너지의본질및진위규명”

이영욱, 강이정, 김영로, 정철

Credit. Y.-L. Kim

MMT

Hicken et al. (2009)

Gemini

GMT

du pont 2.5

Ωm =0.27,ΩΛ =0.00

du pont 2.5

GMT

MMTGemini

Backup Slides


ResultsVelocity dispersion and [M/H] of host galaxies

[M/H] ∝ σv0.70[M/H] ∝ σv0.48

[M/H] ∝ σv0.00 [M/H] ∝ σv0.71

Significance of

Non-zero slope

:1.7σ

Significance

: 0.7σ

Significance

: 0.7 σ

Significance

: 2.3 σ

*1.3 σ w/o this deviant point

No significant correlation (∼81.25% probability, ∼1.6σ).


Preliminary resultsSpectra of Passive Host Galaxies beyond z > 0.05

SN ID Host Galaxy ID g (mag) z

SDSS J001124.57+004207.2 18.8 0.199

SN ID Host Galaxy ID g (mag) z

SN 2005fh 2MASX J23172973+0025473 18.6 0.119

+

SN 2006jz

+

SN 2005fh


Not yet!Even after these light curve correction, stillBrightness of SNe Ia depend on the Environments!

“Effective Standardizable Candle”

- Peak brightness – Light-curve shape relation

The Light-Curve Shape Parameters

- Universal? Evolution with z?

- Light Curve shape parameter in fitters

MLCS2k2 : Δ, Av, t0, …

SALT2 : mBMax, stretch factor x1,color c

The Basic Assumption of SNe Ia cosmology

After the light curve correction,

the look-back time evolution is negligible…?

IntroductionSNe Ia, as the standardizable candles

Perlmutter (2003)


“ Archeological Downsizing”

Bigger ETGs should have older stellar

populations than smaller ETGs

:The stars in more massive galaxies form

at an earlier epoch & over a shorter time span

Mass and Stellar Population Age of ETGs

Thomas et al. (2005)more massive galaxies formed earlier

Zhu et al. (2010)-1923 elliptical galaxies at z< 0.05 from SDSS- Good agreement with previous studies,

(but systematically younger, by ∼3Gyr)

Mass and Stellar Population Age of ETGs :”Downsizing”

Thomas et al. (2005)

Zhu et al. (2010)


[Z/H] vs. Hubble Residual


Determination of Luminosity-Weighted mean Age & Metallicity

- Using four different Evolutionary Population Synthesis (EPS) models

: Yonsei Evolutionary Population Synthesis model (YEPS, Chung et al. 2013)

Thomas et al. 2003 (TMB03), Thomas et al. 2011 (TMJ11), Schiavon 2007 (S07)

- Determine Age, [Fe/H], [α/Fe] and [M/H] iteratively

Determination for Stellar Population Age & Metallicity of Early-type galaxies

Young

Old

Metal Rich

Metal Poor

Hβ


\

Fully-calibrated Spectra ofNGC 4493, a Host galaxy of SN 1994M

— Flux-calibrated spectra— Emission removed spectra— Detected Emissions


Boller & Chivens Spectrograph (B&C Spectrograph)

Telescope:Focal ratio: f/7.5

Collimator:Focal length: 675 mm

Camera:Focal length: 140 mm

Scale:At Focal plane: 10.83 arcsec/mmAt Detector: 51.9 arcsec/mm (0.70

arcsec/pixel)Slit Length:

25 mm (271 arcsec)Detector:

Marconi#1: 2048 x 515 (13.5 µm pixels); Q.E. graph

B&C Spectrograph


Correction for Weak Emissions Gas AND Absorption Line Fitting (GANDALF)

Stellar Model TemplateMILES(Vazdekis et al. 2010)

Flux-Calibrated Galaxy Spectra

Stellar Kinematic ParametersRadial velocity (v)Velocity dispersion (σv)

Flux & Amp. of Emissions

Emission-cleaned SpectraGalactic ReddeningSchlafly & Finkbeiner (2011)

‘Gas AND Absorption Line Fitting’ (GANDALF, Sarzi et al. 2006)

: A simultaneous emission and absorption lines fitting algorithm

Week emission contamination in ETG

: low level of ionized gas likely caused by AGN or residual star formation

(e.g. Ho et al. 1997; Yi et al. 2005)

Outputs

the optimal combination of stellar template

the best-fit stellar model

‘Gas AND Absorption Line Fitting’GANDALF based on pPXF(Cappellari & Emsellem 04): Fitting and removal ofweak emission linesin [OIII] , and hydrogen lines


The Absorption Lines Measurement : Lick/IDS indices

LICK/IDS absorption line indices

- 25 Lick/IDS indices (Worthey et al. 1994)

- ‘lick_ew’ in ‘EZ_ages’ package

(Graves & Schiavon 2008)

: Transform from ours to the Lick/IDS system

- Velocity dispersion broadening correction

Age indicator

: Balmer line indices (Hβ)

Metallicity indicator

: ≣ (Fe5270 + Fe5535)/2

[α/Fe] indicator

: Mg b

Comparison of Lick indices with other studies

Lick/IDS standard stars (Worthey et al. 1994)


ResultsVelocity dispersion and [Fe/H] of host galaxies

[Fe/H] ∝ σv0.58 [Fe/H] ∝ σv0.24

[Fe/H] ∝ σv-0.13 [Fe/H] ∝ σv0.45

1.5σ

0.9 σ

1.1 σ

1.6 σ

*1.3 σ w/o this deviant pointweak correlation (∼77.30%, ∼1.3σ)


Slope of Correlation with log Velocity Dispersion (km/s)


Significance of Non-zero Slope with log Velocity Dispersion (km/s)

spectroscopic survey for the early-type host galaxies of type ia...

Documents