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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
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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)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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?”
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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”
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
“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
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Backup Slides
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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).
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
“ 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)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
[Z/H] vs. Hubble Residual
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
\
Fully-calibrated Spectra ofNGC 4493, a Host galaxy of SN 1994M
— Flux-calibrated spectra— Emission removed spectra— Detected Emissions
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
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)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
Slope of Correlation with log Velocity Dispersion (km/s)
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K-GMT 중대형망원경사용자워크숍 2017. 03. 03. (Fri)
Significance of Non-zero Slope with log Velocity Dispersion (km/s)