IoA @ Cambridge February 26, 2014 Sofia Meneses-Goytia · 2020. 5. 21. · Meneses-Goytia et al. 2014a (submitted) Their characteristics 12 Meneses-Goytia et al. 2014a (submitted)

Single Stellar Populations models in the Near-Infrared range

R. F. Peletier, S. C. Trager

IoA @ Cambridge

February 26, 2014

Sofia Meneses-Goytia

Motivation

 Galactic evolution of “far away” galaxies  Close enough to obtain integrated spectra

 Light at different wavelengths gives information about the stars:   In the NIR cool stars

 Prepare for ELT´s, JWST  Moving to NIR observations requires NIR models

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Spectral Energy Distribution (SED)

  SSP spectra

 Analyze galaxy spectra adapting models to the characteristics of the data   Smoothed to match the resolution of the data and galaxy internal

velocity dispersion

  Full spectrum comparison of a particular set of features, measured on both, the galaxy spectrum and the SSP SEDs.

  Insight into   Ages   Metallicities   Abundance ratios   IMF (not easily probed in resolved systems)   Kinematic parameters determination

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Near–Infrared range  Importance   Early type galaxies / old populations  Contribution of AGB and late phases often dominate the

spectra

  Break age/metallicity degeneracy (potentially)

 Disadvantages  Atmospheric telluric absorption  Varying IR background

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Basic outline 5

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Fits

Basic outline 6

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Fits

Stellar spectral library IRTF spectral library Rayner et al. 2009 and Cushing et al. 2005

  210 stars (292 spectra)

  FWHM varies with wavelength

  0.8 to 2.5 μm or 5.2 μm

  F, G, K and M stars

7

Meneses-Goytia et al. 2014b (submitted)

-3.0-2.5-2.0-1.5-1.0-0.50.00.5

3000450060007500

[Z/Z

!]

Teff (K)

-1.00.01.02.03.04.05.0

log

g

-1.00.01.02.03.04.05.0

log

g

-3.0-2.5-2.0-1.5-1.0-0.50.00.5

[Z/Z

!]

Parameters determination Full-spectrum fitting

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Color-temperature relations

Testing the flux calibration 9

Meneses-Goytia et al. 2014a (submitted) More…

Determining the resolution 10

Meneses-Goytia et al. 2014a (submitted)

More…

The SSP models 11

Re

lativ

e fl

ux

Wavelength (μm)

  Population of stars with a common age and metallicity   For each star

  Mass   Atmospheric parameters   Spectrum   Stellar class + type

  Total (stellar) mass of the population


Their characteristics 12


SED of SSP models 13


0.96

0.98

1.00

1.02

1.0 1.2 1.4 1.6 1.8 2.0 2.2 2.4

Ratio

s

Wavelength (!m)

GirS / MarSBaSS / MarSBaSS / GirS

1.0

2.0

3.0

F/F 1

.65 !

m+c

onst

ant

MarSGirS

BaSSCa Fe PP C Pa Na Si C Ca Ni Pa Al Si Fe K Si C Ti M

gFe Ni Si

Ca Fe Mg

Ca Al K

Br C C Ni Si Fe Al Si Br Na Fe Ca Mg

CO

I I II I

I I I I I

I I I I I I I I I I I

I I I I I I

I I II I I I I

I I I I

14

0.2

0.3

1 10

(H-K

)

Age(Gyr)

0.6

0.7

0.8

(J-H

)

0.8

1.0

1.2

(J-K

)

MarS

- 0.7 dex- 0.4 dex+ 0.0 dex+ 0.2 dex

G04P08

1 10Age (Gyr)

GirS

1 10Age (Gyr)

BaSS

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Integrated colors from the SEDs

Integrated colors from the SEDs 15

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0.1

0.2

0.3

0.62 0.67 0.72 0.77

(H-K

)

(J-H)

0.1

0.2

0.3

0.82 0.92 1.02

(H-K

)

(J-K)

0.62

0.67

0.72

0.77

(J-H

)MarS

F78- 0.7 dex- 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr 7 Gyr

14 Gyr

0.62 0.67 0.72 0.77(J-H)

0.82 0.92 1.02(J-K)

GirS

0.62 0.67 0.72 0.77(J-H)

0.82 0.92 1.02(J-K)

BaSS

Indices from the SEDs 16

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1.16

1.21

1.26

1 10

DC

O (m

ag)

Age (Gyr)

0.1

0.1

0.3

Mg

I (Å)

1.8

2.3

2.8

Ca

I (Å)

0.9

1.4

1.9Fe

I (Å

)1.8

2.3

2.8

3.3

Na

I (Å)

MarS

0.7 dex 0.4 dex

+ 0.0 dex+ 0.2 dex

1 10Age (Gyr)

GirS

1 10Age (Gyr)

BaSS

Comparison with other authors 17


2.20

2.40

2.60

2.80

3.00

3.20

3.40

3.60

1.13 1.14 1.15 1.16 1.17 1.18 1.19 1.20 1.21 1.22 1.23

Na I

DCO

MQ09MarSGirS

BaSS2 Gyr7 Gyr

14 GyrC12

3 Gyr7 Gyr

14 Gyr

0.1

0.2

0.3

1 10

(H-K

)

Age (Gyr)

0.6

0.7

0.8

(J-H

)

0.8

1.0

(J-K

)

MarSGirS

BaSSV10C12M09

BC03

More…

Comparison with early type galaxies

 Mármol-Queraltó et al. 2009   14 bright elliptical

galaxies (12 field, 2 Fornax)

  2.19 to 2.31 μm   FWHM 7.14 Å

  Silva et al. 2008   9 Fornax galaxies   2.19 to 3.43 μm   FWHM 6.90 Å

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F (a

rbitr

ary

un

its)

Indices from the SEDs 19

1.5

2.5

3.5

4.5

0.65 0.75

Na

I

(J H)

1.18

1.22

0.8 1.0 1.1

DC

O

(J Ks)

MarS

MQ09MQ09 Fnx

0.7 dex 0.4 dex

+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr

0.65 0.75(J H)

0.8 1.0 1.1(J Ks)

GirS

0.65 0.75(J H)

0.8 1.0 1.1(J Ks)

BaSS

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Comparisons – an example 20

Through full spectral fitting using pPXF (Cappellari & Emsellem 2004)

– 0.40 dex ~ 4 Gyr

Meneses-Goytia et al. 2014c (in prep)

NGC3605

2.20 2.22 2.24 2.26 2.28 2.30Wavelength, µm

0.5

0.6

0.7

0.8

0.9

1.0

1.1

Rela

tive flu

x

Velocity dispersion 21

σ (

km/s

) –

pre

sen

t w

ork

σ (km/s) – Mármol-Queralto et al. 2009 σ (km/s) – HYPERLEDA

Meneses-Goytia et al. 2014c (in prep)

Conclusions   SED modeling in the NIR works

  Velocity dispersions agree with established methods in the optical

 Current models not sensitive to young populations   Insufficient parameter coverage IRTF   Intrinsic sensitivity NIR   Uncertainties due to AGB   With a combination with optical colors (?)

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Thank you

IoA @ Cambridge

February 26, 2014

Documents

IoA @ Cambridge February 26, 2014 Sofia Meneses-Goytia · 2020. 5. 21. · Meneses-Goytia et al. 2014a (submitted) Their characteristics 12 Meneses-Goytia et al. 2014a (submitted)