Stellar Populations in the Near-Infrared range

Modelling galaxies through cosmic times @ Kavli Institute for Cosmology in Cambridge

September 14, 2015

Sofia Meneses-Goytia

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

¡ NIR (not fully explored, yet)¡ cool, late-type stars (RGB + AGB)¡ Atomic and molecular features

¡ Prepare for JWST & E-ELT¡ Moving to NIR observations requires NIR models

2

Basic outline3

Men

eses

-Goy

tia e

t al.

2015

b (in

pre

ss)

Fits

Stellar spectral libraryIRTF spectral libraryRayner 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

4

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

2000400060008000

[Z/Z

⊙]

Teff (K)

-1.00.01.02.03.04.05.0

log

g

-1.00.01.02.03.04.05.0

log

g

-2.0

-1.5

-1.0

-0.5

0.0

0.5

[Z/Z

⊙]

parameters determinationflux calibrationresolution

Meneses-Goytia et al. 2015a (in press) and 2015b (in press)

Isochrones 5

Meneses-Goytia et al. 2015b (in press)

-2-1 0 1 2 3 4 5 6

3.4 3.5 3.6 3.7 3.8

log

g

log Teff (K)

10.0 Gyr

-2-1 0 1 2 3 4 5 6

3.3 3.4 3.5 3.6 3.7 3.8 3.9

log

g

log Teff (K)

1.0 Gyr

-2-1 0 1 2 3 4 5 6

3.4 3.6 3.8 4 4.2

log

g

log Teff (K)

0.1 GyrMarigo et al., 2008Girardi et al., 2000

BaSTI, 2012

-10

-5

0

5

100.4 0.6 0.8 1.0 1.2 1.4 1.6

K

(J-K)

Marigo et al., 2008

0.4 0.6 0.8 1.0 1.2 1.4 1.6(J-K)

Girardi et al., 2000

0.4 0.6 0.8 1.0 1.2 1.4 1.6(J-K)

BaSTI, 2012

-2-1 0 1 2 3 4 5 6

3.4 3.5 3.6 3.7 3.8

log

g

log Teff (K)

10.0 Gyr

-2-1 0 1 2 3 4 5 6

3.3 3.4 3.5 3.6 3.7 3.8 3.9

log

g

log Teff (K)

1.0 Gyr

-2-1 0 1 2 3 4 5 6

3.4 3.6 3.8 4 4.2

log

g

log Teff (K)

0.1 GyrMarigo et al., 2008Girardi et al., 2000

BaSTI, 2012

-2-1 0 1 2 3 4 5 6

3.4 3.5 3.6 3.7 3.8

log

g

log Teff (K)

10.0 Gyr

-2-1 0 1 2 3 4 5 6

3.3 3.4 3.5 3.6 3.7 3.8 3.9

log

g

log Teff (K)

1.0 Gyr

-2-1 0 1 2 3 4 5 6

3.4 3.6 3.8 4 4.2

log

g

log Teff (K)

0.1 GyrMarigo et al., 2008Girardi et al., 2000

BaSTI, 2012

The SSP models6

Rela

tive

flux

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

Meneses-Goytia et al. 2015b (in press)

SED of SSP models 7

Meneses-Goytia et al. 2015b (in press)

0.96

0.98

1.00

1.02

1.04

1.0 1.2 1.4 1.6 1.8 2.0 2.2 2.4

Ratio

s

Wavelength (µm)

GirS / MarSBaSS / MarSBaSS / GirS

1.0

2.0

3.0

F/F 1

.65

µm

+con

stan

t

MarSGirS

BaSS

Ca Fe PP C Pa Na Si C Ca Ni Pa Al Si Fe K Si C Ti Mg

Fe 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 >4

I I I I I �>4

I I I I I I I I I I I

I I I I I I

�[

?I I II I I I I 6

>[

?

I I I I?

0.95

0.97

0.99

1.01

1.03

1.1 1.3 1.5 1.7 1.9 2.1 2.3

Rat

ios

Wavelength (µm)

14.0 Gyr / 7.00 Gyr0.80

0.90

1.00

1.10

1.20

Rat

ios

7.00 Gyr / 1.00 Gyr14.0 Gyr / 1.00 Gyr

0.50

1.00

1.50

2.00

2.50

F/F 1

.65 µ

m+c

onst

ant

MarS

1.00 Gyr7.00 Gyr14.0 Gyr

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

GirS

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

BaSS

0.95

0.97

0.99

1.01

1.03

1.05

1.1 1.3 1.6 1.8 2.0 2.3R

atio

s

Wavelength (µm)

+0.2 dex / +0.0 dex

0.9

1.0

1.1

Rat

ios

+0.0 dex / -0.7 dex+0.2 dex / -0.7 dex

0.5

1.0

1.5

2.0

2.5

F/F 1

.65 µ

m+c

onst

ant

MarS

-0.7 dex+0.0 dex+0.2 dex

1.1 1.3 1.6 1.8 2.0 2.3Wavelength (µm)

GirS

1.1 1.3 1.6 1.8 2.0 2.3Wavelength (µm)

BaSS

colour vs. agecolour-colourindex vs. ageother authors

Comparison with early type galaxies¡ Mármol-Queraltó et al. (2009) & Silva et al. (2008) ¡ Low redshift ¡ Elliptical and S0 galaxies ¡ 60 ≤ σ ≤ 360 km s1¡ 12 field galaxies and two Fornax @ FWHM = 7.2 Å¡ 7 Fornax galaxies @ FWHM = 6.9 Å¡ 2 Fornax galaxies @ FWHM = 6.1 Å¡ 2.19 to 2.31 µm in K band

8

features

Galaxies vs. models

0.57

0.62

0.67

0.72

0.77

0.85 0.90 0.95 1.00

(J-H

)

(J-Ks)

0.14

0.19

0.24

0.29

(H-K

s)

50

100

150

200

250

300

350

(km

s-1

)

0.14

0.19

0.24

0.29

0.57 0.62 0.67 0.72 0.77(H

-Ks)

(J-H)

fieldFornax

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

2 Gyr7 Gyr

14 Gyr

9

0.70

0.90

1.10

1.30

1.50

1.17 1.18 1.19 1.20 1.21 1.22 1.23 1.24

Fe I

DCO

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr 50 100 150 200 250 300 350

(km

s−1

)

1.80

2.00

2.20

2.40

2.60

2.80

3.00

Ca

I

1.90 2.30 2.70 3.10 3.50 3.90 4.30Na I

0.10

0.30

0.50

0.70

1.16 1.18 1.20 1.22 1.24

Mg

I

DCO

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr

0.70

0.90

1.10

1.30

1.50

1.17 1.18 1.19 1.20 1.21 1.22 1.23 1.24

Fe I

DCO

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr 50

100

150

200

250

300

350

(km

s−1

)

1.80

2.00

2.20

2.40

2.60

2.80

3.00

Ca

I

0.10

0.30

0.50

0.70

Mg

I

1.70

2.10

2.50

2.90

3.30

3.70

4.10

Na

I

0.70 0.90 1.10 1.30 1.50Fe I

1.80 2.00 2.20 2.40 2.60 2.80 3.00Ca I

0.10 0.30 0.50 0.70 0.90Mg I

1.17

1.18

1.19

1.20

1.21

1.22

1.23

1.00 1.40 1.80 2.20 2.60 3.00 3.40

DC

O

H

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr

50

100

150

200

250

300

350

(km

s−1

)

1.50 2.50 3.50 4.50 5.50Mg b

0.100.200.300.400.500.600.700.80

Mg

I

Meneses-Goytia et al. 2015c (in prep)

Optical + NIR

1.17

1.18

1.19

1.20

1.21

1.22

1.23

1.00 1.40 1.80 2.20 2.60 3.00 3.40

D CO

H

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr

0.70

0.90

1.10

1.30

Fe I

1.80

2.00

2.20

2.40

2.60

2.80

3.00

Ca I

0.100.200.300.400.500.600.700.80

Mg

I1.90

2.30

2.70

3.10

3.50

3.90

4.30

Na I

2.50 4.50 6.50 8.50C24668

50 100 150 200 250 300 350 (km s−1)

1.50 2.50 3.50 4.50 5.50Mg b

10

1.17

1.18

1.19

1.20

1.21

1.22

1.23

1.00 1.40 1.80 2.20 2.60 3.00 3.40

DC

O

H

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr

50

100

150

200

250

300

350

(km

s−1

)

1.50 2.50 3.50 4.50 5.50Mg b

0.100.200.300.400.500.600.700.80

Mg

I

Meneses-Goytia et al. 2015c (in prep)

1.17

1.18

1.19

1.20

1.21

1.22

1.23

1.00 1.40 1.80 2.20 2.60 3.00 3.40

DC

O

H

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr

50

100

150

200

250

300

350

(km

s−1

)

1.50 2.50 3.50 4.50 5.50Mg b

0.100.200.300.400.500.600.700.80

Mg

I

Only NIR combo 11

1.171.181.191.201.211.221.23

0.85 0.90 0.95 1.00

D CO

(mag

)

(J−Ks)

0.10

0.30

0.50

0.70

Mg

I (Å)

1.802.002.202.402.602.803.00

Ca I

(Å)

0.700.901.101.301.50

Fe I

(Å)

1.802.202.603.003.403.804.20

Na I

(Å)

50 100 150 200 250 300 350 (km s−1)

0.57 0.62 0.67 0.72 0.77(J−H)

0.14 0.19 0.24 0.29(H−Ks)

fieldFornax

2 Gyr7 Gyr

14 Gyr

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

1.17

1.18

1.19

1.20

1.21

1.22

1.23

1.00 1.40 1.80 2.20 2.60 3.00 3.40

DC

O

H

fieldFornax

− 0.7 dex− 0.4 dex+ 0.0 dex+ 0.2 dex

2 Gyr7 Gyr

14 Gyr

50

100

150

200

250

300

350

(km

s−1

)

1.50 2.50 3.50 4.50 5.50Mg b

0.100.200.300.400.500.600.700.80

Mg

IM

enes

es-G

oytia

et a

l. 20

15c

(in p

rep)

Full-spectrum fittingwith single stellar population

12

050

100150200250300350400

0 50 100 150 200 250 300 350 400

(km

s−1

) MQ

09

(km s−1)

−0.75

−0.45

−0.15

0.15

0.45

0.75

−0.75 −0.45 −0.15 0.15 0.45 0.75

[Z/Z

⊙] T

03

[Z/Z⊙]

02468

10121416

0 2 4 6 8 10 12 14 16

Age

(Gyr

) T03

Age (Gyr)

−0.75

−0.45

−0.15

0.15

0.45

0.75

−0.75 −0.45 −0.15 0.15 0.45 0.75

[Z/Z

⊙] V

03

[Z/Z⊙]

02468

10121416

0 2 4 6 8 10 12 14 16

Age

(Gyr

) V03

Age (Gyr)

−0.75

−0.45

−0.15

0.15

0.45

0.75

−0.75 −0.45 −0.15 0.15 0.45 0.75

[Z/Z

⊙] T

16

[Z/Z⊙]

02468

10121416

0 2 4 6 8 10 12 14 16

Age

(Gyr

) T16

Age (Gyr)

fieldFornax

models limitsESO382−G016 − MarS

1 10Age (Gyr)

−0.6

−0.4

−0.2

0.0

0.2

[ Z/Z

O · ]

2/DOF

6.21e−05 8.40e−05 1.06e−04 1.28e−04 1.50e−04 1.72e−04 1.94e−04

Meneses-Goytia et al. 2015c (in prep)

ESO382−G016

2.20 2.22 2.24 2.26 2.28 2.30Wavelength, µm

0.6

0.7

0.8

0.9

1.0

1.1

Rel

ativ

e flu

x

specifics

Non-classical stellar populationsand AGB stars

0.00

0.20

0.40

0.60

0.80

1.00

90 150 210 330

Nor

mal

ised

wei

ght

fiel

d ga

laxi

es

(km s−1)

8.4 Gyr0.2 dex

7.9 Gyr0.2 dex

9.7 Gyr0.2 dex

7.9 Gyr0.2 dex

0.00

0.20

0.40

0.60

0.80

1.00

Nor

mal

ised

wei

ght

For

nax

gala

xies

12.0 Gyr0.2 dex

11.5 Gyr0.2 dex

7.9 Gyr0.2 dex

7.9 Gyr0.2 dex

0.00

0.20

0.40

0.60

0.80

1.00

7.9 8.9 10.0 11.2 12.6 14.1

Nor

mal

ised

wei

ght

cla

ssic

al S

SP a

t 0.2

dex

Age (Gyr)

SSP with MS up to RGB tipAGB

0.85

0.90

0.95

1.00

1.05

50 100 150 200 250 300 350

2 non−c

lass

ical

/ 2 c

lass

ical

(km s−1)

fieldFornax

13

Men

eses

-Goy

tia e

t al.

2015

c (in

pre

p)

-1.0

0.0

1.0

2.0

3.0

4.0

5.0

2000400060008000

log

g

Teff (K)

C starsAGB

-2.0

-1.5

-1.0

-0.5

0.0

0.5

[Z/Z

⊙]

Summary¡ DCO è AGB stars indicator

¡ é(J − K) è younger age and/or higher metallicities

¡ Field galaxies: é DCO + é AGB + é(J-K)¡ undergone more extended star formation episodes

¡ Na I is strongly enhanced ¡ Bottom-heavy IMF (é dwarfs) + α-enhancement

¡ Early-type galaxies are more complex

¡ Single stellar populations are not enough¡ Detailed AGB treatment¡ Different IMFs¡ Multiple flexible populations¡ Chemical evolution models¡ Cosmological simulations

14

Thank you

Modelling galaxies through cosmic times @ Kavli Institute for Cosmology in Cambridge

September 14, 2015

16

Single Stellar Population models

¡ Single Stellar Population (SSP) models are tools forinterpreting the observed (stellar) light

¡ Single-age single-metallicity models¡ All stars are formed at the same time, with distribution in mass

given by an Initial Mass Function (IMF), with identical chemicalcomposition

17

Spectral Energy Distribution (SED)¡ SSP spectra

¡ Analyze galaxy spectra adapting models to the characteristicsof 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

18

Paper I –Preparation of the IRTF spectral stellar library¡ The library

¡ Determination of stellar parameters ¡ Full−spectrum fitting method¡ Teff and NIR−colour relations¡ Selection of the atmospheric parameters¡ Comparison with recent work

¡ Flux calibration

¡ Determining the spectral resolution

10000 12500 15000 17500 20000 22500 25000Wavelength (Å)

Kselec

J H Katomic Kmolecular

FWHM

Parameters

19

Parameters determinationFull-spectrum fitting

20

Men

eses

-Goy

tia e

t al.

2015

a (in

pre

ss)

-1.0

0.0

1.0

2.0

3.0

4.0

5.0

250035004500550065007500lo

g g

Teff (K)

IRTF templatesMQ08 stars

-3

-2.5

-2

-1.5

-1

-0.5

0

0.5

[Z/Z

⊙]

-500-250

0250500750

1000

4000 5000 6000 7000 8000T e

ff (K

)

FSF Teff (K)

-2

-1

0

1

2

-1 -0.5 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5

log

g

FSF log g

-1

-0.5

0

0.5

1

-0.75 -0.5 -0.25 0 0.25 0.5

[Z/Z

⊙]

FSF [Z/Z⊙]

C97 + S10C07

Parameters determinationColour-temperature relations

21

Men

eses

-Goy

tia e

t al.

2015

a (in

pre

ss)

1000

2000

3000

4000

5000

6000

7000

8000

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0

T eff

(K)

(J-K)

A96 dwarfsR13 M dwarfsP13 L dwarfsP13 T dwarfs

A99 giantsH00 M giants

K05 late-type giants

-1000-500

0500

1000150020002500

2000 3000 4000 5000 6000 7000 8000

T eff

(K)

C07 system Teff (K)

C97 + S10C07

Parameters determinationComparisons with literature

22

Meneses-Goytia et al. 2014a (in press)

1000

2000

3000

4000

5000

6000

7000

8000

F0 G0 K0 M0 L0 T0

T eff

(K)

spectral type

supergiantsAB supergiants

giantsdwarfs

3000

4000

5000

6000

7000

8000

FSF

T eff

(K)

C97 + S10C07

-1000

0

1000

4000 5000 6000 7000 8000

T eff

(K)

C07 system Teff (K)

-1

0

1

2

3

4

5

6

FSF

log

g

C97 + S10C07

-101

-1 0 1 2 3 4 5 6

log

g (d

ex)

C07 system log g (dex)

-1

-0.5

0

0.5

1

FSF

[Z/Z

⊙]

C97 + S10C07

-1-0.5

00.5

1

-1 -0.5 0 0.5 1

[Z/Z

⊙]

C07 system [Z/Z⊙]1000

2000

3000

4000

5000

6000

7000

8000

CTR

Tef

f (K)

C97 + S10C07

-1000

0

1000

1000 2000 3000 4000 5000 6000 7000 8000

T eff

(K)

C07 system Teff (K)

-600-300

0300600

1500 2500 3500 4500 5500 6500 7500T e

ff (K

)This work Teff (K)

-1.0-0.50.00.51.0

-0.5 0.5 1.5 2.5 3.5 4.5

log

g

This work log g

-1-0.5

00.5

1

-0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8

[Z/Z

⊙]

This work [Z/Z⊙]

IRTF-C07IRTF

0

1

2

3

4

53.43.63.844.24.44.6

log

g

log Teff (K)

B0

B0

A0

A0

F0

F0

F5

G0

G0

K0

K0

K0

M0

M0

M0

IaIab

IbII

IIIIV

VZAMS

III

Parameter coverage 23-1.0

0.0

1.0

2.0

3.0

4.0

5.0

10002000300040005000600070008000

log

g

Teff (K)

-3

-2.5

-2

-1.5

-1

-0.5

0

0.5

[Z/Z

⊙]

Meneses-Goytia et al. 2015a (in press)

0

20

40

60

80

100

120

140

160

-2.7 -2.3 -1.9 -1.5 -1.1 -0.7 -0.3 0.1 0.5

N

[Z/Z⊙]

Testing the flux calibration 24

0.0

0.5

1.0

-0.5 0.0 0.5 1.0 1.5 2.0

(J-H

)

(J-K)

3.3

3.6

3.9

4.2

4.5

log

T eff

-0.2

0.0

0.2

0.5

0.8

(H-K

)3.3

3.6

3.9

4.2

4.5

log

T eff

-0.2

0.0

0.2

0.5

0.8

0.0 0.5 1.0

(H-K

)

(J-H)

IRTFPickles

3.23.43.63.84.04.24.44.6

log

T eff

-0.50.00.51.01.52.02.53.0

3.0 3.4 3.8 4.2 4.6

(J-K

)

log Teff

-2.3-1.8-1.3-0.8-0.30.2

[Z/Z

⊙]

0.0

0.5

1.0

1.5

(J-H

)

-2.3-1.8-1.3-0.8-0.30.2

[Z/Z

⊙]

-0.5

0.0

0.5

1.0

1.5

(H-K

)

IRTFPickles

-2.3-1.8-1.3-0.8-0.30.2

[Z/Z

⊙]

Meneses-Goytia et al. 2015a (in press)

Spectral resolution and radial velocity

25

Meneses-Goytia et al. 2015a (in press)

1.05•104 1.10•104 1.15•104 1.20•104 1.25•104 1.30•104 1.35•104Wavelength, Å

1.4

1.6

1.8

2.0

2.2

2.4

2.6

2.8

Rel

ativ

e flu

x

1.50•104 1.55•104 1.60•104 1.65•104 1.70•104 1.75•104Wavelength, Å

1.0

1.2

1.4

1.6

1.8

Rel

ativ

e flu

x

1.95•104 2.00•104 2.05•104 2.10•104Wavelength, Å

0.6

0.7

0.8

0.9

1.0

1.1

Rel

ativ

e flu

x

2.15•104 2.20•104 2.25•104 2.30•104 2.35•104Wavelength, Å

0.50

0.55

0.60

0.65

0.70

0.75

0.80

Rel

ativ

e flu

x

26

0.0

0.2

0.4

0.6

N/N

tota

l

FWHM = 5.9 ± 0.3 Å

0.0

0.2

0.4

0.6

N/N

tota

l

FWHM = 7.6 ± 0.3 Å

0.0

0.2

0.4

0.6

N/N

tota

l

FWHM = 9.3 ± 0.6 Å

0.0

0.2

0.4

0.6

0 4 8 12 16

N/N

tota

l

FWHM (Å)

FWHM = 9.7 ± 0.9 Å

0.0

0.2

0.4

0.6

N/N

tota

l

RV = −4.1 ± 6.6 km s−1

0.0

0.2

0.4

0.6

N/N

tota

l

RV = −8.5 ± 8.0 km s−1

0.0

0.2

0.4

0.6

N/N

tota

l

RV = −13.3 ± 8.7 km s−1

0.0

0.2

0.4

0.6

−50.0 −30.0 −10.0 10.0 30.0 50.0

N/N

tota

l

Radial Velocity (km s−1)

RV = −13.9 ± 8.1 km s−1

1000

1500

2000

2500

3000

3500

4000

4500

10000 12500 15000 17500 20000 22500 25000

R =

/

Wavelength (Å)

0

2

4

6

8

10

12

14

10000 12500 15000 17500 20000 22500 25000

FWH

M (Å

)

Wavelength (Å)

Men

eses

-Goy

tia e

t al.

2015

a (in

pre

ss)

Paper II –Synthesis models¡ Single stellar population synthesis models ¡ The IRTF spectral library¡ Initial mass function¡ Isochrones

¡ Model predictions and discussion ¡ Spectral energy distributions¡ Integrated colours¡ Line-strength indices

¡ Comparisons with other authors

27

28Integrated colors vs. age

0.1

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

G04C07P08

1 10Age (Gyr)

GirS

1 10Age (Gyr)

BaSS

Men

eses

-Goy

tia e

t al.

2015

b (in

pre

ss)

Colours-colour diagrams 29

Men

eses

-Goy

tia e

t al.

2015

b (in

pre

ss)

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

Line-strength indices vs. age 30

Men

eses

-Goy

tia e

t al.

2015

b (in

pre

ss)

1.15

1.17

1.19

1.21

1.23

1.25

1 10

DC

O (m

ag)

Age (Gyr)

−0.1

0.1

0.3

0.5

Mg

I (Å)

1.8

2.0

2.2

2.4

2.6

Ca

I (Å)

0.9

1.1

1.3

1.5

1.7

Fe I

(Å)

1.7

2.0

2.3

2.6

2.9

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 31M

enes

es-G

oytia

et a

l. 20

15b

(in p

ress

)

0.90

1.00

1.10

1.20

1.1 1.3 1.5 1.7 1.9 2.1 2.3

Rat

ios

Wavelength (µm)

M09 / ModelC12 / Model

0.2

0.6

1.0

1.4

1.8

F/F 1

.65 µ

m+c

onst

ant

MarS

ModelM09C12

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

GirS

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

BaSS

0.90

1.00

1.10

2.20 2.24 2.28 2.32 2.36 2.40

Rat

ios

Wavelength (µm)

M09 / ModelC12 / Model

0.20

0.25

0.30

0.35

0.40

0.45

F/F 1

.65 µ

m+c

onst

ant

MarS

ModelM09C12

2.22 2.26 2.30 2.34 2.38Wavelength (µm)

GirS

2.20 2.24 2.28 2.32 2.36 2.40Wavelength (µm)

BaSS

0.90

1.00

1.10

1.20

1.1 1.3 1.5 1.7 1.9 2.1 2.3

Rat

ios

Wavelength (µm)

M09 / ModelC12 / Model

0.2

0.6

1.0

1.4

1.8

F/F 1

.65 µ

m+c

onst

ant

MarS

ModelM09C12

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

GirS

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

BaSS

Comparison with other authors 32

Meneses-Goytia et al. 2015b (in press)

0.80

0.90

1.00

1.10

1.20

1.30

1.40

1.1 1.3 1.5 1.7 1.9 2.1 2.3

Rat

ios

Wavelength (µm)

M09 / Model

0.2

0.6

1.0

1.4

1.8

F/F 1

.65 µ

m+c

onst

ant

MarS

ModelM09

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

GirS

1.1 1.3 1.5 1.7 1.9 2.1 2.3Wavelength (µm)

BaSS

Comparison with other authors 33

Meneses-Goytia et al. 2015b (in press)

1.80

2.10

2.40

2.70

3.00

3.30

3.60

3.90

4.20

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 Gyr

1.80

2.10

2.40

2.70

3.00

3.30

3.60

3.90

4.20

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

C123 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

1.2

(J-K

)

MarSGirS

BaSSV10C12M09

BC03

Paper III –Deciphering the stellar content of early-type galaxies¡ The data sample

¡ Single stellar population synthesis models

¡ Stellar population analysis ¡ Integrated colours and line-strength indices

¡ Fitting spectral energy distributions¡ Influence of AGB stars in early-type galaxies

34

Integrated colours and line-strength indices

0.810.830.850.870.890.910.930.950.970.99

1.80 2.00 2.20 2.40 2.60

(J−K

s)

log (km s−1)

0.560.600.640.680.720.760.80

(J−H

)

0.130.150.170.190.210.230.250.270.29

(H−K

s)

fieldFornax

35

1.181.191.201.211.221.231.24

1.80 2.00 2.20 2.40 2.60

DC

O (m

ag)

log (km s−1)

0.1

0.3

0.5

0.7

0.9

Mg

I (Å)

2.1

2.3

2.5

2.7

2.9

Ca

I (Å)

0.7

0.9

1.1

1.3

Fe I

(Å)

2.3

2.7

3.1

3.5

3.9

4.3

Na

I (Å)

fieldFornax

Men

eses

-Goy

tia e

t al.

2015

b (in

pre

ss)

Comparison with other authors

36

Meneses-Goytia et al. 2015b (in press)