red stellar populationsred stellar populations

IR spectraIR spectra

abundance patterns & kinematics abundance patterns & kinematics

extreme environmentsextreme environments

-- galactic bulgegalactic bulge - young extragalactic clusters- young extragalactic clusters - SB galaxies- SB galaxies

resolvedresolved into single stars: • in galaxy fields up to a few Mpc• in stellar clusters within the LG

integratedintegrated: • stellar clusters up to a few Mpc

• galaxies pop synthesis multiple ages, metallicities

NGC1569 – SSCsNGC1569 – SSCs HHST – NICMOS

D = 2.2 MpcD = 2.2 Mpc

ddSSCSSC 100 mas100 mas

Aloisi et al. 2001, AJ 121, 1425Aloisi et al. 2001, AJ 121, 1425 Origlia et al. 2001, AJ 122, 815Origlia et al. 2001, AJ 122, 815

M31 – G1 M31 – G1 HST – ACS

D = 0.77 MpcD = 0.77 Mpc

ddG1G1 a few arcseca few arcsec

each sequence in the most suitable rangeeach sequence in the most suitable range hothot in the in the UV-opticalUV-optical, , coolcool in the in the IRIR

largerlarger bbaasseelliinne e

betterbetter definition of stellar & population parameters definition of stellar & population parameters

temperature, gravity, metallicity, mass, IMF, reddening etc.temperature, gravity, metallicity, mass, IMF, reddening etc. nebular nebular vsvs stellar contributions, mass loss, SF rates etc. stellar contributions, mass loss, SF rates etc.

each environment in the most suitable rangeeach environment in the most suitable range

metal poormetal poor, , low reddeninglow reddening (e.g. halos) in the (e.g. halos) in the UV-optical UV-optical metal richmetal rich, , high reddeninghigh reddening (e.g bulges) in the (e.g bulges) in the IRIR

Post-Main Sequence stars

Red Supergiant (RSG): 8-40 Mo, age 5-100 Myr

Asymptotic Giant Branch (AGB): <8 Mo, age>100 Myr

Red Giant Branch (RGB): <2 Mo , age > few Gyr

in the near IR dominate

the stellar luminosity of stellar clusters & normal galaxies

over the nebular & AGN emission in active galaxies

Teff < 5000 K

chemical abundances & abundance patterns of Fe,CNO, chemical abundances & abundance patterns of Fe,CNO, -elements -elements SF history, timescales, rates, etc., primordial SF history, timescales, rates, etc., primordial vsvs self-enrichment self-enrichment etc.etc.

radial velocities & velocity dispersionsradial velocities & velocity dispersions distances, masses, dynamical interactions etc.distances, masses, dynamical interactions etc.

near IRnear IR range crucial to study: range crucial to study:galaxy bulgesgalaxy bulgesextragalactic star clustersextragalactic star clustersyoung SSCs & star forming galaxies young SSCs & star forming galaxies host galaxies of both type I & II AGNshost galaxies of both type I & II AGNs

optimal spectral resolutionsoptimal spectral resolutions: :

stars & stellar clusters: 1-10 Km/sstars & stellar clusters: 1-10 Km/s galaxies: 10-100 Km/sgalaxies: 10-100 Km/s

neutral atomic lines neutral atomic lines Fe, Si, Ca, Mg, Ti, Al, NaFe, Si, Ca, Mg, Ti, Al, Na

OH, CO, CN molecular bands OH, CO, CN molecular bands very sensitive to very sensitive to CC, , OO & & NN abundances abundances

the SF history of a stellar system is imprinted the SF history of a stellar system is imprinted in their chemical abundance patterns in their chemical abundance patterns

elementselements: : O, Si, Ca, Mg,TiO, Si, Ca, Mg,Ti type II SNe type II SNe withwith massive progenitors massive progenitors

released released in thein the ISM ISM from thefrom the very beginning very beginning of theof the SF onset SF onset

Fe - group elementsFe - group elements type I SNe type I SNe withwith intermediate mass progenitors intermediate mass progenitors

C, N, s,r-process elementsC, N, s,r-process elements AGB AGB withwith low-intermediate mass progenitorslow-intermediate mass progenitors

released released in thein the ISM ISM afterafter 1 Gyr 1 Gyr from thefrom the SF onset SF onset

elements: O, Si, Ca, Mg, Ti elements: O, Si, Ca, Mg, Ti

[[ /F

e]/F

e]

0.00.0

0.30.3

0.50.5

[Fe/H][Fe/H]0.00.0-1.0-1.0-2.0-2.0

IMFIMF

SFRSFR

Galactic HaloGalactic Halostars formed from a gasstars formed from a gasmainly enriched by SNII mainly enriched by SNII on a relatively short timescale on a relatively short timescale

Galactic DiskGalactic Diskstars formed from a gasstars formed from a gasalso enriched by SNIa also enriched by SNIa on a much longer timescale on a much longer timescale

Galactic Bulge ?Galactic Bulge ?

Optical spectrasee e.g. Fullbright, McWilliam & Rich ‘06; Zoccali et al. ‘06

K giants: (V-K)0<3, Teff >4000 K red clump at V015

outer Bulge with Av < 2

M giants: severly affected by molecular blanketing & blendingIR spectra

K giants: too warm, faint lines

M giants: (V-K)0>3, Teff<4000 K RGB Tip inner Bulge, AIR negligible

lum

ino

sit

y

temperature

RGB Tip

HB

SURVEY of cluster & field M giants SURVEY of cluster & field M giants in collaboration with R.M. Rich & E. Valentiin collaboration with R.M. Rich & E. Valenti

H band H band (1.5-1.8 micron)(1.5-1.8 micron) echelle spectraechelle spectra with with NIRSPEC at Keck IINIRSPEC at Keck II

[/Fe] enhancement

elements: O, Si, Ca, Mg, Ti elements: O, Si, Ca, Mg, Ti

[[ /F

e]/F

e]

0.00.0

0.30.3

0.50.5

[Fe/H][Fe/H]0.00.0-1.0-1.0-2.0-2.0

IMFIMF

SFRSFR

Galactic HaloGalactic Halostars formed from a gasstars formed from a gasmainly enriched by SNII mainly enriched by SNII on a relatively short timescale on a relatively short timescale

Galactic DiskGalactic Diskstars formed from a gasstars formed from a gasalso enriched by SNIa also enriched by SNIa on a much longer timescale on a much longer timescale

Galactic Bulge, E galGalactic Bulge, E galhalo – like but at higher SFR halo – like but at higher SFR

NGC 6946NGC 6946WPC2@HST F555W F555W 6945 SSC6945 SSC

D = 5.9 Mpc

= 10.4 km/sM = 1.7 x 106 Mo

age = 10-15 Myr

L/M consistent with a Salpeter IMF

Larsen et al. 2001, ApJ, 556, 801

Larsen, Origlia, Brodie & Gallagher, 2006, MNRAS, 368, 10

= 9.1 km/s

[Fe/H] = -0.45 +/- 0.1

[Ca,Mg,Al/Fe] = +0.25 +/- 0.15

[O,Ti/Fe] = +0.29 +/- 0.10

[Si/Fe] = +0.08 +/- 0.18

[C/Fe] = -0.25 +/-0 .11

12C/13C = 8 +/- 2

NGC 6946 – SSC NGC 6946 – SSC

NIRSPEC@Keck R=25,000NIRSPEC@Keck R=25,000

… … calibrating suitable stellar abundance calibrating suitable stellar abundance tracers tracers

for integrated spectroscopy of distant for integrated spectroscopy of distant galaxiesgalaxies

velocity dispersion / rotationvelocity dispersion / rotation line line broadeningbroadening

in the visual range:SB galaxies severely contaminated

by nebular emission and AGN

in the near - IR range:SB galaxies poorly contaminated

by nebular emission and AGN

RSGs dominate the luminosity

diagnostics: stellar vs gaseous abundances

stars (red supergiants) in the IR: enrichment before the last burst of SF

hot gas in the X-ray with Chandra & XMM:real-time enrichment by the last burst of SF

cool gas in the visual:enrichment by the previous or the last burst of SF?it depends on the cooling & mixing timescales…

nnear–IRear–IR: TNG/NICS: TNG/NICS XXrayray: XMM RGS/MOS: XMM RGS/MOS

M 82M 82

NGC 253NGC 253

nnear–IRear–IR spectra spectra X-ray spectraX-ray spectra

Teff = 3800 – 4000 K log g = 0.5= 3 km/s

point sourcespoint sources

power law =0.8

NH = 8x1021 cm-2

diffuse hot gas

optically thin thermal plasma kT=0.7 kev

NH = 4x1021 cm-2

Teff = +/- 200 K

log g = +/- 0.5 = +/- 1 km/s

[X/H] = +/- 0.2 dex2 level

best-fit modelsbest-fit models

chemical enrichment by recursive bursts

oxygen puzzling…

[Fe/H] = [Fe/H] = 0.35 +/- 0.20.35 +/- 0.2

stars: [Si,Mg/Fe] = +0.4

[O/Fe] = +0.4

hot gas: [Si,Mg/Fe] = +0.5

[O/Fe] = 0.2

M 82M 82

[Fe/H] = [Fe/H] = 0.50 +/- 0.20.50 +/- 0.2

stars: [Si,Mg/Fe] = +0.3

[O/Fe] = +0.3

hot gas: [Si,Mg/Fe] = +0.7

[O/Fe] = 0.1

NGC 253NGC 253

Origlia et al. 2004, ApJ, 606, 862Origlia et al. 2004, ApJ, 606, 862

oxygen underabundance

working hypothesis

(Marcolini, , Strickland, D’Ercole, Heckman & Hoopes, 2005, MNRAS, 362, 626)

SNII winds interact with cool gas clouds & and heat them

heavier metals (Si, Mg etc.) form in the SNII wind

O forms in the outer region of the wind (OVII & OVIII soft XX) and/or in the heated clouds (OV & OVI UVUV)

IR spectroscopy crucial to measure star kinematics in type I AGNsIR spectroscopy crucial to measure star kinematics in type I AGNs

MMBHBH – – relationrelation

Merritt & Ferrarese 2001, ApJ, 547, 140Merritt & Ferrarese 2001, ApJ, 547, 140

Gebhardt e

t al. ‘

01

Gebhardt e

t al. ‘

01

Ferra

rese

& M

errit

t ‘0

0

Ferra

rese

& M

errit

t ‘0

0

MMBHBH

4.80.5

M/Lstellar :burst on/off

hosts of AGNshosts of AGNs

no nuclear SB in Seys 1no nuclear SB in Seys 1

nuclear SB in 30 – 40 % nuclear SB in 30 – 40 %

obscured / Seys 2obscured / Seys 2

Oliva et al., 1999, A&A 350, 4Origlia & Oliva, 2000, New Astr. Rev. 44, 25

((Cid Fernandes et al. 2001, ApJ 558, 81)Cid Fernandes et al. 2001, ApJ 558, 81)

35 type II Seyferts35 type II Seyferts morphological type: S0, Sa, Sbmorphological type: S0, Sa, Sb

stellar content: stellar content: 50%50% nuclear nuclear SBSB (< 1 kpc scale(< 1 kpc scale), ), 50%50% old SP old SP correlation correlation betweenbetween SB (H SB (H && AGN ([OIII]) luminosity AGN ([OIII]) luminosity

((Kauffman et al. 2003, MNRAS 346, 1055) Kauffman et al. 2003, MNRAS 346, 1055)

22,600 narrow-line AGNs22,600 narrow-line AGNs type 2 Seys type 2 Seys & & QSOs QSOs withwith same [OIII] same [OIII] and and zz have have similar hostssimilar hosts

in massive SB galaxies RSGs dominate over an underlying older SP

1.0 < [Fe/H] < 0.0, 8<age<50 Myr Teff 3600 – 4000 K

log g 0.0 – 1.0 3 5 km/s

< RSG > Teff = 3800 200 K

log g = 0.5 0.5 41 km/s

[A/H] = 0.2 dex

in the in the near IRnear IR: : young SPs:young SPs: red supergiants red supergiants intermediate/oldintermediate/old SPs:SPs: red giants red giants

stellar parameters:

< RSG > from young MC clusters

codecode: : Origlia et al. (1993 Origlia et al. (1993 2004model atmospheresmodel atmospheres: : ATLAS9, Johnson et al. ’80, NextGen, [Plez]ATLAS9, Johnson et al. ’80, NextGen, [Plez]stellar parametersstellar parameters: : near IR photometry + moleculesnear IR photometry + moleculesLTELTE

full spectral synthesisfull spectral synthesis equivalent width measurement of selected linesequivalent width measurement of selected lines

spectral fitting/equivalent width measurements < 0.1 dex< 0.1 dex

log gflog gf 0.2 0.2 0.1 dex 0.1 dex

random errors:random errors:

stellar parameters 0.1 - 0.2 dex0.1 - 0.2 dex

solar abundances 0.1 0.1 0.1 dex 0.1 dex

systematic errors:systematic errors:

nLTE correctionsnLTE corrections negligible at T>3000 Knegligible at T>3000 K

model atmospheres negligible, opacity dominated by Hnegligible, opacity dominated by H--

other sources of error:other sources of error:

• [OI] lines [OI] lines ( ( 6300,6364 6300,6364 Å ))• OI triplet OI triplet ( ( 7772,7774,7775 7772,7774,7775 Å ))

• OH molecular transitionsOH molecular transitions IR lines IR lines ( ( 1.5-1.8 1.5-1.8 mm ))

low temperatures, high metallicity low temperatures, high metallicity domaindomain

bulge

vertical abundance gradientsvertical abundance gradients ? ?

observing old SPs in the galactic centerobserving old SPs in the galactic center

self-enrichmentself-enrichment asas traced traced by by O-NaO-Na & & Mg-AlMg-Al anti-correlationanti-correlation? ? perhaps yes perhaps yes ……

Mg-Al anti-correlation

12C/13C 10 extra - mixing

halo

bulge

nebular spectranebular spectra

emission lines: [OII][OIII][NII][SII]

best ne ,Te diagnostics (e.g. McCall, 1984, MNRAS 208, 253):

ne I([SII] I([SII] Te [++] I([OIII] I([OIII]

Te [+] I([NII] I([NII]

emission lines: [OII][OIII][NII][SII]

best ne ,Te diagnostics (e.g. McCall, 1984, MNRAS 208, 253):

ne I([SII] I([SII] Te [++] I([OIII] I([OIII]

Te [+] I([NII] I([NII]

alternative Te diagnostics at high Z:(e.g. Pagel et al. , 1979, MNRAS, 189, 95

Storchi-Bergmann et al. 1994, ApJ429, 572)

empirical calibrations

alternative Te diagnostics at high Z:(e.g. Pagel et al. , 1979, MNRAS, 189, 95

Storchi-Bergmann et al. 1994, ApJ429, 572)

empirical calibrations

abundances at high Z:(McGaugh, 1991, ApJ 380, 140)

empirical calibrations

abundances at high Z:(McGaugh, 1991, ApJ 380, 140)

empirical calibrations

NGC 1569

BalmerBalmer jumpjump

HeII bumpHeII bump WR starsWR stars

few Myr old few Myr old

Gonzalez Delgado et al. 1997, ApJ 483, 705Gonzalez Delgado et al. 1997, ApJ 483, 705

SB galaxiesSB galaxies

8 SB galaxies

< [ / Fe] > = + 0.3 +/- 0.1 dex

< [ C / O ] > = - 0.5 +/- 0.2 dex

[12C / 13C] < 10

enhancement, enrichement by SNII C mixed in the stellar interiors

see also Read & Stevens 2002, MNRAS, 335, L36see also Read & Stevens 2002, MNRAS, 335, L36

[FeII][FeII] : shock excited, : shock excited, type II SNe type II SNe tracer tracer

Starburst99 modelsStarburst99 models

Origlia & Oliva 2000, A&A, 357, 61 Origlia & Oliva 2000, A&A, 357, 61

near IR near IR dust optically thindust optically thin

emission emission volume volume

LLdustdust ((SB SB ) ) LLdustdust ((AGN AGN ) ) / / NN

stellar clustersstellar clusters lessless efficient efficient thanthan

AGNAGN inin heating dust heating dust

why in AGNs & not in SBs?why in AGNs & not in SBs?TTdustdust 1000 1000

KK

RRdustdust 1 pc 1 pc

diagnostics : : optical photometry & spectroscopyoptical photometry & spectroscopy good for type II AGN not heavily obscured good for type II AGN not heavily obscured type I AGN hosts veiled by the AGN itselftype I AGN hosts veiled by the AGN itself

IR photometry & spectroscopyIR photometry & spectroscopy crucial to study obscured & type I AGNcrucial to study obscured & type I AGN

surveys : : optical: optical: SDSS + small size samples of type SDSS + small size samples of type II AGNII AGN

IR: IR: 2MASS2MASS ++ veryvery small size samples of type small size samples of type I & II AGNI & II AGN

KKVV

BBUU

RGBRGBAGBAGB

MSMS

MSMSMSMS

Renzini & Buzzoni 1986, Renzini & Buzzoni 1986, inin Spectral Evolution of GalaxiesSpectral Evolution of Galaxies, 195, 195Maraston 1998, MNRAS 300, 872Maraston 1998, MNRAS 300, 872

Woosley & Weaver, 1995, ApJS, 101, 181Woosley & Weaver, 1995, ApJS, 101, 181