the seds of quasar host - max planck society€¦ · quasar host galaxies kn ud j ahnk e astroph...

The

SE

Ds

ofquasar

hostgalaxies

Knud

JahnkeA

strophysikalischesInstitutP

otsdamG

alaxiesdivision

MP

E,26.02.2003

Nuclear

model

(Urry

&P

adovani1995)

narrow line region

relativistic jet

dusty torus

broad line region

nuclear black hole

accretion disk

The

SE

Ds

ofquasarhostgalaxies

Introduction

HE

1043–1346

z=0.068

Sb-S

cspiral

The

SE

Ds


Introduction

HE

1029–1401

z=0.085

E0

elliptical

The

SE

Ds


Introduction

Kno

wledg

e

quasarsare

rare:10

4com

paredto

fieldgalaxies

ofequalL(W

isotzki,Kuhlbrodt,Jahnke

2001)

massive

blackholes

(BH

)likely

inallgalaxies

masses

ofBH

connectedto

mass

ofsurroundinggalaxy

(Magorrian

etal.1998)coupled

evolutionofB

Hand

hostgalaxy!

short“dutycycle”

ofquasars

notanisolated

phenomenon!

quasarphase

snapshotofgalaxyevolution?

The

SE

Ds


Introduction

(McLure

&D

unlop2002)

The

SE

Ds


Introduction

morphology

–E

toS

c/SB

c,noIrr

–sym

metric

todisturbed

forhigher

L:m

oreE

,lessinteraction

andcom

panions(e.g.D

unlopetal.

2001,Kuhlbrodtetal.

2003)

luminosities

–correlation:

bulgeL

tonuclear

L(M

cLeodetal.

1999,McLure

etal.2001,2002)–

luminosity

function(LF

)com

patibleto

earlytype

fieldgalaxies

(Wisotzki,

Kuhlbrodt,Jahnke

2001)

interactiontrigger

foractivity?/!

supportinghierarchicalclustering

The

SE

Ds


Introduction

Spectral

information:

anew

dimension

apparentmorphology

vs.stellarcontentvs.gas

content

spectroscopicsigns

ofpasttidalinteraction

dynamics

spectralinformation

veryvaluable

The

SE

Ds


Introduction

Colour

andspectroscopic

studies

(multi-)colour

studies

–expensive

fewstudies

–contradictory

results(norm

alvs.blue)

spectroscopicstudies

–expensive

anddifficultdata

treatment

–larger

studies:B

orosonetal.1982–1985,N

olanetal.2001

The

SE

Ds


Introduction

Two

‘spectroscopic’

approaches

optical/NIR

multicolour

broadband

imaging

longspectralbaseline,coarse

data

on-nucleusspectroscopy

highresolution,shorter

baseline,expensive,difficultseparation

Problem

inboth

cases:extraction

ofthehostgalaxy

fluxS

olutionin

bothcases:

spatialmodelling

ofhostandnucleus

The

SE

Ds


Multicolour

imaging

The

SE

Ds


Multicolour

ima

ging

The

SE

Ds


Multicolour

imaging

observecom

pletelow

-zquasar

sample

inB

,V,R,I,J,H

,Ks

remove

nuclearlightcontribution

investigate

–m

orphologies(lightdistribution,ellipticities,arm

s,asymm

etries,...)–

colours(optical,optical–N

IR)

–stellar

populations(evolution

synthesism

odelfits)

compare

toinactive

galaxies

The

SE

Ds


Multicolour

imaging

Sam

pleselection

19quasars,

z0

2,selected

fromH

ES

,com

pletefrom

611deg

2,subsam

pleof

Kohler

etal.1997

137

V

��

168

217

MV

249

(H0

50km

s1

Mpc

1,q

00

5,Λ0)

The

SE

Ds


Multicolour

imaging

The

SE

Ds


Multicolour

imaging

Modelling

results

The

SE

Ds


Multicolour

imaging

Colours

B–V

V–

RR

–I

I–J

J–H

H–

KV

–K

Ellipticals

Inactive0.96

0.610.70

0.770.71

0.202.99

(0.12)Q

SO

hostsample

0.520.44

0.480.67

0.590.31

2.48(0.25)

∆0.44

0.170.22

0.100.12

–0.110.50

Disks

(Sb)

Inactive0.68

0.540.63

0.670.78

0.252.87

(0.36)Q

SO

hostsample

0.550.53

0.530.87

0.570.24

2.73(0.20)

∆0.13

0.010.10

–0.200.21

0.010.14

K-corrections:

Fukugita

etal.1995(optical),M

annuccietal.2001(N

IR)

inactivecolours:

Fukugita

etal.1995(optical),F

ioc&

Rocca-V

olmerange

1999(optical-N

IR,

NIR

-NIR

)

The

SE

Ds


Multicolour

imaging

The

SE

Ds


Multicolour

imaging

Stellar

populationm

odels

SS

Pm

odelfamily

byB

ruzual&C

harlot1996

–S

caloIM

F–

solarm

etallicity–

but:generalresults

notdependingon

choiceofm

odel!–

0.1,0.7,2,6,14G

yr+

continuousstar

formation

model(C

SF

)

1S

SP

fit:age

free

2S

SP

fit:0.1

Gyr

fixed,secondage

free,relativem

ixingfree

χ2

minim

isationfitting

to6/7

datapoints

The

SE

Ds


Multicolour

imaging

The

SE

Ds


Multicolour

imaging

Model

fittingresults

objectsw

ithB

missing

notreliable

1S

SP

:

–very

similar

fordisks

andellipticals

–only

1objecteach

preferring6

Gyr,none

14G

yr

0.1G

yr+

1S

SP

:

–allconsistentw

ith2

Gyr

andC

SF

–2%

of0.1G

yrrequired

byonly

2disks

intermediately

youngpopulations,also

forE

;evolvedpopulations

ruledout

consistentwith

VK

coloursalone

The

SE

Ds


Multicolour

imaging

Multicolour

ima

ging:sum

mar

y

disksand

ellipticalsfound

wide

rangeofm

orphologiesand

asymm

etries

M

��

M

�� correlation

confirmed

disks:largely

normal,slightly

bluerthan

inactiveS

b

ellipticals:

–as

blueas

latetype

disks–

SS

Pm

odelfittingconsistentw

ithC

SF

or2

Gyr

population

The

SE

Ds


On-nucleus

spectroscopy

The

SE

Ds


On-nucleus

spectroscopy

On-n

ucleusspectroscop

y

techniqueso

far:

–off-nucleus

spectroscopy,r

3avoiding

nucleusplus

removal

ofnuclear

residuals

drawbacks:

–controlofnuclear

residualsdifficult

–sam

plingfar

outsidenuclear

regionpotentially

boring

wanted:


–problem

:very

highcontrastnucleus–host

–solution:

spatialm

odelling,similar

toim

aging

The

SE

Ds


On-nucleus

spectroscopy

0054+144 (R

QQ

) WH

T

(Hughes

etal.2000,Hutchings

&C

rampton

1990)

The

SE

Ds


On-n

ucleusspectroscop

y

techniqueso

far:

–off-nucleus

spectroscopy,r

3avoiding

nucleusplus

removal

ofnuclear

residuals

drawbacks:

–controlofnuclear

residualsdifficult

–sam

plingfar

outsidenuclear

regionpotentially

boring

wanted:


–problem

:very

highcontrastnucleus–host

–solution:

spatialm

odelling,similar

toim

aging

The

SE

Ds


Multi-object-spectroscopy

vs.longslitspectroscopy

The

SE

Ds


r

λ

The

SE

Ds


veryim

portant:use

allinformation

available

–m

orphologicalparameter

inputfromim

aging–

sloww

avelengthdependence

ofparameters

PS

F:analyticalm

odelplusem

piricalcorrection

host:exponentialdisk

orde

Vaucouleurs

spheroidal

reductionofparam

etersin

successivesteps

finalstep:nuclear

andhostflux

onlyfree

parameters

2dnuclear

spectrumm

odel2d

hostgalaxyspectrum

The

SE

Ds


r

λ

The

SE

Ds


Quality

offit

diagnostics

resultingspectra

shouldbe

positive

noforbidden

linesin

absorption

broadem

issionlines

notinabsorption

shapeofresidual(=

quasar–nucleus–host)

broadband

coloursneed

tobe

reconstructable

comparing

differentPS

Fstars

comparing

differentimages

The

SE

Ds


The

“EF

OS

Csam

ple”

8objectsubsam

pleofm

ulticoloursam

ple

ES

O3.6m

with

EF

OS

C:

–w

avelengthrange:

3800–8000A

–resolution:

250–

0.314/pixel

–integration

time:

1200–4800s

morphologicalparam

etersexisting

The

SE

Ds


The

“FO

RS

sample”

10(total20)

objectsfrom

HE

S,

z0

33,M

B24

Collaboration

with

F.Courbin

etal.(Liege)

VLT

Antu

with

FO

RS

1,MO

S:

–w

avelengthrange:

3800–9000A

(3grism

s)–

resolution:700

–0.2

/pixel–

integrationtim

e:1200–2400

s

morphologicalparam

eter:B

.Kuhlbrodt,L.W

isotzki

The

SE

Ds


Modelling

resultsE

FO

SC

EF

OS

C:H

E0952–1552,extracted

spectra:total,nucleus,host,residual

The

SE

Ds


EF

OS

C:H

E0952–1552,extracted

spectrum:

hostgalaxy

The

SE

Ds


Com

parisonto

broadband

colours

andm

odels

HE

0952–1552:100%

2G

yr(disk)

The

SE

Ds


HE

1201–2409:100%

2G

yr(elliptical)

The

SE

Ds


Modelling

resultsF

OR

S

FO

RS

:HE

1503+0228,B

grism:

total,nucleus,host,residual

The

SE

Ds


FO

RS

:HE

1503+0228,B

grism:

hostgalaxy

The

SE

Ds


FO

RS

:HE

1503+0228,R

grism:

total,nucleus,host,residual

The

SE

Ds


FO

RS

:HE

1503+0228,R

grism:

hostgalaxy

The

SE

Ds


FO

RS

:HE

1434–1600,Bgrism

:total,nucleus,host,residual

The

SE

Ds


FO

RS

:HE

1434–1600,Bgrism

:hostgalaxy

The

SE

Ds


FO

RS

:HE

1434–1600,Rgrism

:total,nucleus,host,residual

The

SE

Ds


FO

RS

:HE

1434–1600,Rgrism

:hostgalaxy

The

SE

Ds


Com

parisonto

models

HE

1503+0228:

100%C

SF

vs.97.5%C

SF

+2.5%

0.1G

yr

The

SE

Ds


HE

1009–0702:53%

0.7G

yr+

47%1

Gyr

(elliptical!)

The

SE

Ds


Modelling

results

EF

OS

C

–successful:

3–

successful(afterm

odification):4

–S

/Ntoo

low:

1

FO

RS

–successful:

2–

successful(afterm

odification):5

–S

/Ntoo

low:

3

The

SE

Ds


Rotation:

emission

lines

S SG CC

The

SE

Ds


Rotation

EF

OS

C

–gas

rotationfor

2disks,1

elliptical–

clearlyno

gasrotation

for1

elliptical–

stellarrotation

for2

disks–

clearlyno

stellarrotation

for1

elliptical

rotationvelocities

–gas:

200–470km

/s(observed)

–stars:

215–325km

/s(observed)

The

SE

Ds


Rotation

FO

RS

–gas

rotationfor

7of8

(ofthese3

ellipticals)–

clearlyno

gasrotation

for1

elliptical–

stellarrotation

for2

disks–

clearlyno

stellarrotation

for1

elliptical

rotationvelocities

–gas:

75–180km

/s(observed)

–stars:

40–150km

/s(observed)

spatiallyresolved

for4

objectsrotation

curves

The

SE

Ds


The

SE

Ds


Lineratios

determine

ionisationsource,hotstars

vs.AG

N(V

eilleux&

Osterbrock

1987):

–[O

III]5007/Hβ

vs.[NII]6583/H

α–

[OIII]5007/H

βvs.[S

II](6716+6731)/H

α–

[OIII]5007/H

βvs.[O

I]6300/Hα

temperature:

[OIII](4959+

5007)/4363

electrondensities:

[SII]6716/6731

The

SE

Ds


The

SE

Ds


On-n

ucleusspectroscop

y:sum

mar

y

separationw

orking,multicolour

imaging

fluxesreproduced

spatialresolutionachievable

emission

andabsorption

linesdetectable

qualitydepending

onP

SF

quality,S/N

,nucleus-to-hostratio

The

SE

Ds


On-n

ucleusspectroscop

y:sum

mar

y

disks:

–no

signsofstrong

starbursts–

gasionised

byhotstars

and/ornucleus

–in

totalverysim

ilarto

inactivespirals

ellipticals:

–young

populationsconsistentw

ithm

ulticolourim

aging–

nosigns

ofoldevolved

populations–

excluded:only

addedstarburst

–(m

assive)rotating

gasdisks

inseveralobjects

–ionised

bynucleus

The

SE

Ds


So

whatcould

thism

ean?

The

SE

Ds


Discussion

Nolan

etal.2001:

–higher

luminosity

quasars–

onlyellipticals

with

red,evolvedpopulation

–w

eakor

absentgasem

ission–

nobias

fromoff-nucleus

positionexpected

Boroson

etal.1985:

–lum

inousquasars:

redspectra

+w

eakgas

linesorblue

spectra+

stronggas

lines–

lesslum

inousquasars:

weak

orstrong

gaslines

contradictoryresults?

The

SE

Ds


Discussion

Proposal:

scenariosupporting/supported

byhierarchicalm

erging

intermediately

luminous

(L2L

)ellipticalhostgalaxies:

–created

inm

ajorm

ergeroftw

odisks

–m

ergerinduces

nuclearactivity

–dynam

icallytransform

edin

merger

ellipticalmorphology

–stellar

populationsas

inprogenitor

galaxiescolours,spectra

–(re-)creation

ofgasdisk

afterm

erger?tim

escaleproblem

?–

surfacedensity

ofgasdisk

lowno

strongstarburst

–passive

evolutionto

“red”ellipticalw

ithin1

Gyr

The

SE

Ds


Discussion

luminous

ellipticalhostgalaxies:

–activity

createdby

minor

merger

–m

orem

assivelater

inm

assevolution

diskhostgalaxies:

–activity

createdby

minor

merger

eventsdistortions,com

panions–

(slightly)enhanced

SF

R

directsignfor

hierarchicalclustering?creation

ofluminous

ellipticalscaughtin

theact?

The

SE

Ds


Discussion

Open

questions

specialinitialconditionsrequired

form

erger?gas

diskcreation

whathappens

with

othermerger

geometries?

ULIR

Gs?

radiogalaxies?

why

isthe

gas/ionisationgeom

etryso

differentindisks

andellipticals?

obscuringm

aterialcloseto

nucleus?the

dusttorusitself?

The

SE

Ds


Outlook

techniques:–

more

detailedem

issionline

modelling

–im

provedP

SF

determination

–extention

tointegralfield

spectroscopydata

–absorption

linediagnostics

ages/metallicities/dust

–velocity

dispersionscentralm

asses

more

data:–

secondhalfofF

OR

Ssam

ple,integrationtim

esdoubled

–“m

ulticolour-north”,secondsam

plefrom

Palom

ar-Green

–3d

spectroscopy:P

MA

S,V

IMO

S–

luminosity

dependenceofspectralproperties

–correlation

broad-lineshape

andhostproperties

–w

ithV

IMO

Shostgalaxy

spectraavailable

toz

05

The

SE

Ds


the seds of quasar host - max planck society€¦ · quasar host galaxies kn ud j ahnk e astroph...

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