Post on 07-Sep-2020
transcript
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
ofquasarhostgalaxies
Introduction
HE
1029–1401
z=0.085
E0
elliptical
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Introduction
(McLure
&D
unlop2002)
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Introduction
Spectral
information:
anew
dimension
apparentmorphology
vs.stellarcontentvs.gas
content
spectroscopicsigns
ofpasttidalinteraction
dynamics
spectralinformation
veryvaluable
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Multicolour
imaging
The
SE
Ds
ofquasarhostgalaxies
Multicolour
ima
ging
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Multicolour
imaging
The
SE
Ds
ofquasarhostgalaxies
Multicolour
imaging
Modelling
results
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Multicolour
imaging
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Multicolour
imaging
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
On-nucleus
spectroscopy
The
SE
Ds
ofquasarhostgalaxies
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:
on-nucleusspectroscopy
–problem
:very
highcontrastnucleus–host
–solution:
spatialm
odelling,similar
toim
aging
The
SE
Ds
ofquasarhostgalaxies
On-nucleus
spectroscopy
0054+144 (R
) WH
T
(Hughes
etal.2000,Hutchings
&C
rampton
1990)
The
SE
Ds
ofquasarhostgalaxies
On-n
ucleusspectroscop
y
techniqueso
far:
–off-nucleus
spectroscopy,r
3avoiding
nucleusplus
removal
ofnuclear
residuals
drawbacks:
–controlofnuclear
residualsdifficult
–sam
plingfar
outsidenuclear
regionpotentially
boring
wanted:
on-nucleusspectroscopy
–problem
:very
highcontrastnucleus–host
–solution:
spatialm
odelling,similar
toim
aging
The
SE
Ds
ofquasarhostgalaxies
Multi-object-spectroscopy
vs.longslitspectroscopy
The
SE
Ds
ofquasarhostgalaxies
r
λ
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
r
λ
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Modelling
resultsE
FO
SC
EF
OS
C:H
E0952–1552,extracted
spectra:total,nucleus,host,residual
The
SE
Ds
ofquasarhostgalaxies
EF
OS
C:H
E0952–1552,extracted
spectrum:
hostgalaxy
The
SE
Ds
ofquasarhostgalaxies
Com
parisonto
broadband
colours
andm
odels
HE
0952–1552:100%
2G
yr(disk)
The
SE
Ds
ofquasarhostgalaxies
HE
1201–2409:100%
2G
yr(elliptical)
The
SE
Ds
ofquasarhostgalaxies
Modelling
resultsF
OR
S
FO
RS
:HE
1503+0228,B
grism:
total,nucleus,host,residual
The
SE
Ds
ofquasarhostgalaxies
FO
RS
:HE
1503+0228,B
grism:
hostgalaxy
The
SE
Ds
ofquasarhostgalaxies
FO
RS
:HE
1503+0228,R
grism:
total,nucleus,host,residual
The
SE
Ds
ofquasarhostgalaxies
FO
RS
:HE
1503+0228,R
grism:
hostgalaxy
The
SE
Ds
ofquasarhostgalaxies
FO
RS
:HE
1434–1600,Bgrism
:total,nucleus,host,residual
The
SE
Ds
ofquasarhostgalaxies
FO
RS
:HE
1434–1600,Bgrism
:hostgalaxy
The
SE
Ds
ofquasarhostgalaxies
FO
RS
:HE
1434–1600,Rgrism
:total,nucleus,host,residual
The
SE
Ds
ofquasarhostgalaxies
FO
RS
:HE
1434–1600,Rgrism
:hostgalaxy
The
SE
Ds
ofquasarhostgalaxies
Com
parisonto
models
HE
1503+0228:
100%C
SF
vs.97.5%C
SF
+2.5%
0.1G
yr
The
SE
Ds
ofquasarhostgalaxies
HE
1009–0702:53%
0.7G
yr+
47%1
Gyr
(elliptical!)
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
Rotation:
emission
lines
S SG CC
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
So
whatcould
thism
ean?
The
SE
Ds
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies
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
ofquasarhostgalaxies