Galaxy Evolution Workshop 2019

Tracing the co-evolution path of
SMBHs and spheroids with ULIRGs
selected from AKARI/Herschel catalogs

Xiaoyang Chen
Astronomical Inst., Tohoku Univ.
Collaborators: Masayuki Akiyama (Tohoku Univ.), Kohei Ichikawa (Tohoku
Univ.), Hirofumi Noda (Osaka Univ.), Yoshiki Toba (Kyoto Univ.), Issei
Yamamura (ISAS/JAXA), Toshihiro Kawaguchi (Onomichi City Univ.)Outline•

1. Background•

2. Sample and Method•

3. Results and Discussion•

4. Summary

Ultra-Luminous InfraRed Galaxies
Def:
LIRG : L8-1000μm > 10E+11 L⊙
Ultra-LIRG : L8-1000μm > 10E+12 L⊙
Hyper-LIRG : L8-1000μm > 10E+13 L⊙
Extremely-LIRG : L8-1000μm > 10E+14 L⊙
Antennae~90% radiation emitted ininfrared band by dust
heated by starburst (O/B
stars) and/or AGN.

Lagache+2015

The co-evolution path of SMBHs and spheroids in massive galaxies

SFR

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co-

LAGN

Hopkins+2008

The co-evolution path of SMBHs and spheroids in massive galaxies

ULIRG is the important period
in the co-evolution path.

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Ichikawa+2014
Ichikawa+2014
Hopkins+2008

Two main topics
1)
2)

the process to push the evolution: outflow;
the result of the evolution: luminous AGN andquenched star formation.

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Ichikawa+2014

Outflow study in the literature

U/LIRGs

Outflow kinetic energy

Outflow velocity

high-z QSOs

U/LIRGs

local AGN/SFG
Chen et al. 2019

In the view of outflow, ULIRGs locate at thetransition position between local AGN / star-forming
galaxies, and the very luminous high-z QSOs.

Quenched or Not quenched
Although the merger scenario provide a history of
the phase transition of ULIRGs, the detailed
measurement of evolution time is challenging.

It is hard to get the time
directly.

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Quenched or Not quenched
An alternative method is to evaluate the massfraction of Young Stellar Population (< ~ 100 Myr)with a large sample.

g
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Since the ULIRG evolution
starts from a starburst, if thequenching process reallyoccurs, the young fraction
should decreases
significantly when compared
to its early stage.

t
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b
star

Quenched or Not quenched<100Myr

HII-like(star-forming
dominated)

quenchinghappened

Seyfert 2(AGN dominated)
Hou et al. 2011
160 ULIRGs from 1Jy IRAS catalog

Su et al. 2013
419 ULIRGs from WISE catalog,
no FIR confirmed. biased?

Outline•

1. Background•

2. Sample and Method•

3. Results and Discussion•

4. Summary••Searching ULIRG in the AKARI FISBright Source Catalog
and the Herschel PACS/SPIRE
point source catalogs.

••

Searching ULIRG in the AKARI FISBright Source Catalog,
and the Herschel PACS/SPIRE
point source catalogs.

PACS PSC
70/100/160um

SPIRE PSC
250/350/500um

SDSS DR15
PhotoObj
Catalog(u, g, r, i, z)+

WISE AllWISE
Catalog(3, 4, 12, 22 um)

AKARI Catalog(90um)+
Herschel Catalog(160/250um)

Total cross-matched:
146921

Remove Galactic
dusty region

2-band SED estimation to select ULIRG

Magdis+2012

We can quickly estimate the IR AGN
and starburst luminosity just with 2band observation, when the SED are
fixed to some typical choices.

Fritz+2006

LAGN + LSB >= 1E12 Lsun

LAGN * (SEDtorus⨂T12) + LSB * (SEDSB⨂T12) = Flux12
LAGN * (SEDtorus⨂T90) + LSB * (SEDSB⨂T90) = Flux90
band transmission

2-band SED estimation to select ULIRG

ULIRG

2-band SED estimation to select ULIRG

cover 4000Å

ULIRG
1605 spec-ULRG at z < 1.5 selected(QSOs + SF Galaxies)

Spectral identification
type1 QSO? SF galaxy?
Broad Line Region

XMC-wMwF-160-NCU-J160312.83+552712.2-[ 1], z=0.82334, E(B-V)PL=0.00, E(B-V)HII=0.00(b)0.41(n)Original Data
Corrected Data
Model Outline
PL Cont.(αλ=-0.97)
Balmer Cont. + HOL
Fe II Lines
Narrow Lines
Broad Lines
PL Cont. Lum.

1.2

Mg II

0.8

Lum. density [10

42

-1

-1

erg s A ]

1

Hβ

0.6

0.4

0.2

0

Balmer cont.
2000

2500

3000

Fe II Lines

3500
4000
Rest frame wavelength [A]

4500

5000

5500

Spectral identification
type1 QSO? SF galaxy?
peak at z ~ 0.5

Broad Line Region

XMC-wMwF-160-NCU-J160312.83+552712.2-[ 1], z=0.82334, E(B-V)PL=0.00, E(B-V)HII=0.00(b)0.41(n)Original Data
Corrected Data
Model Outline
PL Cont.(αλ=-0.97)
Balmer Cont. + HOL
Fe II Lines
Narrow Lines
Broad Lines
PL Cont. Lum.

1.2

Mg II

0.8

Lum. density [10

42

-1

-1

erg s A ]

1

Hβ

0.6

0.4

514 spec-ULIRGs
without BLR features

0.2

0Balmer cont.
2000

2500

3000

Fe II Lines

3500
4000
Rest frame wavelength [A]

4500

5000

5500

Joint Opt.Spec + SED fitting
J082445.64+153944.1, AGN: no polar dust
103

Opt Spectrum (obs)
Opt Spectrum (apecor)
SED Model Outline
Main Stellar Population
Diffuse ISM (MSP)
Transparent Starburst
Diffuse ISM (TSB)
Attenuated Starburst
DISM (ASB) + BC
AGN Accretion DiscAGN Torus Dust
AGN Polar Dust
Flux (obs)
IR Flux (model)

210Flux (mJy)

101

100

Best-fitχ2ν, tt/ir = 5.93/4.99
Intrinsic:
LMSP= 11.5 ± 0.0
LTSB= 11.2 ± 0.0
LASB= 12.2 ± 0.0
LAGN= 11.4 ± ***-1

10Re-emitted:
LISMM = 11.1 ± 0.0
LISMT = 10.8 ± 0.0
LBC= 11.9 ± 0.1
LTorus = 11.1 ± 1.8
LPolar = NaN ± NaN

-2

10

10-3

0.1

1

10
Observed Wavelength (µm)

100

1000

Joint Opt.Spec + SED fitting
J082445.64+153944.1, AGN: no polar dust
103

Opt Spectrum (obs)
Opt Spectrum (apecor)
SED Model Outline
Main Stellar Population
Diffuse ISM (MSP)
Transparent Starburst
Diffuse ISM (TSB)
Attenuated Starburst 0.07
DISM (ASB) + BC
AGN Accretion Disc
0.06
AGN Torus Dust
AGN Polar Dust
0.05
Flux (obs)
IR Flux (model)

210Lum. density [1042 erg s-1 A-1]

Flux (mJy)

101

100

-1

10

3.00(b)
XMC-wMwF-090-CCCU-J082445.64+153944.1-[10], z=0.22, E(B-V)Star=0.42(y)0.42(o), E(B-V)HII=1.23(n)Observed Spectrum
Model Outline
Galaxy(old/3.36)
Galaxy(young/2.48)
Galaxy(total)
Narrow Lines
Broad Lines

Best-fitχ2ν, tt/ir = 5.93/4.99

0.04

Intrinsic:
LMSP= 11.5 ± 0.0
LTSB= 11.2 ± 0.0
LASB= 12.2 ± 0.0
LAGN= 11.4 ± ***

0.03

0.02

0.01

-2

10

0

3500

10-3

4000

4500

Re-emitted:
LISMM = 11.1 ± 0.0
LISMT = 10.8 ± 0.0
LBC= 11.9 ± 0.1
LTorus = 11.1 ± 1.8
5000
5500
6000
LPolar= NaN± 6500
NaN

7000

Rest frame wavelength [A]

0.1

1

10
Observed Wavelength (µm)

100

1000

7500

Ca K H

Joint Opt.Spec + SED fitting
J082445.64+153944.1, AGN: no polar dust

2

10

Flux (mJy)

101

[OII]

100

Opt Spectrum (obs)
Opt Spectrum (apecor)
SED Model Outline
OSP
Main Stellar Population
Diffuse ISM (MSP)
3.00(b)
XMC-wMwF-090-CCCU-J082445.64+153944.1-[10], z=0.22, E(B-V)Star=0.42(y)0.42(o), E(B-V)HII=1.23(n)Transparent Starburst
Diffuse ISM (TSB)
Observed Spectrum
0.07
Attenuated Starburst
Model Outline
Galaxy(old/3.36)
DISM (ASB) + BC
Galaxy(young/2.48)
AGN Accretion Disc
Galaxy(total)
0.06
NarrowLines
AGN Torus Dust
Broad
Lines
YSP
AGN Polar Dust
0.05
Flux (obs)
IR FluxHδ
(model) Hγ[NeIII]
Best-fit
0.04
χ2ν, tt/ir = 5.93/4.99
Lum. density [1042 erg s-1 A-1]

103

-1

10

3500 Spectral 4000

0.02

4500
0.01

Aperture-2
Correction

10

0

3500

10-3

0.1

1

Intrinsic:
LMSP= 11.5 ± 0.0
LTSB= 11.2 ± 0.0
LASB= 12.2 ± 0.0
LAGN= 11.4 ± ***

0.03

5000
5500
600
Re-emitted:= 11.1 ± 0.0
Rest frameLL wavelength[A]= 10.8 ± 0.0
4000

4500

ISMM
ISMT
LBC
= 11.9 ± 0.1
LTorus = 11.1 ± 1.8
5000
5500
6000
LPolar= NaN± 6500
NaN
Rest frame wavelength [A]10
Observed Wavelength (µm)

100

7000

1000

7500

Ca K H

Joint Opt.Spec + SED fitting
J082445.64+153944.1, AGN: no polar dust
103

SFR

Flux (mJy)

101

[OII]

100

Lum. density [1042 erg s-1 A-1]

2

10

Opt Spectrum (obs)
Opt Spectrum (apecor)
SED Model Outline
OSP
Main Stellar Population
Diffuse ISM (MSP)
3.00(b)
XMC-wMwF-090-CCCU-J082445.64+153944.1-[10], z=0.22, E(B-V)Star=0.42(y)0.42(o), E(B-V)HII=1.23(n)Transparent Starburst
Diffuse ISM (TSB)
Observed Spectrum
0.07
Attenuated Starburst
Model Outline
Galaxy(old/3.36)
DISM (ASB) + BC
Galaxy(young/2.48)
AGN Accretion Disc
Galaxy(total)
0.06
NarrowLines
AGN Torus Dustmainstellar
Broad
Lines
YSP
AGN Polar Dust
population:
0.05
Flux (obs)starburst:
IR FluxHδ
(model) HγSFR∝EXP(-t)
SFR≃constant[NeIII]
Best-fit
0.04
χ2ν, tt/ir = 5.93/4.99-1

103500 Spectral 4000
Aperture-2
10
Correction

0.02

4500
0.01

SSP: Bruzual andCharlot, 2003
0

0.1

1

5000
5500YSP
600
OSP
Re-emitted:= 11.1 ± 0.0
Rest frameLL wavelength[A]= 10.8 ± 0.0
ISMM
ISMT
LBC
= 11.9 ± 0.1
of ± 1.8
LTorus =start
11.1
5000
5500
6000
LPolar =merger/
NaN ± 6500
NaN
Rest frame wavelength [A]

birth
of
4000
4500
galaxy/main10stellarpopulation
Observed
Wavelength (µm)
3500

10-3

Intrinsic:
LMSP= 11.5 ± 0.0
LTSB= 11.2 ± 0.0
LASB= 12.2 ± 0.0
LAGN= 11.4 ± ***0.03

100 starburst

7000

time

1000

7500

Ca K H

Joint Opt.Spec + SED Fromfittingopt.spec:
J082445.64+153944.1, AGN:
dust
population;1)no polargalaxy
SFR
Opt Spectrum (obs)extinction;
2)
Opt Spectrum (apecor)
SED Model Outline
OSP
outflow velocity.
3)
Main Stellar Population

103

Flux (mJy)

101

[OII]

100

Diffuse ISM (MSP)
Transparent Starburst
Diffuse ISM (TSB)
Attenuated Starburst
DISM (ASB) + BC
AGN Accretion DiscAGN Torus Dust
AGN Polar Dust
Flux (obs)
IR FluxHδ
(model) Hγ[NeIII]
Lum. density [1042 erg s-1 A-1]

2

10

-1

10

3500 Spectral 4000
Aperture-2
10
Correction

3.00(b)
XMC-wMwF-090-CCCU-J082445.64+153944.1-[10], z=0.22, E(B-V)Star=0.42(y)0.42(o), E(B-V)HII=1.23(n)

0.07

0.06

main stellar
population:
SFR∝EXP(-t)

YSP
0.05

0.1

Intrinsic:
LMSP= 11.5 ± 0.0
LTSB= 11.2 ± 0.0
LASB= 12.2 ± 0.0
LAGN= 11.4 ± ***

0.03

0.02

4500
0.01

SSP: Bruzual andCharlot, 2003
0

1

starburst:
SFR≃constantBest-fitχ2ν, tt/ir = 5.93/4.99

0.04

5000
5500YSP
600
OSP
Re-emitted:= 11.1 ± 0.0
Rest frameLL wavelength[A]= 10.8 ± 0.0
ISMM
ISMT
LBC
= 11.9 ± 0.1
of ± 1.8
LTorus =start
11.1
5000
5500
6000
LPolar =merger/
NaN ± 6500
NaN
Rest frame wavelength [A]

birth
of
4000
4500
galaxy/main10stellarpopulation
Observed
Wavelength (µm)
3500

10-3

Observed Spectrum
Model Outline
Galaxy(old/3.36)
Galaxy(young/2.48)
Galaxy(total)
Narrow Lines
Broad Lines

100 starburst

7000

time

1000

7500

Joint Opt.Spec + SED fitting
J082445.64+153944.1, AGN: no polar dust
103

Opt Spectrum (obs)
Opt Spectrum (apecor)
SED Model Outline
Stellar component
ISM dust
AGN Torus
Flux (obs)
IR Flux (model)

210Flux (mJy)

101

100

-1

10

Spectral
Aperture-2
Correction
10

10-3

0.1

1

10
Observed Wavelength (µm)

100

1000

Joint Opt.Spec + SED fitting
Two3 dust emitter: J082445.64+153944.1, AGN: no polar dust
10
Opt Spectrum (obs)
1. ISM dust
Opt Spectrum (apecor)
Model Outline
diffuse ISMSED
dust;
Stellar component
2
ISM dust
10
BirthcloudsAGN(PDR-like)
Torus
Flux (obs)
IR Fluxtorus(model)2. AGN dusty
Flux (mJy)

101

100

-1

10

Spectral
Aperture-2
Correction
10

10-3

0.1

1

10
Observed Wavelength (µm)

100

1000

Joint Opt.Spec + SED fitting
Two3 dust emitter: J082445.64+153944.1, AGN: no polar dust
10
Opt Spectrum (obs)
1. ISM dust
Opt Spectrum (apecor)
Model Outline
diffuse ISMSED
dust;
Stellar component
2
ISM dust
10
BirthcloudsAGN(PDR-like)
Torus
Flux (obs)
IR Fluxtorus(model)2. AGN dusty
Calculated from THEMIS dust model

diffused ISM

Flux (mJy)

101

100

FIR bump

20-40K-1

10Spectral
Aperture-2
Correction10

diffused ISM

birth clouds

10-3

0.1

1

10
Observed Wavelength (µm)

100

1000

Joint Opt.Spec + SED fitting
Two3 dust emitter: J082445.64+153944.1, AGN: no polar dust
10
Opt Spectrum (obs)
1. ISM dust
Opt Spectrum (apecor)
Model Outline
diffuse ISMSED
dust;
Stellar component
2
ISM dust
10
BirthcloudsAGN(PDR-like)
Torus
Flux (obs)
IR Fluxtorus(model)2. AGN dusty
Flux (mJy)

101

100

-1

10

Spectral
Aperture-2
Correction
10

10-3

0.1

1

10
Observed Wavelength (µm)

100

1000

Joint Opt.Spec + SED fitting
Two3 dust emitter: J082445.64+153944.1, AGN: no polar dust
10
Opt Spectrum (obs)
1. ISM dust
Opt Spectrum (apecor)
Model Outline
diffuse ISMSED
dust;
Stellar component
2
ISM dust
10
BirthcloudsAGN(PDR-like)
Torus
Flux (obs)
IR Fluxtorus(model)2. AGN dusty
Flux (mJy)101

Stalevski et al. (2012,2016)
100

-1

10

Spectral
Aperture-2
Correction
10

10-3

Calculated from THEMIS dust model
0.1

1

10
Observed Wavelength (µm)

100

1000

Joint Opt.Spec + SED fitting

J082445.64+153944.1, AGN: no polar dust
103

Opt Spectrum (obs)
Opt Spectrum (apecor)
SED Model Outline
Stellar component
ISM dust
AGN Torus
Flux (obs)
IR Flux (model)

210Flux (mJy)

101

100

AGN

1)
2)
3)

10-1

low AGN IR
contribution

-2

10

10-3

0.1

103

1

10
J204837.26-002437.2,
AGN: nopolar dust
Observed Wavelength
(µm)

100

1000

Opt Spectrum (obs)
Opt Spectrum (apecor)
SED Model Outline
Stellar component
ISM dust
AGN Torus
Flux (obs)
IR Flux (model)

2

10From SED decomp.:
AGN luminosity;
1)2) Starburst lum., SFR

Flux (mJy)

101

AGN

100

From opt.spec:
galaxy population;
extinction;
outflow velocity.

10-1

high AGN IR
contribution

10-2

-3

10

0.1

1

10
Observed Wavelength (µm)

100What about the results?
1000

Outline•

1. Background•

2. Sample and Method•

3. Results and Discussion•

4. Summary

General properties of Spec+SED fitting
469 / 514 galaxies have

LTIR > 1E12 Lsun

AGN contribution= Ltorus / LTIR

General properties of Spec+SED fitting
AGN contribution with BPT diagram check

144 / 514 galaxies have
[NII] flux SNR > 5

AGN dominates the ionization
as it becomes luminous.

Outflow velocity vs. AGN intensity
Outflow can be measured from the shift and width of emission lines.
[OIII]5007 is one of the widely adopted indicators.
245/ 514 with SNR > 5

PCC=0.25

PCC = Pearson correlation coefficient

Vout = |V50| + W80 / 2

Outflow velocity vs. AGN intensity
Outflow can be measured from the shift and width of emission lines.
[OIII]5007 is one of the widely adopted indicators.
More powerful AGN
drives faster outflow.

PCC=0.25

PCC=0.36

Outflow velocity is more tightly related with absolute AGN intensity (LAGN),
and less tightly related with relative intensity (fAGN).

Outflow velocity vs. AGN intensity

0.00(b)
XMC-wMwF-090-CRU-J112657.76+163912.0-[10], z=0.46858, E(B-V)Star=0.17(y)0.17(o), E(B-V)HII=0.31(n)0.3

shift = -960 km/s
fwhm = 2100 km/s

Lum. density [1042 erg s-1 A-1]

0.25

Original Data
Corrected Data
Model Outline
Galaxy(old/3.90)
Galaxy(young/2.34)
Galaxy(total)
Narrow Lines
Broad Lines

identified as
Lya in the
SDSS archive

0.2

0.15

0.1

0.05

0

3000

3500

4000
4500
5000
Rest frame wavelength [A]

5500

6000

Outflow velocity vs. AGN intensity
Outflow can be measured from the shift and width of emission lines.
[OIII]5007 is one of the widely adopted indicators.
More powerful AGN
drives faster outflow.

Does the strong outflow really affect SF?

Outflow velocity is more tightly related with absolute AGN intensity (LAGN),
and less tightly related with relative intensity (fAGN).

Galaxy properties vs. AGN intensity

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Ichikawa+2014

During ULIRG period,
Q1: Does the AGN(SMBH) co-grow with host galaxies?
Q2: Does the feedback really take place?

Galaxy properties vs. AGN intensity

During ULIRG stage,
Q1: co-growth ?
Q2: feedback ?

Galaxy properties vs. AGN intensity

PCC=0.31

The most luminous AGN locatesin the most massive galaxies.

During ULIRG stage,
Q1: co-growth ?
Q2: feedback ?

Galaxy properties vs. AGN intensity

PCC=0.31

The most luminous AGN locatesin the most massive galaxies.

During ULIRG stage,
Q1: co-growth ? Yes
Q2: feedback ?

Galaxy properties vs. AGN intensity

PCC=0.24

During ULIRG stage,
Q1: co-growth ? Yes
Q2: feedback ?

Galaxy properties vs. AGN intensity
PCC=-0.14
diffused ISM

birth clouds(clumps)
bubbles

PCC=0.24
hidden in
opt.spec

During ULIRG stage,
Q1: co-growth ? Yes
Q2: feedback ?

Galaxy properties vs. AGN intensity
PCC=-0.14

PCC=-0.31

PCC=0.24

The star-forming becomes transparent
as AGN becomes luminous.

During ULIRG stage,
Q1: co-growth ? Yes
Q2: feedback ?

Galaxy properties vs. AGN intensity
PCC=-0.14

PCC=-0.31

PCC=0.24

The star-forming becomes transparent
as AGN becomes luminous.

During ULIRG stage,
Q1: co-growth ? Yes
Q2: feedback ? Yes

Galaxy properties vs. AGN intensity
PCC=-0.14

PCC=-0.31

PCC=0.24

The star-forming becomes transparent
as AGN becomes luminous.

During ULIRG stage,
Q1: co-growth ? Yes
Q2: feedback ? Yes?

Galaxy properties vs. AGN intensity

Mstar

Mhalo

Moster et al. 2013

Vescaping ~ Vcircular

Mo & White et al. 2002

Galaxy properties vs. AGN intensity

Mstar

Mhalo

Moster et al. 2013

Vescaping ~ Vcircular

Mo & White et al. 2002

Galaxy properties vs. AGN intensity
Feedback is
not effective?

Quenchedin the future?

Mstar

Mhalo

Moster et al. 2013

Vescaping ~ Vcircular

Mo & White et al. 2002

Galaxy properties vs. AGN intensity

Main-sequence(Renzini & Peng2015, Spilker et
al. 2018)

Outline•

1. Background•

2. Sample and Method•

3. Results and Discussion•

4. Summary

Summary
In order to statistically study the co-evolution of SMBHs andstellar components in ULIRGs, we performed a new method
combining optical spectral fitting and IR SED fitting, to ~ 500
ULIRGs selected with AKARI and Herschel FIR catalog, wefound:
1) the outflow velocity shows a clear dependence on AGN
luminosity;2) as AGN becomes luminous, the star-forming regions in
the host galaxy become from dusty to transparent;
1)+2):
a powerful AGN is capable to blow out the gas and dustout of the host galaxies;

3) currently the star formation in this ULIRG sample is notquenched, with SFR ~ 300-1000 Msun/yr;4) the ULIRG with Mstar ~ 1E11 Msun shows outflow
exceeding the escaping velocity of the halo, those galaxies
might be quenched in the future.
Future step:
1) Hard X-ray follow-up observation to confirm the reliability of
the AGN luminosity from IR SED decomposition;2) ALMA follow-up to determine the distribution of cold gas
reservoirs, and check whether the cold gas is affected by theionized outflow or not.

3) currently the star formation in this ULIRG sample is notquenched, with SFR ~ 300-1000 Msun/yr;4) the ULIRG with Mstar ~ 1E11 Msun shows outflow
exceeding the escaping velocity of the halo, those galaxies
might be quenched in the future.
Future step:
1) Hard X-ray follow-up observation to confirm the reliability of
the AGN luminosity from IR SED decomposition;2) ALMA follow-up to determine the distribution of cold gas
reservoirs, and check whether the cold gas is affected by theionized outflow or not.

Thanks for your attention!