Extreme Outflows in an AKARI-selected ULIRG
at z=0.5

Xiaoyang Chen (D2)
Astronomical Inst., Tohoku Univ.
Collaborators: Masayuki Akiyama (Tohoku Univ.), Hirofumi Noda (Tohoku
Univ.), Abdurro’uf (Tohoku Univ.), Yoshiki Toba (Kyoto Univ./ASIAA), Issei
Yamamura (ISAS), Toshihiro Kawaguchi (Tsukuba Univ.), Kohei Ichikawa(Tohoku Univ./Columbia Univ.)

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⊙
ELIRG : WISE J224607.57-052635.0 (NASA/ART)~90% radiation emitted ininfrared band by dust
heated by starburst (O/B
stars) and/or AGN.
Important stage in theevolution of galaxies.

Lagache+2015

Hopkins+2008

••Searching ULIRG in the AKARI FISBright Source Catalogue (Ver.2).
Covering 10 times wider survey area
compared to the Herschel-ATLAS
survey at the similar depth.

Os whose optical light is dominated by their host galaxy. Five out of
et alsodetectedin theFaintnotSourcehave notSourceCatalog,but IRAS
they have
beenCatalog,
identifiedbut
at they
all becauseof been identified
the• optical.
Although,theytoareextremely
aspositional
an FIR
opticalcounterpart
extremely
faintas an opticalcounterpartof faint
thethebrightsource,they ofoftheWISE
pinpointing
narrow
down
uncertainty
thebright
right
to
be
easilyspectroscopically
identified
with
8-10m
class
telescope.
Once
the
eﬀ
ly identified
with
8-10m
class
telescope.
Oncetheeﬀectivenessofthe
AKARI FIR sources
ction
isconfirmed,
systematic
search
can
be
made
with
more
than
50
AKARI
sources
arch
can
be
made
with
more
than
50
AKARI
sourceswithextremely• An optical follow-up program for optically-faint AKARI FIS Brightandthethecontributionof type-2 QSOs
to examined.
the HyLIRGs
populationfurther
will be examined. Add
Os to
HyLIRGs population
will beAdditionally,sources
to construct
a their
uniquesample inof X-rayULIRGsatChandraz ~ 0.5-1.0.
beeasilyconducted
thankstobrightness:withheir brightness: in X-ray with Chandra and XMM-Newton to constrain and XMM-New• Eight objects were firstly identified as ULIRGs at z = 0.3-0.6 using
ivity
and Compton-thickness,and theirin radio
ALMA to evaluate their gas contents.
d in radiowith ALMA to evaluate
gaswithcontents.
Subaru/FOCAS.
oi
et
al.
PASJ,
67,67,
5051• Takitaal. 2015,
PASJ,ApJ,67, 51Eser,
akita et al.2015,
2015,
PASJ,
• Eser,etGoto,
Doi 2014,
797,• 54
• Goto, Doi 2014
,gao
MNRAS,
410, 820,
573 •46Toba& Nagao
2016, ApJS,ApJ, 820,
2016, ApJ,
• Kim
et al. 1998,
119, 46
41 • Kim et al. 1998, ApJS, 119,
21

SDSS
Broad-line QSOs

14
20

14

13
19

13

18
12

SDSS-spec limit
for galaxies

17
11
16
10
15

Broad-line QSOs
AKARI detection
limit

1

Redshift

1

13
8
0.01
0.01

12
11
10

AKARI detection limit

9

9
14

5”

νLν90 µm [Lsun]

15”

i [mag]νLSDSS[Lsun]
ν90 µmAKARIt

Our targets expected luminosity range

Our targets Our
expectedluminosity
range
targets
mag range

argets mag
range
WISE
12um

0.1
0.1

Redshift

11

8
0.01

0.1

1

Redshift

Exampleof an identification
with aisfaint
opticalcounterpart.
Thereis a bright WISE 12µa faint opticalcounterpart. Therea bright
WISE
12µm source
withinr circle(blue).
A galaxy with ithe
= WISE
20.3 magis associatedwith thevs.
WISE position. L=
20.3 magis associatedposition.
Left) Redshiftectroscopically-identifiedof the AKARI FIR sourcesin thein thespectroscopically-identified
SDSS survey (blue and red).
RedSDSS
dots survey (blue andOs whose optical light is dominated by their host galaxy. Five out of
et alsodetectedin theFaintnotSourcehave notSourceCatalog,but IRAS
they have
beenCatalog,
identifiedbut
at they
all becauseof been identified
the• optical.
Although,theytoareextremely
aspositional
an FIR
opticalcounterpart
extremely
faintas an opticalcounterpartof faint
thethebrightsource,they ofoftheWISE
pinpointing
narrow
down
uncertainty
thebright
right
to
be
easilyspectroscopically
identified
with
8-10m
class
telescope.
Once
the
eﬀ
ly identified
with
8-10m
class
telescope.
Oncetheeﬀectivenessofthe
AKARI FIR sources
ction
isconfirmed,
systematic
search
can
be
made
with
more
than
50
AKARI
sources
arch
can
be
made
with
more
than
50
AKARI
sourceswithextremely• An optical follow-up program for optically-faint AKARI FIS Brightandthethecontributionof type-2 QSOs
to examined.
the HyLIRGs
populationfurther
will be examined. Add
Os to
HyLIRGs population
will beAdditionally,sources
to construct
a their
uniquesample inof X-rayULIRGsatChandraz ~ 0.5-1.0.
beeasilyconducted
thankstobrightness:withheir brightness: in X-ray with Chandra and XMM-Newton to constrain and XMM-New• Eight objects were firstly identified as ULIRGs at z = 0.3-0.6 using
ivity
and Compton-thickness,and theirin radio
ALMA to evaluate their gas contents.
d in radiowith ALMA to evaluate
gaswithcontents.
Subaru/FOCAS.
oi
et
al.
PASJ,
67,67,
5051• Takitaal. 2015,
PASJ,ApJ,67, 51Eser,
akita et al.2015,
2015,
PASJ,
• Eser,etGoto,
Doi 2014,
797,• 54
• Goto, Doi 2014
J0818
J1010
SDSS46
J1219
SDSS J1348,gao
MNRAS,
410,
573 •46Toba
&SDSS
Nagao
2016, ApJS,ApJ, 820,• Kim et al. 1998,
ApJS, 119,2016,SDSS
ApJ,
820,
• Kim
et al.
1998,
119,
41
21

SDSS J0916

SDSS

Broad-line QSOs

14
20

14

13
19

13

18
12

SDSS-spec limit
for galaxies

17
11
16
10
15

1

1

13
8
0.01
0.01

12

SDSS11J1227

SDSS J1034
Broad-line QSOs
AKARI detection
limit

10

SDSS J1402
AKARI detection limit

9

9
14

5”

νLν90 µm [Lsun]

15”

i [mag]νLSDSS[Lsun]
ν90 µmAKARIt

Our targets expected luminosity range

Our targets Our
expectedluminosity
range
targets
mag range

argets mag
range
WISE
12um

0.1
0.1

11

8
0.01

0.1

1

Redshift
Redshift
Exampleof MIR
an identification
with aisfaint
opticalcounterpart.
There
isbyaSubaru/FOCAS
bright WISE 12µa faint opticalcounterpart.
a bright
12µm
withinexcess
Blue: There
Stellar
Green:AGNWISERed:
Dust source
identified
Redshiftr circle(blue).
A galaxy with ithe
= WISE
20.3 magis associatedwith thevs.
WISE position. L=
20.3 magis associatedposition.
Left) Redshiftectroscopically-identifiedof the AKARI FIR sourcesin thein thespectroscopically-identified
SDSS survey (blue and red).
RedSDSS
dots survey (blue andOs whose optical light is dominated by their host galaxy. Five out of
et alsodetectedin theFaintnotSourcehave notSourceCatalog,but IRAS
they have
beenCatalog,
identifiedbut
at they
all becauseof been identified
the• optical.
Although,theytoareextremely
aspositional
an FIR
opticalcounterpart
extremely
faintas an opticalcounterpartof faint
thethebrightsource,they ofoftheWISE
pinpointing
narrow
down
uncertainty
thebright
right
to
be
easilyspectroscopically
identified
with
8-10m
class
telescope.
Once
the
eﬀ
ly identified
with
8-10m
class
telescope.
Oncetheeﬀectivenessofthe
AKARI FIR sources
ction
isconfirmed,
systematic
search
can
be
made
with
more
than
50
AKARI
sources
arch
can
be
made
with
more
than
50
AKARI
sourceswithextremely• An optical follow-up program for optically-faint AKARI FIS Brightandthethecontributionof type-2 QSOs
to examined.
the HyLIRGs
populationfurther
will be examined. Add
Os to
HyLIRGs population
will beAdditionally,sources
to construct
a their
uniquesample inof X-rayULIRGsatChandraz ~ 0.5-1.0.
beeasilyconducted
thankstobrightness:withheir brightness: in X-ray with Chandra and XMM-Newton to constrain and XMM-New• Eight objects were firstly identified as ULIRGs at z = 0.3-0.6 using
ivity
and Compton-thickness,and theirin radio
ALMA to evaluate their gas contents.
d in radiowith ALMA to evaluate
gaswithcontents.
Subaru/FOCAS.
oi
et
al.
PASJ,
67,67,
5051• Takitaal. 2015,
PASJ,ApJ,67, 51Eser,
akita et al.2015,
2015,
PASJ,
• Eser,etGoto,
Doi 2014,
797,• 54
• Goto, Doi 2014
J0818
J1010
SDSS46
J1219
SDSS J1348,gao
MNRAS,
410,
573 •46Toba
&SDSS
Nagao
2016, ApJS,ApJ, 820,• Kim et al. 1998,
ApJS, 119,2016,SDSS
ApJ,
820,
• Kim
et al.
1998,
119,
41
21

SDSS J0916

SDSS

Broad-line QSOs

14
20

14

13
19

13

18
12

SDSS-spec limit
for galaxies

17
11
16
10
15

1

1

13
8
0.01
0.01

12

SDSS11J1227

SDSS J1034
Broad-line QSOs
AKARI detection
limit

10

SDSS J1402
AKARI detection limit

9

9
14

5”

νLν90 µm [Lsun]

15”

i [mag]νLSDSS[Lsun]
ν90 µmAKARIt

Our targets expected luminosity range

Our targets Our
expectedluminosity
range
targets
mag range

argets mag
range
WISE
12um

0.1
0.1

11

8
0.01

0.1

1

Redshift
Redshift
Exampleof MIR
an identification
with aisfaint
opticalcounterpart.
There
isbyaSubaru/FOCAS
bright WISE 12µa faint opticalcounterpart.
a bright
12µm
withinexcess
Blue: There
Stellar
Green:AGNWISERed:
Dust source
identified
Redshiftr circle(blue).
A galaxy with ithe
= WISE
20.3 magis associatedwith thevs.
WISE position. L=
20.3 magis associatedposition.
Left) Redshiftectroscopically-identifiedof the AKARI FIR sourcesin thein thespectroscopically-identified
SDSS survey (blue and red).
RedSDSS
dots survey (blue andOs whose optical light is dominated by their host galaxy. Five out of
et alsodetectedin theFaintnotSourcehave notSourceCatalog,but IRAS
they have
beenCatalog,
identifiedbut
at they
all becauseof been identified
the• optical.
Although,theytoareextremely
aspositional
an FIR
opticalcounterpart
extremely
faintas an opticalcounterpartof faint
thethebrightsource,they ofoftheWISE
pinpointing
narrow
down
uncertainty
thebright
right
to
be
easilyspectroscopically
identified
with
8-10m
class
telescope.
Once
the
eﬀ
ly identified
with
8-10m
class
telescope.
Oncetheeﬀectivenessofthe
AKARI FIR sources
ction
isconfirmed,
systematic
search
can
be
made
with
more
than
50
AKARI
sources
arch
can
be
made
with
more
than
50
AKARI
sourceswithextremely• An optical follow-up program for optically-faint AKARI FIS Brightandthethecontributionof type-2 QSOs
to examined.
the HyLIRGs
populationfurther
will be examined. Add
Os to
HyLIRGs population
will beAdditionally,sources
to construct
a their
uniquesample inof X-rayULIRGsatChandraz ~ 0.5-1.0.
beeasilyconducted
thankstobrightness:withheir brightness: in X-ray with Chandra and XMM-Newton to constrain and XMM-New• Eight objects were firstly identified as ULIRGs at z = 0.3-0.6 using
ivity
and Compton-thickness,and theirin radio
ALMA to evaluate their gas contents.
d in radiowith ALMA to evaluate
gaswithcontents.
Subaru/FOCAS.
oi
et
al.
PASJ,
67,67,
5051• Takitaal. 2015,
PASJ,ApJ,67, 51Eser,
akita et al.2015,
2015,
PASJ,
• Eser,etGoto,
Doi 2014,
797,• 54
• Goto, Doi 2014
J0818
J1010
SDSS46
J1219
SDSS J1348,gao
MNRAS,
410,
573 •46Toba
&SDSS
Nagao
2016, ApJS,ApJ, 820,• Kim et al. 1998,
ApJS, 119,2016,SDSS
ApJ,
820,
• Kim
et al.
1998,
119,
41
21

SDSS J0916

SDSS

Broad-line QSOs

14
20

14

13
19

13

18
12

SDSS-spec limit
for galaxies

17
11
16
10
15

1

1

13
8
0.01
0.01

12

SDSS11J1227

SDSS J1034
Broad-line QSOs
AKARI detection
limit

10

SDSS J1402
AKARI detection limit

9

9
14

5”

νLν90 µm [Lsun]

15”

i [mag]νLSDSS[Lsun]
ν90 µmAKARIt

Our targets expected luminosity range

Our targets Our
expectedluminosity
range
targets
mag range

argets mag
range
WISE
12um

0.1
0.1

11

8
0.01

0.1

1

Redshift
Redshift
Exampleof MIR
an identification
with aisfaint
opticalcounterpart.
There
isbyaSubaru/FOCAS
bright WISE 12µa faint opticalcounterpart.
a bright
12µm
withinexcess
Blue: There
Stellar
Green:AGNWISERed:
Dust source
identified
Redshiftr circle(blue).
A galaxy with ithe
= WISE
20.3 magis associatedwith thevs.
WISE position. L=
20.3 magis associatedposition.
Left) Redshiftectroscopically-identifiedof the AKARI FIR sourcesin thein thespectroscopically-identified
SDSS survey (blue and red).
RedSDSS
dots survey (blue and•••

WISE pinpointing to narrow down the positional uncertainty of the
AKARI FIR sources
An optical follow-up program for optically-faint AKARI FIS Brightsources to construct a unique sample of ULIRGs at z ~ 0.5-1.0.
Eight objects were firstly identified as ULIRGs at z = 0.3-0.6 using
Subaru/FOCAS.
SDSS J0818

SDSS J1010

SDSS J1219

SDSS J1348

SDSS J0916

SDSS J1034

SDSS J1227

SDSS J1402

MIR excess

Blue: Stellar

Green: AGN

Red: Dust

identified by Subaru/FOCASSDSS J0818

SDSS J1010

SDSS J1219

SDSS J1348

SDSS J0916

SDSS J1034

SDSS J1227

SDSS J1402

MIR excess••

Blue: Stellar

Green: AGN

Red: Dust

identified by Subaru/FOCAS

Using pPXF to subtract stellar continuum and Balmer absorptions
from the galaxy spectrum.
Using PySpecKit to fit the emission line features of gases.
• tie the kinetics (position and dispersion)• only set amplitude as free parametershift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

FOCAS slit
w=0.5’’

6a
1
9 .29
0
J 20
i=
6b
1
9 .43
0
J 21
i=

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

FOCAS slit
w=0.5’’

6a
1
9 .29
0
J 20
i=
6b
1
9 .43
0
J 21
i=

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Flux distribution

Velocity shift & FWHM

[OIII]/Hβ & [NII]/Hαshift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Flux distribution

Velocity shift & FWHM
V[OIII] - VHα_nr[OIII]/Hβ & [NII]/Hαshift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Flux distribution

Velocity shift & FWHM
[OIII]/Hβ & [NII]/Hα
V[OIII] - VHα_nr > FWHMHα_nr / 2

~ 12 kpc

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Flux distribution

Velocity shift & FWHM
[OIII]/Hβ & [NII]/Hα
V[OIII] - VHα_nr > FWHMHα_nr / 2

~ 12 kpc

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Flux distribution

Velocity shift & FWHM
[OIII]/Hβ & [NII]/Hα
V[OIII] - VHα_nr > FWHMHα_nr / 2[OIII] 5007

stellar
FWHM~ 9 kpc

~ 12 kpc

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Flux distribution

Velocity shift & FWHM
[OIII]/Hβ & [NII]/Hα
V[OIII] - VHα_nr > FWHMHα_nr / 2[OIII] 5007

stellar
FWHM~ 9 kpc

Power source of fast outflow

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Ionization potential (IP)• High-IP emission line: [OIII] 5007 (35.12 eV), [NeIII] 3869 (40.96 eV),• usually is ionized by AGN, although O/B stars and shock driven
stellar wind can also contribute in some intense starburst case.
• Low-IP emission line: [OII] 3729 (13.62 eV), [NII] 6583 (14.53 eV)• can be ionized by radiation from both (either) AGN and (or) stars.

Power source of fast outflow

shift to Balmer Abs

FWHM

w80 (= v90 - v10)

[OIII] 5007

- 917 km/s

1658 km/s

2607 km/s[OII] 3726,3729- 406 km/s

997 km/s

1555 km/s

Ionization potential (IP)• High-IP emission line: [OIII] 5007 (35.12 eV), [NeIII] 3869 (40.96 eV),• usually is ionized by AGN, although O/B stars and shock driven
stellar wind can also contribute in some intense starburst case.
• Low-IP emission line: [OII] 3729 (13.62 eV), [NII] 6583 (14.53 eV)• can be ionized by radiation from both (either) AGN and (or) stars.
> Can the fast outflow shown by [OII] come from star-forming regions?

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…

z ~ 0.1

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…

z ~ 0.1

SFG
Sy2
LINER

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…
• Selection: S/N > 6 for both [OII] and [OIII]z ~ 0.1

S/N > 6

SFG
Sy2
LINER

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…
• Selection: S/N > 6 for both [OII] and [OIII]z ~ 0.1

S/N > 6

SFG
Sy2
LINER

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…
• Selection: S/N > 6 for both [OII] and [OIII]
x: FWHM > 600
S/N > 6

SFG
Sy2
LINER

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…
• Selection: S/N > 6 for both [OII] and [OIII]
x: FWHM > 600
S/N > 6

SFG
Sy2
LINER

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…
• Selection: S/N > 6 for both [OII] and [OIII]
x: FWHM > 600

Power source of fast outflow: 1) in BPT-diagram view
• We use MPA-JHU catalog of SDSS galaxy spectroscopy survey forstatistics study on [OII] width.
• The catalog consists of ~ 1.8 million local galaxies, including starforming galaxies, Seyfert, LINER…
• Selection: S/N > 6 for both [OII] and [OIII]r < Routr > RoutPower source of fast outflow: 1) in BPT-diagram view

Power source of fast outflow: 1) in BPT-diagram view
• [OII] width: Sy2s > SFGs

Power source of fast outflow: 1) in BPT-diagram view
• [OII] width: Sy2s > SFGs
• J0916a >> local SFGs and Sy2s

Power source of fast outflow: 1) in BPT-diagram view
• [OII] width: Sy2s > SFGs
• J0916a >> local SFGs and Sy2s
• Compared with higher-z
samples observed with fast
outflow and [OII] detection:Power source of fast outflow: 1) in BPT-diagram view
• [OII] width: Sy2s > SFGs
• J0916a >> local SFGs and Sy2s
• Compared with higher-z
samples observed with fast
outflow and [OII] detection:• IR-bright DOGs (Dust obscured
galaxies) (Toba+2017) at
z~0.3-1.0

Power source of fast outflow: 1) in BPT-diagram view
• [OII] width: Sy2s > SFGs
• J0916a >> local SFGs and Sy2s
• Compared with higher-z
samples observed with fast
outflow and [OII] detection:• IR-bright DOGs (Dust obscured
galaxies) (Toba+2017) at
z~0.3-1.0• IR-bright obscured QSOs atz~1.5 (Perna+2015) and z~2.5(Zakamska+2016)

Power source of fast outflow: 1) in BPT-diagram view
• [OII] width: Sy2s > SFGs
• J0916a >> local SFGs and Sy2s
• Compared with higher-z
samples observed with fast
outflow and [OII] detection:• IR-bright DOGs (Dust obscured
galaxies) (Toba+2017) at
z~0.3-1.0• IR-bright obscured QSOs atz~1.5 (Perna+2015) and z~2.5(Zakamska+2016)• J0916a:• one of the fastest at inter-z;• even comparable with samples
at peak-epoch of AGN activity

Power source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF

Power source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALEPower source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALE• Stars+AGN+Dust+RadioPower source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALE• Stars+AGN+Dust+Radio• FracAGN = 0.09±0.01

Power source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALE• Stars+AGN+Dust+Radio• FracAGN = 0.09±0.01• LAGN = 6.06±0.21 E+11 L⊙

Power source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALE• Stars+AGN+Dust+Radio• FracAGN = 0.09±0.01• LAGN = 6.06±0.21 E+11 L⊙• Ldust = 5.31±0.15 E+12 L⊙

Power source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALE• Stars+AGN+Dust+Radio• FracAGN = 0.09±0.01• LAGN = 6.06±0.21 E+11 L⊙• Ldust = 5.31±0.15 E+12 L⊙• SFR = 915±27 M⊙/yr

Power source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALE• Stars+AGN+Dust+Radio• FracAGN = 0.09±0.01• LAGN = 6.06±0.21 E+11 L⊙• Ldust = 5.31±0.15 E+12 L⊙• SFR = 915±27 M⊙/yr• PSF = 7E+41 * SFR• PSF = 6.41E+44 erg/sPower source of fast outflow: 2) in Energetics view
• Method: calculate the energy ejection rate dEout/dt, then derive thecupping efficiencies of dEout/dt with the AGN bolometric luminosity
LAGN and star-formation power PSF.
• 1) estimate LAGN and PSF• SED fitting via CIGALE• Stars+AGN+Dust+Radio• FracAGN = 0.09±0.01
LAGNmaximum= 6.06±0.21
mechanicalE+11 L⊙• theenergy injection fromand stellar
winds• supernovae
Ldust = 5.31±0.15
E+12 L⊙• (Veilleux+2005)
SFR = 915±27 M⊙/yr• PSF = 7E+41 * SFR• PSF = 6.41E+44 erg/sPower source of fast outflow: 2) in Energetics view• 1) estimate LAGN and PSF• LAGN = 6.06E+11 L⊙ = 2.32E+45 erg/s• PSF = 7E+41 * SFR = 6.41E+44 erg/sPower source of fast outflow: 2) in Energetics view• 1) estimate LAGN and PSF• LAGN = 6.06E+11 L⊙ = 2.32E+45 erg/s• PSF = 7E+41 * SFR = 6.41E+44 erg/s• 2) calculate dMout/dt and dEout/dt

Power source of fast outflow: 2) in Energetics view• 1) estimate LAGN and PSF• LAGN = 6.06E+11 L⊙ = 2.32E+45 erg/s• PSF = 7E+41 * SFR = 6.41E+44 erg/s• 2) calculate dMout/dt and dEout/dt• Assuming a spherical volume of outflowing ionized gas (Harrison+2014), dMout/dt and dEout/dt can be derived via:
Ṁout 2
3Mout vṀout =, Ėout =(v + 3 2 ),Rout
2<latexit sha1_base64="2D0ND88BVd3dtozVUohsUMECtcM=">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</latexit>Power source of fast outflow: 2) in Energetics view• 1) estimate LAGN and PSF• LAGN = 6.06E+11 L⊙ = 2.32E+45 erg/s• PSF = 7E+41 * SFR = 6.41E+44 erg/s• 2) calculate dMout/dt and dEout/dt• Assuming a spherical volume of outflowing ionized gas (Harrison+2014), dMout/dt and dEout/dt can be derived via:
Ṁout 2
3Mout vṀout =, Ėout =(v + 3 2 ),Rout
2<latexit sha1_base64="2D0ND88BVd3dtozVUohsUMECtcM=">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</latexit>• where the mass of outflowing gas can be obtained from [OIII] or Hα(broad component):ne
8 Lcor ([OIII])1
Mout ([OIII]) = 5.33 ⇥ 10 ( 44
)(
)
M
1
3
10 erg s
100 cm<latexit sha1_base64="6cyALAOmbXAQKdJLmUKKABXkzP0=">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</latexit>ne
Lcor (H↵)
1
Mout (H↵) = 2.33 ⇥ 10 ( 43
)(
)
M .
1
3
10 erg s
100 cm8<latexit sha1_base64="ctrrAM7ZuIU2wyKB6Jp29aH+pAg=">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</latexit>Power source of fast outflow: 2) in Energetics view• 1) estimate LAGN and PSF• LAGN = 6.06E+11 L⊙ = 2.32E+45 erg/s• PSF = 7E+41 * SFR = 6.41E+44 erg/s• 2) calculate dMout/dt and dEout/dt
dMout/dt

dEout/dt

dEout/dt / LAGN

dEout/dt / PSF[OIII] 5007

588 M⊙/yr

6.89E+44 erg/s

29.70%

107.49%Hα (broad)

467 M⊙/yr

3.52E+44 erg/s

15.17%

54.91%Power source of fast outflow: 2) in Energetics view• 1) estimate LAGN and PSF• LAGN = 6.06E+11 L⊙ = 2.32E+45 erg/s• PSF = 7E+41 * SFR = 6.41E+44 erg/s• 2) calculate dMout/dt and dEout/dt
dMout/dt

dEout/dt

dEout/dt / LAGN

dEout/dt / PSF[OIII] 5007

588 M⊙/yr

6.89E+44 erg/s

29.70%

107.49%Hα (broad)

467 M⊙/yr

3.52E+44 erg/s

15.17%

54.91%• Based on the BPT-diagram and energetics analyses, we suggest that
AGN may play a dominant role in powering the outflow.

Power source of fast outflow: 2) in Energetics view

Power source of fast outflow: 2) in Energetics view

Power source of fast outflow: 2) in Energetics view

Power source of fast outflow: 2) in Energetics view
• The estimation of dEout/dt
depends on the assumption of
outflow velocity.

Power source of fast outflow: 2) in Energetics view
• The estimation of dEout/dt
depends on the assumption of
outflow velocity.
• Harrison+2014:
3Mout vṀout =,Rout
1Ėout = Ṁout (v 2 + 3 2 )2<latexit sha1_base64="tybeImS19OBPrHbVFzeuRgQ3KJc=">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</latexit>Power source of fast outflow: 2) in Energetics view
• The estimation of dEout/dt
depends on the assumption of
outflow velocity.
• Harrison+2014:
3Mout vṀout =,Rout
1Ėout = Ṁout (v 2 + 3 2 )2• Toba+2017:p
3Mout 2 v 2 + 2
Ṁout =,Rout
1Ėout = Ṁout (4v 2 + 4 2 )2<latexit sha1_base64="tybeImS19OBPrHbVFzeuRgQ3KJc=">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</latexit><latexit sha1_base64="/xxv7u7fleejVL7b82PZoV1dFW4=">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</latexit>Power source of fast outflow: 2) in Energetics view
• The estimation of dEout/dt
depends on the assumption of
outflow velocity.
• Harrison+2014:
3Mout vṀout =,Rout
1Ėout = Ṁout (v 2 + 3 2 )2• Toba+2017:p
3Mout 2 v 2 + 2
Ṁout =,Rout
1Ėout = Ṁout (4v 2 + 4 2 )2<latexit sha1_base64="tybeImS19OBPrHbVFzeuRgQ3KJc=">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</latexit><latexit sha1_base64="/xxv7u7fleejVL7b82PZoV1dFW4=">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</latexit>• electron density -> 100 cm^-3

Power source of fast outflow: 2) in Energetics view• Intense outflow in J0916a

Power source of fast outflow: 2) in Energetics view• Intense outflow in J0916a• ~ objects with 10-30 times
brighter luminosity.

Power source of fast outflow: 2) in Energetics view• Intense outflow in J0916a• ~ objects with 10-30 times
brighter luminosity.
• Why is the AGN relatively faint?

Power source of fast outflow: 2) in Energetics view• Intense outflow in J0916a• ~ objects with 10-30 times
brighter luminosity.
• Why is the AGN relatively faint?
• dEout/dt: from ionized gas
emission linePower source of fast outflow: 2) in Energetics view• Intense outflow in J0916a• ~ objects with 10-30 times
brighter luminosity.
• Why is the AGN relatively faint?
• dEout/dt: from ionized gas
emission line
• —> NLR / ionization cone

Power source of fast outflow: 2) in Energetics view• Intense outflow in J0916a• ~ objects with 10-30 times
brighter luminosity.
• Why is the AGN relatively faint?
• dEout/dt: from ionized gas
emission line
• —> NLR / ionization cone
• LAGN: from MIR luminosityPower source of fast outflow: 2) in Energetics view• Intense outflow in J0916a• ~ objects with 10-30 times
brighter luminosity.
• Why is the AGN relatively faint?
• dEout/dt: from ionized gas
emission line
• —> NLR / ionization cone
• LAGN: from MIR luminosity• —> dusty torus

Extreme outflow with fading AGN

Extreme outflow with fading AGN

MIRExtreme outflow with fading AGN

MIR

1-10 pc

Extreme outflow with fading AGN
Ionized emission

MIR

1-10 pc

Extreme outflow with fading AGN
Ionized emission
100 pc - 1kpc

MIR

1-10 pc

Extreme outflow with fading AGN
Ionized emission
100 pc - 1kpc

MIR

1-10 pc
Possible explanation: the outflow traced by ionized emission
reflects the historical effect of AGN when it was brighter.

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 1) Due to the variability of AGN• Transmission timescale: Rout / vout ~ 6 kpc / 1000 km/s ~ 6 Myr
100

AGN variations over one star formation ‘episode’

Eddington ratio

Luminous radiative AGN
10-2

LAGN~1044 erg s-1(for MBH=108 M O• )

5 Myr

10-4

Typically not observableas radiative AGN

10-6
10

-8

0

Simulation (Novak+11)
20

40
Time [Myr]60

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 1) Due to the variability of AGN• Transmission timescale: Rout / vout ~ 6 kpc / 1000 km/s ~ 6 Myr
100

AGN variations over one star formation ‘episode’

outflow was launched

Eddington ratio

Luminous radiative AGN
10-2

LAGN~1044 erg s-1

observed torus/MIR(for MBH=108 M O• )

5 Myr

10-4

Typically not observableas radiative AGN

10-6
10

-8

0

Simulation (Novak+11)
20

40
Time [Myr]60

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 2) Due to the self-regulation of SMBH growth

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 2) Due to the self-regulation of SMBH growth• dMout/dt ~ 500 M⊙/yr

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 2) Due to the self-regulation of SMBH growth• dMout/dt ~ 500 M⊙/yr• AGN exhausts its gas
reservoirs, resulting
decreasing accretion.

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 2) Due to the self-regulation of SMBH growth• dMout/dt ~ 500 M⊙/yr• AGN exhausts its gas
reservoirs, resulting
decreasing accretion.

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 2) Due to the self-regulation of SMBH growth• dMout/dt ~ 500 M⊙/yr• AGN exhausts its gas
reservoirs, resulting
decreasing accretion.

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 2) Due to the self-regulation of SMBH growth• dMout/dt ~ 500 M⊙/yr• AGN exhausts its gas
reservoirs, resulting
decreasing accretion.
• contrary to intense starformation (~ 900 M⊙/yr)

Extreme outflow with fading AGN• Outflow reflects historical effect of AGN• —> Currently AGN is in a fading process.
• 2) Due to the self-regulation of SMBH growth• dMout/dt ~ 500 M⊙/yr• AGN exhausts its gas
reservoirs, resulting
decreasing accretion.
• contrary to intense starformation (~ 900 M⊙/yr)

Summary and Future WorkSummary and Future Work• Eight objects from AKARI FIS Bright Source Catalog were firstly
identified as ULIRGs at z=0.3~0.6 using Subaru/FOCAS.

Summary and Future Work• Eight objects from AKARI FIS Bright Source Catalog were firstly
identified as ULIRGs at z=0.3~0.6 using Subaru/FOCAS.
• One of the objects, J0916a shows extremely powerful outflow. in its
ionized emission line features. However, the AGN in J0916a isrelatively faint, the detected outflow may reflect the historicaleffect of AGN activity.

Summary and Future Work• Eight objects from AKARI FIS Bright Source Catalog were firstly
identified as ULIRGs at z=0.3~0.6 using Subaru/FOCAS.
• One of the objects, J0916a shows extremely powerful outflow. in its
ionized emission line features. However, the AGN in J0916a isrelatively faint, the detected outflow may reflect the historicaleffect of AGN activity.
• The co-existence of the high SFR (~ 900 M⊙/yr) with the strong
outflow can indicate that the galaxy is possibly in the intermediatestage of evolutionary that the feedback just become effective andbegin to sweep out the gas reservoirs.

Summary and Future Work• Further observations are required to reveal the characteristics of thegalaxy, e.g.,• IFU observation to find more details of the outflow structure,• Hard X-ray observation to penetrate the dust and directly detect
the AGN radiation,• sub-mm observation to determine whether the ionized outflow also
affect the cold molecular gas reservoirs.

Summary and Future Work• Further observations are required to reveal the characteristics of thegalaxy, e.g.,• IFU observation to find more details of the outflow structure,• Hard X-ray observation to penetrate the dust and directly detect
the AGN radiation,• sub-mm observation to determine whether the ionized outflow also
affect the cold molecular gas reservoirs.

Thanks for your attention!

Appendix.

No parameter velocity

Energy conserving bubble
The method assuming an energy
conserving bubble in a uniform medium isalso widely used to estimate the upper limitof energy ejection rates (Heckman+1990,
Nesvadba+2006, Harrison+2012, Harrison+2014), which results in the formula:
Rout 2vout
3
Ėout = 3.0 ⇥ 10 n0 (
) (
)
,
1
10 kpc 1000 kms
46<latexit sha1_base64="gJO5ZR0NeviYCcMuyFCggD6FlxI=">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</latexit>
sha1_base64="fnuFCA3EoVbh6+R/tZBlFU2Q4KQ=">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</latexit>
sha1_base64="7XWThP0RpEVF/1AqPhqvj27QupE=">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</latexit>

where n_0=0.5 is the ambient density.

Dust Extinction, HβInteracting components around broad [OII]3926Å region.
75

•

80

28

85

25

90

23

95

20

100

18

105

5650

16

110

5600

13

115

J0916a

5550

11

120

J0916b

5500

8.4

25

Fig.1 Subaru/FOCAS
spectral on [OII]3926Å.

30

6Integration
on [OII]3926Å

J0916aJ0916b

Possibleinteraction

Fig.3 Flux distribution
along slit direction on[OII]3926Å. An intercomponent is required
when fitting the outline(orange arrow). The
ratio of integrated flux
is 2.5:1.0:5.1(J0916b:inter:J0916a).
30
25
20

[OIII]

Hα+[NII]

184

100

205.1

173.4

105

247.7

168

110

331.9

165.3

115

80

5650

85

5600

90

5550

95

5500

164

120

Fig.2 Subaru/FOCAS
spectral on [OII]3926Å
without subtractingnight sky background.

499.7

163.3

25

[OII]

75

16

163

11
6

slit

J0916aNight sky line
[OI]5577Å

J0916b
2

Fig.4 SDSS image(inverted). The
distance between the
cores of two galaxies is2″ (~ 12 kpc).

the 8 sources are also detected in the IRAS Faint Source Catalog, but they have not been identified at all because of
their faintness in the optical. Although, they are extremely faint as an optical counterpart of the bright FIR source, they
are suﬃciently bright to be easily spectroscopically identified with 8-10m class telescope. Once the eﬀectiveness of thetype-2 QSO selection is confirmed, systematic search can be made with more than 50 AKARI sources with extremely
large FIR /Fopt , and the contribution of type-2 QSOs to the HyLIRGs population will be examined. Additionally, further
observations can be easily conducted thanks to their brightness: in X-ray with Chandra and XMM-Newton to constrain
their nuclear activity and Compton-thickness, and in radio with ALMA to evaluate their gas contents.
Reference: • Doi et al. 2015, PASJ, 67, 50 • Takita et al. 2015, PASJ, 67, 51 • Eser, Goto, Doi 2014, ApJ, 797, 54 •Goto et al. 2011, MNRAS, 410, 573 • Toba & Nagao 2016, ApJ, 820, 46 • Kim et al. 1998, ApJS, 119, 41
WISE 12um

21

AKARI

20

SDSS i [mag]

SDSS

18

SDSS-spec limit
for galaxies

17

Broad-line QSOs

16
15

13
0.01

13
12
11
10

AKARI detection limit

9

14

5”

νLν90 µm [Lsun]

14

19

15”

Our targets expected luminosity range

Our targets mag range

0.1

Redshift

1

8
0.01

0.1

1

Redshift

Figure 1: Left) Example of an identification with a faint optical counterpart. There is a bright WISE 12µm source within
the AKARI error circle (blue). A galaxy with i = 20.3 mag is associated with the WISE position. Left) Redshift vs.
i-band magnitude of the AKARI FIR sources spectroscopically-identified in the SDSS survey (blue and red). Red dots
indicate broad-line QSOs. Green dots represents LIRGs/ULIRGs in the IRAS 1Jy sample (Kim et al. 1998). Systematic
follow-ups of IRAS sources only roughly go down to SDSS spectroscopy limit. Right) Redshift vs. FIR luminosity. Samesymbols as in the left panel.