Galaxy Evolu?on Workshop 2018 at Ehime Univ.

Looking at dras?c AGN luminosity
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decline in Arp 187 within 10 yrs
Ichikawa et al. ’16
Ichikawa & Tazaki ’17
Ichikawa et al. ’18 in prep.

Kohei FRIS
Ichikawa(市川幸平)
fellow, Tohoku/Columbia
In collabora*on with

H.-J. Bae, Z. Haiman, M. Imanishi, K. Inayoshi, T. Kawamuro, M. Koss, N. Levenson, E. LopezRodriguez, K. Matsuoka, R. NikuGa, C. Packham, C. Ricci, M. Schirmer, M. Shidatsu, R. Tazaki, B.
Trakhtenbrot, Y. Toba, J. Ueda, Y. Ueda
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Credit: ESO/M. Kornmesser

Galaxy Evolu?on Workshop 2018 at Ehime Univ.

“Dying AGN” in Arp 187
Ichikawa et al. ’16
Ichikawa & Tazaki ’17
Ichikawa et al. ’18 in prep.

Kohei FRIS
Ichikawa(市川幸平)
fellow, Tohoku/Columbia
In collabora*on with

H.-J. Bae, Z. Haiman, M. Imanishi, K. Inayoshi, T. Kawamuro, M. Koss, N. Levenson, E. LopezRodriguez, K. Matsuoka, R. NikuGa, C. Packham, C. Ricci, M. Schirmer, M. Shidatsu, R. Tazaki, B.
Trakhtenbrot, Y. Toba, J. Ueda, Y. Ueda
2

Credit: ESO/M. Kornmesser

Ac?ve Galac?c Nuclei (AGN)
Rees 84;Antonucci & Miller 85; Urry & Padovani95

GalaxySupermassive Black Hole (SMBH)

AGN

dusty torus<10 kpc<10 pc(see Ichikawa+15, Burtscher+13)

Why do we observe AGN for SMBH studies?

☑ AGN is a growing phase of SMBH
☑ easy to es*mate BH mass (e.g., single-epoch method; Kaspi+00,05)☑ Very, very bright in op*cal/UV (and also X-ray, IR!)
Lbol >= 1047 erg/s; which canbe observable even at z~7!
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AGN is bright at all wavelengthfrom R. Hickox’s talk at elusive AGN workshop

dust torus

accre?ondisk
narrow line
regions (NLRs)

coronaAtoAGN is bright at all wavelength (=mul? physical scale)
op?cal/UV(accre?on disk)
X-ray (corona)<10 pcMIR (torus)
uniﬁed motorus del: Antonsize: Jaﬀe+0ucci & Mille4, Hoer
nig+1285; Urry &Pa,13, Burtsche dovani 95
ionized r+13, +16

gas region(NLR)

De[OIII]λ5007ⓒNASA<1 kpcAGN jet1-10 GHzcpk00: 1-1

AGN is bright at all wavelength (=mul? physical scale)
Torus vs. central engine

NLR vs. central engine+ type-1
× type-2

Ichikawa+17a (see also Ichikawa+12)

Ueda, Hashimoto, Ichikawa+15

see also Berney+15 (BASS team result)☑ strong L-correla?on among each AGN component=> AGN should be stably bright for over 103-4 yrs(since NLR size is ~ 1 kpc~ 3000 light yrs)

There are mul?ple AGN indicators
andeach AGN indicator traces “diﬀerent”
physical scale
and this gives us the good science results!!
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Key ques?on: AGN life?me
AGN life ?me: observa?onally poorly constrained☑ Total Accre?on ?me scale: 107-9 yr (e.g., Marconi+04)☑ One AGN lifecycle: 105 yrs?
(AGN ﬂickering; Hopkins & Quataert ’10; Novak+11; Schawinski+15;
see also Schirmer+16, Kawamuro (incl. KI)+17 on the thermal echo)

How fast do AGN drop its luminosity?
☑ 1-2 orders of mag in 105 yr?

(Hanny’s voorwerps e.g., Schawinski+10; Keel+12,15,16, Sartori+17)☑ 1 order of mag in 10 yr(changing-look QSO/AGN; Tohlin & Osterbrock ‘76 ;LaMassa+15, MacLeod+16)

It might be highly related to AGN accre?on disk state?

Here I report an interes?ng8 AGN

Arp 187
Arp187: Merger remnant LIRG (Rothberg & Joseph ‘04)
red 3mm con?nuum

Ueda+14

ALMA observa?ons (Ueda+14)☑ CO(1-0) associates with host galaxy K band emission☑ 3mm con*nuum does not associate with CO(1-0) distribu*ons☑ Some dusty ouhlow occurs?
orradio-jet?
9Arp 187: VLA observa?ons
VLA 5, 8.5 GHz show bipolar jet lobes

Ichikawa+18 in prep.

Jet proper?es☑ Both lobes show spec index α=-1 => synchrotron jet☑ jet kine*c age: 6×104 yr (jet angle=90° w/ v=0.1c)☑ jet core seems absent (f5GHz < 210 μJy )=> current AGN ac?vity might be silent?
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Op?cal spectrum = NLR ac?vity (~ kpc)
BPT diagram: NLR (probably) exists

Ichikawa+18 in prep.

6dF (6.7’’)
spectrum

Op?cal proper?es: suggest quasar class luminosity☑ detec*ons of Ha, [NII], [SII], [OI]λ6300, [OIII]λ5007, Hb☑ log L[OIII](int) =42.5, log L[OI](int)=42.3 => log Lbol = 46.2 (Netzer ’09)11

mid-IR = torus ac?vity (<10 pc)
Spitzer/IRS (w/4.5’’): SB dominant spectra=> AGN torus emission (<10pc) is faintObserved spec
SB template

Ichikawa+16☑ log L12um < 42.2 => L2-10keV < 42.5 => Lbol < 43.3
(see also Gandhi+09; Ichikawa+12;+17)
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X-ray (= electron corona << 0.1 pc)

No previous deep X-ray observa?ons for this target

Swiz/BAT all-sky survey (E=14-195 keV)
☑ Not listed in the catalog (Baumgartner+13)=> L14-195keV < 2.8×1043 erg s-1=> consistent w/IR upper limit: L14-195keV < 5.9×1042 erg s-1

ROSAT all-sky survey (E=0.5-2 keV)
☑ Not listed in the catalog (Voges+99)=> L0.5-2keV < 8.8×1042 erg s-1=> consistent w/IR upper limit: L0.5-2keV < 2.0×1042 erg s-1(Γ=1.9; e.g., Brightman+13)

Not located in the XMM-slew survey region=> Obs. w/ Nustar, XARM, and/or Chandra is crucial=> NuSTAR (cycle-4) obs. is awarded! (PI: KI)
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BH mass of Arp 187
Using MBH - Mbulge rela?on, we es?mate MBH.
☑ LKband => Mstellar = 1.3×1011 Msun w/nsersic ~ 4 (Rothberg & Joseph ‘04)=> Mstellar ~ Mbulge=> MBH ~ 7×108 Msun (Kormendy & Ho 2013)14

BH fundamental plane
If you have either two values of L5GHz (core), L2-10keV, MBH,
then you can es?mate the ﬁnal one.
Merloni+03
Heinz+03
Yuan+14Upper limit of LR, and MBH are given, then☑ log L2-10keV < 39.6 => log Lbol < 40.915

What is happening in Arp 187?
☑ Signs of NLR, jet (> kpc)
☑ Absence of torus, radio core (<10 pc scale) (NLR)☑ AGN “was” ac*ve ~103-4 yrs ago, but AGN “is” dead => dying AGN
normal AGN
ionized cone (NLR; [OIII]5007)

dying AGN
ionized cone (NLR; [OIII]5007)

Ichikawa+16;+17~1 kpc

host galaxy

no current
AGN(X-ray, MIR) AGN ac?vity(X-ray, MIR, radio-core)(e.g., Schawinski+15; Ichikawa+16; Ichikawa & Tazaki ’17)
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AGN “light curve” of Arp 187
Ichikawa et al. (2018) in prep.

Ichikawa+18

LAGN: 103-4 ?mes fainter in ~103-4 yr
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Next ques?ons: searching more dying AGN, but How?

LAGN decreases at least 103-4 ?mes in ~103-4 yr…but, only one source yet!
1. How long can we observe AGN torus azer AGN quenching?
☑ see Ichikawa & Tazaki ’17, ApJ, 844, 21

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Searching more dying AGN☑ L(12um=torus) vs. L[OIII] (=NLR) is a good plane to search dying AGN
Ichikawa & Tazaki ‘17

Ltorus drops by a factor of 100
within 100yrs

Torus luminosity(current AGNac?vity)

Ichikawa & Tazaki ‘17log(電離領域光度[erg/s])

NLR luminosity (past AGN ac?vity)

Conclusion and Summary☑ AGN is bright at all-wavelength, and each band traces thediﬀerent AGN component with diﬀerent physical scale☑ We found a “dying” AGN in Arp 187, whose current AGN ac?vity
is already quenched, but past AGN ac?vity is s?ll observable.
☑ AGN drops its luminosity by a factor of 103-4 within 103-4 yrs☑ AGN torus cools down rapidly with <100 yrs. Finding outliers inthe L(torus) vs. L(NLR) rela?on is a promising method to searchdying AGN

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AGN torus: WISE IR color-color diagram

Ichikawa+18 in prep.
Ichikawa+16☑ WISE IR color-color cannot pick up Arp 187 as AGN☑ L12um(AGN) would be already weak, and probably < 1043 erg/s(see Ichikawa+17)
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What is happening in Arp 187?
☑ Signs of NLR, jet (> kpc)
☑ Absence of torus, radio core(<10 pc scale)

FYI; torus cools downin <100 yr (Ichikawa & Tazaki ’17b)
AGN “was” ac*ve ~103-4 yr ago,but currently AGN “is” dead.

cp01<DⓒNAS
ANarrow
LineRegion 1-10 kpc
jet <10 kpc“AGN light echo” is powerful tool to know AGN acQvity history
see Hanny’s Voorwerp (104-5 yr ago; LintoG+09, Schawinski+10, 15; Keel+12)
or the galac*c center (500 yr ago; Pon*+10; Capelli+12; Ryu+13; Nakashima+14)
or Fermi bubbles study (106 yr ago; Zubovas+11, 12; SU & Finkbeiner ’12)22

Torus cools down in 10-100 yrs
Ichikawa & Tazaki ‘17

Ichikawa & Tazaki ’17

One big assump?on: AGN shut-down abruptly
Considering the energy exchange between the dust and gas
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