shen#etal.#2010# fu#etal.#2011c#€¦ · • use#smoothed#par:cle#hydrodynamics#code# gadget3 •...
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Fu et al. 2011c
Shen et al. 2010
Early merger phase only.
Difficult/impossible to resolve spa9ally.
102
101
100
10-‐1
10-‐2
10-‐3
10-‐4
kpc
• Use smoothed par:cle hydrodynamics code GADGET-‐3
• Contains prescrip:ons for star forma:on, BH accre:on, and SF & AGN feedback
• Simulate merger of two galaxies with central SMBHs
• Construct NLR model in post-‐processing using gas proper:es & kinema:cs, and MBH
• Not including: obscura1on/sca3ering by dust, stellar/AGN ou9lows
.
• Es:mate ionizing photon flux, Q, from MBH (Bondi) • Choose SPH (gas) par:cles that sa:sfy:
(1) Nonzero mass in “cold” gas
(2) Total covering frac:on of cold clouds < 1 (3) Reasonable ranges of ρgas and ioniza:on parameter
• Calculate Hβ luminosity of the “NL-‐emi]ng” clouds in each SPH par:cle sa:sfying (1)-‐(3):
.
dNL AGN induced directly by BH mo:on: -‐ Two dis:nct NLRs -‐ offset by rela:ve BH mo:on -‐ account for a minority of double-‐peaked NL AGN
BH separa,on = 2.3 kpc
dNL AGN induced directly by BH mo:on: -‐ Common NLR -‐ One BH more ac:ve than other -‐ At least 10-‐40% should be sub-‐kpc-‐scale
BH separa,on = 0.17 kpc
150 kpc
Fabbiano et al. 2011
Comerford et al. 2011
dNL AGN influenced by BH mo:on: -‐ Offset double peak in 1 NLR -‐ Offset single peak in other NLR -‐ Up to 80%* affected directly or indirectly (* rota:on in gas disk; also expect ou9lows)
BH separa,on = 1.1 kpc
Early merger phase
kpc-‐scale phase
Post-‐BH merger phase
Observable dNL profile with one AGN (Lbol > LAGN)
Observable dNL profile with two AGN
Strong dependence on observer LOS, also on galaxy merger parameters
15 kpc 43 kpc 43 kpc
BH separa,on = 2.3 kpc BH separa,on = 0.17 kpc
• Measurable overall velocity offset (>~ 150 km/s)
• Large peak velocity spli]ng (>~ 500 km/s)
