spectroscopic search for binary supermassive black holes · 2012. 11. 30. · cgwp spectroscopic...
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CGWP
Spectroscopic Search for Binary Supermassive
Black Holesby Mike Eracleous
spectroscopists: Todd BorosonJules Halpern& Jia Liu
thinkers: Steinn Sigurđsson, Tamara Bogdanović& Hélène Flohic
interferometrists:Sarah Burke-SpolaorJoe Lazio& Joan Wrobel
imagists:Tod Lauer
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The Elusive, Bound Binaries
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1983LIACo..24..473G
3C 227
figure from Gaskell (1983)
In the beginning...
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figure from Eracleous et al. (1997)
from Gaskell (1996)
Double-Peaked Emitters
from
She
n &
Loeb
(201
0)
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figures from Eracleous et al. (1997) ~30 cases now; see Gezari et al. (2007); Lewis et al. (2010); Flohic (2009)
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figures from Shen & Loeb (2010)
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SDSS J1536+0441: old ideas resurrected
Boroson & Lauer 2009, Nature, 458, 53
Rest Wavelength (Å)
ƒ λ (1
0–17 e
rg/s
/cm
2 /Å)
Hβ
[O III]z=0.3727
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A Systematic Search for Close, Bound Binaries
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Figure from Artymowicz & Lubow 1996,ApJ, 467 L77
The hypothesis: only one BH is “active”
Figure from Cuadra et al. 2009, MNRAS, 393, 1423see also Hayasaki et al. 2007, PASJ, 59, 427
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Boroson & Lauer 2009, Nature, 458, 53
Rest Wavelength (Å)
ƒ λ (1
0–17 e
rg/s
/cm
2 /Å)
Hβ
[O III]z=0.3727
u2
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V2
We observe:
u2 = V2 sin i sin φ
V2 sin i sin φ 103 km/su2,3 =
Expected Binary Properties
P =332 M8
(1 + q)3 u32,3
✓sin i
sin 45�| sin �|sin 45�
◆3
yr and a =0.11 M8
(1 + q)2 u22,3
✓sin i
sin 45�| sin �|sin 45�
◆2
pc.
P =332 M8
(1 + q)3 u32,3
✓sin i
sin 45�| sin �|sin 45�
◆3
yr and a =0.11 M8
(1 + q)2 u22,3
✓sin i
sin 45�| sin �|sin 45�
◆2
pc.
����du2
dt
���� = 19
u42,3(1 + q)3
M8km/s/yr
✓sin 45
�
sin i
◆3 ✓sin 45
�
sin�
◆4 | cos�|cos 45
�
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Selection of Candidates from SDSS
Spectroscopic PCA used to find quasars with “oddball” Hβ profiles.
start with z < 0.7 quasars from SDSS DR7
tune of PCA technique to find offset line peaks
~900 candidates ➠ final filtering by visual inspection
at the end of the day: 88 candidates
Volonteri et al 2009 predict ~130 such binaries in the SDSS DR7 spectroscopic sample (~17,000 quasars)
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Rest Wavelength (Å)
ƒ λ (1
0–17 e
rg c
m–2
s–1 Å
–1) χ2=0.91 χ2=0.90
Reconstruction of Line Profiles Using First 5 Eigenspectra
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Rest Wavelength (Å)
ƒ λ (1
0–17 e
rg c
m–2
s–1 Å
–1) χ2=5.83 χ2=3.12
Reconstruction of Line Profiles Using First 5 Eigenspectra
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velocity (km/s)
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Distribution of Velocity Offsets
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υ0
υ0
Correlation between skewness and shift
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Followup Observations
“2nd epoch”Dec 2009 - Mar 2011
MDM 2.4m Hiltner
KPNO 4m Mayall
Palomar 5m Hale
9.2m Hobby-Eberly
“3rd epoch”just completed
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Caveats: Pandora’s Box
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examples from Gezari, Halpern, & Eracleous (2007)
Velocity (103 km/s)
ƒ ν
3C 390.3 Arp 102B PKS 0235+023
Displaced Peaks Do NOT Always Mean Binaries!
from Gezari, Halpern & Eracleous (2007)
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from Eracleous et al. (1997)
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Nor Do Displaced Peaks that Move!
from Eracleous et al. (1997)including data from Gaskell (1996)
Gezari, Halpern & Eracleous (2006)see also Marziani et al. (1996)
Mrk 668
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from Lewis, Eracleous, & Storchi-Bergmann (2010)
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So far, so god, so what?
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Theoretical predictions of population size in broad agreement with observed numbers. We can pick out the short-period binaries (P~10–20 yr) from repeating patterns, even though these will be short-lived.We will learn a lot about the dynamics of the gas in the broad-line region in the process.
Reasons to be (cautiously) optimistic...
Therefore, we push on...
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Continue monitoring observationsverify velocity variations
check for monotonic velocity changes: 3 epochs can constrain a sinusoid ⇒ lower bound on the mass
Simulations of the population properties and assessment of impostors
Optical and radio imaging: test for recoiling BHsHST and EVLA + VLBI
Spectroscopic Test for Perturbed Accretion DisksInvolves comparison of Balmer and Lyman line profiles.
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End of story
for now...