Searching for pairs of accreting supermassive black holessabotin.ung.si › ~agomboc ›...
Transcript of Searching for pairs of accreting supermassive black holessabotin.ung.si › ~agomboc ›...
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Searching for pairs of accreting supermassive black holes
K. É. Gabányi1, S. Frey1, Z. Paragi2, T. An3, S. Komossa4
1SGO, Hungary; 2JIVE, the Netherlands; 3SHAO, P.R.China; 4MPIfR, Germany
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Why?• Galaxies grew via merging
events ⇒ the central BHs merge ⇒ dual/binary BH systems are expected to exist
• AGNs are “easy” to observe compared to non-active SMBHs
• Simultaneous activity is most likely at kpc-scale separation (e.g., van Wassenhove et al., 2012; Fu et al., 2015)
Simulated evolution of a 1:2 spiral–spiral merger
Van Wassenhove+ 2012, ApJ 748, L7
Strong dual AGN activity is expected at small separations (d<1...10 kpc)
Periods of accretion are not necessarily simultaneous in the two components
Small detectable fraction is expected (a few per cent)
van Wassenhove et al. 2012
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Examples
Komossa et al., 2003 Beswick et al., 2001
NGC 6240
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Examples
Komossa et al., 2003 Beswick et al., 2001
NGC 6240
3C75
Hudson et al., 2006
Mrk 739
Koss et al., 2011
LBQS 0103-2753
Junkkarinen et al. 2001
Mrk 463
Bianchi et al. 2008
0402+379
Rodriguez et al. 2006
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How to find them?
• Double-peaked narrow optical emission lines - originating from the two distinct NLRs?
• >70% of the double-peaked AGN are isolated AGN (Fu et al., 2011) • Other reasons behind double-peaked: jet-cloud interaction, rotating
NLR, outflowing NLR, blobby NLR + extinction, single AGN illuminating the ISM of two merging galaxy,… (Xu & Komossa, 2009; Crenshaw et al., 2010; Heckman et al., 1984)
?
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How to find them?
• Double-peaked narrow optical emission lines - originating from the two distinct NLRs?
• >70% of the double-peaked AGN are isolated AGN (Fu et al., 2011) • Other reasons behind double-peaked: jet-cloud interaction, rotating
NLR, outflowing NLR, blobby NLR + extinction, single AGN illuminating the ISM of two merging galaxy,… (Xu & Komossa, 2009; Crenshaw et al., 2010; Heckman et al., 1984)
?
• Double-peaked + Spatially compact emissions, along the host galaxy axes, an indication for a pair of AGN? (Comerford et al., 2012)
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How to find them?
• Double-peaked narrow optical emission lines - originating from the two distinct NLRs?
• >70% of the double-peaked AGN are isolated AGN (Fu et al., 2011) • Other reasons behind double-peaked: jet-cloud interaction, rotating
NLR, outflowing NLR, blobby NLR + extinction, single AGN illuminating the ISM of two merging galaxy,… (Xu & Komossa, 2009; Crenshaw et al., 2010; Heckman et al., 1984)
?
• Double-peaked + Spatially compact emissions, along the host galaxy axes, an indication for a pair of AGN? (Comerford et al., 2012)
• Variability in continuum/emission lines? (e.g. Popovic, 2012, Bon et al., 2012, Charisi et al., 2016)
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How to find them?
• Double-peaked narrow optical emission lines - originating from the two distinct NLRs?
• >70% of the double-peaked AGN are isolated AGN (Fu et al., 2011) • Other reasons behind double-peaked: jet-cloud interaction, rotating
NLR, outflowing NLR, blobby NLR + extinction, single AGN illuminating the ISM of two merging galaxy,… (Xu & Komossa, 2009; Crenshaw et al., 2010; Heckman et al., 1984)
?
• Double-peaked + Spatially compact emissions, along the host galaxy axes, an indication for a pair of AGN? (Comerford et al., 2012)
• Variability in continuum/emission lines? (e.g. Popovic, 2012, Bon et al., 2012, Charisi et al., 2016)
• Checking VLBI archival observations Burke-Spolaor (2011): 1/3114
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Examples of double-peaked sources followed up by radio interferometric
observations
• Tingay & Wayth (2011): 0/11 (VLBA) • Müller-Sanchez et al. (2015): 3/18 (VLA) • Gabányi et al. 2016: 0/4 (VLBA)
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Examples of double-peaked sources followed up by radio interferometric
observations
• Tingay & Wayth (2011): 0/11 (VLBA) • Müller-Sanchez et al. (2015): 3/18 (VLA) • Gabányi et al. 2016: 0/4 (VLBA)
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Examples of double-peaked sources followed up by radio interferometric
observations
• Tingay & Wayth (2011): 0/11 (VLBA) • Müller-Sanchez et al. (2015): 3/18 (VLA) • Gabányi et al. 2016: 0/4 (VLBA)
• Bondi & Pérez-Torres (2010): a pair of sub-mJy AGN at 5 kpc separations (EVN)
• Fu et al. (2011): double in near-infrared, dual radio-emitters (sub-mJy, 7.4 kpc) (VLA) ➞ even triple? Deane et al. Nature 2014
• Yang et al. (2016): in NGC 5252 an ULX turned out to be AGN (EVN), see also poster #5 by Minjin Kim
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The case of J1425+3231
Hβ 4861Å O[III]
4959Å
O[III] 5007Å
Peng et al., 2011, RAA, 11, 141
SDSS spectrum
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The case of J1425+3231
Hβ 4861Å O[III]
4959Å
O[III] 5007Å
Peng et al., 2011, RAA, 11, 141
SDSS spectrum
8.3 × 107 M⊙ 3.4 × 106 M⊙
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European VLBI Network observations
1.7 GHz - 2011 Jan 265 GHz - 2011 Oct 18
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EVN results at 1.7 GHz
443 mas 2.6 kpc
Frey et al., 2012, MNRAS, 425, 1185
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EVN results at 1.7 GHz460 μJy
230 μJy
443 mas 2.6 kpc
C
S
Frey et al., 2012, MNRAS, 425, 1185
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EVN results1.7 GHz
Frey et al., 2012, MNRAS, 425, 1185
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EVN results
• Only the brighter (C) feature was detected
• flat spectrum, 𝛼=−0.23
• brightness temperature: 108K ⇒ suggests AGN
• S: <0.085 mJy at 5 GHz ⇒
• steep spectrum, 𝛼<−0.9
1.7 GHz
5 GHz
Frey et al., 2012, MNRAS, 425, 1185
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e-MERLIN observations
1.6 GHz - 2015 Oct
5 GHz - 2014 Nov
Cm
De
Da
Kn
Pi
Mk2
Jb
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e-MERLIN results at 1.6 GHz
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e-MERLIN results at 1.6 GHzCONT: 1425+323 IPOL 1546.306 MHz 1425+3231 L.ICL001.1PLot file version 2 created 01-SEP-2016 11:23:33
Cont peak flux = 8.3638E-04 JY/BEAMLevs = 1.000E-04 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.37 07.36 07.35 07.34 07.33 07.32 07.31 07.30 07.29 07.28
32 31 38.0
37.8
37.6
37.4
37.2
37.0
36.8
36.6
N
C
S
Peak: 840 μJy/beam 4σ: 100 μJy/beam
1.6 GHz
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e-MERLIN resultsCONT: 1425+323 IPOL 1546.306 MHz 1425+3231 L.ICL001.1PLot file version 2 created 01-SEP-2016 11:23:33
Cont peak flux = 8.3638E-04 JY/BEAMLevs = 1.000E-04 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.37 07.36 07.35 07.34 07.33 07.32 07.31 07.30 07.29 07.28
32 31 38.0
37.8
37.6
37.4
37.2
37.0
36.8
36.6
N
C
S
Peak: 840 μJy/beam 4σ: 100 μJy/beam
1.6 GHz
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e-MERLIN resultsCONT: 1425+323 IPOL 1546.306 MHz 1425+3231 L.ICL001.1PLot file version 2 created 01-SEP-2016 11:23:33
Cont peak flux = 8.3638E-04 JY/BEAMLevs = 1.000E-04 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.37 07.36 07.35 07.34 07.33 07.32 07.31 07.30 07.29 07.28
32 31 38.0
37.8
37.6
37.4
37.2
37.0
36.8
36.6
N
C
S
Peak: 840 μJy/beam 4σ: 100 μJy/beam
1.6 GHzCONT: 1425+323 IPOL 5072.518 MHz 1425+3231T-C.ICL001.10PLot file version 5 created 01-SEP-2016 14:12:53
Cont peak flux = 1.5363E-04 JY/BEAMLevs = 6.850E-05 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.340 07.335 07.330 07.325 07.320 07.315 07.310
32 31 37.65
37.60
37.55
37.50
37.45
37.40
37.35
37.30
C
5 GHz
Peak: 150 μJy/beam 4σ: 70 μJy/beam
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e-MERLIN resultsCONT: 1425+323 IPOL 1546.306 MHz 1425+3231 L.ICL001.1PLot file version 2 created 01-SEP-2016 11:23:33
Cont peak flux = 8.3638E-04 JY/BEAMLevs = 1.000E-04 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.37 07.36 07.35 07.34 07.33 07.32 07.31 07.30 07.29 07.28
32 31 38.0
37.8
37.6
37.4
37.2
37.0
36.8
36.6
N
C
S
712 μJy
1.6 GHzCONT: 1425+323 IPOL 5072.518 MHz 1425+3231T-C.ICL001.10PLot file version 5 created 01-SEP-2016 14:12:53
Cont peak flux = 1.5363E-04 JY/BEAMLevs = 6.850E-05 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.340 07.335 07.330 07.325 07.320 07.315 07.310
32 31 37.65
37.60
37.55
37.50
37.45
37.40
37.35
37.30
C
5 GHz1835 μJy
1122 μJy
319 μJy
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Explaining the radio data of J1425+3231
(I) single AGN:
• core - C
• N - jet
• S - lobe with a compact hotspot
(II) pair of AGN:
• C and S are cores
• N: one-sided jet of C
CONT: 1425+323 IPOL 1546.306 MHz 1425+3231 L.ICL001.1PLot file version 2 created 01-SEP-2016 11:23:33
Cont peak flux = 8.3638E-04 JY/BEAMLevs = 1.000E-04 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.37 07.36 07.35 07.34 07.33 07.32 07.31 07.30 07.29 07.28
32 31 38.0
37.8
37.6
37.4
37.2
37.0
36.8
36.6
N
C
S
712 μJy
1.6 GHz
1835 μJy
1122 μJy
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Explaining the radio data of J1425+3231
(I) single AGN:
• core - C
• N - jet
• S - lobe with a compact hotspot
(II) pair of AGN:
• C and S are cores
• N: one-sided jet of C
CONT: 1425+323 IPOL 1546.306 MHz 1425+3231 L.ICL001.1PLot file version 2 created 01-SEP-2016 11:23:33
Cont peak flux = 8.3638E-04 JY/BEAMLevs = 1.000E-04 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.37 07.36 07.35 07.34 07.33 07.32 07.31 07.30 07.29 07.28
32 31 38.0
37.8
37.6
37.4
37.2
37.0
36.8
36.6
N
C
S
712 μJy
1.6 GHz
1835 μJy
1122 μJy S is undetected at 5 GHz
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Explaining the radio data of J1425+3231
(I) single AGN:
• core - C
• N - jet
• S - lobe with a compact hotspot
(II) pair of AGN:
• C and S are cores
• N: one-sided jet of C
CONT: 1425+323 IPOL 1546.306 MHz 1425+3231 L.ICL001.1PLot file version 2 created 01-SEP-2016 11:23:33
Cont peak flux = 8.3638E-04 JY/BEAMLevs = 1.000E-04 * (-1, 1, 1.414, 2, 2.828, 4, 5.657,8, 11.31, 16, 22.63, 32, 45.25, 64, 90.51, 128, 181,256, 362, 512)
Decl
inat
ion
(J20
00)
Right Ascension (J2000)14 25 07.37 07.36 07.35 07.34 07.33 07.32 07.31 07.30 07.29 07.28
32 31 38.0
37.8
37.6
37.4
37.2
37.0
36.8
36.6
N
C
S
712 μJy
1.6 GHz
1835 μJy
1122 μJy S is undetected at 5 GHz
double-peaked lines are likely
related to outflows
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Conclusion
• Not everything is dual AGN which looks like a dual AGN
• We still need reliable indicators to assemble large sample of dual AGN candidates
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Conclusion
• Not everything is dual AGN which looks like a dual AGN
• We still need reliable indicators to assemble large sample of dual AGN candidates
If you see too many doubles: