Author Topic: Dual/Triple AGNs (found by astronomers)  (Read 20049 times)

zutopian

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Re: Dual/Triple AGNs
« Reply #30 on: March 14, 2012, 06:38:06 am »
"A New Collisional Ring Galaxy at z = 0.111: Auriga's Wheel"
Quote
Analysis of the spectroscopy reveals that the late type galaxy is a LINER class Active Galactic Nuclei while the early type galaxy is also potentially an AGN candidate, this is very uncommon amongst known collision ring galaxies.
Blair C. Conn, Anna Pasquali, Emanuela Pompei, Richard R. Lane, André-Nicolas Chené, Rory Smith, Geraint F. Lewis
(Submitted on 20 Jul 2011 (v1), last revised 25 Jul 2011 (this version, v2))
http://arxiv.org/abs/1107.4099

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Re: Dual/Triple AGNs
« Reply #31 on: May 08, 2012, 06:52:11 am »
"A data-driven model for spectra: Finding double redshifts in the Sloan Digital Sky Survey"
Quote
This method was applied to spectra of 54 586 and 3929 objects spectroscopically classified as QSOs and galaxies respectively in SDSS DR7, with 0.1<z<1.5 in order to detect more candidates of this type of object (Tsalmantza et al. 2011). The search resulted to 32 objects with peculiar spectra, nine of which can be interpreted as BHB candidates.
Quote
In a similar manner, we were able to recover a set of four previously known black-hole binary candidates.
In the future, we plan to perform comprehensive automatic searches for objects of these types in the entire SDSS spectroscopic data set.
Authors: P. Tsalmantza, David W. Hogg
(Submitted on 16 Jan 2012 (v1), last revised 7 May 2012 (this version, v2))
http://arxiv.org/abs/1201.3370
« Last Edit: May 08, 2012, 06:57:25 am by zutopian »

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Re: Dual/Triple AGNs
« Reply #32 on: June 07, 2012, 08:04:54 am »
HUBBLE SPACE TELESCOPE OBSERVING PROGRAM 12521
The Frequency and Demographics of Dual Active Galactic Nuclei
Quote
Abstract
Dual Active Galactic Nuclei (AGNs) are actively accreting supermassive black hole (SMBH) pairs co-rotating in merging galaxies with separations of less than a few kpc. Despite decades of searching, and strong theoretical reasons to believe they exist, unambiguously confirmed dual AGNs are surprisingly scarce, which contradicts naive Lambda-CDM prediction. We propose a SNAP survey with WFC3 to systematically identify dual AGNs. We exploit a well-tested technique, which has a success rate of 10-25% at least, based on the selection of AGNs with double-peaked [O III] emission lines. We have reached the limits of what we can learn from the ground. We request HST's superb image quality in both optical and NIR and its high sensitivity to explore a new regime of dual AGNs at a more advanced merger stage, inaccessible from the ground or any other space facility. With the proposed observations well suited for a SNAP program, we will determine the frequency of dual AGNs down to the smallest scales attainable with current facilities to test the hierarchical merger paradigm, and explore the demographics of dual AGNs as a function of separation to better understand the accretion and evolution of SMBH pairs in merging galaxies.

Quote
Target Names   
                               SDSSJ0002+0045, SDSSJ0006+1548, SDSSJ0009-0036, SDSSJ0107-0053, SDSSJ0116-1025, SDSSJ0118-0826,     
                               SDSSJ0135+1435, SDSSJ0135-0058, SDSSJ0142-0050, SDSSJ0156-0007, SDSSJ0400-0652, SDSSJ0731+4528,     
                               SDSSJ0735+4036, SDSSJ0736+4759, SDSSJ0738+3156, SDSSJ0741+3928, SDSSJ0749+4514, SDSSJ0752+2736,     
                               SDSSJ0802+3046, SDSSJ0803+3926, SDSSJ0804+3051, SDSSJ0807+3900, SDSSJ0808+4813, SDSSJ0814+2657,     
                               SDSSJ0821+5021, SDSSJ0828+0742, SDSSJ0842+0547, SDSSJ0846+4258, SDSSJ0851+1327, SDSSJ0853+2339,     
                               SDSSJ0854+5026, SDSSJ0855+6423, SDSSJ0858+1041, SDSSJ0902+0120, SDSSJ0912+5320, SDSSJ0914+2102,     
                               SDSSJ0915+3009, SDSSJ0916+2835, SDSSJ0921+5153, SDSSJ0924+0510, SDSSJ0930+3430, SDSSJ0941+1436,     
                               SDSSJ0941+3944, SDSSJ0942+1254, SDSSJ0950+4813, SDSSJ0952+2552, SDSSJ0955+3838, SDSSJ0958+2512,     
                               SDSSJ0958-0051, SDSSJ0959+2619, SDSSJ0959-0013, SDSSJ1006+4647, SDSSJ1009+0133, SDSSJ1011+3259,     
                               SDSSJ1012+4943, SDSSJ1016+2003, SDSSJ1018+5127, SDSSJ1019+0134, SDSSJ1023+3243, SDSSJ1027+1049,     
                               SDSSJ1027+3059, SDSSJ1033+2847, SDSSJ1034+3939, SDSSJ1038+0255, SDSSJ1042+3853, SDSSJ1044+3008,     
                               SDSSJ1056+3319, SDSSJ1108+0659, SDSSJ1108+1951, SDSSJ1108+5918, SDSSJ1109+0201, SDSSJ1110+0129,     
                               SDSSJ1110+0300, SDSSJ1112+2750, SDSSJ1113+1657, SDSSJ1118+0626, SDSSJ1123+3028, SDSSJ1123+3105,     
                               SDSSJ1125+0237, SDSSJ1126+2944, SDSSJ1126+4559, SDSSJ1129+3428, SDSSJ1129+5756, SDSSJ1129+6057,     
                               SDSSJ1131-0204, SDSSJ1137+1437, SDSSJ1137+6120, SDSSJ1139+0900, SDSSJ1141-0302, SDSSJ1145+4059,     
                               SDSSJ1146+5110, SDSSJ1146-0226, SDSSJ1148-0216, SDSSJ1150+0441, SDSSJ1152+1016, SDSSJ1152+1903,     
                               SDSSJ1156+0459, SDSSJ1157+5155, SDSSJ1158+3231, SDSSJ1203+0446, SDSSJ1203+1319, SDSSJ1203+2808,     
                               SDSSJ1205+3213, SDSSJ1207+4602, SDSSJ1208+2304, SDSSJ1215+0001, SDSSJ1219+1900, SDSSJ1221+6049,     
                               SDSSJ1222+2726, SDSSJ1227+1248, SDSSJ1235+0608, SDSSJ1236+2616, SDSSJ1236-0141, SDSSJ1238+3037,     
                               SDSSJ1239+5314, SDSSJ1240+3534, SDSSJ1243-0058, SDSSJ1245+3723, SDSSJ1249+3539, SDSSJ1301-0058,     
                               SDSSJ1307+1243, SDSSJ1315+2134, SDSSJ1316+1753, SDSSJ1321+5407, SDSSJ1322+2631, SDSSJ1323+0308,     
                               SDSSJ1323+1039, SDSSJ1325+5450, SDSSJ1327+2023, SDSSJ1328+2135, SDSSJ1328+2752, SDSSJ1332+0606,     
                               SDSSJ1332+4632, SDSSJ1333+3007, SDSSJ1337+0353, SDSSJ1341+2219, SDSSJ1343+1953, SDSSJ1350+2311,     
                               SDSSJ1352+0525, SDSSJ1352+6541, SDSSJ1356+1026, SDSSJ1405+2447, SDSSJ1408+0430, SDSSJ1416+3119,     
                               SDSSJ1420+4959, SDSSJ1441+0948, SDSSJ1441-0007, SDSSJ1445+3341, SDSSJ1448+1825, SDSSJ1450+0838,     
                               SDSSJ1452+5110, SDSSJ1453+2043, SDSSJ1458+2742, SDSSJ1459+2307, SDSSJ1500+3823, SDSSJ1502+1115,     
                               SDSSJ1504+3214, SDSSJ1516+0517, SDSSJ1516+1830, SDSSJ1517+1144, SDSSJ1517+3353, SDSSJ1521+2917,     
                               SDSSJ1523+2629, SDSSJ1524+2743, SDSSJ1526+4140, SDSSJ1532+2601, SDSSJ1532+4532, SDSSJ1532+4750,     
                               SDSSJ1533+5750, SDSSJ1537+1211, SDSSJ1539+3435, SDSSJ1550+0808, SDSSJ1552+0433, SDSSJ1554+0909,     
                               SDSSJ1556+0948, SDSSJ1556+2418, SDSSJ1600+0837, SDSSJ1604+5009, SDSSJ1605+1522, SDSSJ1606+0835,     
                               SDSSJ1606+2736, SDSSJ1606+3427, SDSSJ1610+2107, SDSSJ1619+1610, SDSSJ1623+0808, SDSSJ1630+1649,     
                               SDSSJ1634+4648, SDSSJ1637+3523, SDSSJ1715+6008, SDSSJ1720+3106, SDSSJ2247+0105, SDSSJ2254-0051,     
                               SDSSJ2255-0812, SDSSJ2304-0933, SDSSJ2310-0900
http://www.stsci.edu/observing/phase2-public/12521.pro

« Last Edit: June 07, 2012, 08:12:27 am by zutopian »

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Re: Dual/Triple AGNs
« Reply #33 on: June 07, 2012, 08:28:58 am »
"Chandra Observations of Galaxy Zoo Mergers: Frequency of Binary Active Nuclei in Massive Mergers"
Quote
We present the results from a Chandra pilot study of 12 massive galaxy mergers selected from Galaxy Zoo. The sample includes major mergers down to a host galaxy mass of 10$^{11}$ $M_\odot$ that already have optical AGN signatures in at least one of the progenitors. We find that the coincidences of optically selected active nuclei with mildly obscured ($N_H \lesssim 1.1 \times 10^{22}$ cm$^{-2}$) X-ray nuclei are relatively common (8/12), but the detections are too faint ($< 40$ counts per nucleus; $f_{2-10 keV} \lesssim 1.2 \times 10^{-13}$ erg s$^{-1}$ cm$^{-2}$) to reliably separate starburst and nuclear activity as the origin of the X-ray emission. Only one merger is found to have confirmed binary X-ray nuclei, though the X-ray emission from its southern nucleus could be due solely to star formation. Thus, the occurrences of binary AGN in these mergers are rare (0-8%), unless most merger-induced active nuclei are very heavily obscured or Compton thick.
Stacy H. Teng (UMD/GSFC), Kevin Schawinski (Yale), C. Megan Urry (Yale), Dan W. Darg (Oxford), Sugata Kaviraj (Oxford), Kyuseok Oh (Yonsei), Erin W. Bonning (Yale), Carolin N. Cardamone (Brown), William C. Keel (UAB), Chris J. Lintott (Oxford), Brooke D. Simmons (Yale), Ezequiel Treister (Concepcion)
(Submitted on 6 Jun 2012)
http://arxiv.org/abs/1206.1266

Blog post: http://blog.galaxyzoo.org/2012/06/07/chandra-x-ray-observations-of-mergers-found-in-the-zoo-published/
« Last Edit: June 08, 2012, 06:04:05 am by zutopian »


zutopian

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Re: Dual/Triple AGNs
« Reply #35 on: June 18, 2012, 07:04:08 am »
http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237668680459223353
http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237668680459223352


Seyfert 2 times two

It is presented in Fig. 1 (page 2) in the following paper:
"Understanding Dual AGN Activation in the Nearby Universe"
Authors: Michael Koss, Richard Mushotzky, Ezequiel Treister, Sylvain Veilleux, Ranjan Vasudevan, Margaret Trippe
(Submitted on 13 Jan 2012)
http://arxiv.org/abs/1201.2944

It is also a GZ Voorwerpje, which will be observed by the HST.
« Last Edit: June 18, 2012, 07:15:19 am by zutopian »

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Re: Dual/Triple AGNs (published)
« Reply #36 on: July 19, 2012, 06:38:25 am »
Dual AGN candidates from below paper.:


http://www.galaxyzoo.org/examine/AHZ2001b2g                              http://www.galaxyzoo.org/examine/AHZ2000927

"Morphologies of Radio, X-Ray, and Mid-Infrared Selected AGN"
Roger L. Griffith, Daniel Stern
(Submitted on 5 Jun 2010)
http://arxiv.org/abs/1006.1016v1

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Re: Dual/Triple AGNs
« Reply #37 on: July 23, 2012, 06:00:29 pm »
Quote
Identifying Analogs of NGC 6240: Galaxies with Dual Supermassive Black Holes   
------------------------------------------------------------------------------------
Type             Cycle
GO               19       
------------------------------------------------------------------------------------
Investigators                                                                   
                                                                                     Contact?
    PI: Dr. Julia Comerford               University of Texas at Austin             
   CoI: Mr. Brian Gerke                   Stanford University                           N
   CoI: Dr. Jenny E. Greene               Princeton University                          N
   CoI: Dr. Greg Madejski                 Stanford University                           N
   CoI: Dr. Daniel Stern                  Jet Propulsion Laboratory                     N
   CoI: Dr. Jeffrey Allen Newman          University of Pittsburgh                      N
   CoI: Prof. Karl Gebhardt               University of Texas at Austin                 N
   CoI: Dr. Michael Cooper                University of California - Irvine             N
   CoI: Dr. Nadia L Zakamska              The Johns Hopkins University                  N

12754(  5) - 13-Oct-2011 18:29:31 - [  3]

TARGET LIST    Fixed Targets
------------------------------------------------------------------------------------------------------------------------------------
Tar|   Target   |         Target        |            Target              |Coord   | Radial |             Flux data
No |    Name    |       Description     |           Position             |Eqnx    |  Vel.  |
------------------------------------------------------------------------------------------------------------------------------------
1   SDSS-J084135 GALAXY, SEYFERT         RA=08H41M35.1000S +/- 0.1",      J2000             V = 17.5                               
    .09+010156.3                         DEC=+01D01'56.30" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
2   SDSS-J135646 GALAXY, SEYFERT         RA=13H56M46.1000S +/- 0.1",      J2000             V = 16.2                               
    .11+102609.1                         DEC=+10D26'9.10" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
3   SDSS-J095207 GALAXY, SEYFERT         RA=09H52M7.6000S +/- 0.1",       J2000             V = 18.4                               
    .62+255257.2                         DEC=+25D52'57.20" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
4   SDSS-J123915 GALAXY, SEYFERT         RA=12H39M15.4000S +/- 0.1",      J2000             V = 17.0                               
    .40+531414.6                         DEC=+53D14'14.60" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
5   SDSS-J144804 GALAXY, SEYFERT         RA=14H48M4.2000S +/- 0.1",       J2000             V = 15.5                               
    .17+182537.9                         DEC=+18D25'37.90" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
6   SDSS-J112659 GALAXY, SEYFERT         RA=11H26M59.5000S +/- 0.1",      J2000             V = 17.2                               
    .54+294442.8                         DEC=+29D44'42.80" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
7   SDSS-J085416 GALAXY, SEYFERT         RA=08H54M16.8000S +/- 0.1",      J2000             V = 17.4                               
    .76+502632.0                         DEC=+50D26'32.00" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
8   SDSS-J100654 GALAXY, SEYFERT         RA=10H06M54.2000S +/- 0.1",      J2000             V = 17.2                               
    .2+464717.2                          DEC=+46D47'17.20" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
9   SDSS-J132231 GALAXY, SEYFERT         RA=13H22M31.9000S +/- 0.1",      J2000             V = 17.9                               
    .86+263159.1                         DEC=+26D31'59.10" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
10  SDSS-J014209 GALAXY, SEYFERT         RA=01H42M9.0000S +/- 0.1",       J2000             V = 17.2                               
    .01-005050.0                         DEC=-00D50'50.00" +/- 0.1"                                                                 
    Reference Frame: ICRS
------------------------------------------------------------------------------------------------------------------------------------
http://www.stsci.edu/observing/phase2-public/12754.pro
« Last Edit: July 23, 2012, 06:08:29 pm by zutopian »

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Re: Dual/Triple AGNs
« Reply #38 on: August 17, 2012, 01:14:33 am »
NGC 5256 -- Pair of Galaxies
Mrk 266 A and B paired (NGC 5256 A  / NGC 5256 B )
two AGNs in the merger separated by 11" (5.9 kpc).

Mrk 266B  LINER 
maser emission , z=0.027678       
587732483292266546 SDSS J133817.27+481632.1



to the north
Mrk 266A  Seyfert_2
587732483292266545SDSS J133817.77+481640.9


EDIT:

HubbleSite NewsCenter: Release Date: April 24, 2008:
Quote
NGC 5256 is located in the constellation of Ursa Major, the Great Bear, some 350 million light-years from Earth. Each galaxy also contains an active galactic nucleus, evidence that the chaos is allowing gas to fall into the regions around central black holes as well as feeding starbursts. Recent observations from the Chandra X-ray Observatory show that both nuclei, as well as a region of hot gas in between them, have been heated by the shock waves driven as gas clouds at high velocities collide.
http://hubblesite.org/newscenter/archive/releases/2008/16/image/bt/

"Chandra archival study of (U)LIRGs with a double nucleus: binary AGNs?"
Authors: Wang, Jing-Bo; Gao, Yu
Quote
Our studies suggest that Mrk 266 might be a new candidate in hosting binary AGNs supported by X-ray observations.
Publication: Research in Astronomy and Astrophysics, Volume 10, Issue 4, pp. 309-328 (2010).
Publication Date: 04/2010
http://adsabs.harvard.edu/abs/2010RAA....10..309W

Quote
The system shown in the third column and second row of Figure 6 is Mrk 266, which is a luminous infrared galaxy at z = 0.028. Its northern nucleus is optically classified as a Seyfert 2, whereas the southern nucleus is a LINER. Its double AGN nature is confirmed by Chandra X-ray observations (Mazzarella et al. 2011; see also Brassington et al. 2007 and Wang & Gao 2010).
"Active Galactic Nucleus Pairs from the Sloan Digital Sky Survey. I. The Frequency on ~ 5-100 kpc Scales"
Authors: Xin Liu, Yue Shen, Michael A. Strauss, Lei Hao
(Submitted on 5 Apr 2011 (v1), last revised 14 Jul 2011 (this version, v2))
http://arxiv.org/abs/1104.0950

"Investigation of Dual Active Nuclei, Outflows, Shock-Heated Gas, and Young Star Clusters in Markarian 266"
Mazzarella et al. 2011

"Investigation of Dual Active Nuclei, Outflows, Shock-Heated Gas, and Young Star Clusters in Markarian 266"
J. M. Mazzarella (1), K. Iwasawa (2), T. Vavilkin (3), L. Armus (4), D.-C. Kim (5,6), G. Bothun (7), A. S. Evans (5,6), H. W. W. Spoon ( 8 ), S. Haan (4,9), J. H. Howell (4), S. Lord (10), J. A. Marshall (4,11), C. M. Ishida (12), C. K. Xu (10), A. Petric (4,11), D. B. Sanders (13), J. A. Surace (4), P. Appleton (10), B. H. P. Chan (1), D. T. Frayer (6), H. Inami (4), E. Ye. Khachikian (14), B. F. Madore (15,1), G. C. Privon (5), E. Sturm (16), Vivian U. (13), S. Veilleux (17)
(Submitted on 15 Aug 2012)
http://arxiv.org/abs/1208.3248

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Re: Dual/Triple AGNs
« Reply #39 on: September 26, 2012, 06:04:55 am »
Binary AGNs
arXiv:1003.3467v2  Discovery of Four kpc-Scale Binary AGNs
 last revised 8 Apr 2010

Quote from: Xin Liu
Xin Liu, Jenny E. Greene, Yue Shen, Michael A. Strauss
(Submitted on 17 Mar 2010 (v1), last revised 8 Apr 2010 (this version, v2))
Abstract: We report the discovery of four kpc-scale binary AGNs. These objects were originally selected from the Sloan Digital Sky Survey based on double-peaked [O III] 4959,5007 emission lines in their fiber spectra. The double peaks could result from pairing active supermassive black holes (SMBHs) in a galaxy merger, or could be due to bulk motions of narrow-line region gas around a single SMBH. Deep near-infrared (NIR) images and optical slit spectra obtained from the Magellan 6.5 m and the APO 3.5 m telescopes strongly support the binary SMBH scenario for the four objects. In each system, the NIR images reveal tidal features and double stellar components with a projected separation of several kpc, while optical slit spectra show two Seyfert 2 nuclei spatially coincident with the stellar components, with line-of-sight velocity offsets of a few hundred km/s. These objects were drawn from a sample of only 43 objects, demonstrating the efficiency of this technique to find kpc-scale binary AGNs.

1237657855535218926 SDSS J114642.47+511029.8


587732702332059831 SDSS J110851.03+065901.4


1237671991339188422 SDSS J133226.34+060627.4



http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237650371015671956 SDSS J113126.08-020459.3


New paper:

"Chandra X-ray and Hubble Space Telescope Imaging of Optically Selected kiloparsec-Scale Binary Active Galactic Nuclei I. Nature of the Ionizing Sources"
Xin Liu, Francesca Civano, Yue Shen, Paul J. Green, Jenny E. Greene, Michael A. Strauss
(Submitted on 24 Sep 2012)
http://arxiv.org/abs/1209.5418

CONFIRMED:
SDSS J110851.04+065901.4: http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237658423556964533
SDSS J114642.47+511029.6: http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237657855535218926

UNCLEAR:
SDSS J113126.08-020459.2 : http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237650371015671956
SDSS J133226.34+060627.4: http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237671991339188422

PS: There will be a paper II about these 4.
« Last Edit: September 26, 2012, 06:21:45 am by zutopian »

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Re: Dual/Triple AGNs (found by astronomers)
« Reply #40 on: October 30, 2012, 05:25:18 am »
"The First Spectroscopically Resolved Sub-parsec Orbit of a Supermassive Binary Black Hole"
Quote
One of the most intriguing scenarios proposed to explain how active galactic nuclei are triggered involves the existence of a supermassive binary black hole system in their cores. Here we present an observational evidence for the first spectroscopically resolved sub-parsec orbit of a such system in the core of Seyfert galaxy NGC 4151.
E. Bon, P. Jovanović, P. Marziani, A. I. Shapovalova, N. Bon, V. Borka Jovanović, D. Borka, J. Sulentic, L. Č. Popović
(Submitted on 20 Sep 2012 (v1), last revised 27 Oct 2012 (this version, v2))
http://arxiv.org/abs/1209.4524

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Re: Dual/Triple AGNs (found by astronomers)
« Reply #41 on: December 07, 2012, 09:54:30 am »
New paper:

"Characterization of a sample of intermediate-type AGN. I. Spectroscopic properties and serendipitous discovery of new Dual AGN"
Erika Benítez, Jairo Méndez-Abreu, Isaura Fuentes-Carrera, Irene Cruz-González, Benoni Martínez, Luis López-Martin, Elena Jiménez-Bailón, Jonathan León-Tavares, Vahram H. Chavushyan
(Submitted on 5 Dec 2012)
http://arxiv.org/abs/1212.1189

J121607.08+504930.0 and J141238.14+391836.5 are Dual AGN candidates.:

DR9: http://skyserver.sdss.org/dr7/en/tools/explore/obj.asp?id=587732484360110089 
DR7: http://skyserver.sdss3.org/dr9/en/tools/explore/obj.asp?id=1237658205585014795

DR9: http://skyserver.sdss3.org/dr9/en/tools/explore/obj.asp?id=1237662195072761905
DR7: http://skyserver.sdss.org/dr7/en/tools/explore/obj.asp?id=588017948824567865
« Last Edit: December 07, 2012, 10:02:50 am by zutopian »

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Re: Dual/Triple AGNs (found by astronomers)
« Reply #42 on: March 14, 2013, 01:20:03 pm »
Host galaxies of double-peaked [OIII] emitting AGN: binary AGN or mergers?
Authors: Carolin Villforth, Fred Hamann
(Submitted on 8 Mar 2013)
http://arxiv.org/abs/1303.1875

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Re: Dual/Triple AGNs (found by astronomers)
« Reply #43 on: March 14, 2013, 01:22:22 pm »
Two Compton-Thick Active Nuclei in Arp 220?
Authors: Alessandro Paggi, Giuseppina Fabbiano, Guido Risaliti, Junfeng Wang, Martin Elvis
(Submitted on 11 Mar 2013)
http://arxiv.org/abs/1303.2630
« Last Edit: March 21, 2013, 09:23:22 pm by zutopian »

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Re: Dual/Triple AGNs (found by astronomers)
« Reply #44 on: March 21, 2013, 09:20:06 pm »
Identification of Outflows and Candidate Dual Active Galactic Nuclei in SDSS Quasars at z=0.8-1.6
Authors: R. Scott Barrows, Claud H. Sandberg Lacy, Julia Kennefick, Julia M. Comerford, Daniel Kennefick, Joel C. Berrier
(Submitted on 14 Mar 2013)
http://arxiv.org/abs/1303.3587