2012AJ....144..125M


Query : 2012AJ....144..125M

2012AJ....144..125M - Astron. J., 144, 125 (2012/November-0)

Investigation of dual active nuclei, outflows, shock-heated gas, and young star clusters in Markarian 266.

MAZZARELLA J.M., IWASAWA K., VAVILKIN T., ARMUS L., KIM D.-C., BOTHUN G., EVANS A.S., SPOON H.W.W., HAAN S., HOWELL J.H., LORD S., MARSHALL J.A., ISHIDA C.M., XU C.K., PETRIC A., SANDERS D.B., SURACE J.A., APPLETON P., CHAN B.H.P., FRAYER D.T., INAMI H., KHACHIKIAN E.Y., MADORE B.F., PRIVON G.C., STURM E., U V. and VEILLEUX S.

Abstract (from CDS):

Result. of observations with the Spitzer, Hubble, GALEX, Chandra, and XMM-Newton space telescopes are presented for the luminous infrared galaxy (LIRG) merger Markarian 266. The SW (Seyfert 2) and NE (LINER) nuclei reside in galaxies with Hubble types SBb (pec) and S0/a (pec), respectively. Both companions are more luminous than L* galaxies and they are inferred to each contain a ~2.5x108 M black hole. Although the nuclei have an observed hard X-ray flux ratio of fX(NE)/fX(SW) = 6.4, Mrk 266 SW is likely the primary source of a bright Fe Kα line detected from the system, consistent with the reflection-dominated X-ray spectrum of a heavily obscured active galactic nucleus (AGN). Optical knots embedded in an arc with aligned radio continuum radiation, combined with luminous H2line emission, provide evidence for a radiative bow shock in an AGN-driven outflow surrounding the NE nucleus. A soft X-ray emission feature modeled as shock-heated plasma with T ∼ 107 K is cospatial with radio continuum emission between the galaxies. Mid-infrared diagnostics provide mixed results, but overall suggest a composite system with roughly equal contributions of AGN and starburst radiation powering the bolometric luminosity. Approximately 120 star clusters have been detected, with most having estimated ages less than 50 Myr. Detection of 24 µm emission aligned with soft X-rays, radio continuum, and ionized gas emission extending ∼34'' (20 kpc) north of the galaxies is interpreted as ∼2x107 M of dust entrained in an outflowing superwind. At optical wavelengths this Northern Loop region is resolved into a fragmented morphology indicative of Rayleigh-Taylor instabilities in an expanding shell of ionized gas. Mrk 266 demonstrates that the dust "blow-out" phase can begin in a LIRG well before the galaxies fully coalesce during a subsequent ultraluminous infrared galaxy (ULIRG) phase, and rapid gas consumption in luminous dual AGNs with kiloparsec-scale separations early in the merger process may explain the paucity of detected binary QSOs (with parsec-scale orbital separations) in spectroscopic surveys. An evolutionary sequence is proposed representing a progression from dual to binary AGNs, accompanied by an increase in observed Lx/Lir ratios by over two orders of magnitude.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: interactions - galaxies: nuclei - galaxies: Seyfert - galaxies: starburst - galaxies: star clusters: general

VizieR on-line data: <Available at CDS (J/AJ/144/125): table3.dat table11.dat table12.dat table13.dat table14.dat table15.dat>

Nomenclature: Table 15: [MIV2012] Mrk 266 SCNNN (Nos 1-119) = GOALS JHHMMSS.ss+DDMMSS.s N=119.

Status at CDS : All or part of tables of objects could be ingested in SIMBAD with priority 2.

Simbad objects: 37

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Number of rows : 37
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Taffy System PaG 00 01 40.12 +23 29 23.0           ~ 52 2
2 NGC 34 Sy2 00 11 06.612 -12 06 28.33   14.14 13.52     ~ 318 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9859 1
4 IC 1623 IG 01 07 47.2 -17 30 25   15       ~ 269 1
5 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4225 2
6 3C 75 PaG 02 57 41.64 +06 01 28.0           ~ 287 1
7 ICRF J040549.2+380332 SyG 04 05 49.2627587 +38 03 32.234373   18.5 18.5     ~ 131 3
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15467 1
9 M 42 HII 05 35 17.3 -05 23 28           ~ 3818 0
10 NGC 2346 PN 07 09 22.5216571385 -00 48 23.611157830   11.76 11.58     A5V 558 0
11 2E 1919 Sy1 08 10 58.6637281539 +76 02 42.449416413   15.03 14.71     ~ 427 0
12 NGC 2623 LIN 08 38 24.016 +25 45 16.29 14.10 13.99 13.36     ~ 450 1
13 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5470 6
14 2XMM J100043.1+020637 QSO 10 00 43.1317731847 +02 06 37.388673197 20.25 19.86 19.37   18.79 ~ 101 0
15 IC 694 G 11 28 27.312 +58 34 42.29   18.2       ~ 242 2
16 NGC 3690 IG 11 28 31.326 +58 33 41.80   13.19 12.86     ~ 911 4
17 NGC 4038 GiP 12 01 53.002 -18 52 03.32   10.91   9.74 11.0 ~ 1289 1
18 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1589 0
19 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1843 3
20 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4374 2
21 IC 883 SBG 13 20 35.380 +34 08 21.84   14.8       ~ 378 1
22 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3947 4
23 Mrk 266B LIN 13 38 17.3501948813 +48 16 31.903051043   14.19 13.42     ~ 68 0
24 Mrk 266NE Sy2 13 38 17.777 +48 16 41.02   15.0       ~ 40 0
25 NGC 5256 PaG 13 38 17.8 +48 16 41   14.1 13.42     ~ 406 2
26 Mrk 463 Sy2 13 56 02.9 +18 22 18   14.8 14.22     ~ 359 2
27 2XMM J153244.0+324248 Sy2 15 32 44.0259738182 +32 42 46.719802275     19.8     ~ 106 0
28 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2758 4
29 QSO J1536+0441 QSO 15 36 36.2232172770 +04 41 27.064213945   17.75 17.41     ~ 67 1
30 NGC 6090 PaG 16 11 40.3 +52 27 21   14.0       ~ 404 2
31 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1525 2
32 MCG+08-31-041 Sy1 17 19 14.4925747 +48 58 49.426017   15.86 14.81 9.44   ~ 287 1
33 ICRF J184208.9+794617 Sy1 18 42 08.9910523393 +79 46 17.129210139   16.06 15.38     ~ 1235 0
34 2MASX J20572362+1707445 PaG 20 57 23.628 +17 07 44.60   15.2       ~ 147 0
35 NAME Stephan's Quintet CGG 22 35 57.5 +33 57 36           ~ 385 1
36 NAME South America H2G 22 51 49.307 -17 52 23.96   16.97       ~ 295 3
37 NGC 7714 GiP 23 36 14.099 +02 09 18.07   14.91 14.36     ~ 739 1

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2021.08.02-12:41:00

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