J/AJ/144/125 Photometry and spectroscopy of Markarian 266 (Mazzarella+, 2012)
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., Veilleux S.
<Astron. J., 144, 125 (2012)>
=2012AJ....144..125M 2012AJ....144..125M
ADC_Keywords: Galaxies, IR ; Equivalent widths ; Photometry, HST ;
Spectra, infrared ; Associations, stellar
Keywords: galaxies: active - galaxies: interactions - galaxies: nuclei -
galaxies: Seyfert - galaxies: starburst -
galaxies: star clusters: general
Abstract:
Results 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 ~2.5x108M☉ 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∼107K 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 50Myr. Detection of 24µm
emission aligned with soft X-rays, radio continuum, and ionized gas
emission extending ∼34" (20kpc) north of the galaxies is interpreted
as ∼2x107M☉ 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.
Description:
Mrk 266 was observed on 2005 November 17 with the Advanced Camera for
Surveys (ACS) Wide Field Channel (WFC) as part of a Hubble Space
Telescope (HST) Cycle 14 GOALS program to investigate 88 luminous
infrared galaxies (LIRGs) with Lir>1011.4L☉ (PID 10592, PI:
A. Evans). The system was imaged in the F435W filter (B band,
0.435µm, image J9CV48010) and in the F814W filter (I band,
0.814µm, image J9CV48020). Near-infrared observations at 1.6µm
(F160W, H band, image N44B40010) with the NIC2 aperture of NICMOS were
acquired on 1997 September 13 in Cycle 7 (PID 7328, PI: M. Malkan).
To complement the HST high-resolution imagery, images in the B, V, and
I bands were obtained on 1998 December 22 and 2000 May 4 with the
University of Hawaii 2.2m telescope (effective seeing ∼1.5" FWHM).
Chandra observations were obtained with the Advanced CCD Imaging
Spectrometer (ACIS-S) on 2001 November 2 (PI: A. Read). The spatial
resolution is ∼1" FWHM. These observations were first presented by
Brassington et al. (2007MNRAS.377.1439B 2007MNRAS.377.1439B). The data were taken from the
Chandra Data Archive (http://cxc.harvard.edu/cda/, ObsID: 2044).
X-ray observations with XMM-Newton were acquired with the European
Imaging Photon Camera (EPIC) on 2002 May 15 (PI: A. Read). The data
obtained with the EPIC pn-CCD camera were utilized, providing an
angular resolution of ∼6" FWHM and a spectral resolution of
(E/δE)∼40. The data set (0055990501) was taken from the
XMM-Newton Science Archive (http://xmm.esac.esa.int/xsa/).
Ultraviolet images of Mrk 266 were obtained on 2004 June 4 in the NUV
(2271Å) and FUV (1528Å) bands during the All Sky Imaging Survey
(AIS) conducted by GALEX. The data were extracted from MAST (tile
AISCHV310401135).
Contemporaneously with the X-ray observations by XMM-Newton, the
Optical/UV Monitor Telescope (XMM-OM) obtained observations of Mrk 266
in the U (3000-3900Å), UVW1 (2450-3200Å), and UVW2
(1800-2250Å) filters. These images have a spatial resolution of
∼2"FWHM. The XMM-OM images were obtained from MAST (data set
0055990501).
Imaging observations of Mrk 266 were obtained with the Spitzer Space
Telescope as part of the Cycle 1 General Observing program for GOALS
(PID 3672; PI: J. Mazzarella). The Infrared Array Camera (IRAC) on
board Spitzer was used to image the source at 3.6, 4.5, 5.8, and
8.0µm (AOR 12305408). The Multiband Imaging Photometer for Spitzer
(MIPS) was utilized to image Mrk 266 at 24, 70, and 160µm using the
Photometry and Super Resolution mode (AOR 12349184).
Mid-infrared spectroscopy of Mrk 266 obtained in staring mode with the
Infrared Spectrograph (IRS) on board Spitzer have been published by
Brandl et al. (2006ApJ...653.1129B 2006ApJ...653.1129B), Dudik et al.
(2007ApJ...664...71D 2007ApJ...664...71D), and Bernard-Salas et al. (2009, Cat.
J/ApJS/184/230). Unfortunately, these observations suffer from
aperture effects that resulted in missing emission from some
components in different spectral regions. Table 14 provides
clarification of which emission features have been measured for each
component of the system. The IRS spectral map obtained on 2005 January
10 available in the Spitzer archive (program P03269; PI: J. Gallimore;
AOR 12459264) was used to construct spectra for each nucleus and for
the total system.
Objects:
-------------------------------------------------
RA (2000) DE Designation(s)
-------------------------------------------------
13 38 17.69 +48 16 33.9 Mrk 266 = NGC 5256
-------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table3.dat 57 38 Measurements from low-resolution spectral mapping
table11.dat 54 5 Elliptical apertures for regions of interest
table12.dat 70 35 Photometric data for Mrk 266 - Total system
table13.dat 70 55 Photometric data for Mrk 266 - Components
table14.dat 86 42 Regions covered in published IRS measurements
table15.dat 67 119 Star cluster photometry
refs.dat 77 14 References
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See also:
VIII/42 : Texas Survey of radio sources at 365MHz (Douglas+ 1996)
VIII/13 : A new catalog of 53522 4.85GHz sources (Becker+ 1991)
VIII/22 : 6C Survey of Radio Sources - III. (Hales+ 1990)
VII/172 : First Byurakan Survey (FBS) (Markarian+, 1989)
J/ApJS/184/230 : Spitzer high-resolution MIR spectral atlas
(Bernard-Salas+, 2009)
J/ApJS/161/185 : GIS catalog project : source catalog II (Ueda+, 2005)
J/A+A/422/39 : ISOPHOT 170µm Serendipity Survey II. (Stickel+, 2004)
J/AJ/126/1607 : IRAS Revised Bright Galaxy Sample (Sanders+, 2003)
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Region Mrk 266 region (G1)
7 A1 --- f_Region [ad] Flag on Region (1)
9- 13 F5.2 um lambda [6/35] Spectral line wavelength (µm)
15- 30 A16 --- Line Spectral line identification
31- 37 F7.3 10-16W/m2 Flux Line flux (in 10-20W/cm2)
39- 43 F5.3 10-16W/m2 e_Flux Uncertainty in Flux
45 A1 --- f_Flux [bc] Flag on Flux (2)
47- 50 F4.2 um EW ? Equivalent width; in µm
52- 55 F4.2 um e_EW ? Uncertainty in EW; in µm
57 A1 --- f_EW [bc] Flag on EW (2)
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Note (1): Flag on Mrk 266 component as follows:
a = Spectral measurements for the integrated emission from both galaxies in
Mrk 266. Features in the 5.2-14.5µm (Short-Low, SL) and 14.5-38µm
(Long-Low, LL) regions were measured from the 1D spectrum plotted in
Figure 11; this region is 4*4 LL pixels in size, where each pixel is
5.1"*5.1", as outlined in brown in Figure 10(a).
d = Spectral features measured from the Short-Low (SL) spectra of Mrk 266 SW
and NE as plotted in Figures 12(c) and (b). These 1D spectra were extracted
from the blue and red regions of the spectral map shown in Figure 10, which
have dimensions of 5*5 SL pixels, where each pixel is 1.8"*1.8".
Note (2): Flag as follows:
b = These line fluxes were measured using PAHFIT and include an extinction
correction based on a fit with a τ9.7µm=0.30 dust screen, which
corresponds to AV~5.7mag.
c = Equivalent width measurements for the PAH features were measured using a
spline-fitting technique for estimating the local continuum. Spline fitting
was also used to estimate fluxes of features in the Short-Low (SL) spectra
of the individual galaxies which could not be measured with PAHFIT.
See Section 2.7 for more details.
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Region Region used to perform aperture photometry (G1)
18- 19 I2 h RAh Hour of Right Ascension (J2000)
21- 22 I2 min RAm Minute of Right Ascension (J2000)
24- 28 F5.2 s RAs Second of Right Ascension (J2000)
30 A1 --- DE- Sign of the Declination
31- 32 I2 deg DEd Degree of Declination (J2000)
34- 35 I2 arcmin DEm Arcminute of Declination (J2000)
37- 40 F4.1 arcsec DEs Arcsecond of Declination (J2000)
42- 45 F4.1 arcsec a First parameter for elliptical aperture (1)
47- 50 F4.1 arcsec b Second parameter for elliptical aperture (1)
52- 54 I3 deg PA ? Position angle
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Note (1): Used for photometric measurements, as illustrated in Figure 31.
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Byte-by-byte Description of file: table1[23].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Region Mrk 266 region (G1)
20- 39 A20 --- Band Bandpass
41 A1 --- f_Band [a] The 70 and 160µm flux densities for the
South-West (SW) and North-East (NE) galaxies
were estimated using the 8 and 24µm
measurements as described in Section 2.6.2
43- 50 E8.3 Hz Freq [1.5e8/1.5e18] Frequency (ν)
52- 59 E8.3 Jy Flux Flux density at Freq (fν)
61- 67 E7.2 Jy e_Flux The 1σ uncertainty in Flux σfν
69- 70 I2 --- Ref Reference; in refs.dat file
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Byte-by-byte Description of file: table14.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 27 A27 --- Region Mrk 266 region (G1)
29- 33 F5.2 um lambda [6/35] Spectral line wavelength (µm)
35- 50 A16 --- Line Spectral line identification
52- 53 A2 --- IRS Infrared Spectrograph (IRS) module used (1)
55 A1 --- f_Line [ab] Flag on Line (2)
57 A1 --- l_Flux Upper limit on Flux
59- 67 E9.4 W/m2 Flux ? Flux
69- 76 E8.3 W/m2 e_Flux ? Uncertainty in Flux
78- 82 F5.3 um EW ? Equivalent width; in µm
84- 86 A3 --- Ref Reference; in refs.dat file
--------------------------------------------------------------------------------
Note (1): IRS module as follows:
SL = Short-Low (5.2-14.5µm, 3.7"*57", R∼60-127);
LL = Long-Low (14.0-38.0µm, 10.5"*168.3", R∼57-126);
SH = 9.9-19.6µm, 4.7"*11.3", R∼600;
LH = 18.7-37.3µm, 11.1"*22.3", R∼600.
Note (2): Flag on spectral line identification as follows:
a = These features are visible in the low-res spectrum published by
Brandl et al. (2006ApJ...653.1129B 2006ApJ...653.1129B);
b = This is consistent with an [NeV] 24.32µm flux of
1.19(±0.06)*10-20W.cm-2 measured from the same LH aperture by
Dudik et al. (2007ApJ...664...71D 2007ApJ...664...71D; Table 2).
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Byte-by-byte Description of file: table15.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq Star cluster (candidate) number
<[MIV2012] Mrk 266 SCNNN> in Simbad
5- 6 I2 h RAh Hour of right ascension (J2000) (1)
8- 9 I2 min RAm Minute of right ascension (J2000) (1)
11- 15 F5.2 s RAs Second of right ascension (J2000) (1)
17 A1 --- DE- Sign of the declination (J2000)
18- 19 I2 deg DEd Degree of declination (J2000) (1)
21- 22 I2 arcmin DEm Arcminute of declination (J2000) (1)
24- 27 F4.1 arcsec DEs Arcsecond of declination (J2000) (1)
29- 33 F5.2 mag Bmag Apparent mag in the HST ACS F435W (B) filter
35- 38 F4.2 mag e_Bmag 1σ uncertainty in Bmag
40- 45 F6.2 mag BMag Absolute B magnitude (2)
47- 51 F5.2 mag Imag Apparent mag in the HST ACS F814W (I) filter
53- 56 F4.2 mag e_Imag 1σ uncertainty in Imag
58- 62 F5.2 mag B-I B-I color index (2)
64- 67 F4.2 mag e_B-I 1σ uncertainty in B-I
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Note (1): The 1σ uncertainty in the coordinates is ±0.3".
Note (2): Corrected for foreground Galactic extinction using values from
Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S) as provided by NED:
AB=0.056mag; At=0.025mag. These data have not been corrected for
extinction within Mrk 266 (see Section 3.6.2).
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- Ref Reference code
5- 23 A19 --- BibCode Bibliographic code
25- 44 A20 --- Aut Author's name
46- 77 A32 --- Com Comments
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Global notes:
Note (G1):
SW = The South-West (Seyfert 2) nucleus;
NE = The North-East (LINER) nucleus.
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History:
From electronic version of the journal
(End) Sylvain Guehenneux [CDS] 15-Nov-2013