J/MNRAS/430/60 Suzaku view of highly ionized outflows in AGN (Gofford+, 2013)
The Suzaku view of highly ionized outflows in AGN.
I. Statistical detection and global absorber properties.
Gofford J., Reeves J.N., Tombesi F., Braito V., Turner T.J., Miller L.,
Cappi M.
<Mon. Not. R. Astron. Soc., 430, 60-80 (2013)>
=2013MNRAS.430...60G 2013MNRAS.430...60G
ADC_Keywords: Active gal. nuclei ; X-ray sources
Keywords: line: identification - galaxies: active - galaxies: nuclei -
X-rays: galaxies
Abstract:
We present the results of a new spectroscopic study of Fe K-band
absorption in active galactic nuclei (AGN). Using data obtained from
the Suzaku public archive we have performed a statistically driven
blind search for FeXXV Heα and/or FeXXVI Lyα absorption
lines in a large sample of 51 Type 1.0-1.9 AGN. Through extensive
Monte Carlo simulations we find that statistically significant
absorption is detected at E≳6.7keV in 20/51 sources at the PMC≥95%
level, which corresponds to ∼40% of the total sample. In all cases,
individual absorption lines are detected independently and
simultaneously amongst the two (or three) available X-ray imaging
spectrometer detectors, which confirms the robustness of the line
detections. The most frequently observed outflow phenomenology
consists of two discrete absorption troughs corresponding to FeXXV
Heα and FeXXVI Lyα at a common velocity shift. From xstar
fitting the mean column density and ionization parameter for the FeK
absorption components are log(NH/cm2)∼23 and
log(ξ/erg/cm/s)∼4.5, respectively. Measured outflow velocities span
a continuous range from <1500km/s up to ∼100000km/s, with mean and
median values of ∼0.1c and ∼0.056c, respectively. The results of this
work are consistent with those recently obtained using XMM-Newton and
independently provides strong evidence for the existence of very
highly ionized circumnuclear material in a significant fraction of
both radio-quiet and radio-loud AGN in the local universe.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 103 110 Summary of observation parameters
tabled4.dat 136 105 Principal emission components in the 5-10keV band
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Source Source name
18 A1 --- n_Source [a] Note (repetition of n_Ct2) (1)
20- 25 A6 --- Type Source type (3)
27- 33 F7.5 --- z Cosmological redshift according to the NED
34- 39 F6.3 10+21cm-2 NHgal Galactic absorption column density
41- 49 I9 --- ObsID ? Suzaku observation ID
50 A1 --- n_ObsID [s] s for stacked (time-averaged) spectrum
52- 54 A3 --- o_ObsID [abcdefg all] Indicates observations used for
stacked data
55 A1 --- f_ObsID [*+] Note about the spectrograph (2)
57- 66 A10 "date" Date Starting date of observation
68- 72 F5.1 ks tXIS ?=- XIS net exposure time
74- 78 F5.1 ks tHXD ? HXD net exposure time
80- 85 F6.1 10+3ct Ct Total number of 2-10keV counts for the
XIS-FI(BI) spectra
87- 91 F5.1 10+3ct Ct2 ? Total number of background subtracted
2-10keV counts for the co-added
XIS-FI(BI) spectra
92 A1 --- n_Ct [a] Counts in 0.6-10keV range (1)
93 A1 --- --- [/]
94- 97 F4.1 10+3ct Ct2l ? Lower value of interval for total number of
background subtracted 2-10keV counts for
the co-added XIS-FI(BI) spectra
99-103 F5.1 10+3ct PIN ?=- Total background subtracted PIN counts
in the 15-50keV band
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Note (1): Note as follows:
a = The total net source counts listed in column tHXD for APM 08279+5255
are taken from 0.6-10keV in the observer frame.
See text for further details.
Note (2): Notes on ObsID as follows:
+ = Only the XIS 3 spectrum was available during the observation of
SWIFT J2127.4+5654
* = Indicates that the XIS 2 was operational during the observation and
is included as part of the co-added XIS-FI spectrum
Note (3): the source types are:
Sy = Seyfert active galaxy (with type 1.0 to 1.9)
RQQ = Radio Quiet Galaxy
BLRG = Broad-Line Radio Galaxy
NLSy1 = Narrow-line Seyfert type 1.
QSO = Quasar
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Byte-by-byte Description of file: tabled4.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Source Source name
17 A1 --- n_Source [*] ionised outflow detected (1)
19- 27 I9 --- ObsID ? Suzaku observation ID
29 A1 --- n_ObsID [s] s for stacked (time-averaged)
30 A1 --- --- [[]
31- 33 A3 --- o_ObsID [abcdefg all] Indicates observations used for
stacked data
34 A1 --- --- []]
36- 52 A17 --- Line Emission line identification (2)
54- 57 F4.2 keV E Measured line energy in the source rest-frame
59- 62 F4.2 keV E_E ? Error on E (upper value)
64- 67 F4.2 keV e_E ? Error on E (lower value)
68 A1 --- n_E [f] f for fixed energy value
69 A1 --- l_Ew Limit flag on Ew
70- 72 I3 eV Ew ? Measured line energy-width, sigma-width
74- 76 I3 eV E_Ew ? Error on Ew (upper value)
78- 80 I3 eV e_Ew ? Error on Ew (lower value)
81 A1 --- n_Ew [f] f for fixed Ew (10eV)
83- 88 F6.2 ph/cm2/Ms Int Line intensity (10-2ph/m2/s)
90- 94 F5.2 ph/cm2/Ms E_Int ? Error on Int (upper value)
96-100 F5.2 ph/cm2/Ms e_Int ? Error on Int (lower value)
101-104 I4 eV EW Line equivalent width
106-107 I2 eV E_EW ? Error on EW (upper value)
110-111 I2 eV e_EW ? Error on EW (lower value)
113-114 I2 eV EWb ? Equivalent width of the FeKβ line
(for Line=FeKα)
116 I1 eV E_EWb ? Error on EWb (upper value)
118 I1 eV e_EWb ? Error on EWb (lower value)
121-127 F7.2 --- Dchi2 Change in fit statistic, Δχ2 (3)
129 I1 --- Dnu ? Change in degree of freedom δν (3)
131 A1 --- l_PF Limit flag on PF
132-136 F5.2 % PF [99/100] Line significance
according to the F-test
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Note (1): *: indicates that a ionised outflow is detected in this source
Note (2): Broad(GA) and Broad(DL) indicate that a broadened FeK emission
component, which was fitted with either a broadened Gaussian or a
Disk-Line, respectively
Note (3): changes in the χ2 statistic when the line is removed from
the best-fit model (a negative Δχ2 means an improvement)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 26-Mar-2014