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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 103 110 Summary of observation parameters tabled4.dat 136 105 Principal emission components in the 5-10keV band
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
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
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
Byte-by-byte Description of file: tabled4.dat
Bytes Format Units Label Explanations
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
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)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 26-Mar-2014
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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