J/A+A/639/A51 185 bright XMM-CDFS sources spectral properties (Iwasawa+, 2020)
The XMM deep survey in the CDFS. XI. Spectral properties of 185 bright sources.
Iwasawa K., Comastri A., Vignali C., Gilli R., Lanzuisi G., Brandt W .N.,
Tozzi P., Brusa M., Carrera F.J., Ranalli P., Mainieri V.,
Georgantopoulos I., Puccetti S., Paolillo M.
<Astron. Astrophys. 639, A51 (2020)>
=2020A&A...639A..51I 2020A&A...639A..51I (SIMBAD/NED BibCode)
ADC_Keywords: X-ray sources ; Redshifts ; Equivalent widths ; Spectroscopy
Keywords: atlases - galaxies: active - X-ray: galaxies
Abstract:
We present X-ray spectra of 185 bright sources detected in the
XMM-Newton deep survey of the Chandra Deep Field South, combining the
three EPIC cameras. The 2-10keV flux limit of the sample is
2x10-15erg/s/cm2. The sources are distributed over a redshift
range of z=0.1-3.8. Eleven new X-ray redshift measurements are
included. A spectral analysis was performed using a simple model to
obtain absorbing column densities, rest-frame 2-10keV luminosities and
Fe K line properties of 180 sources at z>0.4. Obscured AGN are found
to be more abundant toward higher redshifts. Using the XMM-Newton data
alone, seven Compton-thick AGN candidates are identified, which makes
the Compton-thick AGN fraction to be ~=4%. An exploratory spectral
inspection method with two rest-frame X-ray colours and an Fe line
strength indicator is introduced and tested against the results from
spectral fitting. This method works reasonably well to characterise a
spectral shape and can be useful for a pre-selection of Compton-thick
AGN candidates.We found six objects exhibiting broad Fe K lines out of
21 unobscured AGN of best data quality, implying a detection rate of
30%. Five redshift spikes, each of which has more than six sources,
are identified in the redshift distribution of the X-ray sources.
Contrary to the overall trend, the sources at the two higher-redshift
spikes at z=1.61 and z=2.57 have puzzlingly low obscuration.
Description:
X-ray source identification numbers, basic properties, spectral
analysis results on 185 bright sources detected in the XMM deep survey
of the Chandra Deep Field South (CDFS) are presented.
X-ray flux density spectra of 185 bright sources in the XMM deep
survey in the Chandra Deep Field South, obtained from the XMM-Newton
EPIC cameras. Data from the three EPIC cameras are averaged after
correcting for the detector responses. The Galactic absorption has
been corrected. The energy-scale is as observed. PID is the source
identification number.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 122 185 Properties of 185 XMM-CDFS sources
sp/* . 185 *0.5-7keV spectra of 185 XMM-CDFS sources
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Note on sp/*: FileName as fn_PID.dat, where PID is the source identification
number, as in table1.dat
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See also:
J/MNRAS/436/3759 : ECDFS sources optical/IR counterparts (Bonzini+, 2013)
J/ApJS/224/15 : Improved 2Ms and 250ks Chandra catalogs (Xue+, 2016)
J/ApJS/228/2 : Chandra Deep Field-South survey: 7Ms sources (Luo+, 2017)
J/A+A/555/A42 : The XMM-CDFS catalogues (Ranalli+, 2013)
J/A+A/556/A114 : Obscured AGNs in XMM deep survey in CDF-S
(Castello-Mor+, 2013)
J/A+A/574/A49 : XMMOMCDFS catalogue (Antonucci+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- PID XMM-CDFS source identification number
5- 9 F5.3 --- z Redshift
11- 12 A2 --- ztype Redshift type (1)
14- 15 I2 --- r_z Reference for the adopted redshift (2)
17- 21 F5.2 [cm-2] logNH Logarithmic of absorbing column density
23- 27 F5.2 [cm-2] b_logNH The 68% lower bound of NH
29- 33 F5.2 [cm-2] B_logNH The 68% upper bound of NH
35- 39 F5.2 [10-7W] logLXobs Logarithmic of rest-frame 2-10keV
luminosity as observed
41- 45 F5.2 [10-7W] logLXcor Logarithmic of rest-frame 2-10keV
luminosity corrected for absorption
47 I1 --- D90 [0/1]? Fe K line detection flag with
threshold of the 90% significance
(0: no detection/1 detection)
49 I1 --- D68 [0/1]? Fe K line detection flag with
threshold of the 68% significance
(0: nodetection/1: detection)
51- 54 F4.2 keV Eline ? Adopted Fe K line energy
56- 59 F4.2 keV EW ? Equivalent width of Fe K line
61- 64 F4.2 keV b_EW ? The 68% lower bound of EW
66- 69 F4.2 keV B_EW ? The 68% upper bound of EW
71- 75 F5.2 --- S/M ? Rest-frame X-ray colour
S/M=(2-5keV)/(5-9keV)
77- 80 F4.2 --- e_S/M ? Uncertainty of S/M
82- 86 F5.2 --- H/M ? Rest-frame X-ray colour
H/M=(9-14keV)/(5-9keV)
88- 91 F4.2 --- e_H/M ? Uncertainty of H/M
93- 97 F5.2 --- Rfe ? Fe K line strength indicator
99-102 F4.2 --- e_Rfe ? Uncertainty of Rfe
104-109 F6.2 --- SNe310 ? Signal-to-noise indicator of spectral data
in the rest-frame 3-10keV band
111-114 I4 --- L17 ? Chandra source identification number in
Luo et al., 2017, Cat. J/ApJS/228/2,
[LBX2017] NNNN in Simbad
116-118 A3 --- X16 ? Chandra source identification number in
Xue et al., 2016, Cat. J/ApJS/224/15 (3)
120-122 I3 --- RID ? Radio source identification number in
Bonzini et al., 2013, Cat. J/MNRAS/436/3759,
[MBF2013] in Simbad (4)
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Note (1): Redshift type as follows:
sp = spectroscopic
ph = photometric
x = X-ray
Note (2): References as follows:
1 = Treister et al. (2009, Cat. J/ApJ/693/1713)
2 = Silverman et al. (2010, Cat. J/ApJS/191/124)
3 = Cooper et al. (2012, Cat. J/MNRAS/425/2116)
4 = Hsu et al. (2014, Cat. J/ApJ/796/60)
5 = Balestra et al. (2010, Cat. J/A+A/512/A12)
6 = Iwasawa et al. (2012A&A...546A...8K 2012A&A...546A...8K)
7 = This work
8 = Vanzella et al. (2008, Cat. J/A+A/478/83)
9 = Ravikumar et al. (2007, Cat. J/A+A/465/1099)
10 = Rafferty et al. (2011, Cat. J/ApJ/742/3)
11 = Szokoly et al. (2004, Cat. J/ApJS/155/271)
12 = Luo et al. (2010, Cat. J/ApJS/187/560)
13 = Taylor et al. (2009, Cat. J/ApJS/183/295)
14 = Popesso et al. (2009A&A...494..443P 2009A&A...494..443P)
15 = Le Fevre et al. (2013A&A...559A..14L 2013A&A...559A..14L)
16 = Kurk et al. (2013, Cat. J/A+A/549/A63)
17 = Georgantopoulos et al. (2013A&A...555A..43G 2013A&A...555A..43G)
18 = Mignoli et al. (2005, Cat. J/A+A/437/883)
19 = Morris et al. (2015, Cat. J/AJ/149/178)
20 = Mignoli et al (2004A&A...418..827M 2004A&A...418..827M)
21 = Straatman et al. (2016, Cat. J/ApJ/830/51)
22 = Cardamone et al. (2010, Cat. J/ApJS/189/270)
23 = Pentericci et al. (2018, arXiv e-prints, arXiv:1811.05298)
24 = Urrutia et al. (2019, Cat. J/A+A/624/A141)
Note (3): For ECDFS sources.
Note (4): RID appears only when the source is classified as radio-loud AGN.
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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1- 5 F5.3 keV E Observed energy
7- 11 F5.3 keV e_E Observed energy error
13- 22 E10.4 10-18W/m2/keV Fluxdens Flux density in (0.5-7)keV band
(in 10^-15 erg/s/cm^2/keV unit)
24- 33 E10.4 10-18W/m2/keV e_Fluxdens Flux density error
(in 10^-15 erg/s/cm^2/keV unit)
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Acknowledgements:
Kazushi Iwasawa, kazushi.iwasawa(at)icc.ub.edu
References:
Comastri et al., Paper I 2011A&A...526L...9C 2011A&A...526L...9C
Iwasawa et al., Paper II 2012A&A...546A..84I 2012A&A...546A..84I
Ranalli et al., Paper III 2013A&A...555A..42R 2013A&A...555A..42R, Cat. J/A+A/555/A42
Georgantopoulos et al., Paper IV 2013A&A...555A..43G 2013A&A...555A..43G
Falocco et al., Paper V 2013A&A...555A..79F 2013A&A...555A..79F
Castello-Mor et al., Paper VI 2013A&A...556A.114C 2013A&A...556A.114C, Cat. J/A+A/556/A114
Antonucci et al., Paper VII 2015A&A...574A..49A 2015A&A...574A..49A, Cat. J/A+A/574/A49
Iwasawa et al., Paper VIII 2015A&A...574A.144I 2015A&A...574A.144I
Vignali et al., Paper IX 2015A&A...583A.141V 2015A&A...583A.141V
Falocco et al., Paper X 2017A&A...608A..32F 2017A&A...608A..32F
(End) Patricia Vannier [CDS] 20-Apr-2020