J/ApJS/187/64 The simultaneous optical-to-X-ray SED of AGNs (Grupe+, 2010)
The simultaneous optical-to-X-ray spectral energy distribution of soft X-ray
selected active galactic nuclei observed by Swift.
Grupe D., Komossa S., Leighly K.M., Page K.L.
<Astrophys. J. Suppl. Ser., 187, 64-106 (2010)>
=2010ApJS..187...64G 2010ApJS..187...64G
ADC_Keywords: Active gal. nuclei ; Energy distributions ; Photometry, UBV ;
Photometry, ultraviolet ; X-ray sources
Keywords: galaxies: active
Abstract:
We report Swift observations of a sample of 92 bright soft X-ray
selected active galactic nuclei (AGNs). This sample represents the
largest number of AGNs observed to study the spectral energy
distribution (SED) of AGNs with simultaneous optical/UV and X-ray
data. The principal motivation of this study is to understand the SEDs
of AGNs in the optical/UV to X-ray regime and to provide bolometric
corrections which are important in determining the Eddington ratio
L/LEdd. In particular, we rigorously explore the dependence of the
UV-EUV contribution to the bolometric correction on the assumed EUV
spectral shape. We find strong correlations of the spectral slopes
αX and αUV with L/LEdd.
Description:
The AGNs in the sample presented here were selected from the bright
soft X-ray selected AGN sample of Grupe et al. (2001A&A...367..470G 2001A&A...367..470G,
2004, Cat. J/AJ/127/156) which contains a total of 110 AGNs. Table 1
lists all AGNs presented here. In total, Swift has observed 92 bright
soft X-ray selected AGNs so far. A summary of all XRT and UVOT
observations is given in Table 2. Note that most AGNs have been
observed multiple times allowing us also to search for UV and X-ray
variabilities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 97 92 List of soft X-ray selected AGNs observed by Swift
table2.dat 110 301 Observation summary of the Swift-XRT and UVOT
observations
table3.dat 92 272 Results of the Swift-UVOT photometry
table4.dat 115 322 Spectral analysis of the Swift/XRT data
table5.dat 118 91 Properties of the Spectral Energy Distribution
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See also:
J/AJ/127/156 : Soft X-Ray-Selected AGNs complete sample (Grupe+, 2004)
J/ApJ/633/L77 : SWIFT/BAT detections of AGN (Markwardt+, 2005)
J/ApJ/663/81 : SED of hard X-ray selected AGN in XMDS (Polletta+, 2007)
J/ApJ/681/113 : Swift BAT survey of AGNs (Tueller+, 2008)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Running number
4- 18 A15 --- Name Object identification
20- 21 I2 h RAh Optical hour of right ascension (J2000)
23- 24 I2 min RAm Optical minute of right ascension (J2000)
26- 29 F4.1 s RAs Optical second of right ascension (J2000)
31 A1 --- DE- Optical sign of declination (J2000)
32- 33 I2 deg DEd Optical degree of declination (J2000)
35- 36 I2 arcmin DEm Optical arcminute of declination (J2000)
38- 39 I2 arcsec DEs Optical arcsecond of declination (J2000)
41- 45 F5.3 --- z Redshift
47- 50 F4.2 10+20/cm2 N Galactic column density from Dickey &
Lockman HI maps (1990ARA&A..28..215D 1990ARA&A..28..215D)
52- 55 F4.2 --- alphaX X-ray energy spectral slope in the 0.2-2.0keV
band (1)
57- 60 F4.2 --- u_alphaX Uncertainty on alphaX
62- 67 F6.2 [W/m2] logFx Rest-frame 0.2-2.0keV X-ray flux (1)
69- 73 F5.3 mag E(B-V) Galactic reddening E(B-V) from
Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S)
75- 78 I4 km/s FWHM(Hb) FWHM(Hβ) from Grupe et al. (2004,
Cat. J/AJ/127/156) (2)
80- 84 F5.1 MsolMass MBH Black hole mass MBH (3)
86- 89 F4.2 --- Ha/Hb ?=- Hα/Hβ ratio
91 A1 --- f_Ha/Hb [h] from Lira et al. (1999MNRAS.305..109L 1999MNRAS.305..109L)
93- 97 F5.3 mag E(B-V)i ?=- Intrinsic reddening E(B-V)-intr derived
from the Balmer decrement
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Note (1): during the RASS as given in Grupe et al. (2001A&A...367..470G 2001A&A...367..470G)
Note (2): We separated NLS1s and BLS1s by the common criterion of 2000km/s.
Note (3): determined by the method described in Kaspi et al.
(2000ApJ...533..631K 2000ApJ...533..631K) using FWHM(Hβ) and L5100Å
as given in Grupe et al. (2004, Cat. J/AJ/127/156).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Running number
4- 18 A15 --- Name Object identification
19 A1 --- n_Name [bdefh] Note on Swift observation (1)
21- 25 I5 --- Target Target identification number
27 A1 --- f1 [c] Flag on RX J0148.3-2758 (2)
29- 31 I3 --- Segment ? Segment number (3)
33 A1 --- f2 [g] Flag on MCG+08-23-067 (4)
35- 44 A10 "YYYY/MM/DD" Ts.date Starting date of observation
46- 50 A5 "h:m" Ts.time Starting time of observation
52- 61 A10 "YYYY/MM/DD" Te.date Ending date of observation
63- 67 A5 "h:m" Te.time Ending time of observation
69- 73 I5 s Txrt ? XRT exposure time
75- 78 I4 s Tv ? UVOT exposure time in V filter
79 A1 --- f_Tv [ij] Flag on Tv (5)
81- 84 I4 s Tb ? UVOT exposure time in B filter
85 A1 --- f_Tb [ij] Flag on Tb (5)
87- 90 I4 s Tu ? UVOT exposure time in U filter
91 A1 --- f_Tu [ij] Flag on Tu (5)
93- 96 I4 s Tw1 ? UVOT exposure time in UVW1 filter (260nm)
97 A1 --- f_Tw1 [oij] Flag on Tw1 (5)
99-102 I4 s Tm2 ? UVOT exposure time in UVM2 filter (220nm)
103 A1 --- f_Tm2 [ij] Flag on Tm2 (5)
105-109 I5 s Tw2 ? UVOT exposure time in UVW2 filter (180nm)
110 A1 --- f_Tw2 [ij] Flag on Tw2 (5)
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Note (1): Flags as follows:
b = Swift observed Mkn 335 several times as a monitoring project (Grupe et
al. 2007ApJ...668L.111G 2007ApJ...668L.111G, 2008ApJ...681..982G 2008ApJ...681..982G). Here we used one of the
observations during the more typical high state.
d = PG 1211+143 was monitored by Swift for more than a month (Bachev et al.
2009MNRAS.399..750B 2009MNRAS.399..750B). Here we picked only one of the observations during
high state.
e = Mkn 766 has been observed through a monitoring campaign by Swift
(D. Grupe et al. 2010, in preparation). Here we only present the first
segment of data as a representative observation.
f = 3C 273 has been observed by Swift many times as a calibration target as
well as a science target. Here we only picked two recent observations in
2009 which were observed in five UVOT filters in the 5'x5'UVOT hardware
window.
h = The data of NGC 5548 are from an observing campaign in 2007 with
simultaneous observations with Suzaku (Krongold et al.,
2010ApJ...710..360K 2010ApJ...710..360K).
Note (2): The NLS1 galaxy RX J0148.3-2758 has been observed by Swift
multiple times, and the results of the observations obtained in 2005
have already been published in Grupe et al. (2006AJ....132.1189G 2006AJ....132.1189G).
Therefore, here we only list the new, previously unpublished
observations.
Note (3): Segments are used for Swift planning purposes. Typically, one
segment covers a time span of 1 or 2 days.
Note (4): MCG+08-23-067 was previously observed in 2005. However, these
observations were all performed with the UV grism.
Note (5): Flags as follows:
i = UVOT observations done with the grisms.
j = Due to a bright star 3' away from the position of RX J2248.6-5109 UVOT
could not observe the field in order to avoid damaging the instrument.
o = other value is 128.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Running index number
4- 18 A15 --- Name Object name
20- 26 A7 --- Segment Segment(s)
28- 32 F5.2 mag Vmag ? Swift/UVOT V band magnitude (1)
34- 37 F4.2 mag e_Vmag ? Uncertainty in Vmag
39- 43 F5.2 mag Bmag ? Swift/UVOT B band magnitude (1)
45- 48 F4.2 mag e_Bmag ? Uncertainty in Bmag
50- 54 F5.2 mag Umag ? Swift/UVOT U band magnitude (1)
56- 59 F4.2 mag e_Umag ? Uncertainty in Umag
61- 65 F5.2 mag W1mag ? Swift/UVOT UVW1 band (260nm) magnitude (1)
67- 70 F4.2 mag e_W1mag ? Uncertainty in UVW1mag
72- 76 F5.2 mag M2mag ? Swift/UVOT UVM2 band (220nm) magnitude (1)
78- 81 F4.2 mag e_M2mag ? Uncertainty in UVM2mag
83- 87 F5.2 mag W2mag ? Swift/UVOT UVW2 band (180nm) magnitude (1)
89- 92 F4.2 mag e_W2mag ? Uncertainty in UVW2mag
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Note (1): UVOT magnitudes corrected for Galactic reddening using the
E_(B-V) values by Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S) as given
in Table 1. UVOT filters are centered at 260nm (W1) 220nm (M2) and
180nm (W2)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Running index number
4- 18 A15 --- Name Object name
20- 26 A7 --- Segment Segment(s)
28 I1 --- Model ? Model code (1)
30- 33 F4.2 --- alphaSX ? Soft X-ray spectral slope
35- 38 F4.2 --- E_alphaSX ? Upper limit uncertainty in alphaSX
40- 43 F4.2 --- e_alphaSX ? Lower limit Uncertainty in alphaSX
45- 48 F4.2 keV Ebreak ? Energy break
50- 53 F4.2 keV E_Ebreak ? Upper limit uncertainty in Ebreak
55- 58 F4.2 keV e_Ebreak ? Lower limit Uncertainty in Ebreak
60- 64 F5.2 --- alphaHX ? Hard X-ray spectral slope
66- 69 F4.2 --- E_alphaHX ? Upper limit uncertainty in alphaHX
71- 74 F4.2 --- e_alphaHX ? Lower limit Uncertainty in alphaHX
76- 81 F6.2 [W/m2] logF ? Log unabsorbed rest-frame 0.2-2 keV X-ray
flux
83- 87 F5.1 --- chi2 ? Reduced χ2; χ2/dof
88 A1 --- --- [/]
89- 91 I3 --- dof ? degrees of freedom
93- 97 F5.3 ct/s CR ? Swift/XRT count rate (0.2-10keV)
99-103 F5.3 ct/s e_CR ? Uncertainty in CR
105-109 F5.2 --- HR ? Hardness ratio (2)
111-115 F5.3 --- e_HR ? Uncertainty in HR
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Note (1): Model code as follows:
1 = absorbed power law;
2 = absorbed broken power law;
3 = absorbed blackbody plus power law.
Note (2): Defined as HR=(H-S)/(H+S) where S and H are the background
subtracted numbers of counts in the 0.3-1 and 1-10keV energy bands,
respectively.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Running number
4- 18 A15 --- Name Object identification
20- 26 A7 --- Segment Segment number(s)
28- 31 F4.2 --- alphaX X-ray slope in the 0.2-2.0keV energy range
33- 36 F4.2 --- e_alphaX Uncertainty on AlphaX
38- 42 F5.2 --- alphaUV Optical/UV slope corrected for Galactic
reddening
44- 47 F4.2 --- e_alphaUV Uncertainty on AlphaUV
49- 52 F4.2 --- alphaOX UV-to-X-ray spectra slope αox, as
defined by Tananbaum et al.
(1979ApJ...234L...9T 1979ApJ...234L...9T)
54- 58 F5.2 --- alphaUVc ?=- Optical/UV slope corrected for Galactic
and intrinsic reddening
60- 63 F4.2 --- e_alphaUVc ? Uncertainty on AlphaUVc
65- 68 F4.2 --- alphaOXc ?=- UV-to-X-ray spectra slope αox,
corrected for Galactic & intrinsic reddening
70- 74 F5.2 [W] logLx Rest-frame 0.2-2.0keV X-ray luminosity
76- 80 F5.2 [W] logLbbb Luminosity in the BBB (big-blue-bump)
emission (1)
82- 87 F6.3 --- L/LEdd L/LEdd ratio
89- 93 F5.2 [W] logLbbb2 Luminosity using the broken power-law model
as shown in Figure 1
95- 99 F5.2 [W] log5100 Luminosity at 5100Å
101-105 F5.2 [W] logLbbbc ?=- logLbbb corrected for intrinsic reddening
107-112 F6.3 --- L/LEddc ?=- L/LEdd corrected for intrinsic reddening
114-118 F5.2 [W] log5100c ?=- log5100 corrected for intrinsic reddening
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Note (1): Note that throughout this paper we use the BBB luminosity LBBB
rather than the bolometric luminosity Lbol. Although most of the SED
continuum energy in a Seyfert galaxy is deposited in the
optical-to-X-ray band, we miss emission in the radio band. However, we
do not consider the radio contribution significant in most of our
AGNs. Therefore, LBBB basically represents Lbol. This luminosity
is used to determine L/LEdd. See section 3.4 for further details.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 26-Apr-2010