J/ApJS/274/8 X-WING. I. Galaxies with ultrafast outflows (Yamada+, 2024)
X-ray Winds In Nearby-to-distant Galaxies (X-WING).
I. Legacy surveys of galaxies with ultrafast outflows and warm absorbers in
z∼0-4.
Yamada S., Kawamuro T., Mizumoto M., Ricci C., Ogawa S., Noda H., Ueda Y.,
Enoto T., Kokubo M., Minezaki T., Sameshima H., Horiuchi T., Mizukoshi S.
<Astrophys. J. Suppl. Ser., 274, 8 (2024)>
=2024ApJS..274....8Y 2024ApJS..274....8Y
ADC_Keywords: Active gal. nuclei; X-ray sources; References; Redshifts;
Black holes
Keywords: Black hole physics ; Active galactic nuclei ;
X-ray active galactic nuclei ; Supermassive black holes ;
Observational astronomy
Abstract:
As an inaugural investigation under the X-ray Winds In
Nearby-to-distant Galaxies (X-WING) program, we assembled a data set
comprising 132 active galactic nuclei (AGNs) spanning redshifts z∼0-4
characterized by blueshifted absorption lines indicative of X-ray
winds. Through an exhaustive review of previous research, we compiled
the outflow parameters for 583 X-ray winds, encompassing key
attributes such as outflow velocities (Vout), ionization parameters
(ξ), and hydrogen column densities. By leveraging the parameters
Vout and ξ, we systematically categorized the winds into three
distinct groups: ultrafast outflows (UFOs), low-ionization parameter
(low-IP) UFOs, and warm absorbers (WAs). Strikingly, a discernible
absence of linear correlations in the outflow parameters, coupled with
distributions approaching instrumental detection limits, was observed.
Another notable finding was the identification of a velocity gap
around Vout ∼10000km/s. This gap was particularly evident in the winds
detected via absorption lines within the ≲2keV band, indicating
disparate origins for low-IP UFOs and WAs. In cases involving
FeXXV/FeXXVI lines, where the gap might be attributed to potential
confusion between emission/absorption lines and the Fe K-edge, the
possibility of UFOs and galactic-scale WAs being disconnected is
considered. An examination of the outflow and dust sublimation radii
revealed a distinction: UFOs appear to consist of dust-free material,
whereas WAs likely comprise dusty gas. From 2024, the X-Ray Imaging
and Spectroscopy Mission is poised to alleviate observational biases,
providing insights into the authenticity of the identified gap, a
pivotal question in comprehending AGN feedback from UFOs.
Description:
We attempted to identify all galaxies wherein X-ray winds (ultrafast
outflows (UFOs) and outflowing warm absorbers (WAs)) were reported by
the end of 2023, as detected by their X-ray blueshifted ionized
absorption lines. In this study, we focused on the X-ray instruments
utilized to identify X-ray winds over the past 20yr:
(1) Chandra/High Energy Transmission Grating Spectrometer (HETGS),
(2) Chandra/Low Energy Transmission Grating Spectrometer (LETGS),
(3) Chandra/Advanced CCD Imaging Spectrometer (ACIS),
(4) XMM-Newton/Reflection Grating Spectrometer (RGS),
(5) XMM-Newton/European Photon Imaging Camera (EPIC) PN,
(6) XMM-Newton/EPIC MOS,
(7) Nuclear Spectroscopic Telescope Array (NuSTAR)/Focal Plane Modules
(FPM),
(8) Suzaku/X-ray Imaging Spectrometer (XIS), and
(9) Swift/X-Ray Telescope (XRT).
We adopt the cosmological parameters H0=70km/s/Mpc, ΩM=0.3,
and {Omaga}Λ= 0.7.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 128 132 Target information in the X-WING sample
tableb2.dat 142 583 X-ray wind properties
tableb3.dat 132 583 Observations and references of the X-ray winds
refs.dat 93 396 References
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See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
B/swift : Swift Master Catalog (HEASARC, 2004-)
B/xmm : XMM-Newton Obs. Log (XMM-Newton Science Operation Center, 2012-)
VII/258 : Quasars and Active Galactic Nuclei (13th Ed.) (Veron-Cetty+ 2010)
J/ApJ/613/682 : Broad-line region sizes (Peterson+, 2004)
J/A+A/451/457 : X-ray properties of AGN in CDFS (Tozzi+, 2006)
J/ApJ/658/815 : Radio loudness of active galactic nuclei (Sikora+, 2007)
J/ApJ/660/1072 : Unified model of active galactic nuclei (Wang+, 2007)
J/A+A/495/421 : AGN in XMM-Newton archive (CAIXA) (Bianchi+, 2009)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/ApJ/727/20 : The Megamaser Cosmology Project (MCP). III. (Kuo+, 2011)
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
J/MNRAS/426/2522 : FeK lines in Seyfert 1 galaxies (Patrick+, 2012)
J/A+A/542/A83 : CAIXA. II. AGNs from excess variance analysis (Ponti+, 2012)
J/MNRAS/430/60 : Highly ionized outflows in AGN (Gofford+, 2013)
J/A+A/562/A21 : AGN feedback from CO observations (Cicone+, 2014)
J/ApJ/802/89 : Luminosity function of X-ray-selected AGNs (Buchner+, 2015)
J/ApJ/806/22 : SEAMBHs IV. Hβ time lags (Du+, 2015)
J/ApJ/813/82 : z<0.06 broad-line AGN emission-line measures (Reines+, 2015)
J/A+A/593/A30 : Detection of fast HI outflow in Mrk231 (Morganti+, 2016)
J/ApJS/233/17 : Swift/BAT AGN spectroscopic survey. V. X-ray (Ricci+, 2017)
J/A+A/597/A51 : Physical properties of Spitzer/IRS galaxies (Vika+, 2017)
J/A+A/615/A72 : NGC 7469 X-ray spectra (Mehdipour+, 2018)
J/ApJ/876/102 : Reverberation mapping of the Seyfert Zw I 1 (Huang+, 2019)
J/A+A/629/A54 : NGC4388 and NGC2110 spectral files (Ursini+, 2019)
J/ApJS/253/20 : SEAMBHs XII. Reberberation mapping for PG QSOs (Hu+, 2021)
J/A+A/645/A74 : XMM-Newton spectral-fit redshift catalogue (Ruiz+, 2021)
J/ApJS/257/61 : X-ray spectral study of 57 local U/LIRGs (Yamada+, 2021)
J/ApJS/261/2 : BASS. XXII. Swift/BAT AGN Sp. Survey DR2 cat. (Koss+, 2022)
J/ApJS/261/6 : BASS. XXVI. DR2 stellar velocity dispersions (Koss+, 2022)
J/ApJ/925/52 : LAMP 2016: velocity-resolved Hb lags in Seyfert (U+, 2022)
J/ApJ/944/29 : Reverberation mapping of IC 4329A (Bentz+, 2023)
J/ApJS/269/15 : Survey of bare z<0.2 AGNs. I. X-ray (Nandi+, 2023)
J/ApJS/265/37 : Multiwavelength SED analysis of GOALS ULIRGs (Yamada+, 2023)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq [1/132] Identification number
5 I1 --- Group [1/3] Group number (1)
7- 28 A22 --- Name Object name
30- 35 F6.4 --- z [0.001/3.91] Spectroscopic redshift
37- 43 F7.1 Mpc DL [3.7/34896] Light distance (2)
45- 50 A6 --- Class Optical class
52- 57 F6.2 10-15W/m2 F2-10 [0.01/185] Observed 2-10keV flux;
10-12erg/cm2/s (3)
59- 63 F5.2 [10-7W] logL2-10 [40.5/46.2] Log of intrinsic AGN
luminosity in 2-10keV band; erg/s (3)
65- 69 F5.2 [Msun] logMBH [5.4/10.2] Log of supermassive black hole
mass
71- 76 A6 --- Method Method of supermassive black hole mass
estimation (4)
78- 79 I2 --- Nw [1/37] Number of X-ray winds reported in
the study
81 A1 --- f_Nw Flag on Nw (5)
83- 84 A2 --- UFO Presence of UFOs (6)
86- 89 A4 --- r_z/DL Reference for z and DL (see refs.dat file)
91- 94 A4 --- r_Class Reference for Class (see refs.dat file)
96- 99 A4 --- r_2-10keV Reference for F2-10 and logL2-10
(see refs.dat file)
101- 104 A4 --- r_logMBH Reference for logMBH and Method
(see refs.dat file)
106- 116 F11.7 deg RAdeg Right ascension (J2000)
118- 128 F11.7 deg DEdeg Declination (J2000)
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Note (1): Group as follows:
1 = Nearby (z<1) Galaxies (109 occurrences)
2 = High-z (z>1) Galaxies (17 occurrences)
3 = X-WING Candidates (6 occurrences)
Note (2): For the closest objects at DL<50Mpc, we adopted
redshift-independent distance measurements (Koss+ 2022, J/ApJS/261/2).
Note (3): Many values are from Ricci+ (2017, J/ApJS/233/17) and
Bianchi+ (2009, J/A+A/495/421).
Note (4): Method as follows:
RM = reverberation mapping;
maser = H2O megamaser;
Ha = broad emission lines of Hα;
Hb = broad emission lines of Hβ;
CIV = broad emission lines of C IV;
VLTI = near-infrared interferometric observations of the BLR with Very
Large Telescope Interferometer;
Vdisp = stellar velocity dispersion;
Ms = stellar mass to MBH ratio;
Xvar = X-ray variability;
others = other methods.
Note (5): Flag as follows:
* = uncertain AGN with X-ray winds as explained in Section 2.2.
Note (6): Presence of UFOs with Fe XXV/Fe XXVI lines detected in the >6keV
band (Section 3.3). Code as follows:
Y = AGN with UFOs (77 occurrences)
Y? = AGN with UFO candidates (10 occurrences), all of which only Vout
were constrained (but not ξ and NH, see also Section 2.2);
n = AGN with warm absorbers but no UFOs (45 occurrences)
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Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq [1/132] Target identification number as
in Table B1
4- 5 A2 --- ID [a-z ] Detection ID of outflow component
within Seq
7- 28 A22 --- Name Object name
30- 51 A22 --- Date Start date of observation (1)
53- 54 A2 --- Inst1 Instrument 1 of observation (2)
56- 57 A2 --- Inst2 Instrument 2 of observation (2)
59 A1 --- Inst3 [FM] Instrument 3 of observation (2)
61 A1 --- Fe-K [Yn] Fe-K absorption line detection (3)
63- 63 A1 --- l_logNH [~>< ] Limit on logNH
67- 71 F5.2 [cm-2] logNH [19/25.2]? Log of hydrogen column density
of ionized gas
73- 76 F4.2 [cm-2] E_logNH [0.01/1.3]? Upper uncertainty in logNH (4)
78- 81 F4.2 [cm-2] e_logNH [0.01/2.2]? Lower uncertainty in logNH,
negative values (4)
83- 83 A1 --- l_logVout [~>< ] Limit on logVout
87- 90 F4.2 [km/s] logVout [1.6/5.4] Log of outflow velocity
92- 95 F4.2 [km/s] E_logVout [0.01/0.6]? Upper uncertainty in logVout (4)
97-100 F4.2 [km/s] e_logVout [0.01/1.5]? Lower uncertainty in logVout,
negative values (4)
102-102 A1 --- l_logXi [~>< ] Limit on logXi
106-110 F5.2 [10-7W.cm] logXi [-1.4/6.6]? Log of ionization parameter,
ξ; erg/s.cm (5)
112-115 F4.2 [10-7W.cm] E_logXi [0.01/3.1]? Upper uncertainty in logXi
117-120 F4.2 [10-7W.cm] e_logXi [0.01/3]? Lower uncertainty in logXi,
negative values
122 A1 --- f_logXi Flag on logXi (6)
124-128 F5.2 [10-7W] logLion [40.7/47]? Log of ionizing luminosity; erg/s
130-132 A3 --- Type Outflow type (7)
134-142 A9 --- Model X-ray fitting models of X-ray winds (8)
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Note (1): The start dates of the oldest and latest observations are shown
when multiple observations are used to identify the ionized outflows.
Note (2): Instrument as follows:
A = Chandra/ACIS;
F = NuSTAR/FPM;
H = Chandra/HETGS;
L = Chandra/LETGS;
M = XMM-Newton/MOS;
P = XMM-Newton/PN;
R = XMM-Newton/RGS;
Su = Suzaku/XIS;
Sw = Swift/XRT.
Note (3): The method of outflow detection utilizes blueshifted Fe-K
absorption lines. Code as follows:
Y = Fe XXV/Fe XXVI Kα/Kβ absorption lines above the rest-frame
6keV band;
n = Fe XXV/Fe XXVI Kα/Kβ absorption lines below the 6keV band.
Note (4): When the uncertainties of Vout or NH are not constrained, we
assume that they are ±0.5, which are conservative values larger
than the typical errors (∼0.1-0.2) in Figures 3-7.
Note (5): The ionization parameter is defined as ξ=Lion/(nH*r2),
where Lion represents ionizing luminosity in the 13.6eV to 13.6keV
band or the 1-1000Ryd range, nH is the hydrogen number density, and
r is the distance from the source.
Note (6): Flag as follows:
* = indicates that the values are presented assuming logU=logξ-1.75
(Section 2.2).
Note (7): The OBSIDs and the references for each ID are listed in Table B4.
Type as follows:
UFO = ultrafast outflow (249 occurrences)
LIP = low-ionization parameter ultrafast outflow (28 occurrences)
WA = warm absorber (306 occurrences)
Note (8): See Appendix A. Model as follows:
XSTAR = XSTAR ionized absorber model;
zxipcf = partial covering of partially ionized absorbing material model;
xabs = photoionized absorption model;
gaussian = Gaussian model;
CLOUDY = Cloudy photoionization simulation;
warmabs = XSTAR photoionization model for warm absorber;
PHASE = PHotoionized Absorption Spectral Engine;
AMD = Absorption Measure Distribution;
MPI_XSTAR = parallel implementation involving multiple XSTAR runs;
pion = SPEX photoionized plasma model;
residual = residuals in spectral fittings;
windabs = XSTAR photoionization model for outflowing ionized absorber;
ABSORI = XSPEC model for ionized absorbing plasma;
FEV = Fractional Excess Variance.
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Byte-by-byte Description of file: tableb3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq Target identification number as in Table B1
4- 5 A2 --- ID [a-z ] Detection ID of outflow components
within Seq
7- 28 A22 --- Name Object name
30- 69 A40 --- OBSID OBSID
71- 76 A6 --- Ref1 Reference 1 for adopted X-ray winds
(see refs.dat file)
78- 83 A6 --- Ref2 Reference 2, pertinent paper on duplicated
reports (see refs.dat file)
85- 90 A6 --- Ref3 Reference 3, pertinent paper on duplicated
reports (see refs.dat file)
92- 97 A6 --- Ref4 Reference 4, pertinent paper on duplicated
reports (see refs.dat file)
99-104 A6 --- Ref5 Reference 5, pertinent paper on duplicated
reports (see refs.dat file)
106-111 A6 --- Ref6 Reference 6, pertinent paper on duplicated
reports (see refs.dat file)
113-118 A6 --- Ref7 Reference 7, pertinent paper on duplicated
reports (see refs.dat file)
120-125 A6 --- Ref8 Reference 8, pertinent paper on duplicated
reports (see refs.dat file)
127-132 A6 --- Ref9 Reference 9, pertinent paper on duplicated
reports (see refs.dat file)
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Ref Reference code
8- 35 A28 --- Auth First author's name(s)
37- 55 A19 --- BibCode Bibcode of the reference
57- 93 A37 --- Comm Comment
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-Apr-2025