J/A+A/687/A235 SUBWAYS. III. (Gianolli+, 2024)
Supermassive Black Hole Winds in X-rays: SUBWAYS.
III. A population study on Ultra-Fast Outflows.
Gianolli V.E., Bianchi S., Petrucci P-O., Brusa M., Chartas G., Lanzuisi G.,
Matzeu G.A., Parra M., Ursini F., Behar E., Bischetti M., Comastri A.,
Costantini E., Cresci G., Dadina M., De Marco B., De Rosa A., Fiore F.,
Gaspari M., Gilli R., Giustini M., Guainazzi M., King A.R., Kraemer S.,
Kriss G., Krongold Y., La Franca F., Longinotti A.L., Luminari A.,
Maiolino R., Marconi A., Mathur S., Matt G., Mehdipour M., Merloni A.,
Middei R., Miniutti G., Nardini E., Panessa F., Perna M., Piconcelli E.,
Ponti G., Ricci F., Serafinelli R., Tombesi F., Vignali C., Zappacosta L.
<Astron. Astrophys. 687, A235 (2024)>
=2024A&A...687A.235G 2024A&A...687A.235G (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Radio sources ; Redshifts ; Ultraviolet
Keywords: line: identification - galaxies: active - galaxies: nuclei -
X-ray: galaxies
Abstract:
The detection of blueshifted absorption lines likely associated with
ionized iron K-shell transitions in the X-ray spectra of many active
galactic nuclei (AGNs) suggests the presence of a highly ionized gas
outflowing with mildly relativistic velocities (0.03c-0.6c) named
ultra-fast outflow (UFO). Within the SUBWAYS project, we characterized
these winds starting from a sample of 22 radio-quiet quasars at an
intermediate redshift (0.1≤z≤0.4) and compared the results with
similar studies in the literature on samples of local Seyfert galaxies
(i.e., 42 radio-quiet AGNs observed with XMM-Newton at z≤0.1) and
high redshift radio-quiet quasars (i.e., 14 AGNs observed with
XMM-Newton and Chandra at z≥1.4). The scope of our work is a
statistical study of UFO parameters and incidence considering the key
physical properties of the sources, such as supermassive black hole
(SMBH) mass, bolometric luminosity, accretion rates, and spectral
energy distribution (SED) with the aim of gaining new insights into
the UFO launching mechanisms. We find indications that highly luminous
AGNs with a steeper X-ray/UV ratio, alpha_ox, are more likely to host
UFOs. The presence of UFOs is not significantly related to any other
AGN property in our sample. These findings suggest that the UFO
phenomenon may be transient. Focusing on AGNs with UFOs, other
important findings from this work include:
(1) faster UFOs have larger ionization parameters and column densities;
(2) X-ray radiation plays a more crucial role in driving highly
ionized winds compared to UV;
(3) the correlation between outflow velocity and luminosity is
significantly flatter than what is expected for radiatively driven
winds;
(4) more massive black holes experience higher wind mass losses,
suppressing the accretion of matter onto the black hole;
(5) the UFO launching radius is positively correlated with the
Eddington ratio. Furthermore, our analysis suggests the involvement of
multiple launching mechanisms, including radiation pressure and
magneto-hydrodynamic processes, rather than pointing to a single,
universally applicable mechanism.
Description:
We report all the AGN and UFO global parameters adopted during our
population study.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 415 77 AGN global parameters
tablea2.dat 352 34 UFO global parameters
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Source name
20- 29 A10 --- Sample Sample and sub-sample
31- 38 F8.6 --- z Redshift (1)
39- 57 F19.16 [Msun] logMBH Black Hole mass (1)
59- 76 F18.16 [Msun] e_logMBH Negative uncertainty on BH mass (3)
78- 95 F18.16 [Msun] E_logMBH Positive uncertainty on BH mass (3)
97-107 F11.8 [10-7W] logLX 2-10keV X-ray luminosity (1)
109-118 F10.8 [10-7W] e_logLX Negative uncertainty on X-ray
luminosity (3)
120-129 F10.8 [10-7W] E_logLX Positive uncertainty on X-ray
luminosity (3)
131-148 F18.15 [10-7W] logLbol Bolometric luminosity
150-167 F18.16 [10-7W] e_logLbol Negative uncertainty on bolometric
luminosity (3)
169-186 F18.16 [10-7W] E_logLbol Positive uncertainty on bolometric
luminosity (3)
188-205 F18.15 [10-7W/Hz] logL2500 ?=- 2500 angstrom (UV) luminosity
207-219 F13.11 [10-7W/Hz] e_logL2500 ?=- Negative uncertainty on UV
luminosity (3)
221-233 F13.11 [10-7W/Hz] E_logL2500 ?=- Positive uncertainty on UV
luminosity (3)
235-241 F7.5 --- Gamma X-ray power-law photon index
243-251 F9.7 --- e_Gamma Negative uncertainty on photon index (3)
253-261 F9.7 --- E_Gamma Positive uncertainty on photon index (3)
264-267 I4 km/s FWHMbHb ?=- FWHM broad Hbeta emission line
269-272 I4 km/s e_FWHMbHb ?=- Negative uncertainty on
FWHM Hbeta (3)
274-277 I4 km/s E_FWHMbHb ?=- Positive uncertainty on
FWHM Hbeta (3)
278 A1 --- l_NH Limit flag on NH
279-284 F6.1 10+20cm-2 NH ?=- Neutral absorber intrinsic
equivalent hydrogen column density
286-290 F5.1 10+20cm-2 E_NH ?=- Positive uncertainty on
column density (3)
291-295 F5.1 10+20cm-2 e_NH ?=- Negative uncertainty on
column density (3)
298-315 F18.16 --- Redd Eddington ratio (Redd = Lbol/Ledd)
317-337 E21.19 --- e_Redd Negative uncertainty on
Eddington ratio (3)
339-359 E21.19 --- E_Redd Positive uncertainty on
Eddington ratio (3)
361-367 F7.4 --- alphaox ? X-ray/UV slope (2)
369-374 F6.4 --- e_alphaox ? Negative uncertainty on
X-ray/UV slope (3)
376-381 F6.4 --- E_alphaox ? Positive uncertainty on
X-ray/UV slope (3)
383-389 F7.4 --- delta-aox ? X-ray weakness proxy
391-396 F6.4 --- e_delta-aox ? Negative uncertainty on
X-ray weakness (3)
398-403 F6.4 --- E_delta-aox ? Positive uncertainty on
X-ray weakness (3)
405-409 A5 --- Ref Reference (4)
411-415 A5 --- Notes Notes (5)
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Note (1): redshift, black hole masses, 2-10keV luminosities, X-ray photon
indices and neutral column densities of the S23 sample have been taken from
Matzeu et al. (2023A&A...670A.182M 2023A&A...670A.182M) and references therein, unless stated
otherwise.
Redshift, 2-10keV luminosities and X-ray photon indices of the T10 sample
have been taken from Tombesi et al. (2010A&A...521A..57T 2010A&A...521A..57T) and references
therein. As the X-ray luminosity uncertainties were not reported in the
paper, we adopted those documented in the XMM archive for the 2-10 keV flux,
and we applied them as a percentage to the luminosity.
Redshift, black hole masses, 2-10keV luminosities, X-ray photon indices
and alpha_ox of the C21 sample have been taken from Chartas et al.
(2021ApJ...920...24C 2021ApJ...920...24C) and references therein. All the reported luminosities
are corrected for lensing magnification.
We report the references of the BH mass, FWHM broad Hbeta, and neutral
column density for the T10 sample. References of the FWHM and neutral column
density for the S23 and C21 samples. '-' denotes values not documented in the
literature. Parameters without references have been estimated within
this work.
Note (2): The reported alphaox and delta-aox values refer only to the unabsorbed
sample defined in Sect. 3.2.
Note (3): We note that all the reported uncertainties are taken from the
literature and no systematic errors are taken into account.
Note (4): References as follows:
a = values from the automatic fit in the SDSS
b = Ricci et al., 2017A&A...598A..51R 2017A&A...598A..51R
c = Runnoe et al., 2013MNRAS.434..848R 2013MNRAS.434..848R
d = Sani et al., 2010MNRAS.403.1246S 2010MNRAS.403.1246S
e = Ho & Kim, 2014ApJ...789...17H 2014ApJ...789...17H
f = Vestegaard et al., 2002ApJ...571..733V 2002ApJ...571..733V
g = Peterson et al., 2004ApJ...613..682P 2004ApJ...613..682P
h = Ponti et al., 2012A&A...542A..83P 2012A&A...542A..83P
i = Kelly & Bechtold, 2007ApJS..168....1K 2007ApJS..168....1K
l = Botte et al., 2004AJ....127.3168B 2004AJ....127.3168B
m = Marin et al., 2016MNRAS.460.3679M 2016MNRAS.460.3679M
n = Middleton et al., 2008MNRAS.383.1501M 2008MNRAS.383.1501M
o = Wang & Zhang, 2007ApJ...660.1072W 2007ApJ...660.1072W
p = Bentz & Katz, 2015PASP..127...67B 2015PASP..127...67B
q = Markowitz et al., 2009ApJ...698.1740M 2009ApJ...698.1740M
s = Danehkar et al., 2018ApJ...853..165D 2018ApJ...853..165D
t = Woo & Urry, 2002ApJ...579..530W 2002ApJ...579..530W
u = Mckernan et al., 2010MNRAS.407.2399M 2010MNRAS.407.2399M
v = Assef et al., 2011ApJ...742...93A 2011ApJ...742...93A
A = Matzeu et al., 2023A&A...670A.182M 2023A&A...670A.182M
B = Tombesi et al., 2010A&A...521A..57T 2010A&A...521A..57T
C = Laha et al., 2019MNRAS.486.3124L 2019MNRAS.486.3124L
D = Winter et al., 2012ApJ...745..107W 2012ApJ...745..107W
E = Chartas et al., 2021ApJ...920...24C 2021ApJ...920...24C
F = Chartas et al., 2009ApJ...706..644C 2009ApJ...706..644C
G = Chartas et al., 2003ApJ...595...85C 2003ApJ...595...85C
H = Gondoin et al., 2003A&A...397..883G 2003A&A...397..883G
Note (5): Notes as follows:
* = multi-epochs sources. We report the mean values of each parameter.
In case of a multi-epochs AGNs hosting UFO, the means refer only to
observations with detected ultra-fast outflows.
+ = AGN with intrinsic column density below the adopted threshold (i.e.,
5*1020cm-2; see Sect. 3.2), but with Galactic absorbing column
density above it.
++ = BH masses were taken from Parker et al. (for PG 0052+251 and
PG 1307+085; 2020MNRAS.492.1363P 2020MNRAS.492.1363P) and Matzeu et al.
(2023A&A...670A.182M 2023A&A...670A.182M). However, as the uncertainties are not reported
in the papers, we opted to apply an uncertainty of 0.3dex. This accounts
for the dependence of the BH mass on the square of FWHM, alongside the
uncertainties in luminosity (whether line or continuum) and zero point.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Source name
19 A1 --- n_Name [*] Note on Name (1)
20- 22 A3 --- Sample Sample and sub-sample
24 A1 --- l_logNH Limit flag on logNH
25- 42 F18.15 [cm-2] logNH Ionized absorber column density (2) (3)
44- 53 F10.8 [cm-2] e_logNH ? Negative uncertainty on column density (4)
55- 64 F10.8 [cm-2] E_logNH ? Positive uncertainty on column density (4)
66 A1 --- l_logxi Limit flag on logxi (3)
67- 73 F7.5 [mW/m2] logxi Ionization parameter
75- 82 F8.6 [mW/m2] e_logxi ? Negative uncertainty on
ionization parameter (4)
84- 91 F8.6 [mW/m2] E_logxi ? Positive uncertainty on
ionization parameter (4)
93- 97 F5.3 c vout Outflow velocity (3)
99-103 F5.3 c e_vout Negative uncertainty on outflow velocity (4)
105-109 F5.3 c E_vout Positive uncertainty on outflow velocity (4)
111 A1 --- l_logrwind Limit flag on logrwind (2)
112-129 F18.15 [cm] logrwind Distance outflow-SMBH
131-148 F18.16 [cm] e_logrwind ? Negative uncertainty on wind location (4)
150-167 F18.16 [cm] E_logrwind ? Positive uncertainty on wind location (4)
169 A1 --- l_logMwind Limit flag on logMwind
170-187 F18.15 [g/s] logMwind Outflow mass rate
189-206 F18.16 [g/s] e_logMwind ? Negative uncertainty on mass rate (4)
208-225 F18.16 [g/s] E_logMwind ? Positive uncertainty on mass rate (4)
227 A1 --- l_logEkwind Limit flag on logEkwind
228-245 F18.15 [10-7W] logEkwind Outflow mechanical power
247-264 F18.16 [10-7W] e_logEkwind ? Negative uncertainty on
mechanical power (4)
266-283 F18.16 [10-7W] E_logEkwind ? Positive uncertainty on
mechanical power (4)
285 A1 --- l_logPwind Limit flag on logPwind
286-303 F18.15 [-] logPwind Outflow momentum rate
305-322 F18.16 [-] e_logPwind ? Negative uncertainty on momentum rate (4)
324-341 F18.16 [-] E_logPwind ? Positive uncertainty on momentum rate (4)
343-352 F10.8 --- Psi Relativistic effects correction factor
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Note (1): Note as follows:
PG 1114+445: PG 1114+445 is a multi-epoch source with detected UFO in Obs ID:
0651330101 and 0651330301; the reported values are means.
PG 0947+396: In PG 0947+396 the detected UFO is in Obs ID 0841481001.
PG 0804+761: In PG 0804+761 the detected UFO is in Obs ID 0102040401.
Note (2): the correction factor has to be applied on the N_H and r_wind values
reported in the Table.
Note (3): NH, xi and vout values of each sample are taken from the respective
papers.
Note (4): We note that all the reported uncertainties are taken from the
literature and no systematic errors are taken into account.
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Acknowledgements:
Vittoria Gianolli, vittoria.gianolli(at)univ-grenoble-alpes.fr
References:
Matzeu et al., Paper I 2023A&A...670A.182M 2023A&A...670A.182M
Mehdipour et al., Paper II 2023A&A...670A.183M 2023A&A...670A.183M
(End) Patricia Vannier [CDS] 30-Mar-2024