J/MNRAS/456/1195 KMOS AGN Survey at High redshift (KASHz) (Harrison+, 2016)
The KMOS AGN Survey at High redshift (KASHz): the prevalence and drivers of
ionized outflows in the host galaxies of X-ray AGN.
Harrison C.M., Alexander D.M., Mullaney J.R., Stott J.P., Swinbank A.M.,
Arumugam V., Bauer F.E., Bower R.G., Bunker A.J., Sharples R.M.
<Mon. Not. R. Astron. Soc., 456, 1195-1220 (2016)>
=2016MNRAS.456.1195H 2016MNRAS.456.1195H (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Redshifts
Keywords: galaxies: active - galaxies: evolution -
galaxies: kinematics and dynamics - quasars: emission lines
Abstract:
We present the first results from the KMOS (K-band Multi-Object
Spectrograph) AGN (active galactic nuclei) Survey at High redshift
(KASHz), a VLT/KMOS integral-field spectroscopic (IFS) survey of
z≳0.6 AGN. We present galaxy-integrated spectra of 89 X-ray AGN
(L2-10keV= 1042-1045erg/s), for which we observed [OIII]
(z∼1.1-1.7) or Hα emission (z∼0.6-1.1). The targets have X-ray
luminosities representative of the parent AGN population and we
explore the emission-line luminosities as a function of X-ray
luminosity. For the [OIII] targets, ∼50 per cent have ionized gas
velocities indicative of gas that is dominated by outflows and/or
highly turbulent material (i.e. overall line widths ≳600km/s). The
most luminous half (i.e. LX>6x1043erg/s) have a≳2 times higher
incidence of such velocities. On the basis of our results, we find no
evidence that X-ray obscured AGN are more likely to host extreme
kinematics than unobscured AGN. Our KASHzsample has a distribution of
gas velocities that is consistent with a luminosity-matched sample of
z<0.4 AGN. This implies little evolution in the prevalence of
ionized outflows, for a fixed AGN luminosity, despite an
order-of-magnitude decrease in average star formation rates over this
redshift range. Furthermore, we compare our Hα targets to a
redshift-matched sample of star-forming galaxies and despite a similar
distribution of Hα luminosities and likely star formation rates,
we find extreme ionized gas velocities are up to ∼10 times more
prevalent in the AGN-host galaxies. Our results reveal a high
prevalence of extreme ionized gas velocities in high-luminosity X-ray
AGN and imply that the most powerful ionized outflows in high-redshift
galaxies are driven by AGN activity.
Description:
KASHz is designed to ultimately obtain spatially resolved
emission-line kinematics of ~(100-200) high-redshift (z∼0.6-3.6) AGN.
For our target selection we make use of deep X-ray surveys performed
in extragalactic fields (COSMOS, see Scoville et al., 2007, Cat.
J/ApJS/171/1; CDF-S, see Giacconi et al. 2001ApJ...551..624G 2001ApJ...551..624G and Xue
et al., 2011, Cat. J/ApJS/195/10 (CDFS); UDS, SXDS: see Furusawa et
al. 2008, Cat. J/ApJS/176/1 (UDS) and SSA22, see Steidel et al.
1998ApJ...492..428S 1998ApJ...492..428S).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 120 89 Properties for the KASHz targets observed so far
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See also:
J/ApJS/176/1 : Subaru/XMM-Newton deep survey (SXDS). II. (Furusawa+, 2008)
J/ApJS/195/10 : The CDF-S survey: 4Ms source catalogs (Xue+, 2011)
J/ApJS/171/1 : Census of QSOs Narrow Absorption Lines (Misawa+, 2007)
J/ApJS/184/158 : Chandra COSMOS survey I. (Elvis+, 2009)
J/ApJS/201/30 : Chandra COSMOS survey. III. (Civano+, 2012)
J/A+A/497/635 : XMM-Newton wide-field survey in COSMOS field (Cappelluti+ 2009)
J/ApJ/716/348 : XMM-Newton survey of the COSMOS field (Brusa+, 2010)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Source name (Field-X-ray ID) (1)
10 A1 --- n_Name [*] Note on Name (2)
12- 16 F5.3 --- zA Archival redshift
18 A1 --- n_zA [spi] Archival redshift type (3)
20 A1 --- l_F0.5-2 Limit flag on F0.5-2
21- 25 F5.2 10-18W/m2 F0.5-2 Soft-band (0.5-2keV) X-ray flux
27- 31 F5.2 10-18W/m2 F2-10 Hard-band (2-10keV) X-ray flux
32 A1 --- n_F2-10 [+] Note on F2-10 (4)
34 A1 --- Obs [UO?] obscured/unobscured candidate flag (5)
36 A1 --- RL [xv?] radio luminous flag (6)
38 A1 --- Inst [KS] Instrument used for the observations
(K = KMOS and S = SINFONI)
40 A1 --- Line [OH] Primary targeted emission line (7)
42- 45 F4.1 ks texp On-source exposure time
47 A1 --- Note [CLN] Note on data (8)
49- 53 A5 --- BLR [alpha beta -] Note for the identification of
a BLR component (alpha for Hα and
beta for Hβ)
55- 59 F5.3 --- zl ?=- Redshift derived from the narrowest
Gaussian component of the emission-line
profile fit
61 A1 --- l_SA Limit flag on SA
62- 65 F4.1 10-20W/m2 SA ?=- Flux of the narrower Gaussian component
67- 69 F3.1 10-20W/m2 e_SA ? rms uncertainty on SA (10)
71- 73 I3 km/s FWA ?=- FWHM of the narrower Gaussian component
75- 77 I3 km/s e_FWA ? rms uncertainty on FWA (10)
79- 83 F5.1 10-20W/m2 SB ?=- Flux of the broader Gaussian component (9)
85- 87 F3.1 10-20W/m2 e_SB ? rms uncertainty on SB (10)
89- 92 I4 km/s FWB ?=- FWHM of the broader Gaussian component (9)
94- 97 I4 km/s e_FWB ? rms uncertainty on FWB (10)
99-102 I4 km/s DV ?=- Velocity offset between the two Gaussian
components
104-106 I3 km/s e_DV ? rms uncertainty on DV (108)
108 A1 --- l_S[NII] Limit flag on S[NII]
109-112 F4.2 10-20W/m2 S[NII] ?=- Flux of [NII] 6583 where applicable
114-116 I3 km/s W80 ? Overall emission-line width
118-120 I3 km/s e_W80 ? rms uncertainty on W80 (10)
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Note (1): Field are
CDFS for Chandra Deep Field South, Xue et al. (2011, Cat. J/ApJS/195/10)
UDS for Ultra Deep Survey, Furusawa et al. (2008, Cat. J/ApJS/176/1)
COS for C-COSMOS, Civano et al. (2012, Cat. J/ApJS/201/30)
XCOS for XMM-COSMOS, Brusa et al. (2010, Cat. J/ApJ/716/348)
SSA22 for SSA22 z=3.09 protocluster field (see Steidel et al.
1998ApJ...492..428S 1998ApJ...492..428S)
Note (2): * for targets excluded from the analyses presented in this paper
(see Section 4.1).
Note (3): Archival redshift type as follows:
p = photometric
s = secure spectroscopic redshift
i = insecure spectroscopic redshift
Note (4): + for hard-band values estimated from the soft-band fluxes
(see Section 2.1).
Note (5): Flag as follows:
O = X-ray obscured candidates
U = unobscured
? = candidates without sufficient constraints
Note (6): Flag to indicate the 'radio luminous' targets with
L1.4GHz>1024W/Hz (Section 2.5).
Note (7): Primary targeted emission line flag as follows:
O = [OIII]
H = Halpha
Note (8): Note on data as follows:
L = line detected
C = continuum only detected
N = no detection
Note (9): for sources with 'alpha' in column BLR, this is the BLR component
Note (10): All of the quoted uncertainties are the random errors on the fits due
to the noise in the spectra; however, we note that throughout this work we
add an extra 30 per cent systematic error to the emission-line fluxes to
account for the uncertainty in the flux calibration (see Section 3.2).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 03-Aug-2016