J/MNRAS/510/4909 Chandra X-ray's study of LeMMINGs galaxies (Williams+, 2022)
LeMMINGs - IV. The X-ray properties of a statistically complete sample of the
nuclei in active and inactive galaxies from the Palomar sample.
Williams D.R.A., Pahari M., Baldi R.D., Mchardy I.M., Mathur S.,
Beswick R.J., Beri A., Boorman P., Aalto S., Alberdi A., Argo M.K.,
Dullo B.T., Fenech D.M., Green D.A., Knapen J.H., Marti-Vidal I.,
Moldon J., Mundell C.G., Muxlow T.W.B., Panessa F., Perez-Torres M.,
Saikia P., Shankar F., Stevens I.R., Uttley P.
<Mon. Not. R. Astron. Soc., 510, 4909-4928 (2022)>
=2022MNRAS.510.4909W 2022MNRAS.510.4909W (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Active gal. nuclei ; Galaxies, IR ;
Galaxies, radio ; Galaxies, Seyfert ; Black holes ; Optical ;
X-ray sources ; Positional data ; Line Profiles ; Spectroscopy ;
Photometry
Keywords: X-rays: galaxies - galaxies: active
Abstract:
All 280 of the statistically complete Palomar sample of nearby (< 120 Mpc)
galaxies δ > 20° have been observed at 1.5 GHz as part of
the LeMMINGs e-MERLIN legacy survey. Here, we present Chandra X-ray
observations of the nuclei of 213 of these galaxies, including a
statistically complete sub-set of 113 galaxies in the declination
range 40° < δ < 65°. We observed galaxies of all optical
spectral types, including 'active' galaxies [e.g. low-ionization
nuclear emission line regions (LINERs) and Seyferts] and 'inactive'
galaxies like H II galaxies and absorption line galaxies (ALG). The
X-ray flux limit of our survey is 1.65*10-14 erg/s/cm2 (0.3-10
keV). We detect X-ray emission coincident within 2 arcsec of the
nucleus in 150/213 galaxies, including 13/14 Seyferts, 68/77 LINERs,
13/22 ALGs and 56/100 H II galaxies, but cannot completely rule out
contamination from non-AGN processes in sources with nuclear
luminosities ≲ 1039 erg/S. We construct an X-ray Luminosity
function (XLF) and find that the local galaxy XLF, when including all
active galactic nucleus (AGN) types, can be represented as a single
power law of slope -0.54 ± 0.06. The Eddington ratio of the Seyferts
is usually 2-4 decades higher than that of the LINERs, ALGs, and H II
galaxies, which are mostly detected with Eddington ratios ≲ 10-3.
Using [O III] line measurements and black hole masses from the
literature, we show that LINERs, H II galaxies and ALGs follow similar
correlations to low luminosities, suggesting that some 'inactive'
galaxies may harbour AGN.
Description:
In our study context, we have constructed a catalogue of nuclear X-ray
emission in nearby galaxies selected from the Palomar survey covered
by LeMMINGs data, compiling all available data in the Chandra archive.
We obtained 48 new observations of nearby galaxies to complete the
sample in a declination range. Our catalogue has subarcsecond imaging
in the X-ray band and is unbiased towards 'inactive' galaxies due
to the parent sample selection.
As detailed in section 2 Sample selection and chandra observations, we
build a statistically complete sample of nearby LLAGN based on Palomar
sample (Filippenko & Sargent 1985ApJS...57..503F 1985ApJS...57..503F; Ho et al.
1995ApJS...98..477H 1995ApJS...98..477H, Cat. J/ApJS/98/477; Ho et al.
1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315; Ho et al.
1997ApJS..112..391H 1997ApJS..112..391H; Ho et al. 1997ApJ...487..568H 1997ApJ...487..568H; Ho et al.
1997ApJ...487..591H 1997ApJ...487..591H; Ho et al. 2003ApJ...583..159H 2003ApJ...583..159H; Ho et al.
2009ApJS..183....1H 2009ApJS..183....1H, Cat. J/ApJS/183/1). In other part, 280 radio
conuterpart galaxies represented in the LeMMINGs radio survey of
nearby galaxies (Beswick et al. 2014evn..confE..10B; Baldi et al.
2018MNRAS.476.3478B 2018MNRAS.476.3478B; Baldi et al. 2021MNRAS.500.4749B 2021MNRAS.500.4749B,
Cat. J/MNRAS/500/4749; Baldi et al. 2021MNRAS.508.2019B 2021MNRAS.508.2019B) probing
accretion and SF in nearby galaxies in the radio waveband at 1.5 and
5 GHz with resolutions of up to 150 and 50 mas, respectively, in
concert with ancillary multiwavelength data. Thus far, all 280 of the
LeMMINGs objects have been observed by e-MERLIN at 1.5 GHz. To
diagnose the central engine, all of the objects in the LeMMINGs survey
were re-classified using their optical spectra from the Palomar sample
into the Seyfert, LINER, ALG or H II galaxy classifications according
to updated diagnostic diagrams. Their properties are presented in
table1.dat.
Of the 280 Palomar galaxies above δ = 20°, 125/280 had been
observed by Chandra observing programmes as of June 2015 and the data
were publicly available. An additional 48 objects were observed as
part of Chandra observing cycle 17 (programme ID 19708646 and
18620515), to provide complete Chandra coverage of all Palomar
galaxies, selected in the declination range of 40°-65° and
Galactic latitude |b| > 20°. Additional observations of the
Palomar objects in our sample have been observed as part of other
Chandra programmes, and these have also been included in our final
sample. Therefore, we analyse all publicly available Chandra X-ray
data up to June 2018, and now Chandra X-ray data exist for 213/280
objects (∼76 per cent) in the LeMMINGs sample. Next, as explained in
the section 3 Chandra data reduction, we proceed to properties
extraction for our galaxy sample. We performed standard reduction
procedures using the Chandra Interactive Analysis of Observations. We
extracted flux and luminosity from fits of X-ray spectra and from
images via photometry and spectroscopy Chandra softwares. Results are
synthesized in the table2.dat.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 94 280 Basic properties of our X-ray sample
table2.dat 91 213 Flux and luminosity measurements obtained from
Chandra X-ray spectral fitting
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See also:
J/ApJS/98/477 : Optical spectral atlas of Seyfert nuclei (Ho+ 1995)
J/ApJS/112/315 : Spectroscopic parameters of Seyfert nuclei (Ho+ 1997)
J/ApJS/183/1 : Catalog of central stellar velocity dispersions (Ho+, 2009)
J/MNRAS/500/4749 : LeMMINGs II e-MERLIN survey of nearby galaxies (Baldi+,2021)
J/ApJ/831/134 : BH masses & host galaxy dispersion vel. (van den Bosch,2016)
Chandra data : https://heasarc.gsfc.nasa.gov/db-perl/W3Browse/w3browse.pl
Chandra observation home page : http://cxc.harvard.edu/ciao/
NED extragalactic database : https://ned.ipac.caltech.edu/
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Galaxy name (Galaxy)
10- 16 F7.3 deg RAdeg Right ascension (J2000) (RA)
18- 22 F5.2 deg DEdeg Declination (J2000) (Dec)
24- 29 F6.2 deg GLAT Galactic latitude δ (GalLat)
31- 35 F5.1 Mpc D Distance of the galaxy (Dist) (1)
37- 41 I5 --- ID ? Chandra observation ID (ObsID)
43- 48 I6 s ExpTime ? The exposure length (Exposure)
50- 52 A3 --- f_ID [C C+Y] Flag indicates if this Chandra
observation is new or not (Sample) (2)
54- 61 A8 --- Sig The detection significance (Sig) (3)
63 A1 --- l_logMBH Upper limit flag of logMBH
65- 68 F4.2 [Msun] logMBH ? A black hole mass measurement taken from
the literature where possible (Mass) (4)
70- 73 F4.2 [Msun] e_logMBH ? Mean error on logMBH (errMass)
75 A1 --- l_logL[OIII] Upper limit flag of logL[OIII]
77- 81 F5.2 [10-7W] logL[OIII] ? Line luminosity of [O III] in erg/s
(O[III]) (5)
83- 89 A7 --- AGN The new AGN classification given to the
source based on the AGN re-classification
scheme (AGN) (6)
91- 94 A4 --- HType Hubble types simplified version
(Hubble) (7)
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Note (1): Distance in Mpc, which is obtained from
(Ho et al. 1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315, and references
therein).
Note (2): Flag for Chandra observations as follows:
C = If part of the 'Complete' sample described in section 2
Sample selection and chandra observations
Y = If this is a new Chandra observations obtained in observing
cycle 17 (programme ID 19708646 and 18620515, PI: McHardy)
C + Y = If part of the 'Complete' sample and a new Chandra
observation
Note (3): The detection significance where a source is observed or detected,
'Undet.' if the source is not detected in the observations or
'Not obs.' if there is no data in the Chandra archive.
Note (4): A black hole mass measurement taken from the literature where possible
(e.g. van den Bosch 2016ApJ...831..134V 2016ApJ...831..134V, Cat. J/ApJ/831/134), but
where no dynamical measurements exist, we use the M-σ
relationship of Tremaine et al. (2002ApJ...574..740T 2002ApJ...574..740T), using the
stellar velocity dispersions of (Ho et al. 1997ApJS..112..315H 1997ApJS..112..315H,
Cat. J/ApJS/112/315).
Note (5): A measurement of the [O III] line luminosity from
(Baldi et al. 2018MNRAS.476.3478B 2018MNRAS.476.3478B) or Baldi et al.
(2021MNRAS.500.4749B 2021MNRAS.500.4749B, Cat. J/MNRAS/500/4749), taken from the
literature or (Ho et al. 1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315).
Note (6): AGN re-classification scheme described in Baldi et al.
(2018MNRAS.476.3478B 2018MNRAS.476.3478B) and Baldi et al. (2021MNRAS.500.4749B 2021MNRAS.500.4749B,
Cat. J/MNRAS/500/4749) as follows:
ALG = 'Inactive' galaxies like absorption line galaxies ALG, 28
objects in our sample
HII = 'Inactive' galaxies like H II galaxies, 141 objects in our
sample
LINER = Low-ionization nuclear emission-line region LINERs galaxies,
94 objects in our sample
Seyfert = Seyfert galaxies, 18 objects in our sample
Note (7): A simplified version of the Hubble types originally shown in Ho et al.
(1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315) as follows:
Ell. = Elliptical galaxies, 26 objects in our sample
Irr. = Irregular galaxies, 16 objects in our sample
Len. = Lenticular galaxies, 54 objects in our sample
Spi. = Spiral galaxies, 184 objects in our sample
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Galaxy name (Galaxy)
10- 16 F7.2 --- Sig ? The detection significance (Sig) (1)
18 A1 --- l_logFX1 Upper limit flag of logFX1
20- 25 F6.2 [mW/m2] logFX1 The logarithm of the flux in the 0.3-10.0 keV
band (logFlux0.3-10keV)
27- 30 F4.2 [mW/m2] e_logFX1 ? Mean 1σerror on logFX1
(errlogFlux0.3-10keV)
32 A1 --- l_logFX2 Upper limit flag of logFX2
34- 39 F6.2 [mW/m2] logFX2 ? The logarithm of the flux in the 0.3-2.0 keV
band (logFlux0.3-2keV)
41- 44 F4.2 [mW/m2] e_logFX2 ? Mean 1σerror on logFX2
(errlogFlux0.3-2keV)
46- 51 F6.2 [mW/m2] logFX3 ? The logarithm of the flux in
the 2.0-10.0 keV band (logFlux2-10keV)
53- 56 F4.2 [mW/m2] e_logFX3 ? Mean 1σerror on logFX3
(errlogFlux2-10keV)
58- 62 F5.2 [10-7W] logLX1 The logarithm of the X-ray luminosity in the
0.3-10.0 keV band (logLum0.3-10keV)
64- 67 F4.2 [10-7W] e_logLX1 ? Mean 1σerror on logLX1
(errlogLum0.3-10keV)
69 A1 --- l_logLX2 Upper limit flag of logLX2
71- 75 F5.2 [10-7W] logLX2 ? The logarithm of the X-ray luminosity in
the 0.3-2.0 keV band (logLum0.3-2keV)
77- 80 F4.2 [10-7W] e_logLX2 ? Mean 1σerror on logLX2
(errlogLum0.3-2keV)
82- 86 F5.2 [10-7W] logLX3 ? The logarithm of the X-ray luminosity in
the 2.0-10.0 keV band (logLum2-10keV)
88- 91 F4.2 [10-7W] e_logLX3 ? Mean 1σerror on logLX3
(errlogLum2-10keV)
--------------------------------------------------------------------------------
Note (1): Flux and luminosity are calculated using the cflux command in xspec
algorithm (i.e see section 3 Chandra data reduction).
The detection significance if detected, else a non detected source
where the flux and luminosity measurements given in the 0.3-10 keV
band are 3σ upper limits. For all three X-ray bands, if
undetected then the model-independent flux and luminosity upper
limits are given from the srcflux tools.
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 25-Nov-2024