J/A+A/641/A162 Water maser data of 380 galaxies (Panessa+, 2020)
Water megamaser emission in hard X-ray selected AGN.
Panessa F., Castangia P., Malizia A., Bassani L., Tarchi A., Bazzano A.,
Ubertini P.
<Astron. Astrophys. 641, A162 (2020)>
=2020A&A...641A.162P 2020A&A...641A.162P (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Masers ; X-ray sources
Keywords: galaxies: active - galaxies: Seyfert - masers - X-rays: galaxies -
gamma-rays: galaxies - surveys
Abstract:
Water megamaser emission at 22GHz has proven to be a powerful tool
for astrophysical studies of active galactic nuclei (AGN) because it
allows an accurate determination of the mass of the central black hole
and of the accretion disc geometry and dynamics. However, after
searches among thousands of galaxies, only ∼200 of them have shown
such spectroscopic features, most of them of uncertain classification.
In addition, the physical and geometrical conditions under which a
maser activates are still unknown.
We characterize the occurrence of water maser emission in an unbiased
sample of AGN by investigating the relation with the X-ray properties
and the possible favourable geometry that is required to detect water
maser.
We searched for 22GHz maser emission in a hard X-ray selected sample
of AGN, taken from the INTEGRAL/IBIS survey above 20keV. Only half of
the 380 sources in the sample have water maser data. We also
considered a volume-limited sub-sample of 87 sources, for which we
obtained new observations with the Green Bank and Effelsberg
telescopes (for 35 sources). We detected one new maser and increased
its radio coverage to 75%.
The detection rate of water maser emission in the total sample is
15±3%. This fraction increases to 19±5% for the complete
sub-sample, especially when we consider type 2 (22±5% and 31±10%
for the total and complete samples, respectively) and Compton-thick
AGN (56±18% and 50±35% for the total and complete samples,
respectively).
No correlation is found between water maser and X-ray luminosity. We
note that all types of masers (disc and jet) are associated with hard
X-ray selected AGN. These results demonstrate that the hard X--ray
selection may significantly enhance the maser detection efficiency
over comparably large optical or infrared surveys. A possible decline
in detection fraction with increasing luminosity might suggest that an
extremely luminous nuclear environment does not favour maser emission.
The large fraction of CT AGN with water maser emission could be
explained in terms of geometrical effects. The maser medium would then
be the very edge-on portion of the obscuring medium.
Description:
Table A1 lists all 380 INTEGRAL/IBIS AGN with their optical
coordinates, redshift, class, hard X-ray (20-100keV) flux, X-ray
(2-10keV) flux, X-ray column density, a note to indicate if the source
was observed or not at 22GHz, which maser type was detected and
relative references. Finally, for those sources for which maser
emission was detected, we also list the reported water maser isotropic
luminosity and the reference to the maser data; for objects observed
at 22GHz but not detected, the 1σ rms and an upper limit to the
maser luminosity are reported. Objects belonging to the complete
sample are marked with * for clarity.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 148 380 Water maser data of 380 galaxies detected by
INTEGRAL/IBIS
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See also:
J/ApJ/695/276 : Search for megamasers in type-2 AGNs (Bennert+, 2009)
J/MNRAS/426/1750 : INTEGRAL/IBIS AGN catalogue (Malizia+, 2012)
J/MNRAS/460/19 : Update of INTEGRAL/IBIS AGN catalogue (Malizia+, 2016)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 21 A21 --- Name Name of the source
22 A1 --- n_Name [*12] Note on Name (1)
24- 25 I2 h RAh Right Ascension (J2000) (2)
27- 28 I2 min RAm Right Ascension (J2000) (2)
30- 34 F5.2 s RAs Right Ascension (J2000) (2)
36 A1 --- DE- Declination sign (J2000) (2)
37- 38 I2 deg DEd Declination (J2000) (2)
40- 41 I2 arcmin DEm Declination (J2000) (2)
43- 46 F4.1 arcsec DEs Declination (J2000) (2)
48- 54 F7.5 --- z ? Redshift
56- 65 A10 --- Class Optical classification
68 A1 --- l_F20-100 Limit flag on F20-100
69- 74 F6.3 10-14W/m2 F20-100 20-100keV flux (3)
76 A1 --- l_F2-10 Limit flag on F2-10
77- 83 F7.4 10-14W/m2 F2-10 ? 2-10keV flux (3)
85- 93 A9 --- n_F2-10 Interval of 2-10keV flux when variable
95 A1 --- l_logNH Limit flag on NH
96-101 F6.3 [cm-2] logNH ? X-ray column density
103-111 A9 --- Notes Notes on the water maser (4)
112-113 I2 mJy rms ? 1 sigma rms in mJy (5)
115 A1 --- --- [(]
116-119 F4.2 km/s Channel ? Wide channel if not 0.3km/s for rms
120 A1 --- --- [)]
122 A1 --- l_L(H2O) Limit flag on L(H2O)
123-131 F9.4 Lsun L(H2O) ? Water maser isotropic luminosities (6)
132-136 F5.1 Lsun e_L(H2O) ? rms uncertainty on L(H20)
139-147 A9 --- Ref References for the rms (7)
148 A1 --- n_Ref [*] Note on Ref (8)
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Note (1): Note on Name as follows:
* = sources that belong to the complete AGN catalog reported in
Malizia et al. (2009MNRAS.399..944M 2009MNRAS.399..944M)
1 = 1 and 2 indicates two set of data for the same source,
from different references
2 = 1 and 2 indicates two set of data for the same source,
from different references
Note (2): The format on the relevant digits in the coordinates are those
originally reported (Malizia et al. 2012, Cat. J/MNRAS/426/1750,
Malizia et al. 2016, Cat. J/MNRAS/460/19).
Note (3): 2-10keV and 20-100keV flux in units of 10-11erg/cm2/s.
Note (4): Maser types as follows:
D = disc
J = jet
O = outflow
/ = or
+ = plus
For possible limits on this classification see Sect. 6.
References for the Maser type:
a = MCP at https://safe.nrao.edu/wiki/bin/view/Main/PublicWaterMaserList
(web page updated at November 10, 2018)
b = Henkel et al. (2005A&A...436...75H 2005A&A...436...75H)
c = Kamali et al. (2017A&A...605A..84K 2017A&A...605A..84K)
d = Kondratko et al. (2005ApJ...618..618K 2005ApJ...618..618K)
e = Tarchi et al. (2011A&A...532A.125T 2011A&A...532A.125T)
f = Humphreys et al. (2016A&A...592L..13H 2016A&A...592L..13H)
g = Ott et al. (2013ApJ...771L..41O 2013ApJ...771L..41O)
h = Greenhill et al (2003ApJ...590..162G 2003ApJ...590..162G)
i = Greenhill et al. (2009ApJ...707..787G 2009ApJ...707..787G)
j = Hagiwara et al. (2015ApJ...815..124H 2015ApJ...815..124H)
k = Sato et al. (2005PASJ...57..587S 2005PASJ...57..587S)
l = Wang et al. (2010RAA....10..915W 2010RAA....10..915W)
Note (5): 1 sigma rms in mJy, calculated over a 0.3km/s wide channel, unless
otherwise specified (different channel widths are reported in n_rms column)
Note (6): Water maser isotropic luminosities are in unit of L☉, where
L☉=3.826x1033erg/s. We calculate the upper limits for the undetected
sources using the formula:
L(H2O)[L☉]=0.023*S[Jy]*Δv[km/s]*D2[Mpc2], where S[Jy] and
Δv[km/s, are the 5σ rms and the channel spacing, respectively;
D is the distance in Mpc, derived using the redshift in column "z" and
H0=70km/s/Mpc.
Note (7): References for the rms (undetected sources) or the isotropic maser
luminosity (detected sources) as follows:
B96 = Braatz et al. (1996ApJS..106...51B 1996ApJS..106...51B)
B09 = Bennert et al. (2009ApJ...695..276B 2009ApJ...695..276B, Cat. J/ApJ/695/276) and
references therein
G96 = Gallimore et al. (1996ApJ...458..136G 1996ApJ...458..136G)
G02 = Greenhill et al. (2002ApJ...565..836G 2002ApJ...565..836G)
H84 = Henkel et al. (1984A&A...141L...1H 1984A&A...141L...1H)
K05 = Kameno et al. (2005ApJ...620..145K 2005ApJ...620..145K)
K06 = Kondratko et al. (2006ApJ...638..100K 2006ApJ...638..100K)
MCP = Megamaser Cosmology Project webpage
(https://safe.nrao.edu/wiki/bin/view/Main/MegamaserCosmologyProject)
O13 = Ott et al. (2013ApJ...771L..41O 2013ApJ...771L..41O)
P03 = Peck et al. (2003ApJ...590..149P 2003ApJ...590..149P)
P15 = Pesce et al. (2015ApJ...810...65P 2015ApJ...810...65P)
T03 = Tarchi et al. (2003A&A...407L..33T 2003A&A...407L..33T)
T11 = Tarchi et al. (2011A&A...532A.125T 2011A&A...532A.125T)
Note (8): *: the maser in IGRJ16385-2057 was detected during our survey
(Sect. 3.3), a detailed analysis have been reported in
Tarchi et al. 2011A&A...532A.125T 2011A&A...532A.125T.
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Acknowledgements:
Francesca Panessa, francesca.panessa(at)inaf.it
(End) Patricia Vannier [CDS] 03-Jul-2020