Table 5: Nuclear X-ray absorbing column densities of extragalactic H2O maser galaxies*.
Source Typea Telescopeb Epochc $N_{\rm H}$ Referencesd
        (1023 cm-2)  
IC 10 X-1 C 2003.03.12 $\rm0.06^{+0.002}_{-0.0008}$ BB04
NGC 235A S2 R  $\cdots$  see Table 3 HEASARC
NGC 253 SBG B 1996.11.29 $\rm0.12_{-0.04}^{+0.03}$ Cap99b
    C 1999.12.16 $\rm 2.0^{+1.3}_{-0.9}$ Wea02
NGC 262 (Mrk 348) S2 A 1995 $\rm 1.60_{-0.10}^{+0.20}$ Ris02
IRAS F01063-8034e S2 X 2003.04.21 see Sect. 4.2  
NGC 449 (Mrk 1) S2 A 1996.08.06 see Table 3 TARTARUS
NGC 598 (M 33)   A 1993.07 $\rm0.016^{+0.002}_{-0.002}$ Tak94
  X-8 X 2000-2002 $\rm0.019^{+0.005}_{-0.005}$ Fos04
NGC 591 S2 A 1997.07.28 see Table 3 TARTARUS
NGC 613 S R  $\cdots$  see Table 3 HEASARC
IC 184 S2 R  $\cdots$  see Table 3 HEASARC
NGC 1052 LINER A 1996.08 $\rm 2.0_{-0.83}^{+0.79}$ Ter02
    X 2001.08.15 $\sim $7 Kad06
NGC 1068 S2, C A 1993.07.24 >100 B99, Iwa97
    B 1996, 1998 >100 Mat97, Gua99
    C 2000.02.21 >100 Mat04
    X 2000.07.29 >100 Mat04
Mrk 1066 S2, C A 1997.07.24 >10 Ris99
NGC 1386 S2, C B 1996.12.10 >10 Mai98
    X 2002.12.29 $\geq$22 Gua05
IC 342   A 2000.02.24 $\rm0.084^{+0.042}_{-0.042}$ Kub02
  X-21 X 2001.02.11 $\rm0.087^{+0.013}_{-0.025}$ Kon03
UGC 3255 S2 R  $\cdots$  see Table 3 HEASARC
Mrk 3 S2, C A 1993 $\rm 13^{+22}_{-6}$ Tur97b
    B 1997.04.16 $\rm 12.7^{+2.4}_{-2.2}$ Cap99a, Matt00
    X 2000.10.19 $\rm 13.6^{+0.3}_{-0.4}$ Bia05
NGC 2146 SBG A 1997.03.26 $\rm0.021^{+0.022}_{-0.011}$ Del99
VII ZW 73 S2 R  $\cdots$  see Table 3 HEASARC
NGC 2273 S2, C B 1997.02.12 >100 Mai98
    X 2003.09.05 $\geq$18 Gua05
Mrk 78 S2 R  $\cdots$  see Table 3 HEASARC
Mrk 1210 S2, C? A 1995 >10 B99
    B 2001.05.05 $\rm 1.83^{+0.08}_{-0.12}$ Ohno04
    X 2001.05.05 $\rm 2.14^{+0.20}_{-0.16}$ Gua02b
J0804+3607 Type 2 Quasar R  $\cdots$  see Table 3 HEASARC
NGC 2639 LINER A 1997.04.16 $\rm 4.2^{+5.6}_{-2.3}$ B99, Wil98
NGC 2782e SBG, C C 2002.05.17 >10 this paper
NGC 2824 (Mrk 394) S2 R  $\cdots$  see Table 3 HEASARC
NGC 2960 (Mrk 1419) LINER R  $\cdots$  see Table 3 HEASARC
UGC 5101 ULIRG C 2001.05.28 0.1 (<0.65) Ptak03
    C,X 2001 $\rm 13^{+2}_{-2}$ Arm04
NGC 2979 S2 R  $\cdots$  see Table 3 HEASARC
NGC 3034 (M 82)f SBG B 1997.12.06 $\rm0.058^{+0.014}_{-0.015}$ Cap99b
    X 2001.05.06 $\rm0.017^{+0.018}_{-0.016}$ Ste03
    C 2002 0.012 Str04
NGC 3079 S2/LINER, C? A 1993.05.09 $\rm0.17^{+0.18}_{-0.12}$ B99, Ter02
    B 2000.05.26 $\sim $100 Iyo01
    C 2001.03.07 $\rm0.17^{+0.02}_{-0.02}$ Cec02
Mrk 34 S2 A 1997.11.17 see Table 3 TARTARUS
IC 2560 S2 A 1996.12.19 $\sim $3 Ish01
    C 2000.10.29 >10 Iwa02
    C 2004.02.16 $\ga$30 Mad06
NGC 3393 S2, C X 2003.01.05 $\rm 44^{+25}_{-11}$ Gua05
NGC 3556 X-35 C 2001.09.08 $\rm0.03^{+0.017}_{-0.009}$ Wang03
Arp 299 (NGC 3690) SBG, C X 2001.05.06 $\sim $26 Ball04
    C 2001.07.13 $\rm 25^{+4.4}_{-2.5}$ Zez03
    B 2001.12.14 $\rm 25.2^{+1.39}_{-0.56}$ Del02
NGC 3735 S2 R  $\cdots$  see Table 3 HEASARC
NGC 4051 S1/1.5 A 1993.04.25 $\rm0.045_{-0.035}^{+0.035}$ Geo98
    C 2000.04.25 $\sim $0.01 Col01
    X 2001.05.16 $\sim $3.6 Pou04
NGC 4151 S1.5 A 1993.12.07 $\rm0.635_{-0.035}^{+0.041}$ Geo98
    A,B 1999-2000 $\rm 2.0^{+0.1}_{-0.1}$ Sch02a
NGC 4258 S1.9 A 1999.05.15 $\rm0.95^{+0.21}_{-0.09}$ Rey00
    B 1998.12.19 $\rm 1.21^{+0.07}_{-0.06}$ Ris02
    C 2000-2001 $\sim $0.7 You04
    X 2000.12.08 $\rm0.80^{+0.04}_{-0.04}$ Pie02
    X,C 2000-2002 $\sim $1.0 Fru05
NGC 4293 LINER R  $\cdots$  see Table 3 HEASARC
NGC 4388 S2 A 1995.07.21 $\rm 3.34^{+1.00}_{-0.90}$ For99
    B 2000.01.03 $\rm 4.80^{+1.80}_{-0.80}$ Ris02
    X 2002.12.12 $\rm 2.79^{+0.07}_{-0.07}$ Bec04
    C 2001.06.08 $\rm 3.5^{+0.4}_{-0.3}$ Iwa03
ESO 269-G012e S2 C 2004.01.05 see Sect. 4.2  
NGC 4922 S2 C 2004.11.02 see Sect. 4.2  
NGC 4945 S2, C A 1993.08.31 $\rm 40^{+2.0}_{-1.2}$ B99, Don96
    B 1999.07.01 $\rm 22^{+3}_{-4}$ Gua00
NGC 5194 (M 51) S2, C A 1993.05.11 $\rm 7.5^{+2.5}_{-2.5}$ B99,Ter98
    B 2000.01.18 $\rm 56^{+40}_{-16}$ Fuk01
NGC 5256 (Mrk 266) S2 A 1999.05 $\rm0.16^{+0.33}_{-0.15}$ Lev01
NGC 5347 S2, C A 1997 >10 Ris99
NGC 5495 S2 R  $\cdots$  see Table 3 HEASARC
Circinus S2, C A 1995.08.14 >10 B99, Mat96
    B 1998.03.13 $\rm 43^{+4}_{-7}$ Mat99
    C 2000.06.06 $\sim $60 Sam01
NGC 5506 (Mrk1376) S1? B 1998.01.14 $\rm0.37^{+0.05}_{-0.05}$ Ris02
NGC 5643 S2, C B 1997.03.01 >100 Mai98, B99
    X 2003.02.08 6-10 Gua04
NGC 5728e S2 C 2003.05.27 $\rm 7.7^{+0.55}_{-0.51}$ this paper
NGC 5793 S2 A 1998.08.05 see Table 3 TARTARUS
NGC 6240 ULIRG, C A 1994.03.27 >20 Iwa98
    B 1998.08.15 $\rm 21.8^{+4.0}_{-2.7}$ Vig99
    X 2000.09.22 $\rm 10.0^{+3.0}_{-3.0}$ Bol03
    X 2001.07.29 $\rm 13.0^{+17.0}_{-8.0}$ Ptak03
NGC 6300 S2, C? RX 1997.02 >100 Lei99
    B 1999.08 $\rm 2.10^{+0.10}_{-0.10}$ Gua02a
    X 2001.03.02 $\rm 2.15^{+0.08}_{-0.09}$ Mats04
NGC 6323 S2 R  $\cdots$  see Table 3 HEASARC
ESO 103-G035 S2 A 1996.03.18 $\rm 2.16^{+0.26}_{-0.25}$ For99
    B 1997.10.14 $\rm 2.02^{+0.28}_{-0.28}$ Wil01
IRAS F19370-0131 S2 R  $\cdots$  see Table 3 HEASARC
3C 403 FRII C 2002.12.07 $\rm 4.00^{+0.20}_{-0.20}$ Kra05
NGC 6926 S2 R  $\cdots$  see Table 3 HEASARC
AM2158-380NED02 S2 R  $\cdots$  see Table 3 HEASARC
TXS 2226-184 LINER A 1997.11.21 see Table 3 TARTARUS
IC 1481 LINER A 1997.11.28 see Table 3 TARTARUS
* Chandra and XMM-Newton results are given whenever possible. For sources not observed by these satellites most recent (but usually older) results are quoted. Sources in italics: kilomaser sources.
a Type of nuclear activity. In the absence of a starburst and a prominent nuclear source, the X-ray source (e.g. X-1 or X-8) is given. SBG: StarBurst Galaxy; S2: Seyfert 2; LINER: Low-Ionization Nuclear Emission Line Region; ULIRG: UltraLuminous InfraRed Galaxy; FRII: Fanarov-Riley Type II galaxy; C: Compton-thick, i.e. $N_{\rm H}$ $\ga$ 10 $^{24}~{\rm cm}^{-2}$; C?: possibly varying between Compton-thick and Compton-thin.
b A: ASCA; B: BeppoSAX; C: Chandra; R: ROSAT; RX: RXTE; X: XMM-Newton.
c Year, month and day.
d Arm04: Armus et al. (2004); Ball04: Ballo et al. (2004); B99: Bassani et al. (1999); BB04: Bauer & Brandt (2004); Bec04: Beckmann et al. (2004); Bia03: Bianchi et al. (2003); Bia05: Bianchi et al. (2005); Bol03: Boller et al. (2003); Cap99a: Cappi et al. (1999); Cap99b: Cappi et al. (1999); Cec02: Cecil et al. (2002); Col01: Collinge et al. (2001); Del99: Della Ceca et al. (1999); Del02: Della Ceca et al. (2002); Don96: Done et al. (1996); For99: Forster et al. (1999); Fos04: Foschini et al. (2004); Fru05: Fruscione et al. (2005) Fuk01: Fukazawa et al. (2001); Geo98: George et al. (1998); Gua99: Guainazzi et al. (1999); Gua00: Guainazzi et al. (2000); Gua02a: Guainazzi (2002); Gua02b: Guainazzi et al. (2002); Gua04: Guainazzi et al. (2004b); Gua05: Guainazzi et al. (2005a); Ish01: Ishihara et al. (2001); Iwa97: Iwasawa et al. (1997); Iwa98: Iwasawa & Comastri (1998); Iwa02: Iwasawa et al. (2002); Iwa03: Iwasawa et al. (2003); Iyo01: Iyomoto et al. (2001); Kad06: Kadler et al. (2006), in prep.; Kon03: Kong (2003); Kra05: Kraft et al. (2005); Kub02: Kubota et al. (2002); Lei99: Leighly et al. (1999); Lev01: Levenson et al. (2001); Mad06: Madejski et al. (2006); Mai98: Maiolino et al. (1998); Mat96: Matt et al. (1996); Mat97: Matt et al. (1997); Mat99: Matt et al. (1999); Mat00: Matt et al. (2000); Mat04: Matt et al. (2004); Mats04: Matsumoto et al. (2004); Mil90: Miller & Goodrich (1990); Ohno04: Ohno et al. (2004); Per98: Persic et al. (1998); Pie02: Pietsch et al. (2002); Pou04: Pounds et al. (2004); Ptak03: Ptak et al. (2003); Rey00: Reynolds et al. (2000); Ris99: Risaliti et al. (1999); Ris02: Risaliti et al. (2002); Sam01: Sambruna et al. (2001); Sch02a: Schurch et al. (2002a); Sch02b: Schurch et al. (2002b); Smi96: Smith & Done (1996); Ste03: Stevens et al. (2003); Str04: Strickland et al. (2004); Tak94: Takano et al. (1994) Ter98: Terashima et al. (1998); Ter02: Terashima et al. (2002); Tur97a: Turner et al. (1997a); Tur97b: Turner et al. (1997b); Vig99: Vignati et al. (1999); Wang03: Wang et al. (2003); Wea02: Weaver et al. (2002); Wil01: Wilkes et al. (2001); Wil98: Wilson et al. (1998); You04: Young & Wilson (2004); Zez03: Zezas et al. (2003).
e Absorbing column densities were obtained by processing XMM-Newton and Chandra Archive data (see Sect. 4.2).
f For NGC 3034 (M 82), lacking a well defined nucleus, the Chandra data refer to the diffuse halo component.


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