Table 4: Extragalactic H2O masers beyond the magellanic clouds.
Source RA Dec $V_{\rm sys}$ D log  $L_{\rm FIR}^{a}$ $T_{\rm dust}^{a}$ log  $L_{\rm H_2O}^{a}$ Ref.b
  (J2000) (cz) (Mpc) (log $L_{\odot}$) (K) (log $L_{\odot}$)  
IC 10 00 20 17.9 +59 18 31 -350 1.2 8.2 40 -1.7 1
  00 20 27.0 +59 17 29         -0.8 2, 3
NGC 253 00 47 33.1 -25 17 17 240 3.0 10.3 52 -0.8 4, 5
  00 47 33.6 -25 17 14         -1.7 5
NGC 262 (Mrk348) 00 48 47.1 +31 57 25 4505 62.0 10.6 42 2.6 6, 7
IRAS F0106-8034 01 07 00.9 -80 18 24 5045 67.0 10.7 32 2.7 8
NGC 449 (Mrk 1) 01 16 07.2 +33 05 22 4780 64.0 10.6 55 1.7 9
NGC 598 (M 33) 01 33 16.5 +30 52 50 -180 0.7 9.0 36 -0.5 10, 11
  01 33 29.4 +30 31 55         -1.5 12
NGC 591 (Mrk 1157) 01 33 31.2 +35 40 06 4555 61.0 10.5 46 1.4 13
NGC 1052 02 41 04.8 -08 15 21 1470 17.0 9.1 54 2.1 9, 14
NGC 1068 02 42 40.7 -00 00 48 1135 14.5 11.2 54 2.2 15, 16
Mrk 1066 02 59 58.6 +36 49 14 3600 48.0 10.9 55 1.5 13, 17
NGC 1386 03 36 46.4 -36 00 02 870 17.0 9.8 46 2.1 18
IC 342$^{\rm c)}$ 03 46 46.3 +68 05 46 40 2.0 9.0 49 -2.0 19
UGC 3255 05 09 50.2 +07 29 00 5675 75.0 10.5 40 1.2 13
Mrk 3 06 15 36.3 +71 02 15 4010 54.0 10.7 69 1.0 13
NGC 2146 06 18 36.6 +78 21 28 900 14.5 10.9 53 0.0 20
  06 18 38.6 +78 21 24         0.0 20
Mrk 78 07 42 41.7 +65 10 37 11195 150.0 11.0 60 1.5 13
Mrk 1210 08 04 05.8 +05 06 50 4045 54.0 10.5 75 1.9 9
NGC 2639 08 43 38.1 +50 12 20 3335 44.0 10.4 34 1.4 9, 21
NGC 2782 09 14 05.1 +40 06 49 2560 34.0 10.5 47 1.1 13
NGC 2824 (Mrk 394) 09 19 02.2 +26 16 12 2760 37.0 9.7 47 2.7 22
NGC 2960 (Mrk 1419) 09 40 36.4 +03 34 37 4930 66.0 10.5 38 2.6 23
NGC 2979 09 43 08.5 -10 23 01 2720 36.0 9.9 38 2.1 22
NGC 3034 (M 82) 09 55 52.2 +69 40 47 200 3.7 10.6 65 0.0 15, 24
NGC 3079 10 01 57.8 +55 40 47 1120 15.5 10.6 42 2.7 25, 26, 27
IC 2560 10 16 18.7 -33 33 50 2925 35.0 10.2 47 2.0 18, 28
Mrk 34 10 34 08.6 +60 01 52 15140 205.0 11.2 55 3.0 17
NGC 3556 11 11 31.2 +55 40 25 700 12.0 10.5 38 0.0 17
Arp 299 (Mrk 171) 11 28 32.2 +58 33 44 3120 42.0 11.7 61 2.1 17
NGC 3735 11 35 57.3 +70 32 09 2695 36.0 10.6 38 1.3 29
NGC 4051 12 03 09.6 +44 31 53 730 10.0 9.6 38 0.3 30
NGC 4151 12 10 32.6 +39 24 21 1000 13.5  $\cdots$   $\cdots$  -0.2 13
NGC 4258 12 18 57.5 +47 18 14 450 7.2 9.9 33 1.9 15, 31
NGC 4388 12 25 46.7 +12 39 44 2520 34.0 10.7 47 1.1 13
ESO 269-G012 12 56 40.7 -46 55 31 4950 66.0  $\cdots$   $\cdots$  3.0 22
NGC 4922 13 01 25.2 +29 18 50 7080 95.0 11.2 61 2.3 13
NGC 4945 13 05 27.5 -49 28 06 560 4.0 10.3 45 1.7 32, 33
NGC 5194 (M 51) 13 29 52.7 +47 11 43 450 10.0 10.3 33 -0.2 4, 34
NGC 5256 (Mrk 266) 13 38 17.2 +48 16 32 8365 112.0 11.5 46 1.5 13
NGC 5347 13 53 17.8 +33 29 27 2335 31.0 9.9 44 1.5 18
Circinus 14 13 09.3 -65 20 21 450 4.0 10.1 54 1.3 35, 36
NGC 5506 (Mrk 1376) 14 13 14.8 -03 12 27 1850 25.0 10.3 59 1.7 9
NGC 5643 14 32 40.7 -44 10 28 1200 16.0 10.3 39 1.4 22
NGC 5728 14 42 23.9 -17 15 11 2795 37.0 10.6 45 1.9 13
NGC 5793 14 59 24.7 -16 41 36 3490 47.0 10.6 47 2.0 37, 38
NGC 6240 16 52 58.1 +02 23 50 7340 98.0 11.8 58 1.6 39, 40, 41, 42
NGC 6300 17 17 00.3 -62 49 15 1110 15.0 10.2 36 0.5 22
NGC 6323 17 13 18.0 +43 46 56 7790 104.0  $\cdots$   $\cdots$  2.7 13
ESO103-G035 18 38 20.3 -65 25 42 3985 53.0 10.5 121 2.6 18
IRAS F19370-0131 19 39 38.9 -01 24 33 6000 80.0 10.7 59 2.2 22
3C403 19 52 15.8 +02 30 24 17690 235.0 11.2  $\cdots$  3.3 43
NGC 6926 20 31 38.7 -80 49 58 5970 80.0 11.1 39 2.7 22
TXS2226-184 22 29 12.5 -18 10 47 7495 100.0  $\cdots$   $\cdots$  3.8 44
IC 1481 23 19 25.1 +05 54 21 6120 82.0 10.4 65 2.5 18
a For the determination of $L_{\rm FIR}$ and $T_{\rm dust}$ (60/100 $\mu$m color temperatures), see Wouterloot & Walmsley (1986). The IRAS fluxes were taken from Fullmer & Lonsdale (1989) and, for a few sources (NGC 598, NGC 4258, IRAS F19370-1031 and 3C 403), from NED. While, as already noted by HWB and Braatz et al. (1997), the derived dust temperatures are mostly well above 30 K and thus rather large, a correlation between $T_{\rm dust}$ and $L_{\rm H_2O}$ is not apparent.
b References: (1) Henkel et al. (1986); (2) Becker et al. (1993); (3) Argon et al. (1994); (4) Ho et al. (1987); (5) Henkel et al. (2004); (6) Falcke et al. (2000); (7) Peck et al. (2003); (8) Greenhill et al. (2002); (9) Braatz et al. (1994); (10) Churchwell et al. (1977); (11) Greenhill et al. (1993); (12) Huchtmeier et al. (1978); (13) Braatz et al. (2004); (14) Claussen et al. (1998); (15) Claussen et al. (1984); (16) Gallimore et al. (2001); (17) This paper; (18) Braatz et al. (1996); (19) Tarchi et al. (2002a); (20) Tarchi et al. (2002b); (21) Wilson et al. (1995); (22) Greenhill et al. (2003b); (23) Henkel et al. (2002); (24) Baudry & Brouillet (1996); (25) Henkel et al. (1984); (26) Haschick & Baan (1985); (27) Trotter et al. (1998); (28) Ishihara et al. (2001); (29) Greenhill et al. (1997a); (30) Hagiwara et al. (2003b); (31) Herrnstein et al. (1999); (32) Dos Santos & Lépine (1979); (33) Greenhill et al. (1997b); (34) Hagiwara et al. (2001b); (35) Gardner & Whiteoak (1982); (36) Greenhill et al. (2003a); (37) Hagiwara et al. (1997); (38) Hagiwara et al. (2001a); (39) Hagiwara et al. (2002); (40) Nakai et al. (2002); (41) Braatz et al. (2003); (42) Hagiwara et al. (2003a); (43) Tarchi et al. (2003); (44) Koekemoer et al. (1995).
c The maser luminosity refers to a brief flaring episode.

Source LaTeX | All tables | In the text

Article Contents
1 Introduction and sample selection
2 Observations
3 Results
4 Discussion
5 Conclusions
References
List of tables
List of figures