**Table 3:** Line parameters of newly detected masers.
Source	Adopted	Epoch	$\int{S{\rm d}V}^{a}$	$V_{\rm LSR,opt}^{a,b}$	$\Delta V_{1/2}^{a}$	Channel	rms	log $L_{\rm H_2O}^{d}$	Comments
	distance					width^c
	(Mpc)	(2002)	(mJy km s^-1)	(km s^-1)	(km s^-1)	(km s^-1)	(mJy)	( $L_{\odot}$ )
Mrk 1066	48	Mar. 07	$696\pm61$	$3547.2\pm1.4$	$38.7\pm04.6$	1.08	5.3	1.6	see Fig. 1
			$169\pm12$	$3635.9\pm0.1$	$2.1\pm00.2$	1.08	5.3	1.0	see Fig. 1
			$171\pm17$	$3635.9\pm0.1$	$1.9\pm00.2$	0.07	29.7	1.0	see Fig. 2
		Mar. 10	$822\pm59$	$3547.8\pm1.3$	$38.3\pm03.4$	1.08	5.6	1.6	see Fig. 1
			$193\pm13$	$3636.2\pm0.1$	$2.1\pm00.2$	1.08	5.6	1.0	see Fig. 1
			$157\pm16$	$3636.1\pm0.1$	$1.2\pm00.2$	0.07	34.9	0.9	see Fig. 2
		May 03	$566\pm16$	$3552.8\pm7.7$	$46.2\pm16.9$	1.08	15.0	1.5	see Fig. 1
			$166\pm33$	$3635.9\pm0.2$	$1.7\pm00.4$	1.08	15.0	0.9	see Fig. 1
		Sep. 27	$143\pm31$	$3635.2\pm0.2$	$2.0\pm00.5$	1.08	13.7	0.9	see Fig. 1
Mrk 34^e	205	Mar. 08	$\phantom{0}46\pm14 \phantom{0}$	$14661.2\pm0.4$	$2.1\pm00.8$	1.16	5.8	1.6	see Fig. 3
			$354\pm52 \phantom{0}$	$14837.6\pm2.3$	$31.9\pm05.3$	1.16	5.8	2.5	see Fig. 3
			$417\pm78 \phantom{0}$	$15771.7\pm8.7$	$88.2\pm16.2$	9.29	1.9	2.6	see Fig. 4
		Mar. 17	$335\pm57\phantom{0}$	$14840.5\pm2.9$	$36.5\pm07.8$	1.16	5.5	2.5	see Fig. 3
		May 07	$\phantom{0}77\pm24\phantom{0}$	$14674.9\pm0.8$	$5.0\pm01.9$	1.16	6.6	1.9	see Fig. 3
			$323\pm62 \phantom{0}$	$14838.7\pm2.9$	$31.2\pm07.6$	1.16	6.6	2.5	see Fig. 3
			$995\pm122$	$15754.9\pm8.0$	$130.4\pm18.4$	9.30	2.3	3.0	see Fig. 4
		May 09	$\phantom{0} 67\pm25 \phantom{0}$	$14658.2\pm0.8$	$4.7\pm02.2$	4.67	3.4	1.8	see Fig. 3
			$559\pm81 \phantom{0}$	$14837.4\pm3.1$	$43.9\pm08.2$	4.67	3.4	2.7	see Fig. 3
			$607\pm92 \phantom{0}$	$15787.2\pm9.6$	$115.5\pm19.9$	18.67	1.4	2.8	see Fig. 4
			$117\pm32 \phantom{0}$	$15738.2\pm1.1$	$6.9\pm03.0$	4.67	3.2	2.1	see Fig. 4
			$394\pm87 \phantom{0}$	$15803.1\pm4.2$	$47.8\pm15.0$	4.67	3.2	2.6	see Fig. 4
NGC 3556	12	Mar. 12	$505\pm72 \phantom{0}$	$738.5\pm1.1$	$15.1\pm2.2$	1.06	11.6	0.2	see Fig. 5
		Mar. 15	$\phantom{0} 99\pm29\phantom{0}$	$738.0\pm0.3$	$2.1\pm0.5$	1.06	10.1	-0.5	see Fig. 5
			$421\pm78 \phantom{0}$	$740.3\pm1.6$	$17.9\pm4.8$	1.06	10.1	0.1	see Fig. 5
		May 05	$229\pm35 \phantom{0}$	$737.2\pm0.4$	$4.8\pm0.8$	1.06	10.9	-0.1	see Fig. 5
		Sep. 27	$329\pm75 \phantom{0}$	$737.1\pm1.1$	$10.0\pm2.9$	4.21	6.5	0.0	see Fig. 5
Arp 299	42	Mar. 16	$6210\pm242$	$3101.8\pm05.1$	$260.2\pm11.5$	4.30	4.8	2.4	see Fig. 6

^a Obtained from Gaussian fits.
^b See the caption to Fig. 1.
^c Channel width of the spectra used for the Gaussian fits. Some of the spectra shown in Figs. 1-7 are smoothed.
^d $L_{\rm H_2O}$ /[ $L_{\odot}$ ] = 0.023 $\times$ $\int{S {\rm d}V}$ /[Jy km s^-1] $\times$ D²/[Mpc²].
^e To the observations of the high velocity feature (15787 km s^-1) from May 9: the first Gaussian fit refers to the smoothed profile shown in Fig. 4; the latter two component fit refers to the unsmoothed spectrum with a channel spacing of 4.7 km s^-1.

Source LaTeX | All tables | In the text

	1 Introduction and sample selection
	2 Observations
	3 Results
	4 Discussion
	5 Conclusions
	References