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Table A.4

As Table A.2, for the foreground clouds.

Source V LSR ΔV 1113 GHz 1669 GHz N(H2O) o/p

IRAS 16272 –41.38(8) 1.67(3) –2.16 >6.33 >35 >5.9
–38.80(23) 1.94(5) –1.36 –2.50 15 3.7
NGC6334I(N) +6.86(13) 1.49(12) –1.52 >5.12 >27 >6.6
W43 MM1 +62.1(6) 1.04(8) –0.094 –0.11 0.73 2.4
+67.21(4) 1.81(8) –1.13 –1.80 11 3.2
+70.96(8) 1.6(2) –0.73 –1.15 7.1 3.2
+77.(7) 4.1(6) –1.63 –1.11 9.0 1.4
+79.7(1) 1.93(5) –1.48 –3.67 21 5.0
+82.4(2) 2.49(5) –1.63 –2.58 16 3.2
+87.83(12) 2.1(4) –0.20 –0.49 2.75 4.9
DR21(OH) +14.9(1) 1.5(2) –0.35 –0.90 5.0 5.1
+12.3(1) 1.8(2) –0.47 –2.03 11 8.6
+10.0(1) 1.7(7) –0.51 –2.53 13 9.9
+8.4(4) 1.9(2) –3.78 –0.80 13 0.4
+6.9(1) 1.22(1) –0.51 –0.38 3.0 1.5
W3 IRS5 –20.8(1) 1.04(8) –0.61 >3.56 >18 >12
IRAS 18089 +17.6(1) 3.4(6) –2.81 –7.24 40.3 5.2
+19.7(3) 2.8(11) –0.91 –2.34 13.0 5.1
+21.1(1) 2.2(4) –0.95 –1.42 8.8 3.0
+23.9(2) 1.9(1) –0.82 –2.68 14.4 6.5
+25.7(2) 2.67(7) –1.46 –4.00 22.0 5.5
W33A +24.01(7) 1.5(1) –0.66 –1.26 7.4 3.8
IRAS 18151 +27.7(2) 0.7(2) –0.36 –1.06 5.8 5.9
AFGL 2591 –0.67(13) 3.0(6) >9.54 >7.63 >58 ~1.6
+13a
G327–0.6d –38.02(4) 1.18(33) –0.06 –0.19 1.1 6.0
NGC 6334I +0.48(11) 2.58(52) –1.45 –3.42 13.8 2.7
+6.63(17) 1.61(16) –2.11 >5.63 >31.2 >5.3
+8.72(39) 1.27(52) –0.20 –0.17 1.3 1.7
G29.96 +103.5(1) 1.7(1) –1.09 –2.91 16 5.3
+91.6(2) 3.4(5) –0.67 –0.59 4.3 1.8
G31.41 +83.0(3) 3.4(6) –0.48 –1.27 7.0 5.3
G5.89 +19.85(1) 4.4(6) –1.90 –25.17b 121.7b 26.5b
G10.47 +42.3(1) 1.1(3) –0.16 –0.24 1.5 3.0
+47.06(4) 1.35(7) –0.09 –0.19 1.1 4.5
+84.9(1) 2.6(10) –0.19 –1.67b 8.2b 17.7b
+91.21(6) 1.4(4) –0.08 –0.32 1.7 8.3
G34.26 +11.4(1) 2.6(1) –6.43 –14.0 80 4.4
+14.26(3) 1.18(1) –0.35 –0.55 3.4 3.1
+27.09(1) 1.6(3) –1.52 –5.48 29 7.2
W51e +48.66(1) 2.27(1) –0.42 –1.14 6.3 5.4
+45.57(9) 1.2(1) –2.51 >4.42 >26 >3.5
+12.7c
+6.48(5) 2.4(2) –2.63 –2.99 20 2.3
+4.87(1) 1.1(2) –0.27 –0.84 4.5 6.2

Notes.The last two columns list the derived H2O column density (in 1012 cm-2) and ortho/para ratio.

(a)

Blended with H2O 1661 GHz line emission from other sideband; see Choi et al. (in prep.).

(b)

Highly uncertain because 1669 GHz line is saturated.

(c)

Only detected at 1113 GHz.

(d)

WBS spectra of this source show spatially extended H2O foreground absorbers between –20 and –3 km s-1 (Leurini, priv. comm.).

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