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Table 7

Regions associated with molecular or optical outflow observed in NH3.

Source Outflow Ref. TMBa N(NH3)b Ref. D Ref.
associated (K) (1014 cm-2) (pc)

M120.1+3.0-N (IRAS 00213+6530) CO 1 0.65 0.9 2 850 1
M120.1+3.0-S (IRAS 00259+6510) CO 1 0.57 0.7 2 850 1
L1287 CO 1 2.51 4.6 2 850 1
L1293 CO 1 1.06 1.1 2 850 1
L1448 IRS1 CO, HH 72, 70 0.3 0.3 4 350 3
L1448 IRS2 CO, HH 70 1.9 1.8 4 350 3
L1448 IRS3 CO, HH 23, 5 3.1 4.2 4 350 3
L1448 C CO, HH 23, 70 2.5 3.3 4 350 3
GL490 CO 6  ≤ 0.5  ≤ 0.6 7 900 8
L1455 IRS1 CO, HH 9, 70 1.9 1.0 4 350 3
L1455 IRS2 CO, HH 9, 70 2.5 1.6 4 350 3
L1489 CO, HH 10, 71 0.8 1.8 11 140 8
HH 156 HH 1  ≤ 0.2  ≤ 0.4 2 140 1
HH 159 CO, HH 1  ≤ 0.4  ≤ 0.8 2 160 1
HH 158 HH 1  ≤ 0.3  ≤ 0.6 2 160 1
HH 31 CO?, HH 1 0.56 0.7 2 160 1
L1524 (Haro 6–10) CO, HH 73, 14  ≤ 0.6  ≤ 1 4 140 13
L1551 IRS 5 CO, HH 15, 16 2.72 2.3 7 140 13
HL Tau CO, HH 17, 18  ≤ 1  ≤ 1 7 140 13
L1551 NE CO, HH 1 0.79 1.0 2 160 1
L1642 CO, HH 1  ≤ 0.1  ≤ 0.1 2 125 1
L1527 CO, HH 20, 74, 19 2.12 5.0 11 140 13
L1634 (IRAS 05173–0555) CO, HH 1 1.0 1.1 2 460 1
L1634 (IRS 7) CO, HH 83, 84 0.59 0.8 2 460 1
RNO 43 (IRAS 05295+1247) CO, HH 21, 22 0.40 0.4 2 400 24
HH 83 CO, HH 26, 25 0.46 0.4–0.5 85 470 13
HH 84 HH 25 0.3 0.5–1 85 470 13
HH 33/40 HH 27  ≤ 0.3  ≤ 0.5 28 470 13
HH 86/87/88 HH 25  ≤ 0.2  ≤ 0.1 85 470 13
HH 34 CO, HH 30, 29 1.3 1.1 4 480 31
L1641-N CO, HH 32, 69 2.2 2.8 85 480 33
HH 38-43 HH 27  ≤ 0.5  ≤ 0.5 4 480 31
Haro 4-255 FIR CO 72 2.2 2.1 4 480 31
L1641-S3(high velocity) CO 1 2.0 2.4 2 480 1
HH 68 HH 1  ≤ 0.3  ≤ 0.4 2 460 1
B35 CO 10 1.2 4.0 11 500 34
HH 26 IR CO, HH 36, 35 2.8 2.5 7 470 13
HH 25 MMS CO, HH 75, 35 2.4 2.1 7 470 13
NGC 2071 CO 37 2.44 2.5 7 500 8
HH 270 IRS HH 1 0.67 0.7 2 460 1
IRAS 05487+0255 CO 1 0.8 0.7 2 460 1
HH 111 CO, HH 1 0.56 0.5 2 460 1
Mon R2 CO 38 1.2 1.2 7 800 8
Mon R2-N CO 76 1.0 1.0 7 800 8
GGD 12-15 CO 39 1.52 2.0 7 1000 8
RMon CO, HH 40, 35  ≤ 0.5  ≤ 0.6 7 800 13
NGC 2264 (HH 14-4/5/6) HH 41  ≤ 1  ≤ 1 4 800 13
HH 120 CO, HH 43, 77, 42 1.8 2.5 44 400 45
L1709 CO 1  ≤ 0.4  ≤ 0.6 2 160 1
L43 CO 72 2.7 2.2 4 160 46
L100 CO 47 0.5 0.3–0.5 85 225 48
L483 CO 47 4.54 14 85 200 49
L588 CO, HH 1 1.3 4.1 2 310 1
R CrA (HH 100-IR) CO, HH 72, 50, 79 2.8 2.0 4 130 51
R CrA (IRS 7) CO, HH 72, 50, 78 1.6 1.8 4 130 51
L673 CO 52 2.1  ≥ 2.2 2, 85 300 3
CB 188 CO 1  ≤ 0.2  ≤ 0.4 2 300 1
HH 32a CO, HH 17, 35  ≤ 0.6  ≤ 0.7 4 300 13
L778 CO 10 1.8 6.3 11 250 8
B335 CO, HH 53, 54 1.2 7.9 11 250 13
L797 CO 1  ≤ 0.2  ≤ 0.4 2 700 1
IRAS 20050 CO 1 1.7 3.6 2 700 1
V1057 Cyg CO 1 0.3 0.2 2 700 1
L1228 CO, HH 55, 56 2.71 5.3 85 300 56
V1331 Cyg CO, HH 72, 80 0.5 2.3 4 700 57
L1172 CO 10 1.8 7.9 11 440 8
CB 232 CO 1 0.58 0.9 2 600 1
IC 1396 E CO 1 0.86 1.4 2 750 1
NGC 7129 CO, HH 58, 59 0.52 0.36 7 1000 13
HHL73 (IRAS 21429+4729) CO 60 1.66 3.2 85 900 61
HHL73 (IRAS 21432+4719) CO, HHL, HH 60, 61, 81 1.25 1.1 28 900 61
HHL73 (IRAS 21441+4722) CO 60 0.7  ≥ 0.9 85 900 61
L1165 CO, HH 1 0.35 0.9 2 750 1
S140N (IRAS 22178+6317) CO 32 0.88 1.4 28 900 63
S140N (Star 2) CO, HH 82, 62 1.2 1.9 28 900 63
L1221 CO, HH 1 2.5 3.9 2 200 1
L1251 (IRAS 22343+7501) CO, HH 64, 65 0.29 1.7 85 300 66
L1251 (IRAS 22376+7455) CO, HH 64, 67 1.71 3.1 85 300 66
L1262 CO 47 1.57  ≥ 4.9 85 200 68

Notes. Regions with distance  ≤ 1 kpc.

a

Main brightness temperature at the position of the suspected exciting source.

b

Lower limit of the beam-averaged column density at the position of the suspected exciting source.

References. (1) see Table 1; (2) this paper; (3) Herbig & Jones (1983); (4) Anglada et al. (1989); (5) Eiroa et al. (1994a); (6) Snell et al. (1984); (7) Torrelles et al. (1983); (8) Fukui et al. (1993); (9) Goldsmith et al. (1984); (10) Myers et al. (1988); (11) Benson & Myers (1989); (12) Strom et al. (1986); (13) Reipurth (1994); (14) Elias (1978); (15) Snell et al. (1980); (16) Mundt & Fried (1983); (17) Edwards & Snell (1982); (18) Mundt et al. (1988); (19) Eiroa et al. (1994a); (20) Heyer et al. (1987); (21) Edwards & Snell (1984); (22) Jones et al. (1984); (23) Bachiller et al. (1990); (24) Maddalena & Morris (1987); (25) Reipurth (1989); (26) Bally et al. (1994); (27) Haro (1953); (28) Verdes-Montenegro et al. (1989); (29) Haro (1959); (30) Chernin & Masson (1995); (31) Genzel et al. (1981); (32) Fukui et al. (1986); (33) Chen et al. (1993); (34) Felli et al. (1992); (35) Herbig (1974); (36) Snell & Edwards (1982); (37) Bally (1982); (38) Loren (1981); (39) Rodríguez et al. (1982); (40) Cantó et al. (1981); (41) Adams et al. (1979); (42) Cohen & Schwartz (1987); (43) Olberg et al. (1989); (44) Persi et al. (1994); (45) Petterson (1984); (46) Chini (1981); (47) Parker et al. (1988); (48) Reipurth & Gee (1986); (49) Ladd et al. (1991a); (50) Strom et al. (1974); (51) Marraco & Rydgren (1981); (52) Armstrong & Winnewisser (1989); (53) Frerking & Langer (1982); (54) Vrba et al. (1986); (55) Haikala & Laureijs (1989); (56) Bally et al. (1995); (57) Chavarría-K (1981); (58) Loren (1977); (59) Ray et al. (1990); (60) Dobashi et al. (1993); (61) Gyulbudaghian et al. (1987); (62) Eiroa et al. (1993); (63) Crampton & Fisher (1974); (64) Sato & Fukui (1989); (65) Balázs et al. (1992); (66) Kun & Prusti (1993); (67) Eiroa et al. (1994b); (68) Parker et al. (1991); (69) Reipurth et al. (1998); (70) Bally et al. (1997); (71) Gómez et al. (1997); (72) Levreault (1985); (73) Hogerheijde et al. (1998); (74) Tamura et al. (1996); (75) Gibb & Davis (1998); (76) Tafalla et al. (1997); (77) Nielsen et al. (1998); (78) Anderson et al. (1997); (79) Whittet et al. (1996); (80) Mundt & Eislöffel (1998); (81) Devine, Reipurth & Bally (1997); (82) Davis et al. (1998); (83) Davis et al. (1997); (84) Hoddap & Ladd (1995); (85) Anglada et al. (1997).

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