Notes on Individual HH Objects

HH 1/2 (5 33, -06 48)

Original papers: Herbig (1951), Haro (1952),(1953). These are among the brightest HH objects in the sky, and form bow shocks in a highly collimated bipolar outflow with dimension 2.5 arcmin (0.34 pc projected). A small jet originates from the embedded central source.

Optical Spectroscopic Studies: Herbig (1951), Böhm (1956), Osterbrock (1958), Haro & Minkowski (1960), Böhm, Perry, Schwartz (1973), Böhm, Siegmund, Schwartz (1976), Dopita (1978a), Schwartz (1978), Böhm & Brugel (1979), Brugel, Böhm, Mannery (1981a), Schwartz (1981), Dopita, Binette, Schwartz (1982), Hartmann & Raymond (1984), Böhm & Solf (1985), Cantó& Rodríguez (1986), Solf, Böhm, Raga (1988), Noriega-Crespo, Böhm, Raga (1989), Solf & Böhm (1991), Solf et al. (1991), Böhm & Solf (1992).

Studies of Blue Continua: Böhm, Schwartz, Siegmund (1974), Brugel, Böhm, Mannery (1981b), Dopita, Binette, Schwartz (1982), Solf, Böhm, Raga (1988).

Ultraviolet Spectroscopy: Ortolani & D'Odorico (1980), Böhm, Böhm-Vitense, Brugel (1981), Brugel, Shull, Seab (1982), Böhm-Vitense et al. (1982), Brugel et al. (1985), Böhm et al. (1987), Lee et al. (1988), Böhm, Raga, Binette (1991), Böhm, Noriega-Crespo, Solf (1993).

Structure and CCD Imaging: Strom et al. (1985a)(1986), Mundt, Brugel, Bührke (1987), Raga & Mateo (1988a), Raga et al. (1988), Schwartz et al. (1993), Reipurth et al. (1993b), Eislöffel, Mundt, Böhm (1994).

Variability of Knots: Herbig (1969) (1973), Schwartz (1976), Herbig & Jones (1981), Brugel et al. (1985), Raga, Barnes, Mateo (1990).

Infrared observations: Elias (1980), Harvey et al. (1986), Zinnecker et al. (1989), Zealey et al. (1992), Davis, Eislöffel, Ray (1994), Kelly, Rieke, Campbell (1994), Noriega-Crespo & Garnavich (1994).

Radio continuum studies: Pravdo et al. (1985), Curiel, Cantó, Rodríguez (1987), Rodríguez et al. (1990b).

Search for X-rays: Pravdo & Marshall (1981),Strom et al. (1990), Pravdo & Angelini (1993).

Polarization studies: Strom, Strom, Kinman (1974), Schmidt & Vrba (1975).

Energy Source:Pravdo et al. (1985), Rodríguez, Roth, Tapia (1985), Strom et al. (1985a), Harvey et al. (1986), Pravdo & Chester (1987), Tapia et al. (1987), Reipurth (1989b), Rodríguez et al. (1990b), Reipurth et al. (1993a) .

Studies of Jet: Strom et al. (1985a), Bohigas et al. (1985), Cohen & Fuller (1985), Schwartz, Cohen, Williams (1987), Mundt, Brugel, Bührke (1987), Roth et al. (1989), Reipurth et al. (1993b).

Proper Motions: Herbig & Jones (1981) ,Reipurth et al. (1993b), Eislöffel, Mundt, Böhm (1994).

Mm Studies: Loren, Evans, Knapp (1979), Edwards & Snell (1984), Torrelles et al. (1985b), Levreault (1988), Marcaide et al. (1988), Davis, Dent, Burnell (1990), Cernicharo (1990), Morgan et al. (1991), Torrelles et al. (1992b)(1993c)(1994), Chernin & Masson (1994).

Various model calculations: Hartmann & Raymond (1984), Choe, Böhm, Solf (1985), Hartigan, Raymond, Hartmann (1987), Raga et al. (1988), Hartigan (1989), Noriega-Crespo, Böhm, Raga (1989)(1990).

See also notes for HH 144 and HH 145.

HH 3 (5 33, -06 44)

Original papers: Herbig (1951), Haro (1952),(1953). Bright HH object with a jet-like protrusion (Ray 1987) and associated with a group of faint HH knots (Reipurth (1989b)). Associated with faint near-infrared object (Roth et al. 1989). No molecular outflow detected by Edwards & Snell (1984).

Optical spectroscopy: Dopita (1978a), Brugel, Böhm, Mannery (1981a).

HH 4 (3 26, +31 09)

Herbig (1974) notes that this is ``a faint nebulosity 7-8 arcsec in diameter with a sharp condensation or faint star on the west edge''. It is seen in the infrared images of Aspin, Sandell, Russell (1994).

HH 5 (3 26, +31 02)

Originally found by Herbig (1974). H_2 detection by Lane & Bally (1986). CCD image presented by Ray (1987). Astrometry and proper motion by Herbig & Jones (1983). Detailed optical/infrared imaging and spectroscopic study by Cohen, Jones, Hereld (1991). Low excitation object. It is seen in the infrared images of Aspin, Sandell, Russell (1994).

HH 6 (3 26, +31 08)

Originally found by Herbig (1974). H_2 detection by Lane & Bally (1986) and Schwartz, Cohen, Williams (1987). Detailed optical/infrared imaging and spectroscopic study by Cohen, Jones, Hereld (1991). Low excitation object. A weak VLA 6 cm continuum source is found nearby (Snell & Bally 1986) as well as an H_2O maser source (Henkel, Haschick, Güsten 1986). Energy source of 33 L_sun detected at 50 and 100 µm in IRAS CPC observations (Jennings et al. (1987)). The HH object is seen in the infrared images of Aspin, Sandell, Russell (1994).

HH 7-11 (3 26, +31 05)

This is a chain of bright HH knots about 1 arcmin long, first discussed by Herbig (1974) and Strom, Grasdalen, Strom (1974).

CCD Imaging: Strom et al. (1986), Solf & Böhm (1987), Raga & Mateo (1988a), Hartigan, Curiel, Raymond (1989), Aspin, Sandell, Russell (1994).

Optical Spectroscopy: Strom, Grasdalen Strom (1974), Böhm, Brugel, Mannery (1980), Cohen & Schmidt (1981), Böhm, Brugel, Olmsted (1983), Goodrich (1986a), Solf & Böhm (1987), Böhm & Solf (1990).

Infrared Observations: Simon & Joyce (1983), Zealey, Williams, Sandell (1984), Lightfoot & Glencross (1986), Cohen et al. (1988), Zinnecker et al. (1989), Burton et al. (1989), Hartigan, Curiel, Raymond (1989), Garden, Russell, Burton (1990), Stapelfeldt et al. (1991), Carr (1993), Aspin, Sandell, Russell (1994).

Ultraviolet Observations: Cameron & Liseau (1990).

Proper Motions: Herbig & Jones (1983).

Radio Observations: Lada et al. (1974), Ho & Barrett (1980), Snell & Edwards (1981), Liseau et al. (1988) , Rudolph & Welch (1988) , Lizano et al. (1988), Koo (1990) , Masson, Mundy, Keene (1990), Rodríguez et al. (1990a) , Bachiller & Cernicharo (1990), Giovanardi et al. (1992), Dent et al. (1993).

Source: Strom, Vrba, Strom (1976), Cohen & Schwartz (1983), Cohen et al. (1984a), Hodapp (1984), Snell & Bally (1986), Goodrich (1986), Cohen & Schwartz (1987), Grossman et al. (1987), Jennings et al. (1987), Sandell et al. (1990 ), Eislöffel et al. (1991), Carr & Tokunaga (1992), Liseau, Lorenzetti, Molinari (1992) , Molinari, Liseau, Lorenzetti (1993), Reipurth et al. (1993a), Aspin & Sandell (1994).

Magnetic Field Direction: Heyer, Strom, Strom (1987).

H_2O Masers: Dickinson, Kojoian, Strom (1974), Lo et al. (1976), Haschick et al. (1980), Haschick, Moran, Rodríguez (1980).

Distance: Herbig & Jones (1983), Cernis (1990) and references therein; a distance of 220 pc is adopted here.

HH 12 (3 25, +31 09)

Originally found by Herbig (1974).

CCD Imaging: Strom, Strom, Stocke (1983), Strom et al. (1986), Stapelfeldt et al. (1991), Aspin, Sandell, Russell (1994).

Spectroscopy: Strom, Grasdalen, Strom (1974), Strom, Strom, Stocke (1983), Cohen & Jones (1987).

IR Observations: Simon & Joyce (1983) ,Lane & Bally (1986), Schwartz, Cohen, Williams (1987), Garden, Russell, Burton (1990), Stapelfeldt et al. (1991), Aspin, Sandell, Russell (1994).

Mm Observations: Ho & Barrett (1980), Edwards & Snell (1983).

Magnetic Field Direction: Heyer, Strom, Strom (1987).

Source: The source has not been unequivocally identified, but there are two candidates, star 107 proposed by Strom, Strom, Stocke (1983), and SVS 12 (Strom, Vrba, Strom (1976) , Cohen & Schwartz (1987), Jennings et al. (1987), Stapelfeldt et al. (1991), Molinari, Liseau, Lorenzetti (1993)); the latter appears the more likely.

HH 13 (3 25, +30 56)

Herbig (1974) describes this as ``a very faint smudge of uncertain type''.

HH 14 (3 25, +30 50)

Herbig (1974) notes that this is ``a group of about 6 nebulous spots distributed over an area of about 20 x 60 arcsec.'' Cohen & Schwartz (1987) draw attention to the nearby IRAS source 03254+3050 as a candidate energy source.

HH 15 (3 25, +30 57)

Herbig (1974) writes that this is ``only a very faint wisp about 3 x 10 arcsec.'' Cohen & Schwartz (1987) suggest IRAS 03256+3055 could be a possible energy source.

HH 16 (3 26, +30 58)

Herbig (1974) describes this as ``a faint elongated smudge about 3 x 7 arcsec.'' Cohen & Schwartz (1987) suggest IRAS 03256+3055 could be a possible energy source.

HH 17 (3 26, +31 08)

Herbig (1974) writes that this is ``a very faint nebulosity 5 to 10 arcsec across, with a sharp condensation or star at the northern edge''. An infrared source (SVS 5 = ASR 112) was detected by Strom, Vrba, Strom (1976) and Aspin, Sandell, Russell (1994).

HH 18 (3 26, +30 57)

Herbig (1974) notes that this is ``a group of at least 5 faint nebulous spots distributed over an area of about 20 x 35 arcsec.''

HH 19 (5 43, -00 06)

Original paper: Herbig (1974). CCD images presented by Mundt et al. (1984) and Strom et al. (1986). Spectroscopy by Jones et al. (1987) and Mundt, Brugel, Bührke (1987) . Proper motions by Jones et al. (1987) suggest an origin near SSV 63 and HH 24. Infrared H_2 spectroscopy by Zinnecker et al. (1989). Infrared imaging by Zealey et al. (1992).

HH 20/21 (5 43, -00 05)

Original paper: Herbig (1974). These objects form a loose group of HH knots together with HH 70 (Reipurth & Graham (1988)) and HH 37 of Strom et al. (1986); both papers present CCD images. Located near HH 19. The proper motion study by Jones et al. (1987) suggests HH 20 originates near SSV 63 and HH 24. HH 20 was observed spectroscopically by Jones et al. (1987).

HH 22/23 (5 43, -00 05)

Original paper: Herbig (1974). Two faint knots. Jones et al. (1987) attempted to measure the proper motion of HH 23.

HH 24 (5 43, -00 11)

Originally discovered by Herbig & Kuhi (1963). This is a very complex region with at least two and perhaps three outflows. For an overview of the region, source locations and nomenclature of knots see Figs. 17 and 19 of Mundt, Ray, Raga (1984).

Structure and CCD Images: Strom et al. (1986), Jones et al. (1987), Mundt, Ray, Raga (1984).

Optical Spectroscopy: Strom, Grasdalen, Strom (1974), Dopita (1978a), Schmidt & Miller (1979), Brugel, Böhm, Mannery (1981a),(1981b), Solf (1987).

Ultraviolet Spectroscopy: Lee et al. (1988), Böhm et al. (1992).

Infrared Observations: Zealey et al. (1992).

Proper Motions: Jones et al. (1987).

Polarization Measurements: Strom, Grasdalen, Strom (1974), Strom, Strom, Kinman (1974) , Schmidt & Miller (1979), Scarrott, Gledhill, Warren-Smith (1987).

Source(s): Strom, Grasdalen, Strom (1974), Strom, Strom, Vrba (1976a) , Cohen & Schwartz (1983), (1987), Cohen et al. (1984a), Bieging, Cohen, Schwartz (1984), Cohen, Dopita, Schwartz (1986b), Lane (1989), Zealey et al. (1989), (1992), Reipurth et al. (1993a) , Molinari, Liseau, Lorenzetti (1993).

Radio Observations: Lada et al.(1974), Snell & Edwards (1982), Wootten et al. (1982), Matthews & Little (1983), Torrelles et al. (1983a), Edwards & Snell (1984), Little et al. (1985), Torrelles et al. (1989), Pastor et al. (1991), Lada et al. (1991), Gibb & Heaton (1993), Harju, Walmsley, Wouterloot (1993).

HH 25/26 (5 43, -00 15)

Original paper: Herbig (1974). The comment by Cohen & Schwartz (1987) that HH 25 is not an emission nebula is incorrect (e.g. Jones et al. 1987). Structure and CCD images discussed by Strom et al. (1986) and Jones et al. (1987). Optical spectroscopy presented by Jones et al. (1987). A 2.0 - 2.5 µm spectrum of HH 26 is given by Schwartz, Cohen, Williams (1987). An embedded near-infrared source, SSV 59 (= IRAS 05435-0015), is located between HH 25 and 26, and is a likely energy source (Strom, Strom, Vrba 1976a, Cohen & Schwartz (1983), Cohen et al. 1984a). The region is very complex at mm wavelengths (see Gibb & Heaton 1993 for summary, and references to radio observations under HH 24).

HH 27 (5 43, -00 14)

Original paper: Herbig (1974). Structure and CCD images discussed by Strom et al. (1986) and Jones et al. (1987). Optical spectroscopy presented by Jones et al. (1987). H_2 detected by Schwartz, Cohen, Williams (1987). Mm observations summarized by Gibb & Heaton (1993), see also notes under HH 24.

HH 28/29 (4 28, +17 58)

Original paper: Herbig (1974). These are two rather bright objects, which form bow shocks in the large outflow from L1551 IRS 5 starting in the HH 154 jet. CCD images are presented by Snell et al. (1985), Strom et al. (1986), Stocke et al. (1988), Graham & Heyer (1990), Garnavich, Noriega-Crespo, Green (1992) and Fridlund, Liseau, Perryman (1993). Optical spectroscopy is discussed by Strom, Grasdalen, Strom (1974) and Stocke et al. (1988) . Ultraviolet spectroscopy of HH 29 is presented by Cameron & Liseau (1990). The objects have large proper motions in a direction away from IRS 5 (Cudworth & Herbig (1979)). The molecular outflow from IRS 5 has an abrupt velocity change at HH 29. (Fridlund et al. 1984). For references on the molecular outflow and the source, see notes on the HH 154 jet.

HH 30 (4 28, +18 06)

Original paper: Herbig (1974).

Structure and CCD Images: Mundt & Fried (1983), Cohen & Jones (1987), Mundt, Ray, Bührke (1988) , Mundt et al. (1990), Graham & Heyer (1990), Mundt, Ray, Raga (1991).

Optical Spectroscopy: Brugel, Böhm, Mannery (1981a), Cohen & Schmidt (1981), Mundt, Brugel, Bührke (1987) , Cohen & Jones (1987), Mundt et al. (1990).

Proper Motions: Cudworth & Herbig (1979), Mundt et al. (1990).

Source: Cohen & Schwartz (1981), Vrba, Rydgren, Zak (1985), Cohen & Schwartz (1987).

Mm Data: Calvet, Cantó, Rodríguez (1983).

HH 31 (4 25, +26 11)

Original paper: Herbig (1974). CCD images are discussed by Strom et al. (1986). A likely energy source, HH 31 IRS 2 (IRAS 04248+2612) was found by Cohen & Schwartz (1983), and further studied by Cohen et al. (1984a), Cohen, Harvey, Schwartz (1985) and Cohen & Schwartz (1987). A spectrum of a little nebula at the location of the source (identified as knot D by Herbig (1974) by Cohen & Fuller (1985) showed little emission, but Strom et al. (1986) found a southern emission line extension. Limited ¹²CO data of Edwards & Snell (1983) revealed no high-velocity gas.

HH 32 (19 18, +10 56)

Original paper: Herbig (1974).

CCD Images: Mundt, Stocke, Stockman (1983), Hartigan, Mundt, Stocke (1986).

Optical Spectroscopy: Dopita (1978a), Brugel, Böhm, Mannery (1981a),(1981b), Herbig & Jones (1983), Solf, Böhm, Raga (1986), Hartigan, Mundt, Stocke (1986).

UV Spectroscopy: Böhm & Böhm-Vitense (1984) , Lee et al. (1988).

IR Observations: Zealey et al. (1986) , Zinnecker et al. (1989).

Radio Continuum Emission: Anglada et al. (1992).

Proper Motions: Herbig & Jones (1983).

Source: AS353A (=V1352 Aql) was discovered by Merrill & Burwell (1950). The spectrum of the star has been extensively discussed by Cohen & Kuhi (1979), Herbig & Jones (1983), Mundt, Stocke, Stockman (1983), Hartigan, Mundt, Stocke (1986), Böhm & Raga (1987) and Eislöffel, Solf, Böhm (1990). IR and sub-mm photometry is given by Cohen & Schwartz (1983), (1987), and Reipurth et al. (1993a). Edwards & Snell (1982) report high-velocity CO emission.

Various model calculations: Raga, Böhm, Solf (1986), Hartigan, Raymond, Hartmann (1987).

HH 33/40 (5 32, -06 19)

HH 40 was discovered by Haro (1953), who also later found HH 33 (see Herbig (1974)). HH 33 and 40 are physically connected with an emission-line filament. Mundt et al. (1984) suggest the HH objects form a jet, but Bally & Devine (1994) propose they are really a distant bow shock in the HH 34 flow. CCD images are presented by Mundt et al. (1984), Strom et al. (1986) and Bally & Devine (1994). Optical spectroscopy is discussed by Dopita (1978a), Brugel, Böhm, Mannery (1981a), Goodrich (1986a), and Mundt, Brugel, Bührke (1987). Infrared H_2 observations are discussed by Elias (1980), Schwartz, Cohen, Williams (1987), Zinnecker et al. (1989), and Zealey et al. (1992). Heyer, Strom, Strom (1987) suggest an alignment with magnetic field lines. No convincing energy source has been found so far near HH 33/40 (Cohen & Schwartz (1983), (1987), in further support of the idea that the complex is driven by HH 34 IRS (Bally & Devine (1994)). Edwards & Snell (1983) found no high-velocity gas in the region.

HH 34 (5 33, -06 29)

Discovered by Haro, see Herbig (1974). HH 34, located in L1641 in Orion, is a large bright bow shock in the approaching lobe of a major bipolar HH complex which includes a very fine jet. This jet, the discovery of which was announced by Reipurth (1985b), was studied in detail by Reipurth et al. (1986) , who present CCD images and low-dispersion spectrocopy. Further CCD images were made by Raga & Mateo (1988b), who resolved the width of the jet knots. Bührke, Mundt, Ray (1988) used CCD images and medium-dispersion spectroscopy for their study, in which they also pointed out a counter-bow shock, HH 34-North, placed symmetrically to HH 34 on the other side of the source. Very high resolution images were discussed by Raga, Mundt, Ray (1991). The existence of multiple bow shocks in the blue lobe of the HH 34 flow was discussed by Reipurth & Heathcote (1992), pointing to eruptive events in the driving source. Cohen & Jones (1987) drew attention to the extremely low Halpha/[SII] ratio of the jet. High-resolution long-slit spectroscopy was presented of the entire approaching lobe of the HH 34 system by Heathcote & Reipurth (1992), and Fabry-Perot observations of the HH 34 bow shock and jet were analyzed by Morse et al. (1992), (1993b). Proper motion studies were discussed by Heathcote & Reipurth (1992), and Eislöffel & Mundt (1992). The optical polarization study of Scarrott (1988b) showed the reflection nebulae in the blue lobe to be illuminated by the source. Stapelfeldt et al. (1991) noted that neither the HH 34 bow shocks nor the HH 34 jet emit in the infrared molecular hydrogen lines, but the jet was mapped in the 1.644 µm line of [FeII]. Zealey, Suters, Randall (1994) and Moneti & Reipurth (1994) present broadband infrared images of the region. The driving source of the HH 34 complex was identified by Reipurth et al. (1986), who gave optical/infrared photometry and a red spectrum. Cohen et al. (1984) detected the source at 100 µm, Cohen & Schwartz (1987) derived a luminosity of 45 L_sun from IRAS data, and Reipurth et al. (1993a) detected the cold dust around the source at 1300 µm. Mm-observations of various molecular species are discussed by Reipurth et al. (1986), Anglada et al. (1989), Cernicharo (1990), Rudolph & Welch (1992), Stapelfeldt & Scoville (1993) and Davis & Dent (1993). A weak molecular outflow is detected by Chernin & Masson (1994). The mass loss rate in the jet is estimated by Hartigan, Morse, Raymond (1994). From a large-field CCD imaging study, Bally & Devine (1994) have suggested that the HH 34 complex is much larger than previously thought, including HH 173 and HH 86/87/88 in the blue lobe, and HH 126, HH 85 and HH 33/40 in the red lobe.

HH 35 (5 33, -06 43)

Herbig (1974) found this small elongated object and suggested it originates in V380 Ori. CCD images are presented by Strom et al. (1986). The Herbig Ae/Be star V380 Ori is discussed in detail by Herbig (1960); see also Cohen & Kuhi (1979) and Finkenzeller & Mundt (1984). Edwards & Snell (1984), Levreault (1988) and Morgan et al. (1991) discuss high velocity gas around the star. A companion to V380 Ori was found with a separation of 0.17 arcsec by Leinert et al. (1994). For further references to V380 Ori see Herbig (1960) and Herbig & Bell (1988). See also notes on HH 130 and HH 148.

HH 36 (5 34, -06 46)

Original paper: Herbig (1974). A small chain of HH knots south-east of the HH 1/2 and V380 region.

HH 37 (5 43, -00 06)

Original paper: Strom et al. (1986), who present CCD images. This is a single HH object in the little group of HH objects HH 20, 21 and 70 in the NGC 2068 region. It is no. 37 of the list of Strom et al. (1986), their Table 18. The nature of the nearby objects 18-42 and 18-43 of Strom et al. (1986) is unclear. All objects are seen on the CCD images of Reipurth & Graham (1988).

HH 38 (5 35, -07 13)

Originally found by Haro (see Herbig (1974)). See notes for HH 43, to which HH 38 may be associated.

HH 39 (6 36, +08 54)

Original papers: Herbig (1968),(1974). This is a small cluster of knots forming a bow shock in a flow from R Mon.

Structure and CCD Imaging: Jones & Herbig (1982), Brugel, Mundt, Bührke (1984), Walsh & Malin (1985), Mundt, Brugel, Bührke (1987) , Schwartz & Schultz (1992).

Spectroscopy: Brugel, Mundt, Bührke (1984), Walsh & Malin (1985).

Proper Motions: Jones & Herbig (1982).

Source: R Mon and its reflection nebula NGC 2261 has been extensively studied by many authors, and the following is only a partial list of the literature: Hubble (1916), Knox-Shaw (1916), Herbig (1960), (1968), Greenstein et al. (1976,1979), Harvey, Thronson, Gatley (1979), Bellingham & Rossano (1980), Gething et al. (1982), Cohen & Schwartz (1983), Persson et al. (1984), Aspin, McLean, Coyne (1985), Cohen, Harvey, Schwartz (1985), Edwards et al. (1987), Warren-Smith, Draper, Scarrott (1987), Ménard, Bastien, Robert (1988), Lightfoot (1989) , Scarrott, Draper, Warren-Smith (1989), Yamashita et al. (1989b), Hodapp (1990), Natta et al. (1993), Kelly, Rieke, Campbell (1994).

Mm Data: Cantó et al. (1981) , Beckwith et al. (1984),(1986), Sargent & Beckwith (1987).

HH 40 (5 32, -06 20)

see notes for HH 33.

HH 41/42 (5 33, - 05 05)

Original paper: Haro (1953). The little-studied objects, HH 41 and 42, form, together with HH 128 and 129, a small cluster of HH objects in the NGC 1976/77 region. Photographic plates of the region are presented by Schwartz (1977a), Reipurth (1985a) and Ogura & Walsh (1991). Infrared observations are discussed by Schwartz, Cohen, Williams (1987) and Cohen et al. (1988).

HH 43 (5 35, -07 11)

Original paper: Haro (1953).

Structure and CCD Images: Herbig (1974), Strom et al. (1986), Schwartz et al. (1988).

Optical Spectra: Herbig (1957), Strom, Grasdalen, Strom (1974), Dopita (1978a), Cohen & Schmidt (1981), Dopita, Binette, Schwartz (1982), Böhm, Brugel, Olmsted (1983), Schwartz, Dopita, Cohen (1985) , Böhm & Solf (1990).

Infrared Observations: Schwartz, Cohen, Williams (1987), Schwartz et al. (1988) , Cohen et al. (1988), Zinnecker et al. (1989), Gredel (1994).

Ultraviolet Observations: Schwartz (1983a) , Schwartz, Dopita, Cohen (1985), Lee et al. (1988), Böhm, Scott, Solf (1991).

Polarization: Cohen & Schmidt (1981).

Source: Cohen & Schwartz (1980), (1983), (1987), Cohen et al. (1984a), Cohen, Harvey, Schwartz (1985), Schwartz et al. (1988), Strom et al. (1989). Reipurth et al. (1993a), Molinari, Liseau, Lorenzetti (1993). The source is a binary star (Gredel 1994, Moneti & Reipurth 1994).

Mm Data: Loren, Evans, Knapp (1979), and Anglada et al. (1989).

HH 44 (5 32, - 05 12)

Discovered by Schwartz (1977a). Located close to the OMC-2 region.

HH 45 (5 33, - 04 52)

Discovered by Schwartz (1977a). CCD images and spectroscopy by Reipurth (1989b). It has a strong morphological resemblance to a bow shock.

HH 46/47 (8 24, - 50 50)

Discovered by Schwartz (1977a), (1977b). This is a major bipolar highly collimated Herbig-Haro jet with several bow shocks and emanating from an infrared source embedded in the Bok globule ESO 210-6A (= Sa 111 = DC 267.4-7.5). The globule is part of the system of cometary globules in the Gum Nebula (Reipurth 1983).

Structure and CCD imaging: Bok (1978), Dopita (1978b), Dopita, Schwartz, Evans (1982), Graham & Elias (1983), Raga & Mateo (1987), (1988a), Hartigan, Raymond, Meaburn (1990), Reipurth & Heathcote (1991), Hartigan et al. (1993), Eislöffel & Mundt (1994).

Optical spectroscopy: Dopita (1978a),(1978b), Dopita, Schwartz, Evans (1982), Dopita, Binette, Schwartz (1982), Graham & Elias (1983), Meaburn & Dyson (1987), Hartigan, Raymond, Meaburn (1990), Reipurth & Heathcote (1992), Hartigan et al. (1993).

Ultraviolet spectroscopy: Schwartz (1983), Lee et al. (1988), Böhm, Scott, Solf (1991).

Infrared observations: Elias (1980), Graham & Elias (1983), Graham & Heyer (1989), Wilking et al. (1990), Zealey, Suters, Randall (1994) , Eislöffel et al. (1994).

Proper motions: Schwartz, Jones, Sirk (1984), Eislöffel & Mundt (1994).

Reflection nebula: Graham (1987), Scarrott & Warren-Smith (1988).

Molecular outflow: Chernin & Masson (1991), Olberg, Reipurth, Booth (1989), (1992).

Source: Elias et al. (1982), Graham & Elias (1983), Cohen et al. (1984b), Emerson et al. (1984), Cohen, Dopita, Schwartz (1986b), Graham & Heyer(1989), Sahu, Sahu, Pottasch (1989), Reipurth & Heathcote (1991), Reipurth et al. (1993a), Molinari, Liseau, Lorenzetti (1993).

Globule: Kuiper et al. (1987), Hodapp (1987), Sahu, Sahu, Pottasch (1989), Olberg, Reipurth, Booth (1992).

Shock structure and modelling: Hartigan (1989), Raga et al. (1990), Hartigan, Raymond, Meaburn (1990), Morse et al. (1994) , Raymond et al. (1994) , Hartigan, Morse, Raymond (1994).

HH 48 (11 03, -77 01)

Discovered by Schwartz (1977a) . The object, which consists of two knots, coincides with an infrared source (Elias (1980)) and a weak IRAS source 11030-7702 (Cohen & Schwartz (1987)). The source may be a faint T Tauri star (Cohen, Dopita, Schwartz (1986b)). No proper motion was found by Schwartz, Jones, Sirk (1984).

HH 49/50 (11 04, -77 17)

Discovered by Schwartz (1977a) . The two closely associated objects are located in a high extinction region of the Cha I clouds, and are illustrated by Schwartz, Jones, Sirk (1984) , who find a very large and similar proper motion for the two objects. Schwartz & Dopita (1980) have obtained spectrophotometric data. Combining radial velocities and proper motions show a space motion close to the plane of the sky. Cohen & Schwartz (1987) suggest a low-luminosity far-infrared source IRAS 11054-7706C, on the axis of the proper motion vectors, as the energy source. Prusti et al. (1991) show this source to be multiple, and identifies one of them, Ced 110-IRS4, as the energy source. It was detected at 1300 µm by Reipurth et al. (1993a), and has a weak molecular outflow (Mattila, Liljeström, Toriseva 1989).

HH 51 (11 08, -76 08)

Discovered by Schwartz (1977a) . Very faint object north of the Cha I clouds. Schwartz, Jones, Sirk (1984) speculate that it is a counterflow to HH 49/50.

HH 52/53/54 (12 52, -76 41)

Discovered by Schwartz (1977a) . The objects may form a giant fractured bow shock driven by an embedded source IRAS 12496-7650 located fourteen arcmin to the south-west. The source has a faint optical counterpart with the small HH 274 object on the side towards the HH objects (Reipurth, unpublished).

Structure and CCD images: Schwartz (1977a), Schwartz, Jones, Sirk (1984), Sandell et al. (1987), Graham and Heyer (1988).

Optical spectroscopy: Schwartz & Dopita (1980), Graham & Hartigan (1988).

Infrared observations: Elias (1980), Sandell et al. (1987), Zealey, Suters, Randall (1994), Gredel (1994).

Source: Cohen & Schwartz (1987) , Hughes et al. (1989), (1991), Reipurth et al. (1993a), Molinari, Liseau, Lorenzetti (1993). Mm observations: Knee (1992).

HH 55 (15 53, -37 42)

Discovered by Schwartz (1977a ). The object consists of a compact knot surrounded by a faint envelope (Heyer & Graham (1990)). Spectra are presented by Krautter, Reipurth, Eichendorf (1984), Cohen, Dopita, Schwartz (1986b), and Heyer & Graham (1990). The HH object is coincident with a faint IRAS source 15533-3742 (Cohen & Schwartz 1987), which appears to be a T Tauri star (Cohen, Dopita, Schwartz (1986b), Heyer & Graham (1990)).

HH 56 (16 28, -44 48)

Discovered by Schwartz (1977a) . It is a bright bow shock in a bipolar collimated outflow (Reipurth et al. (1994)). Optical spectra are presented by Schwartz & Dopita (1980), Wilking et al. (1990) detected it in molecular hydrogen emission, and Gredel (1994) obtained infrared spectra. Schwartz, Jones, Sirk (1984) attempted a proper motion determination. A little reflection nebula, Re 13, is illuminated by the energy source (Reipurth 1981), which is detected in the infrared (Prusti et al. 1993) and at 1.3 mm (Reipurth et al. (1993a). Spectra of Re 13 show Halpha emission (Alvarez et al. (1986)), Cohen, Dopita, Schwartz (1986a). Mm observations are presented by Alvarez et al. (1986), and a molecular outflow has been mapped by Reipurth et al. (1994) and Evans et al. (1994).

HH 57 (16 28, -44 49)

Discovered by Schwartz (1977a) . This is a small Herbig-Haro knot, studied spectroscopically by Schwartz & Dopita (1980). CCD images are shown by Graham & Frogel (1985), Reipurth (1985c) , and Reipurth et al. (1994). A proper motion determination was attempted by Schwartz, Jones, Sirk (1984). The energy source is a bright near- and far-infrared (IRAS 16289-4449) source (Elias 1980, Reipurth & Wamsteker (1983) , Cohen et al. (1984b)(1985), Cohen & Schwartz (1987), Prusti et al. (1993)). Near-infrared photometry is summarized by Molinari, Liseau, Lorenzetti (1993) and Reipurth et al. (1994). Graham (1983) announced that a visible star had appeared at the source, which was identified as an FU Orionis object by Graham & Frogel (1985) and Reipurth (1985c). A weak stellar absorption spectrum was seen by Cohen, Dopita, Schwartz (1986b). The star is partly embedded and surrounded by a reflection nebula (Graham & Frogel 1985, Reipurth 1985c , Scarrott, Gledhill, Warren-Smith 1987). Circumstellar dust has been detected at sub-mm wavelengths by Weintraub, Sandell, Duncan (1991) and Reipurth et al. (1993a). The 3 µm water ice band was detected by Graham & Chen (1991). Mm observations are presented by Alvarez et al. (1986), and a molecular outflow has been mapped by Reipurth et al. (1994) and Evans et al. (1994).

HH 58 (5 28, -04 11)

Original paper: Reipurth & Graham (1988), where a CCD image is shown. The object consists of a northern and a southern group of knots. Cohen (1990) suggests that IRAS 05283-0412 could be a possible energy source.

HH 59 (5 29, -06 31)

Original paper: Reipurth & Graham (1988), where a CCD image is shown. The object is large and amorphous and located in the eastern outskirts of the L1641 complex.

HH 60 (5 30, -06 28)

Original paper: Reipurth & Graham (1988), where a CCD image is shown. The object is a curved diffuse emission nebula only 5 arcmin NE of HH 59, and they may be related.

HH 61/62 (5 33, -07 10)

Original paper: Reipurth & Graham (1988), where CCD images are presented. The two objects are situated on a north-south line with a separation of 4 arcmin, and are most likely related. HH 61 has a diffuse bow shape, while HH 62 consists of a little cluster of knots. Ogura & Walsh (1991) show a photographic plate of the region (note that their knot D is incorrectly identified), and present spectroscopy of HH 61. Cohen(1990) suggests that IRAS 05339-0708C could be a possible energy source for HH 61.

HH 63 (5 34, -04 27)

Original paper: Reipurth & Graham (1988), where a CCD image is given. It is a small group of moderately bright HH knots embedded in a faint bow shaped nebula. Located next to the emission line binary star P2441.

HH 64 (5 35, -07 07)

Original paper: Reipurth & Graham (1988), where a CCD image is shown. It consists of two faint closely attached knots, and is located in the same region of L1641 as HH 38 and HH 43. Cohen(1990) suggests that IRAS 05355-0709C could be a possible energy source. Anglada et al. (1989) has detected a dense ammonia condensation, which they suggest may contain an energy source.

HH 65 (5 37, -07 26)

Original paper: Reipurth & Graham (1988), where a CCD image is shown. It is a small faint nebula, located in the red lobe of the molecular outflow driven by Re50 IRS = IRAS 05380-0728 (Reipurth & Bally 1986). The outflow was also found by Fukui et al. (1986) and further studied by Morgan et al. (1991). The source illuminates the large variable reflection nebula Re50 (Reipurth 1985a). An optical polarization study of the Re50 nebula has been done by Scarrott & Wolstencroft (1988), and infrared observations of the source and nebula are presented by Heyer et al. (1990) and Casali (1991). Strom & Strom (1993) suggest that Re50 IRS is an FU Orionis star. It was detected at 6 cm at the VLA (Morgan, Snell, Strom 1990), and at 1300 µm by Reipurth et al. (1993a).

HH 66 (5 37, -02 04)

Original paper: Reipurth & Graham (1988), where a CCD image is presented. The object consists of two knots, and is located in the HII region IC434 in the western low extinction region of the L1630 cloud.

HH 67 (5 38, -01 48)

Original paper: Reipurth & Graham (1988), where a CCD image is presented. The object consists of a little chain of compact knots, located in a very opaque area of L1630 at the northwestern edge of NGC 2024. There are several nearby IRAS sources, including IRAS 05386-0149C (Cohen (1990)).

HH 68/69 (5 39, -06 29)

Original paper: Reipurth & Graham (1988), where CCD images are shown. This is a chain of three groups of knots, located with equidistant spacing on a well defined straight line. A faint red star is found underneath the HH 68b knot. HH 68c and HH 69 resemble small bow shocks. The energy source is most probably located on the flow axis somewhere to the NNW of HH 68c and HH 69. Cohen(1990) suggests separate driving sources for HH 68 and HH 69.

HH 70 (5 43, -00 06)

Original paper: Reipurth & Graham (1988), who show Halpha and [SII] CCD images. The object is a small knot among a group of other HH knots, including HH 20 and 21. The region is also discussed by Strom et al. (1986).

HH 71 (5 44, +00 39)

Original paper: Reipurth & Graham (1988), who show a CCD image. It consists of two closely spaced knots and a faint diffuse tail, and is located in a region active in low-mass star formation. Cohen(1990) discusses several nearby young stars as potential driving sources.

HH 72 (7 18, -23 56)

Original paper: Reipurth & Graham (1988), who present a large-field Schmidt plate, an Halpha CCD image and a low-dispersion spectrum. This is a small chain of HH knots emanating from a bright-rimmed Bok globule, which is illuminated by the young OB cluster NGC 2362. The energy source is the nearby bright class I IRAS source 07180-2356 embedded in the globule. It was detected at 1300 µm by Reipurth et al. (1993a). Cohen(1990) estimates a luminosity of 280 L_sun. The source drives a molecular outflow (Schwartz, Gee, Huang 1988). An H_2O maser was detected by Wouterloot, Brand, Fiegle (1993).

HH 73 (9 00, -44 39)

Original paper: Reipurth & Graham (1988), who present CCD images. This is a 29" long, finely collimated HH flow located one arcmin south of a PMS binary illuminating the reflection nebula Re 6. It probably belongs to the Vela star forming complex at a distance of about 700 pc (Liseau et al. 1992).

HH 74 (9 00, -44 37)

Original paper: Reipurth & Graham (1988), who show CCD images. This is a single HH knot located about 20 arcsec north of a PMS binary illuminating the reflection nebula Re 6, which could be the energy source.

HH 75 (9 09, -45 30)

Original paper: Reipurth & Graham (1988), who present a CCD image and a low-dispersion spectrum. This is a large complex of many rather bright HH knots. It probably is part of the Vela star forming complex (Liseau et al. 1992). Cohen(1990) suggests that IRAS 09094-4522 could be the energy source.

HH 76 (14 56, -62 52)

Original paper: Reipurth & Graham (1988), who show a CCD image. This object consists of two compact HH knots with sub-structure. They are lying on a line through the nearby IRAS source 14563-6250, which is most probably the energy source (Cohen (1990)). It was detected in the 1300 µm survey of Reipurth et al. (1993a). The distance of 1 kpc is very uncertain.

HH 77 (14 56, -62 55)

Original paper: Reipurth & Graham (1988), who show CCD images. This is a small curved object located in a region of nebulous stars and several IRAS sources. Cohen(1990) suggests IRAS 14564-6253 as the energy source.

HH 78 (16 05, -38 57)

Original paper: Reipurth & Graham (1988), where a CCD image and a low-dispersion spectrum are presented. It is a faint knot with a diffuse tail, located in a region with many Halpha emission stars in the Lupus 3 association. Graham & Heyer (1988) point out that HH 78 lies close to the axis of the HH 228 (= Th28) jet complex.

HH 79 (16 23, -24 13)

Original paper: Reipurth & Graham (1988), who present a large-scale photographic plate. It is located in the dense region of the rho Ophiuchi cloud core, which is very active in star formation. It is a small, highly structured object.

HH 80/81 (18 16, -20 53)

Original paper: Reipurth & Graham (1988), who present a CCD image and low-dispersion spectra. HH 80 has a bright core and is associated with a cluster of HH knots, whereas HH 81 is more isolated. Both HH 80 and 81 belong among the brightest HH objects in the sky, and at an assumed distance of 1700 pc they are the intrinsically most luminous HH objects known. Heathcote & Reipurth (1994) present detailed CCD images, high-resolution spectroscopy and a proper motion study. A line drawn through the objects intersects the 16000 L_sun embedded IRAS source 18162-2048, which is the driving source. Rodríguez et al. (1980) detected a compact HII region there, as well as OH and H_2O masers, and the source was detected at 1300 µm by Reipurth et al. (1993a). Rodríguez & Reipurth (1989) detected both HH objects in radio continuum and found the source to be elongated towards the HH objects. Higher resolution observations at 6 cm and 3.6 cm by Martí , Rodríguez, Reipurth (1993) revealed a highly collimated bipolar radio continuum jet emanating from the source. On the opposite side of the source with respect to HH 80/81 they found a resolved object, HH 80-North, with the same negative spectral index as HH 80 and 81. Next to the source there is a small nebula, GGD 27 (Gyulbudaghian, Glushkov, Denisyuk 1978), which was shown to be a reflection nebula by Hartigan & Lada (1985). Yamashita et al. (1987a) found a large infrared reflection nebula, coincident with a large molecular outflow (Yamashita et al. 1989a). A dense CS disk was found around the HH driving source perpendicular to the outflow direction by Yamashita et al. (1990). Aperture synthesis observations by Yamashita et al. (1991) revealed three unresolved peaks. Aspin et al. (1991 ) performed near-infrared imaging and spectroscopy of the source region, and Aspin & Geballe (1992) did mid-infrared spectroscopy, finding evidence for a cluster of sources. Aspin (1994) found extended infrared CO emission around the source.

HH 82 (18 57, -37 01)

Original papers: Strom et al. (1986) and Reipurth & Graham (1988), both of which present CCD images. Two groups of HH knots are found on a line straight east of S CrA. This star is a close visual binary (Joy and van Biesbrock 1944) and Strom et al. (1986) suspect that the fainter companion may be the driving source. S CrA has been studied spectroscopically in detail (e.g. Bertout et al. (1982), Appenzeller, Jankovics, Östreicher 1984, Appenzeller, Jankovics, Jetter 1986 and references therein). Photometric variability is discussed by Bellingham & Rossano (1980).

HH 83 (5 31, -06 31)

Original papers: Reipurth (1985a) ,(1989b). This is a well collimated jet with a bow shock, a counterflow and a bright infrared source (IRAS 05311-0631), which is associated with a reflection nebula, where the jet breaks out of the cloud. Designations of knots are defined by Reipurth (1989b). Spectroscopic observations are presented by Reipurth (1989b) and Ogura & Walsh (1991). CCD images are discussed by Reipurth (1989b) and Mundt, Ray, Raga (1984). The source was observed in the near-infrared by Reipurth (1989b) and Moneti & Reipurth (1994), and at 1300 µm by Reipurth et al. (1993a). A polarization study of the reflection nebula was done by Rolph, Scarrott, Wolstencroft (1990). Mm-observations are discussed by Bally, Castets, Duvert (1994) and Nakano et al. (1994).

HH 84 (5 31, -06 35)

Original papers: Reipurth (1985a),(1989b). This is a large chain of relatively bright HH knots in a small cloud at the edge of the L1641 complex. The CCD image of Reipurth (1989b) shows a multitude of knots on a fairly well defined line, suggesting it could be a jet, but no energy source has been found. Low-dispersion spectra are given by Reipurth (1989b). A search for ¹²CO wings was done by Morgan et al. (1991).

HH 85 (5 32, -06 22)

Original papers: Reipurth (1985a),(1989b). The CCD image of Reipurth (1989b) shows a long chain of knots, which resembles a finely collimated jet. Bally & Devine (1994), however, suggest it is part of a large bow shock in the red lobe of the HH 34 flow. Low dispersion spectra are presented by Reipurth (1989b). The positions listed by Reipurth (1989b) for HH 85 are in error, and are corrected in Bally & Devine (1994).

HH 86/87/88 (5 33, -06 39)

Original papers: Reipurth (1985a), (1989b). The CCD image of Reipurth (1989b) shows the three objects to be closely associated and have complex sub-structure. No local energy source has been found, but Bally & Devine (1994) suggest that they form a southern bow shock of the HH 34 complex. HH 33/40 would be the equivalent northern counterpart in this major outflow region. Low-dispersion spectra are given by Reipurth (1989b).

HH 89 (5 35, -06 47)

Original paper: Reipurth (1985a) . This object consists of two HH knots and a reflection nebula. Moneti & Reipurth (1994) found a near-infrared source next to the reflection nebula.

HH 90/91 (5 39, -01 15)

Original paper: Reipurth (1985a). A detailed optical/infrared/mm study is presented by Gredel, Reipurth, Heathcote (1992). HH 90 is a large outlying bow shock, whereas HH 91 consists of several oppositely facing bow shocks moving away from a central emission region, which may contain a faint near-infrared source. The central part of HH 91 is very intense in near-infrared H_2 emission. A K-band image is shown by Moneti & Reipurth (1994).

HH 92 (5 39, -01 19)

Original paper: Reipurth (1985a). CCD images show this to be a little chain of faint HH knots in the L1630 cloud (Reipurth, unpublished).

HH 93 (5 40, -01 27)

Original paper: Reipurth (1985a). CCD images show this to be a little group of faint HH knots (Reipurth, unpublished).

HH 94/95 (5 41, -02 37)

Original papers: Reipurth (1985a) ,(1989b). CCD images and low-dispersion spectra are given by Reipurth (1989b), who suggested that HH 94 is a bent HH jet. This idea no longer appears tenable. Rather, HH 94 and HH 95 are probably bow shocks in a large bipolar outflow. Curiel et al. (1989a) found a radio continuum source located precisely mid-way between the two HH objects, which is a likely energy source.

HH 96/97/98 (18 58, -37 04)

Original paper: Hartigan & Graham (1987), who show a large-scale photographic plate and obtained spectra. HH 96 and 97 are small HH knots on the line between HH 100 and HH 101 and they are, like these objects, blueshifted. HH 98 is on the same line, but on the opposite side of the source. See also notes for HH 100.

HH 99 (18 58, -36 59)

Original paper: Cohen et al. (1984b). Two small knots in the HH 100 flow in the red north-eastern lobe. Proper motions by Schwartz, Jones, Sirk (1984) suggest an origin near HH 100 IRS. Spectroscopy by Hartigan & Graham (1987). Molecular hydrogen emission detected by Wilking et al. (1990) , and infrared spectra obtained by Gredel (1994). See also notes for HH 100.

HH 100 (18 58, -37 02)

Original papers: Strom, Strom, Grasdalen (1974), Strom, Grasdalen, Strom (1974). This is an HH object surrounded by a large highly structured reflection nebula, seen in the plates and CCD images of Hartigan & Lada (1985), Strom et al. (1986), and Hartigan & Graham (1987). Polarization measurements of the reflection nebula have been done by Vrba, Strom, Strom (1975) and Scarrott et al. (1987), and Graham (1993) reports changes in its morphology. Spectroscopy is discussed by Strom, Grasdalen, Strom (1974). A large molecular outflow was mapped by Levreault (1988), and Loren (1979), Anglada et al. (1989) and Harju et al. (1993) mapped various molecular species in the region. The energy source, HH 100 IRS, was discovered by Strom, Strom, Grasdalen (1974) and Glass & Penston (1975); it is highly variable (Axon et al. (1982), Reipurth & Wamsteker (1983), (see Molinari, Liseau, Lorenzetti (1993) for a summary of infrared observations), and was detected in the far-infrared by Cohen et al. (1984b), in the radio continuum at 6 cm by Brown (1987), and at 1300 µm by Reipurth et al. (1993a). Spectroscopy of the reflection nebula shows the source to be an active T Tauri star (Cohen, Dopita, Schwartz (1986b)). Strong 3 µm water-ice absorption has been observed towards the source (Whittet & Blades (1980), Graham & Chen (1991), Chen & Graham (1993)).

HH 101 (18 58, -37 07)

Discovered by Strom, Grasdalen, Strom (1974). This is a large bow shock in the blue lobe of the HH 100 flow. Structure and CCD images are discussed by Morgan et al. (1984), Hartigan & Lada (1985), Reipurth (1985c) , Strom et al. (1986), Hartigan & Graham (1987). Proper motions are directed away from the driving source HH 100 IRS (Schwartz, Jones, Sirk 1984) . Spectroscopy is analyzed by Strom, Grasdalen, Strom (1974), Dopita (1978a) and Schwartz (1981). H_2 emission was detected by Brown et al. (1983), and HH 101 was also detected in the radio continuum at 6 cm (Brown 1987). The bow shock nature of HH 101 is discussed by Hartigan (1989).

HH 102 (4 28, +18 00)

Original paper: Strom, Grasdalen, Strom (1974). This is not an HH object, but a large amorphous reflection nebula illuminated by the L1551 IRS 5 source. It is further discussed by e.g. Cudworth & Herbig (1979), Draper, Warren-Smith, Scarrott (1985b) and Graham & Heyer (1990).

HH 103 (21 41, +65 49)

Original paper: Strom, Grasdalen, Strom (1974). This is the brightest HH object in the very complex star forming region around NGC 7129, which is rich in HH objects. It is a large C-shaped object connected to HH 232 (formerly GGD 32) with faint knots and filamentary emission (Eiroa, Gómez de Castro, Miranda (1992)). CCD images are shown by Hartigan & Lada (1985), Strom et al. (1986), Eiroa, Gómez de Castro, Miranda (1992), and Goodrich (1993). Spectra are discussed by Strom, Grasdalen, Strom (1974) and Cohen & Fuller (1985). Proper motion is measured by Ray et al. (1990). King & Scarrott (1981) did not measure any polarization in the object. Wilking et al. (1990) detected H_2 in HH 103. Cohen & Schwartz (1983) did an infrared search for an energy source. Further references on the NGC 7129 region are given in the notes to the HH 167 jet.

HH 104 (18 58, -37 01)

Original papers: Schwartz, Jones, Sirk (1984) and Graham (1993). This HH flow contains four HH knots located pair-wise and symmetrically on a straight line through R CrA. HH 104A,B form the eastern lobe (Schwartz, Jones, Sirk (1984), Strom et al. (1986), Hartigan & Graham (1987)), and HH 104C,D form the western lobe (Graham (1993)). The latter reference gives astrometry of all four objects. HH 104A was detected in molecular hydrogen by Wilking et al. (1990). A molecular outflow was mapped by Levreault (1988). R CrA is a Herbig Ae/Be star (e.g. Herbig (1960)), and is surrounded by a large reflection nebula (e.g. Graham & Phillips (1987), Graham (1989)). Far-infrared photometry is reported by Cruz-Gonzalez, McBreen, Fazio (1984). Further references to observations of R CrA is given in Herbig & Bell (1988).

HH 105 (21 42, +65 54)

Original paper: Hartigan & Lada (1985). This is a faint HH object in the NGC 7129 region. CCD images are presented by Hartigan & Lada (1985), Strom et al. (1986), Ray (1987), Eiroa, Gómez de Castro, Miranda (1992), and Goodrich (1993). The object was detected in H_2 by Wilking et al. (1990). Cohen & Schwartz (1983) did an infrared search for an energy source.

HH 106/107 (18 27, +01 18)

Original paper: Reipurth & Eiroa (1992), who present CCD images. HH 106 has a bow shock morphology. Gredel (1994) did infrared spectroscopy. HH 107 is larger and brighter and has a complex structure. In a dense cloud region in between the two objects one finds the faint Halpha emission star ESO Halpha 279 (= IRAS 18269+0116), which is the presumed energy source. It was detected at 1300 µm by Reipurth et al. (1993a), and has been studied in detail at optical and infrared wavelengths by Aspin, Reipurth, Lehmann (1994).

HH 108/109 (18 33, -00 37)

Original paper: Reipurth & Eiroa (1992), who present CCD images. The HH objects are only an arcminute apart and are lying on a line through the nearby IRAS source 18331-0035, which was detected at 1300 µm by Reipurth et al. (1993a).

HH 110 (5 48, +02 54)

Original reference: Reipurth & Olberg (1991). This is a major collimated HH flow, with a rich sub-structure of knots and a flow-pattern with graceful curves. CCD images, spectroscopy and mm-observations are discussed by Reipurth & Olberg (1991).

HH 111 (5 49, +02 47)

Original reference: Reipurth (1989a). This is a major bipolar and highly collimated Herbig-Haro complex with a very fine jet and multiple bow shocks. Various parts of the HH flow have been imaged by Reipurth (1989a), Reipurth, Raga, Heathcote (1992), and Morse et al. (1993a). Spectra are discussed by Reipurth (1989a), Morse et al. (1993a) (1993b) and motions are found for all parts of the jet complex (Reipurth, Raga, Heathcote 1992), directed away from the energy source HH 111 VLA (= IRAS 05491+0247), which is also detected at 1300 µm (Reipurth et al. 1993a) and as a 3.6 cm and 2 cm VLA source (Rodríguez & Reipurth 1994). A small one-sided radio continuum jet emanates from the VLA source in the direction of the optical HH jet. A near-infrared reflection nebula is slightly displaced from the VLA source. A counter-jet has been found in the optical by Reipurth, Raga, Heathcote (1992) and in the infrared by Gredel & Reipurth (1994). A major molecular outflow is found along the jet-axis (Reipurth & Olberg 1991). Near-infrared images and spectroscopy are discussed by Gredel & Reipurth (1993), who also find a second bipolar infrared jet, HH 121, emanating from the source, suggesting that it is a close binary. Stapelfeldt & Scoville (1993) find evidence of a circumstellar disk around the source based on ¹³CO interferometer observations. Hartigan, Morse, Raymond (1994) estimate the mass loss rate through the jet.

HH 112 (5 49, +02 59)

Original paper: Reipurth & Olberg (1991) , who show a CCD image. It is a group of very faint HH knots.

HH 113 (5 50, +02 42)

Original paper: Reipurth & Olberg (1991). A large complex of HH knots, including a jet-like collimated feature.

HH 114/115 (5 16, +07 08)

Original paper: Reipurth & Bally (1994). This is one of the largest bipolar HH complexes known, with a projected extent of 2.5 pc. It is driven by the IRAS source 05155+0707, located mid-way between the lobes of the HH flow and an associated molecular outflow.

HH 116 (5 49, +08 24)

Original paper: Reipurth & Bally (1994). This is a small HH object located at the edge of the L1598 cloud close to the class I IRAS source 05494+0820.

HH 117/118 (5 49, +08 09)

Original paper: Reipurth & Bally (1994). A bipolar HH complex centered on IRAS 05496+0812. Schwartz, Gee, Huang (1988) has reported a molecular outflow from the same source.

HH 119 (19 34, +07 27)

Original papers: Vrba et al. (1986), Reipurth, Heathcote, Vrba (1992). This is a chain of three little HH objects located on a line through the cold central source of the Bok globule B335, with HH 119A,B in the western red lobe of the associated molecular outflow and HH 119C in the eastern blue lobe, and proper motions in opposite directions away from the source (Reipurth, Heathcote, Vrba 1992). The molecular outflow has been studied by, among others, Frerking & Langer (1982), Goldsmith et al. (1984), Langer, Frerking, Wilson (1986), Davidson (1987), Cabrit, Goldsmith, Snell (1988), Moriarty-Schieven & Snell (1989), Hirano et al. (1988),(1992) and Chandler & Sargent (1993). The source B335 IRS (= IRAS 19345+0727) was discovered by Keene et al. (1983), and has been observed at sub-mm wavelengths (e.g Gee et al. (1985), Davidson (1987), Chandler et al. (1990) and at centimeter wavelengths (Anglada et al. (1992). The globule has been extensively studied at mm-wavelengths by, among others, Menten et al. (1984) , Walmsley & Menten (1987) , Frerking, Langer, Wilson (1987), Menten et al. (1989) , Zhou et al. (1990), and Hasegawa, Rogers, Hayashi (1991).

HH 120 (8 07, -35 56)

Original papers: Westerlund (1963) , Reipurth (1981). This is a bright low-excitation HH object emanating from one of the cometary globules, CG30, in the Gum Nebula. Pettersson (1984) has presented a detailed study with CCD images and spectroscopy, and he identified the driving source, CG30-IRS4, later detected in the far-infrared (Cohen et al. 1984b) and as an IRAS source (08076-3556, see Cohen & Schwartz (1987)). Cohen(1990) presents an IRAS LRS spectrum of the source. It was detected at 1300 µm by Reipurth et al. (1993a) and Persi et al. (1994). Near-infrared images are shown by Graham & Heyer (1989), Persi et al. (1994), and Gredel (1994). Molecular hydrogen emission was detected by Schwartz, Cohen, Williams (1987) and Wilking et al. (1990), and infrared spectra are discussed by Gredel (1994). An optical polarization study was made by Scarrott et al. (1990). Pettersson (1984) and Cohen, Dopita, Schwartz (1986b) studied the stellar continuum via the reflection nebula around the infrared source. Olberg, Reipurth, Booth (1989) mapped the globule in ¹²CO. The globule is part of a larger complex of globules (Reipurth 1983), and other star formation has taken place in the vicinity (Pettersson 1987).

HH 121 (5 49, +02 47)

Original paper: Gredel & Reipurth (1993). This is a small bipolar jet emanating from the HH 111 jet source, at almost right angles to the HH 111 jet, suggesting that the source is a binary. The jet is located in a high extinction region and is only detected in infrared emission lines.

HH 122 (5 52, +01 43)

Original paper: Reipurth & Madsen (1989). This is a small HH flow located in a high extinction region of the L1622 cloud in Orion.

HH 123 (4 32, -14 19)

Original paper: Reipurth & Heathcote (1990). This is a small amorphous HH object originating in the main component of the PMS binary L1642-2, located in the high galactic latitude cloud L1642. CCD images and spectra by Reipurth & Heathcote (1990). The source is IRAS 04325-1419 (Sandell, Reipurth, Gahm (1987)), which was detected at 1300µm (Reipurth et al. 1993a), and it drives a small molecular outflow (Liljeström, Mattila, Friberg 1989). The cloud has low extinction (Sandell et al. (1981)), and its gas and dust has been studied by e.g. Magnani, Blitz, Mundy (1985), Laureijs, Mattila, Schnur (1987) and Liljeström & Mattila (1988).

HH 124 (6 38, +10 17)

Original paper: Walsh, Ogura, Reipurth (1992). This is a long chain of what appears to be a bipolar HH flow in NGC 2264, driven by the IRAS source 06382-1017, which was detected at 1300 µm by Reipurth et al. (1993a). Moneti & Reipurth (1994) searched for a near-infrared counterpart to the source. See also notes for HH 125.

HH 125 (6 38, +09 50)

Original paper: Walsh, Ogura, Reipurth (1992), who present CCD images and spectroscopy. This is a group of giant interconnected filaments, presumably bow shocks. No energy source has been identified, but the HH objects appear to be closely associated with HH 225 and 226 (see notes for these objects), with which they form a line. The region of NGC 2264 is rich in young low mass stars (e.g. Herbig (1954a)), with large amounts of molecular material (e.g. Krügel et al. 1987), and much evidence for molecular outflows ( e.g. Original papers: Reipurth (1985a), Ogura & Walsh (1991). CCD images and spectroscopy by Ogura & Walsh (1991). These objects may be part of a large outflow from HH 34 (Bally & Devine (1994).

HH 127 (5 33, -07 02)

Original papers: Reipurth (1985a), Ogura & Walsh (1991). Two small HH knots; a spectrum of the brighter one shows very low excitation (Ogura & Walsh 1991).

HH 128/129 (5 33, -05 06)

Original papers: Reipurth (1985a ), Ogura & Walsh (1991). Spectra show both objects to be of low excitation (Ogura & Walsh 1991). Together with HH 41 and 42 (Haro (1953)), they form a small cluster of HH objects.

HH 130 (5 34, -06 51)

Original papers: Reipurth (1985a), Ogura & Walsh (1991). Spectroscopy by Ogura & Walsh (1991). CCD image by Ray & Mundt (1993). This arcuate HH object appears to be a bow shock in a flow driven by V380 Ori. The opposite lobe of the flow contains HH 35.

HH 131 (5 32, -08 30)

Original paper: Ogura (1991). This is a smattering of emission-line wisps and filaments stretching over almost half a degree south of and well outside the L1641 cloud. It does not appear to be associated with any young object, and is most likely not a Herbig-Haro object.

HH 132 (8 33, -40 28)

Original paper: Ogura (1990), who presents CCD images. These are very faint HH knots associated with a reflection nebula close to the IRAS source 08337-4028, which is embedded in the globule DC259.9-0.0. The object is very close to the bright nebula NGC 2626.

HH 133 (9 09, -45 18)

Original paper: Ogura (1990), who presents CCD images. The object consists of a little cluster of faint HH knots.

HH 134 (5 33, -06 32)

Original paper: Reipurth & Heathcote (1992). This is a small group of HH knots close to HH 34, but it is not clear if they are related to that flow or not.

HH 135/136 (11 10, -58 30)

Discovered by Ogura & Walsh (1992), who present CCD images and long-slit spectroscopy. HH 135 is a single bright HH knot, and HH 136 forms a long chain of bright HH knots. The objects are located in the dark cloud DC290.4+1.9 in Carina, at the considerable distance of 2.7 kpc, making the HH objects intrinsically very luminous. Ogura & Walsh (1992) suggest that the two objects are not part of the same flow, but that rather HH 135 is driven by IRAS 11101-5829, while HH 136 is driven by an unidentified source in the middle of the chain of knots.

HH 137/138 (11 12, -60 36)

Discovered by Ogura (1993), who presents CCD images and long-slit spectroscopy. These two objects form a long well-collimated chain of numerous bright HH knots located in the small cloud DC291.4-0.2. Assuming an association with the nearby open cluster NGC 3590, this would place the HH objects at the considerable distance of 2.2 kpc.

HH 139 (14 56, -63 04)

Original paper: Reipurth et al. (in preparation). This is a small chain of HH knots emanating from the cometary nebula vBH 65a ( van den Bergh & Herbst (1975), Herbst (1975)). The nebula is illuminated by an embedded infrared source, and not as suggested by Perrin & Sivan (1993) by a nearby star. The energy source was detected at 1300 µm by Reipurth et al. (1993a).

HH 140 (14 59, -63 11)

Original paper: Ray & Eislöffel (1994), who present a CCD image. This is a bipolar HH flow emanating from the young Herbig Ae/Be star vBH 65b (Sanduleak & Stephenson (1973), van den Bergh & Herbst (1975), Herbst (1975)), located in the Circinus clouds. Spectroscopic observations of vBH 65b are reported by Allen (1978 ), Gahm & Malmort (1980), and Manchado et al. (1990). H_2O maser emission was detected by Scalise, Gahm, Sandell (1981).

HH 141 (14 59, -63 12)

Original paper: Ray & Eislöffel (1994), who present a CCD image. This is a small chain of HH knots in the Circinus clouds.

HH 142 (14 59, -63 10)

Original paper: Ray & Eislöffel (1994), who present a CCD image. This is a small cluster of HH knots in the Circinus clouds.

HH 143 (14 59, -63 11)

Original paper: Ray & Eislöffel (1994), who present a CCD image. This is a single HH knot in the Circinus clouds.

HH 144 (5 33, -06 47)

Original papers: Bohigas et al. (1985), Strom et al. (1985). Both of these papers comment on two faint knots just west of the HH 1 jet. Using deep CCD images, Reipurth et al. (1993b) found a number of additional faint HH knots, altogether forming an 83 arcsec long collimated jet, with proper motions pointing away from the HH 1/2 source region. Rodríguez et al. (1990b) found two VLA sources here, and the infrared K-band images of Reipurth et al. (1993b) show HH 1/2 VLA2 to be the driving source of HH 144. HH 1/2 VLA1/2 thus appears to be a pre-main sequence binary with each component driving an HH flow. Structure and proper motions are further discussed by Eislöffel, Mundt, Böhm (1994). For references to mm-studies see notes on HH 1/2.

HH 145 (5 33, -06 48)

Original paper: Reipurth et al. (1993b), who present CCD images. This is a cluster of faint HH knots west of HH 144, but it is not clear if HH 144 and 145 are related. Structure and proper motions are discussed by Eislöffel, Mundt, Böhm (1994).

HH 146 (5 33, -06 50)

Original paper: Reipurth et al. (1993b). An isolated faint HH knot south-west of HH 2.

HH 147 (5 33, -06 47)

Original paper: Davis, Eislöffel, Ray (1994), who present CCD images and near-infrared H_2 images. It is an HH object associated with reflection nebulosity from an embedded infrared source (IRAS 05339-0646) about an arcminute east of HH 1. The star is number 50 in the list of Nakajima et al. (1986) and number 31 in the list of Strom et al. (1989); the latter reference gives optical/infrared/far-infrared photometry and a spectral classification. Structure and proper motions are discussed by Eislöffel, Mundt, Böhm (1994).

HH 148 (5 33, -06 44)

Original paper: Strom et al. (1986), who show CCD images. This is a small chain of three HH knots emanating to the south-west from the Herbig Ae/Be star V380 Ori. It is orthogonal to the line defined by HH 35 and HH 130, which may suggest the presence of another source in the region. Leinert et al. (1994) found a companion with a separation of 0.17 arcsec.

HH 149 (22 34, +75 01)

Original paper: Balázs et al. (1992), who present CCD images. This is a small group of HH knots clustered around the IRAS source 22343+7501 in the L1251 cloud. A molecular outflow around this source was discovered by Schwartz, Gee, Huang (1988) and further studied by Sato & Fukui (1989). Kun & Prusti (1993) discuss the presence of young stars in L1251 and give further references to the region.

HH 150 (4 28, +18 07)

Original paper: Mundt, Ray, Bührke (1988). This is a fine bipolar jet emanating from HL Tau. It can be traced for 13 arcsec in the NE lobe before it becomes confused with the HH 151 jet, and longer in the SW lobe.

Structure and CCD images: Mundt, Ray, Bührke (1988) , Mundt et al. (1990), Mundt, Ray, Raga (1991).

Spectroscopy: Mundt et al. (1990).

Proper motions: Mundt et al. (1990).

Polarization data: Bastien (1982), Hodapp (1984), Gledhill & Scarrott (1989).

Molecular outflow: Edwards & Snell (1982), Calvet, Cantó , Rodríguez (1983), Torrelles et al. (1987), Levreault (1988).

Source: There is a large body of literature on HL Tau and its circumstellar environment, the following is only some of many references: Cohen & Kuhi (1979), Cohen (1980b),(1983), Grasdalen et al. (1984), Beckwith et al. (1984), Brown, Drake, Mundt (1985), Beckwith et al. (1986),(1989), Edwards et al. (1987), Sargent & Beckwith (1987),(1991), Monin et al. (1989), Grasdalen et al. (1989), Adams, Emerson, Fuller (1990), Carr (1990), Ohashi et al. (1991), Blake, van Dishoeck, Sargent (1992), Rodríguez et al. (1992) , Schuster et al. (1993), Reipurth et al. (1993a), Molinari, Liseau, Lorenzetti (1993), Hayashi, Ohashi, Miyama (1993), Gómez et al. (1993), Rodríguez et al. (1994a).

HH 151 (4 28, +18 07)

Original paper: Mundt & Fried (1983). This is a fine bright bipolar jet apparently emanating from the VLA 1 source between HL and XZ Tau.

Structure and CCD images: Mundt & Fried (1983), Strom et al. (1986), Mundt, Ray, Bührke (1988) , Mundt et al. (1990), Mundt, Ray, Raga (1991).

Spectroscopy: Mundt, Brugel, Bührke (1987), Cohen & Jones (1987), Mundt et al. (1990).

Proper motions: Mundt et al. (1990).

Source: Brown, Drake, Mundt (1985). The reality of the VLA 1 source is controversial, and Rodríguez et al. (1994a) were not able to detect it in a deep high resolution VLA study.

HH 152 (4 28, +18 07)

Original paper: Mundt, Ray, Bührke (1988). This is a short bipolar jet emanating from XZ Tau and stretching about 10 arcsec on either side of the star.

Structure and CCD images: Strom et al. (1986), Mundt, Ray, Bührke (1988) , Mundt et al. (1990).

Spectroscopy: Mundt et al. (1990).

Proper motions: Mundt et al. (1990).

Polarization data: Bastien (1982), Hodapp (1984), Gledhill & Scarrott (1989).

Source: Cohen & Kuhi (1979), Brown, Drake, Mundt (1985), Carr (1990), Molinari, Liseau, Lorenzetti (1993). Haas, Leinert, Zinnecker (1990) resolved XZ Tau as a close binary star.

HH 153 (4 28, +18 07

Original paper: Mundt, Ray, Bührke (1988). A more detailed study (CCD images, spectroscopy, proper motions) was carried out by Mundt et al. (1990). As seen in Halpha this is a short well-collimated jet. In [SII] the morphology changes dramatically, the jet being replaced by two bright knots, which may be part of the working surface where the jet flow terminates. No source has been identified yet. This jet is part of a small group of flows (HH 150-153) in the HL/XZ Tau region.

HH 154 (4 28, +18 01)

Original paper: Mundt & Fried (1983), who show CCD images of a short (about 20 arcsec) jet emanating from the L1551 IRS 5 source.

CCD images of the region are presented by Mundt & Fried (1983) , Snell et al. (1985), Strom et al. (1986), Campbell et al. (1988), Graham & Heyer (1990) and, in most detail, Mundt, Ray, Raga (1984).

Proper motion of the knots in the jet are demonstrated by Neckel & Staude (1987b) and Campbell et al. (1988).

Optical spectra are discussed by Cohen & Fuller (1985), Sarcander, Neckel, Elsásser (1985) and Stocke et al. (1988).

Molecular hydrogen emission from the jet has been observed by Yamashita & Tamura (1992) and [OI] 63µm emission was detected by Cohen et al. (1988).

Optical/infrared polarization measurements of the reflection nebula around the source and the jet are discussed by Nagata, Sato, Kobayashi (1983), Hodapp (1984), Draper, Warren-Smith, Scarrott (1985b), Lenzen (1987), Scarrott (1988a), Campbell et al. (1988) and Stocke et al. (1988).

A major molecular outflow is driven by L1551 IRS 5, it has been studied by, among others, Knapp et al. (1976) , Snell, Loren, Plambeck (1980), Calvet, Cantó, Rodríguez (1983) , Fridlund et al. (1984), Snell & Schloerb (1985), Mirabel et al. (1985) , (1987), Moriarty-Schieven et al. (1987b), Rainey et al. (1987), Uchida et al. (1987), Moriarty-Schieven & Snell (1988), Lizano et al. (1988), Levreault (1988), Fridlund & White (1989), Rodríguez et al. (1989c), van der Werf et al. (1989), Liljeström (1989), Pound & Bally (1991), Parker et al. (1991), Rudolph (1992), Giovanardi et al. (1992), Barsony, Scoville, Chandler (1993), Fridlund & Knee (1993), Bachiller, Tafalla, Cernicharo (1994).

Extended far-infrared emission from dust in the outflow cavity is discussed by Clark & Laureijs (1986), Edwards et al. (1986) and Clark et al. (1986).

The L1551 IRS 5 source has been intensely studied and only a selection of references can be given here. It was discovered by Strom, Strom, Vrba (1976b) , and near- and far-infrared and sub-millimeter photometric observations are given by Fridlund et al. (1980), Beichman & Harris (1981), Phillips et al. (1982), Davidson & Jaffe (1984), Cohen, Harvey, Schwartz (1985), Cohen & Schwartz (1987), Woody et al. (1989), Walker et al. (1990), Butner et al. (1991), Molinari, Liseau, Lorenzetti (1993).

Optical/infrared spectroscopy of L1551 IRS 5 and its reflection nebula shows that it is an FU Orionis object (Mundt et al. 1985, Carr, Harvey, Lester 1987, Stocke et al. 1988, Sato et al. 1992).

Near-infrared imaging of the source and its close environment is discussed by Strom et al. (1985b) , Moneti et al. (1989) and Hodapp et al. (1988).

VLA radio continuum observations are discussed by Cohen, Bieging, Schwartz (1982), Bieging, Cohen, Schwartz (1984), Snell et al. (1985), Bieging & Cohen (1985), Rodríguez et al. (1986), Snell & Bally (1986), Gómez et al. (1993).

Evidence for extended structures or a disk is discussed by, among others, Kaifu et al. (1984), Batrla & Menten (1985), Menten & Walmsley (1985), Moriarty-Schieven et al. (1987a), Duncan et al. (1987), Walmsley &Menten (1987), Sargent et al. (1988), Menten et al. (1989), Keene & Masson (1990), Walker, Adams, Lada (1990), Butner et al. (1991), Ohashi et al. (1991).

A small high-density clump has been observed at the head of HH 154 by Torrelles et al. (1985a).

The presence of magnetic fields is discussed by Simonetti & Cordes (1986).

The L1551 molecular cloud itself has been studied at mm-wavelengths by Snell (1981) . See also notes for HH 28/29.

HH 155 (4 19, +19 25)

Original paper: Schwartz (1975). This is a Herbig-Haro flow stretching from T Tauri to the west and including a knot located 32 arcsec west of T Tau (formerly HH 1555) and the spatiokinematic flow components A and B very close to T Tauri (Böhm and Solf (1994)). All emission of HH 155 is blue-shifted; presumably the receding lobe is obscured by a circumstellar disk around T Tauri. The region of T Tauri contains another HH flow, HH 255, which lies in a north-south direction and includes Burnham's Nebula south of T Tauri and the two spatiokinematic flow components C and D of Böhm & Solf (1994) close to T Tauri; HH 255 appears to be driven by T Tau-S. It is not clear if knot A found by Schwartz (1990) south-west of T Tauri belongs to HH 155 or HH 255. CCD images of HH 155 are shown by Bührke, Brugel, Mundt (1986) and Schwartz (1990) , and spectroscopy of HH 155 is discussed by Schwartz (1975) and Bührke, Brugel, Mundt (1986). [OI] 63 µm emission was detected by Cohen et al. (1988), and weak 3.6 cm emission extends about 1 arcsec west of T Tau ( Skinner & Brown 1994). The molecular hydrogen emission detected towards T Tauri appears to come from Burnham's Nebula, see notes for HH 255. In addition to Burnham's Nebula south of T Tauri, which is shock-excited, there is a large reflection nebula, NGC 1555, west of the star that was discovered by Hind in 1852 (Astronomische Nachtrichten No.839) and described by Burnham (1890), (1894) , Barnard (1895), (1899), Keeler (1900) , Lampland (1936) , Herbig (1953), and Lorre (1975). Spectra show the nebula to reflect light from T Tauri ( Schwartz 1975). T Tauri has been extensively studied, and only a few references are given here; see Herbig & Bell (1988) for further references. Its spectrum is described by Joy (1945), and high-resolution line profiles are discussed by e.g. Hartmann (1982), Mundt (1984), and Persson et al. (1984). Infrared spectroscopy is reported by Kelly, Rieke, Campbell (1994). It is irregularly variable in addition to a regular variability with period 2.8 days (e.g. Herbst et al. (1986), Zaitseva (1989)). T Tauri has a companion, T Tau-S, 0.6 arcsecond to the south which is a bright infrared and radio continuum source, as discussed by Dyck, Simon, Zuckerman (1982), Cohen, Bieging, Schwartz (1982), de Vegt (1982), Hanson, Jones, Lin (1983), Schwartz et al. (1984), Schwartz, Simon, Campbell (1986), Maihara & Kataza (1991) , Ghez et al. (1991), Phillips, Lonsdale, Feigelson (1993), and Skinner & Brown (1994). A third component, located 0.3 arcsec north of T Tau, was discovered by Nisenson et al. (1985) and confirmed by Maihara & Kataza (1991), but not seen by Gorham et al. (1992). H_2O maser emission has been detected near T Tauri (Knapp & Morris (1976) , Thum, Bertout, Downes (1981)). High-velocity CO and possibly HI emanates from the T Tauri system (Edwards & Snell (1982), Ruiz, Alonso, Mirabel (1992)). Evidence for circumstellar material or a disk is given by Weintraub, Masson, Zuckerman (1987), Weintraub et al. (1992), Schuster et al. (1993), and van Langevelde, van Dishoeck, Blake (1994).

HH 156 (4 15, +28 13)

Original paper: Strom et al. (1986). This is a small bipolar jet emanating from the star labelled Tau 1 by Cohen & Kuhi (1979) near CZ and DD Tau. Cohen & Kuhi (1979) and Strom & Strom (1994) obtained spectra of the star, and Strom et al. (1986) and Goodrich (1993) obtained CCD images. Movsesyan & Magakyan (1990) obtained long slit spectra of the jet. Infrared photometry of the star is reported by Strom & Strom (1994). The source is detected by IRAS at 12 µm (IRAS 04155+2812). Skinner, Brown, Stewart (1993) report a possible radio continuum detection.

HH 157 (4 18, +26 50)

Original paper: Mundt et al. (1984). This is an HH jet powered by the T Tauri star Haro 6-5B, a companion about 20 arcsec west of Haro 6-5 (= FS Tau). CCD images are discussed by Mundt et al. (1984) and Strom et al. (1986). Spectra of the jet are presented by Mundt, Brugel, Bührke (1987), and of the reflection nebula by Cohen & Fuller (1985). Polarization data are given by Gledhill, Warren-Smith, Scarrott (1986) and Gledhill & Scarrott (1989). The source was observed in the near-infrared by Vrba, Rydgren, Zak (1985), in H_2 by Carr (1990), in the far-infrared by Cohen & Schwartz (1987) and at 1300 µm by Reipurth et al. (1993a).

HH 158 (4 24, +25 59)

Original paper: Mundt & Fried (1983) . This is a short jet emanating from the T Tauri star DG Tau.

CCD images are discussed by Mundt & Fried (1983), Strom et al. (1986), Mundt, Brugel, Bührke (1987), and

HST images are presented by Kepner et al. (1993).

Spectroscopic observations are analyzed by Mundt & Fried (1983), Cohen & Fuller (1985), Mundt, Brugel, Bührke (1987) and Solf & Böhm (1993).

Optical spectra of DG Tau are given by e.g. Cohen & Kuhi (1979) and Levreault (1988).

DG Tau is detected in the radio continuum (Bertout & Thum (1982), Cohen, Bieging, Schwartz (1982)), and Bieging, Cohen, Schwartz (1984) find it is extended in the same direction as the jet.

Polarization measurements are given by Bastien (1982), Moneti et al. (1984), and Hodapp (1984).

Infrared lunar occultation observations are analyzed by Leinert et al. (1991) and Bogdanov & Cherepashchuk (1993).

Near-infrared observations are discussed by Carr (1990), Chandler et al. (1993) and Molinari, Liseau, Lorenzetti (1993), and

far-infrared observations by Cohen, Harvey, Schwartz (1985) and Cohen & Schwartz (1987).

Levreault (1988) did not detect clear evidence for a molecular outflow.

Circumstellar gas or dust has been detected by Ohashi et al. (1991), Chen et al. (1992), Schuster et al. (1993), and Mannings & Emerson (1994).

HH 159 (4 23, +25 59)

Original paper: Mundt & Fried (1983). This is a more than one arcmin long highly collimated jet emanating from the low-luminosity star DG Tau B, located approximately 50 arcsec southwest of DG Tau. CCD images are presented by Mundt & Fried (1983) , Mundt, Brugel, Bührke (1987) and Mundt, Ray, Raga (1984). Spectroscopy is discussed by Jones & Cohen (1986) and Mundt, Brugel, Bührke (1987). The source was observed in the near-infrared by Vrba, Rydgren, Zak (1985), and in the far-infrared by Cohen, Harvey, Schwartz (1985) and Cohen & Schwartz (1987).

HH 160 (7 01, -11 28)

Original paper: Poetzel, Mundt, Ray (1989), who present CCD images and long-slit spectroscopy. This is a finely collimated bipolar jet emanating from Z CMa with the very large extent of 3.6 pc. Parts of the flow have very high radial velocities, and the jet near the source shows complex velocity-structure. Z CMa itself has been very extensively studied, see Herbig (1960),(1991) for references. It is an FU Orionis object (Hartmann et al. 1989, Hessman et al. (1991), Welty et al. (1992), Sato et al. (1992)) and it has an infrared companion (e.g. Koresko et al. (1991), Haas et al. (1993), Whitney et al. (1993), Barth, Weigelt, Zinnecker (1994). Submillimeter observations are discussed by Weintraub, Sandell, Duncan (1991), and radio continuum observations by Bieging, Cohen, Schwartz (1984) and Skinner, Brown, Stewart (1993). Evidence for a disk is presented by Malbet et al. (1993). Optical photometry is summarized by Kolotilov (1991). X-ray observations are reported by Preibisch & Zinnecker (1994). A molecular outflow was detected by Evans et al. (1994).

HH 161 (0 08, +58 33)

Original paper: Strom et al. (1986), who present CCD images. This is a single bright HH knot next to the luminous Herbig Ae/Be star LkHalpha 198 (= V633 Cas). A deeply embedded companion to LkHalpha 198 has been detected by infrared imaging (Lagage et al. 1993) and by polarization measurements (Corcoran, Ray, Bastien (1994)); the latter paper presents CCD images that show the object has a tail pointing back towards the companion LkHalpha 198B. This orientation coincides with the axis of a molecular outflow (Cantó et al. (1984), Levreault (1988) , Nakano et al. (1990). The LkHalpha 198 region has been extensively studied, see the following papers and references therein: Herbig (1960), Schwartz & Buhl (1975), Loren (1977), Harvey, Thronson, Gatley (1979), Chavarria (1985), Leinert, Haas, Lenzen (1991).

HH 162 (0 08, +58 33)

Original paper:Corcoran, Ray, Bastien (1994). This is a group of HH objects east of the Herbig Ae/Be star V376 Cas. This star is about 35 arcsec north of LkHalpha 198. See also notes for HH 161.

HH 163 (2 57, +60 17)

Original paper: Ray et al. (1990), who present CCD images and long-slit spectroscopy. This is a short jet in the region of the luminous star AFGL 4029 (IRAS 02575+6017). The CCD images of Ray et al. (1990) show that AFGL 4029 consists of two components, A and B, of which B may be the more likely driving source. Snell et al. (1988) found a molecular outflow from AFGL 4029. Cohen & Lewis (1978) discuss a low-dispersion spectrum of the star. An H