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1983Apj. . .270 . .605E the Astrophysical Journal, 270:605-619 .605E . .270 The Astrophysical Journal, 270:605-619, 1983 July 15 . © 1983. The American Astronomical Society. All rights reserved. Printed in U.S.A. 1983ApJ. A SURVEY OF HIGH-VELOCITY MOLECULAR GAS IN THE VICINITY OF HERBIG-HARO OBJECTS. I. Suzan Edwards Five College Astronomy Department, Smith College AND Ronald L. Snell Five College Radio Astronomy Observatory, University of Massachusetts Received 1982 October 20; accepted 1982 December 21 ABSTRACT A survey of high-velocity molecular gas toward 49 Herbig-Haro objects is presented. Observations of the 12 CO / = 1-0 transition obtained with the 14 m telescope of the Five College Radio Astronomy Observatory reveal three new spatially extended high-velocity molecular outflows. One is in the NGC 1333 region near HH 12, and two are in the NGC 7129 region, the first near LkHa 234 and the second near a far-infrared source. The relationship between optical Herbig-Haro emission knots and large-scale motions of the ambient molecular material is investigated, and the properties of high-velocity molecular outflows in the vicinity of Herbig-Haro objects are discussed. Of 11 energetic outflows in the vicinity of Herbig-Haro objects, eight are found in four pairs separated by 0.2-1.0 pc. We estimate that energetic outflows characterized by mass loss rates > 10-7 -1 4 M0 yr occur for at least 10 yr once in the lifetime of all stars with masses greater than 1 M0. Subject headings: interstellar: molecules — nebulae: general — stars: mass loss — stars: pre-main-sequence — stars: winds I. INTRODUCTION and Silk 1979), and the focused stellar wind model (Cantó 1980; Cantó and Rodríguez 1980). The Herbig Haro (HH) objects are semistellar nebu- Additional evidence that winds from young stars un- lous knots (Haro 1950; Herbig 1951) whose low-excita- dergo dynamical interactions with surrounding interstel- tion emission-Hne spectra have been interpreted as being lar material comes from observations of high-velocity formed in the recombination regions of shock waves molecular gas. Often the high-velocity molecular gas is characterized by shock velocities of * < 100 km s'1 and distributed in a bipolar configuration around an em- preshock densities of - 100 cm-3 (Schwartz 1975, 1978; bedded star (Snell, Loren, and Plambeck 1980; Bally Raymond 1979; Dopita 1978). Surveys of the dark and Lada 1983). In several of these bipolar flow regions clouds surrounding HH objects (Ho and Barrett 1980; a striking spatial and kinematic relation exists between Loren, Evans, and Knapp 1979) reveal that although the high-velocity molecular gas and optical HH objects. HH objects are often associated with high-density In LI551, the large space motion HH objects HH 28 material, they are generally displaced from the dense and 29 are coincident with the blueshifted lobe of cloud cores. The presence of high-velocity H20 maser molecular gas centered on 1RS 5. The motions of both emission found in the vicinity of several HH objects has the HH objects and the high-velocity molecular gas are been interpreted as evidence that HH objects may be directed away from 1RS 5 in a collimated flow (Snell, evolved high-velocity condensations ejected by stellar Loren, and Plambeck 1980). In the NGC 1333 region, a winds from pre-main-sequence stars (Rodriguez etal. string of large negative radial velocity HH objects, HH 1980). The large tangential motions of several HH ob- 7-11, are aligned along the axis of the bipolar molecular jects directed away from nearby pre-main-sequence stars flow driven by HH 7-11 IR, an embedded 80 L0 provide further evidence that these objects are driven or infrared source, and are spatially coincident with the excited by stellar winds (Cudworth and Herbig 1979; peak intensity of the blueshifted lobe of molecular gas Herbig and Jones 1981; Jones and Herbig 1982). Several (Snell and Edwards 1981). models for the excitation of HH objects by a pre-main- If all HH objects result from wind-cloud interactions, sequence stellar wind interacting with an ambient clumpy one might expect to find high-velocity molecular gas interstellar material have been proposed; these include toward many of these objects. Furthermore, if the spa- the accelerated cloudlet model (Schwartz 1978; Schwartz tial configuration of high-velocity molecular gas and and Dopita 1980), the interstellar bullet model (Norman HH objects found in L1551 and NGC 1333 is repre- 605 © American Astronomical Society • Provided by the NASA Astrophysics Data System .605E . .270 606 EDWARDS AND SNELL . sentative of other flows, the presence of a bipolar molec- just fills the main diffraction beam, such as the high- ular flow might locate or confirm suspected positions of velocity molecular gas regions observed here, is given by exciting stars for HH objects. We have conducted a 1983ApJ. search for high-velocity molecular gas toward 49 HH objects using as a probe the /= 1-0 transition of 12 CO. III. RESULTS Preliminary results toward several of the HH objects have been published (Snell, Loren, and Plambeck 1980; a) Overview Snell and Edwards 1981, 1982; Edwards and Snell 1982; The goal of our survey is to search for high-velocity hereafter SLP, SE I, SE II, and ES). We present here the (HV) molecular gas associated with HH objects and to results of our completed survey of HH objects, including elucidate any physical relation between the small optical the detection of three previously unreported high-veloc- HH emission knots and the larger scale radial motions ity molecular outflows, and we discuss the association of of the surrounding molecular cloud material. The 49 HH objects and high-velocity molecular gas. HH objects observed in the 12CO /= 1-0 transition are listed in Table 1. This list includes 38 objects from the II. OBSERVATIONS “Draft Catalogue of Herbig-Haro Objects” (Herbig Observations of the / = l-0 transition of 12CO and 1974) and seven objects from the list of Gyulbudaghian, 13 CO have been obtained using the Five College Radio Glushkov, and Denisyuk (1978, hereafter called GGD Astronomy Observatory (FCRAO) 14 m telescope objects), five of whose spectra identify them as HH located in New Salem, Massachusetts. These observa- emission nebulae. The remaining four HH objects are tions were made in the fall and winter of 1980-1981 and the following: Haro 6-10 (Elias 1978), HH 102 in L1551 1981-1982. The receiver and quasi-optical sideband filter (Strom, Grasdalen, and Strom 1974, hereafter SGS), HH are discussed in detail in Predmore etal (1980). A 512 103 in NGC 7129 (SGS), and the emission nebulosity channel filter-bank spectrometer with 250 kHz (0.65 located 0Í5 west of T Tau on the inner edge of NGC km s-1) spectral resolution was employed. The data 1555 (Schwartz 1975). Coordinates for these HH objects were calibrated using a chopper wheel to switch alter- are taken from the references cited above. Several of nately from the sky to an ambient temperature load. these objects have been previously reported to be in the Measurements of the Moon and Jupiter were used to vicinity of high-velocity molecular gas and are included determine the half-power beamwidth (0Hpbw)> the ef- here for the sake of completeness (SLP; SE I; SE II; ficiency on a spatially extended source (i]FSS), and a Calvet, Cantó, and Rodriguez 1983; Lada and Gautier further correction to estimate the coupling to a source 1982). Five cataloged HH objects, HH 7-11, he within about 2' in extent mostly filling the main beam (tjc). one telescope beam and have been treated as a single These definitions follow the convention described by object in our statistics, as are the multiple knots of other Kutner and Ulich (1981). Between the 1980-1981 and HH objects such as HH 4, HH 6, and HH 12. 1981-1982 observing seasons, both the receiver and the The results of our observations are presented in Table telescope performance at FCRAO were improved. Dur- 1, which lists the peak antenna temperature (7^*), the ing the 1980-1981 observing, the receiver had a single- velocity with respect to the local standard of rest (FlSR), sideband noise temperature measured through the the full width of the line at half-intensity (AFfwhm), quasi-optics feed system of 450 K (Predmore et al 1980). and the full velocity extent (AKmax) of the CO emission = The antenna parameters were measured to be 0Hpbw line toward the optical position of each HH object. For 50", tjfss = 0.62, and tjc = 0.58. The efficiency tjfss in- most spectra, the full velocity extent of the line profile cludes both the effects of scattering by the space frame has been determined at roughly the 100 mK level. We and the radome and also spillover past the subreflector. have reobserved many positions in the NGC 1333, NGC During the 1981-1982 observing season, improvements 2068, and NGC 1999 regions at which we previously in the receiver resulted in a single-sideband noise tem- reported a null detection of HV molecular gas (SE I; SE perature of 120 K measured at the feed horn of the II). These new spectra, obtained during the 1981-1982 receiver (Raisanen et al 1981), and improvements in the observing season, have higher signal-to-noise ratios than = antenna produced the following values: 0Hpbw 50", our earlier measurements, and in several cases weak = ïJfss 0-64, and tjc = 0.72. wings, previously missed, are found to be present at the All line temperatures (7^*) quoted in this paper have 100 mK level. been corrected only for the effects of the Earth’s atmo- A histogram of the distribution of AKmax toward the sphere and ambient temperature telescope losses.
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