Astron. J., 130, 2745-2756 (2005/December-0)
The intriguing giant bow shocks near HH 131.
WANG M., NOUMARU J., WANG H., YANG J. and CHEN J.
Abstract (from CDS):
Using the High Dispersion Spectrograph (HDS) at the Subaru Telescope, echelle spectra of two giant arcs, i.e., nebulosities Cw and L associated with HH 131 in Orion are presented. Typical emission lines of Herbig-Haro (HH) objects have been detected toward nebulosity Cw with the broadband filter KV 408. With the low-dispersion spectrograph at the National Astronomical Observatories (NAO) 2.16 m telescope, spectra of nebulosities C, L, and K are obtained, which also show strong [S II] λ6717/λ6731, Hα, and [N II] λ6583 emission lines. Position-velocity distributions of Cw and L are analyzed from the long-slit spectra observed with the HDS Hα narrowband filter. The fastest radial velocity of Cw is Vr~-18.0 km/s. When the flow at L goes to the south, it slows down. The fastest radial velocity of L has been observed at -45.0 km/s, and the slowest value is about -18.3 km/s; the radial velocity gradient is about 200 km/s/pc. The similarity of the fastest radial velocity of Cw to the slowest value of L and their positional connection indicate that they are physically associated. There is a tendency for the entire flow to become less excited and less ionized when going further to the south (i.e., from nebulosities K to L and C), where the most extended (and presumably evolved) objects are seen. The electron densities of all the observed nebulosities are low (ne∼102/cm3). Double-peaked kinematic signatures have been found in Cw from its [N II] λ6583 profiles, while the observed Hα profiles of Cw are almost symmetric. Bow shock models appear to agree with the observed position-velocity diagrams of the [N II] spectra better than Hα spectra, and a bow shock with its wing, apex, and postshock has been possibly revealed near Cw from the [N II] emission. With the suggestion that these arcs are HH shocks possibly ejected out of the Orion A molecular cloud by an uncertain source, their spectra show low to intermediate excitation from their diagnostic line ratios.
ISM: Herbig-Haro Objects - ISM: individual (HH 131) - ISM: Jets and Outflows
Fig.1, Table 1: [O91b] Nebulosity aw (No. cw) added.
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