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LONG-SLIT SPECTROSCOPY

LONG-SLIT SPECTROSCOPY. Characteristic optical spectra: emission lines; weak or lack continuum. [SII] images of HH 83. Relative line strengths vary along the jet. Reipurth, A&A, 220, 249 (1989 ). Continuum contribution from the source. Spectra at different distances from the source. PA.

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LONG-SLIT SPECTROSCOPY

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  1. LONG-SLIT SPECTROSCOPY Characteristic optical spectra: emission lines; weak or lack continuum

  2. [SII] images of HH 83. Relative line strengths vary along the jet. Reipurth, A&A, 220, 249 (1989)

  3. Continuum contribution from the source Spectra at different distances from the source

  4. PA Ex: HH223

  5. 2006:NOT/ALFOSC PA 96 HH 223 star Lambda [SII] Ha+[NII] [OI] Pixel (1=0.19´´) E W

  6. Ha 1D spectrum [OI] [NII] [SII] ~3 arcsec Mapa P-V Red Blue A B

  7. 1D spectra, integrated the emission, for different knots of HH223

  8. Physical The knots move away from the source with velocities in the range 100-200 km/swith a large spread (velocities as high as 500 km/s have been measured). In contrast, the shock velocities (inferred from their spectrum) never exceed 100 km/s. Estimated electron densities are typically in the range 100-1000 cm-3. Ionization fractions are quite uncertain but have estimated values around 0.1. Derived Flow velocities:100- 500 km/s Mass loss rates: (quite uncertain) : 10-9 to 10-7 Msun/yr. Momentum rates:10-7 and 10-5 Msun/yr km/s ( much greater than the momentum rate available in radiation Lsource/c). Mechanical luminosities: typically around one solar luminosity.

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