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Imaging: clues on the jet/environment interactions

Imaging: clues on the jet/environment interactions. Two exemples: 1) HH 110 : “deflection” of the outflow 2) HH 30 : bending of the jet. HH 110. HH 110 is a long (~0.45pc) jet extending ~ N-S: unknown powering source? HH 270, NE of HH 110, extending ~E-W

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Imaging: clues on the jet/environment interactions

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  1. Imaging: clues on the jet/environment interactions Two exemples: 1) HH 110 : “deflection” of the outflow 2) HH 30 : bending of the jet

  2. HH 110 HH 110 is a long (~0.45pc) jet extending ~ N-S: unknown powering source? HH 270, NE of HH 110, extending ~E-W P. source: IRAS 05489+0256 (Class I) IRAS: powering source of both jets: HH 270 jet suffers a grazin collision with a dense molecular clump and then reappears as HH 110, which propagates in a inhomogeneous ambient environment. “Evidences” from detection of dense clump proper motion measurements Kajdic et al. 2012, AJ, 143,106

  3. Observing at NIR wavelengths (H2, K band)

  4. Observing at mm wavelengths (dense gas) Sepúlveda et al., 2011, AA, 527, 41

  5. From proper motions….

  6. HH 30 : bending of the jet/counterjet Large scale bending: “C” shape: jet/counterjet is beingentrained toward the NW: Proper motion of the source toward SE with respect to the ambient : ~2 kms-1 ~ 0.003 arcsec yr-1 (undetectable). Deflection by an isotropic stellar wind blowing the jet /counterjet toward SE: modeling: Estalella et al,2012,AJ,144,61

  7. Fit of the model based onisotropic Stellar wind of a CTTS (W): Momentum rate needed to deflect the jet ~8 10-7 M0 yr-1 km s-1 Typical values in CCTS: 10-8-10-6 M0 yr-1 km s-1 The 2MASS source J04314418+181047, located at an (a,d) offset of -158’, -70’’ from W, has (J-H), (H-K) colours of CTTS: could be the responsible of the wind? (It should be noted that this bending is not easy to detect, since is only appreciable when the jet is imaged over a long lenght ~0.35 pc in this case)

  8. Imaging: clues on the nature of the powering jet source The YSO that power a jet remains invisible (optical/ir), highly extinguished. Indirect evidence on its nature can be derived by modeling the morphology (“wiggling”) + kinematics (proper motions) An example: following with HH 30 ….

  9. The jet of HH 30 (1rst chap.) Jet proper motions from two images in [SII] with the NOT Wiggling path of the jet (Burrows et al. 1996) (Anglada, López, Estalella, Masegosa, Riera, Raga 2007)

  10. Detail of proper Motions obtained From two epochs (1998-1999) HH30*

  11. “far” from the source

  12. The wiggling path of the jet is fitted assuming that the jet source forms part of a low-mass binary system The HST dust disk is thuscircumbinary. Modeling the jet gives two possibilities PrecessionOrbital motion Binary separation: 0.''01 (1 AU) 0.''1 (10 AU) Symetry jet-cj: point (S ) mirror ( C )

  13. The jet of HH 30 (2ond chap.) To discriminate between the two alternative scenarios  Modeling the jet/counterjet system orbital motion of the jet source

  14. Imaging: clues on differences in physical conditions through the jet Compare the spatial brightness distribution through different narrow-band filters: variations on the excitation, density, degree of ionization …through the jet (also from spectra, we will see later)

  15. Differences in the gas excitation:

  16. HH 223 [SII] 6716/31 A Ha

  17. Excitation of the gas, from [SII] / Ha line ratio: “Divide” two images after appropriate recentering and flux scaling using field stars

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