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 Kajdic et al. 2012, AJ, 143,106 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

3. Observing at NIR wavelengths (H 2, 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 Estalella et al,2012,AJ,144,61 Large scale bending: “C” shape: jet/counterjet is being entrained 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:

7. Fit of the model based on isotropic Stellar wind of a CTTS (W):  Momentum rate needed to deflect the jet ~8 10 -7 M 0 yr -1 km s -1  Typical values in CCTS: 10 -8 -10 -6 M 0 yr -1 km s -1  The 2MASS source J04314418+181047, located at an (  ) 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 (1 rst chap.) (Anglada, López, Estalella, Masegosa, Riera, Raga 2007) Jet proper motions from two images in [SII] with the NOT Wiggling path of the jet (Burrows et al. 1996)

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

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

16. 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)

17. Differences in the gas excitation:

18. [SII] 6716/31 A HH HH 223

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