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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

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

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


Observing at mm wavelengths (dense gas)

Sepúlveda et al., 2011, AA, 527, 41


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


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)


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 ….


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)


Detail of proper

Motions obtained

From two epochs




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 )


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


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)


HH 223

[SII] 6716/31 A



Excitation of the gas, from

[SII] / Ha line ratio:

“Divide” two images after appropriate recentering and flux scaling

using field stars