Imaging: clues on the jet/environment interactions
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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

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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 NIR wavelengths (H2, K band)


Observing at mm wavelengths (dense gas)

Sepúlveda et al., 2011, AA, 527, 41


From proper motions….


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

(1998-1999)

HH30*


“far” from the source


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)


Differences in the gas excitation:


HH 223

[SII] 6716/31 A

Ha


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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