Imaging: clues on the jet/environment interactionsImaging: clues on the jet/environment interactions

Two exemples:

1) HH 110 : “deflection” of the outflow

2) HH 30 : bending of the jet

HH 110HH 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

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/counterjetHH 30 : bending of the jet/counterjet

Estalella et al,2012,AJ,144,61Estalella 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:

Fit of the model based on isotropicStellar 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() 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.)

(Anglada, López, Estalella, Masegosa, Riera, Raga 2007)

Jet proper motions from two images in [SII] with the NOTWiggling path of the jet

(Burrows et al. 1996)

HH30*

Detail of properMotions obtainedFrom two epochs(1998-1999)

““far” from the far” from the source source

The wiggling path of the jet is fitted assuming that the jet source forms part of a low-mass binary systemThe HST dust disk is thus circumbinary.

Modeling the jet gives two possibilitiesPrecession Orbital motion

Binary separation: 0.''01 (1 AU) 0.''1 (10 AU)Symetry jet-cj: point (S ) mirror ( C )

To discriminate between the two alternative scenarios Modeling the jet/counterjet system orbital motion of the jet source

The jet of HH 30 (2ond chap.)

Imaging: clues on differences in physical conditions through the jetImaging: clues on differences in physical conditions through the jet

Compare the spatial brightness distribution through differentnarrow-band filters: variations on the excitation, density, degreeof ionization …through the jet (also from spectra, we will see later)

Differences in the gas excitation:

[SII] 6716/31 A H

HH 223HH 223

Excitation of the gas, from [SII] / Hline ratio:

“Divide” two images after appropriate recentering and flux scaling using field stars