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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