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
1) HH 110 : “deflection” of the outflow
2) HH 30 : bending of the jet
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.
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
From two epochs
“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
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:
[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