TY - JOUR
T1 - The Intricate Structure of HH 508, the Brightest Microjet in the Orion Nebula
AU - Wu, Ya Lin
AU - Close, Laird M.
AU - Kim, Jinyoung Serena
AU - Males, Jared R.
AU - Morzinski, Katie M.
N1 - Funding Information:
2 IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.
Funding Information:
This material is based upon work supported by the National Science Foundation under grant No. 1506818 (PI Males) and NSF AAG grant No. 1615408 (PI Close). Y.-L.W. and L.M.C. are supported by the NSF AAG award and the TRIF fellowship. K.M.M. s and L.M.C. s work is supported by the NASA Exoplanets Research Program (XRP) by cooperative agreement NNX16AD44G.
Funding Information:
We are grateful to the reviewer, John Bally, for very helpful comments. We also thank Megan Reiter for discussions. This material is based upon work supported by the National Science Foundation under grant No. 1506818 (PI Males) and NSF AAG grant No. 1615408 (PI Close). Y.-L.W. and L.M.C. are supported by the NSF AAG award and the TRIF fellowship. K.M.M.ʼs and L.M.C.ʼs work is supported by the NASA Exoplanets Research Program (XRP) by cooperative agreement NNX16AD44G. This paper includes data gathered with the 6.5 m Magellan Clay Telescope at Las Campanas Observatory, Chile.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/2/20
Y1 - 2018/2/20
N2 - We present Magellan adaptive optics Hα imaging of HH 508, which has the highest surface brightness among protostellar jets in the Orion Nebula. We find that HH 508 actually has a shorter component to the west, and a longer and knotty component to the east. The east component has a kink at 0.″3 from the jet-driving star θ 1 Ori B2, so it may have been deflected by the wind/radiation from the nearby θ 1 Ori B1B5. The origin of both components is unclear, but if each of them is a separate jet, then θ 1 Ori B2 may be a tight binary. Alternatively, HH 508 may be a slow-moving outflow, and each component represents an illuminated cavity wall. The ionization front surrounding θ 1 Ori B2B3 does not directly face θ 1 Ori B1B5, suggesting that the EUV radiation from θ 1 Ori C plays a dominant role in affecting the morphology of proplyds even in the vicinity of θ 1 Ori B1B5. Finally, we report an Hα blob that might be ejected by the binary proplyd LV 1.
AB - We present Magellan adaptive optics Hα imaging of HH 508, which has the highest surface brightness among protostellar jets in the Orion Nebula. We find that HH 508 actually has a shorter component to the west, and a longer and knotty component to the east. The east component has a kink at 0.″3 from the jet-driving star θ 1 Ori B2, so it may have been deflected by the wind/radiation from the nearby θ 1 Ori B1B5. The origin of both components is unclear, but if each of them is a separate jet, then θ 1 Ori B2 may be a tight binary. Alternatively, HH 508 may be a slow-moving outflow, and each component represents an illuminated cavity wall. The ionization front surrounding θ 1 Ori B2B3 does not directly face θ 1 Ori B1B5, suggesting that the EUV radiation from θ 1 Ori C plays a dominant role in affecting the morphology of proplyds even in the vicinity of θ 1 Ori B1B5. Finally, we report an Hα blob that might be ejected by the binary proplyd LV 1.
KW - H II regions
KW - ISM: individual objects (Orion Nebula, HH 508, LV 1)
KW - protoplanetary disks
KW - stars: formation
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U2 - 10.3847/1538-4357/aaa96b
DO - 10.3847/1538-4357/aaa96b
M3 - Article
AN - SCOPUS:85042688886
VL - 854
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 144
ER -