We request that all of the fields and visits maintain the sameorientation angle between 90 and 102 degrees to ensure proper relative orientation of each of the three fields. Orientations closer to 90 are optimal, but any angle up to 102 degrees is acceptable.1881080319----- Attempting Submission 1 (Wed Feb 24 18:17:49 GMT 2021) -----Investigating the Outflows and Shocks of HOPS 361Abstract: We propose a HST near-IR + SOFIA far-IR study of NGC 2071, a system of at least two outflows from a small group of intermediate to low luminosity stars. Protostellar outflows are ubiquitous part of the star formation process. They provide a record of variable accretion onto stars, have significant impact on the surrounding molecular cloud, and may disrupt or trigger star formation in molecular clouds. Intermediate-luminosity (30 < Lbol < 1000 solar luminosities) protostars bridge the gap between low- and high-mass star formation, forming stars with masses between 2 and 10 solar masses (Di Francesco et al. 1997; Mannings & Sargent 2000). Outflows from these systems of protostars have a significant impact on the surrounding ISM, may play an important role in cloud evolution, and are an important laboratory for understanding the origin of far-IR line emission from outflows. In this study, WFC3/IR images of [FeII] and Paschen Beta lines will trace J-type shocks in the near-IR. Proper motions of knots will be derived from a 2009 WFC3/IR image. SOFIA 4GREAT will trace emission from far-IR transitions of [OI] and four additional CO transitions tracing shock heated gas. These lines will provide both radial velocities of the shocked emission as well as measurements of the mass flow and heating by shocks and UV radiation. The combined data will provide 3D space motions of the knots of shock accelerated gas where the outflow is interacting with the surrounding molecular cloud. Additionally, shock velocities and mass and energy momentum flows through the shocks will provide one of the most detailed measurements of the feedback from a system of protostars to date.We will observe three positions extended along the axis of the HOPS 361/NGC 2071-IR outflow. Each position will be observed in the F164N, F167N, F126N, F128N and F130N filters to obtain images in the FeII 1.257 um and 1.644 um lines and the Paschen Beta line at 1.282 um. This will be executed in twelve orbits. Six of the visits will be for the F164N and F167N filters, with four 10 minute exposures along a diagonal dither line pattern. The pattern is aligned at an angle of 41.788 degree with the diagonal of each rectangular pixel, and the adopted offsets of 10.25 pixels will improve the spatial sampling of the data. These data will be used to map the FeII 1.644 line and, comparing to a previous F160W image of the outflow, measure the proper motions of the outflow knots. The F167N filter will be used for the continuum subtraction. For the remaining six visits, we will obtain two visits at each of the positions: the F126N & F130N filters in one visit - each with three 10 and 3.33 minute integrations per orbit - and then the F128N & F130N filters in the next visit - again with three 10 and 3.33 minute integrations per orbit. The F130N filter observations from both visits at a given position will be combined to provide a sensitive measurment of the continuum. Again, the three exposures will be observed along a diagonal dither line with an offset of 10.33 pixels after each integration. To ensure that the three fields cover the outflow, the orient angle is constrained between 90 and 102 degrees. This range is optimized for observations in the spring of 2021. These should all be taken with the same orientation to ensure proper relative orientation of each of the three fields. Orientations closer to 90 degrees are better, but any angle in this range will be acceptable.The scientific team assembled here is composed of experts in Young Stellar Objects (YSOs), particularly on outflows and jets.
The PI Dr. Nicole Karnath is a staff scientist at the SOFIA Science Center and has experience in near-IR high resolution spectroscopy, mid-IR imaging and spectroscopy, and sub-mm and mm wavelength expertise on YSOs. She focusses on the fundamental properties of YSOs and the earliest phases of star formation by studying outflows, disks, grain properties, magnetic fields, and accertion properties.
Co-I Dr. Tom Megeath is a Professor at the University of Toledo who is a highly distinguished star formation scientist in the field of YSOs. His work has focussed on the visible to far-IR wavelength regimes and has lead the Herschel Orion Protostellar Survey that laid the groundwork for a continuous study of YSOs in the Orion Molecular Clouds. He has lead multiple HST proposals on YSOs and continues to have an active role in the outflow community.
Co-I Dr. Dan Watson of the University of Rochester is one of the leading experts on YSO jets and outflows in the field today. He has extensive experience with observations and modelling of YSO jets with a large team of collaborators in the field. His knowledge of shock physics and the importance they play in detroying the natal molecular clouds is unmatched in the YSO community.
Co-I Dr. Joel Green is a staff scientist at STScI and has studied the process that influence the formation of protoplanetary disks, envelopes, and environments for many years. His work has focussed on outbursting young stars, accretion processes, shocks, and tracers in the IR, Xray, and sub-mm regimes. His knowledge and experience in the YSO outflow community is essential to understanding the physics in the birth environments of YSOs.
Co-I Dr. Will Fischer is a staff scientist at STScI and has studied outbursts and the properties of YSOs throughout his career. His contribution to the HOPS team specifically on outflows has resulted in multiple papers and has had greatly influenced the communities undertanding of outburst rates in the star formation process.Stellar Physics and Stellar Types0falseSUPPORTEDSTARYSOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ISMKNOTYESJ2000ISMKNOTYESJ2000WFC3/IRImagingNoNoF126NWFC3/IRImagingNoNoF128NPOS-TARGDITHER1.858LINEfalsefalse441.788WFC3-IR-DITHER-LINE1falsePOS-TARGDITHER1.873LINEfalsefalse341.788WFC3-IR-DITHER-LINE2falseHst Same orient constraint links visits (01 02 03 04 05 06 07 08 09 10 11 12)The scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.(Tic-Visit
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