WFC3-IR Imaging of Dense, Embedded Outflows from Intermediate-Mass Protostars in Carina

WFC3-IR Imaging of Dense, Embedded Outflows from Intermediate-Mass Protostars in Carina Based on H-alpha imaging of the Carina Nebula with ACS, we discovered 40 new Herbig-Haro (HH) jets marking outflows from young stars. This is valuable because (1) it is a large sample of jets at one distance, (2) the driving sources are intermediate-mass (IM) stars (1-8 Msun), allowing us to investigate the bridge between low- and high-mass star formation, and (3) the jets are exposed to the same feedback source and trace various stages of being uncovered by the advancing ionization front. This sample is all the more valuable because it can be placed in the context of a well-understood environment that has been studied extensively with HST, Spitzer, Chandra, and from the ground. We propose to image 13 of these jets in the [Fe II] 1.26-micron and 1.64-micron lines. These lines suffer less extincton than optical lines, trace embedded jets, and are essential to measure the total mass in these dense outflows. Four jets have already been imaged in the F126N and F164N filters to make public release images; these images demonstrate that [FeII] emission traces a large mass of neutral gas not seen in H-alpha emission and traces the jet back into the cloud to the Spitzer-identified driving source. This study will permit a detailed comparison of the jet properties (e.g. mass-loss rate, momentum injection, mass-loss history) to IM protostar properties (e.g. accretion rate, luminosity, envelope mass and structure) during the most active accretion. These relationships are poorly determined for IM protostars. Additionally, the flux ratio of [Fe II] lines will trace the spatially dependent extinction through the cloud, providing a map of the density structure in the extended envelope. We propose to obtain WFC3-IR images of a sample of embedded HH jets in the Carina Nebula, using the F126N, F164N, F130N, and F167N filters to trace [Fe II] emission and adjacent continuum from the portions of the jets that are inside dark globules. We will essentially duplicate the ERO images of HH 666 and HH 901/902 taken by the instrument teams with WFC3-IR. We will obtain images in the F126N and F164N filters to trace [Fe II] emission, and F130N and F167N for the nearby continuum to subtract. Total on-source integration times in the F164N filter were 2400-2800 sec (40-47 min) in the ERO/DD programs. We will adopt the same observing strategy, with a box-dither pattern to avoid dead-pixel artifacts. Exposure times in the [Fe II] (F126N and F164N) and the line-free continuum filters (F130N and F167N) must be equal in order to subtract continuum emission at the same signal-to-noise. The Carina Nebula can be observed in CVZ mode, with 96 minutes available per orbit. The on-source exposures require 43 + 43 = 86 min. With guide-star acquisition (6 min) and exposure overheads, we fit all four exposures in two CVZ orbits. We have constructed 8 visits of two orbits each corresponding to our 8 proposed pointings for a total of 16 orbits with CVZ viewing. Each visit is composed of four primary exposures corresponding to the F126N, F164N, F130N, and F167N filters. We use a modified box dither pattern (pattern D4, as suggested in the WFC3 instrument manual) with four pointings to avoid the death star and minimize the impact of the IR blobs. Parallel ACS: We also propose to obtain coordinated parallel ACS/WFC Halpha images in the F658N filter for all pointings. This will effectively increase the total area of our previous Halpha survey of Carina, substantially increasing its archival value for our own studies and for other users. Exposure times for the parallel ACS fields are long (and not CR-SPLIT) in order to maximize on-sky time in the parallel observations without the ACS buffer dump requirements compromising the WFC3-IR primary observations. 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