Assigned ID: 754 ----- Attempting Submission 1 (Fri Feb 25 23:06:04 GMT 2011) ----- HST Phase I Proposal 754 (ngc1266_apt) successfully submitted. ----- Attempting Submission 2 (Fri Feb 25 23:14:39 GMT 2011) ----- ----- Attempting Submission 1 (Fri Jul 08 17:58:58 GMT 2011) ----- ----- Attempting Submission 2 (Mon Oct 03 21:01:28 GMT 2011) ----- ok Mapping Recent Star Formation and Dust in NGC 1266, a Local Example of AGN-driven Feedback NGC 1266 is a nearby lenticular galaxy with a unique property: it hosts a massive outflow of molecular gas. This outflow appears to be driven by an AGN. AGN feedback may play an important role in galaxy evolution, particularly as a star formation quenching mechanism, but the details are not well understood. At only 30 Mpc away, NGC 1266 presents the best local laboratory for studying the AGN feedback process in action. A large multi-wavelength data set already exists, including high resolution X-ray imaging and radio observations, as well as resolved stellar kinematics from integral field unit data. The existing ground-based optical imaging shows hints of a dust cone along the direction of the outflow, and possibly indications of a recent minor merger, which may have triggered the current outflow and AGN activity. However, the images are of modest resolution, significantly worse than the resolution necessary to provide information about the star formation history and dust distribution associated with the outflow. This proposal aims to acquire high resolution optical, near-infrared, and NUV imaging using ACS/WFC, WFC3/IR, and WFC3/UVIS. The primary goals are to resolve the sites of recent star formation, create multi-stellar population models on the same scale as the molecular gas features (> 1"), to map the detailed dust morphology and properties, and to further constrain the total mass of outflowing material.
NGC 1266 will be observed isng WFC3 and ACS The near UV image uses the WFC3 UVIS channel with the F225W filter, with which we can detect the presence of young, hot stars. We estimate the time to obtain a S/N ∼ 3 per PSF based on the GALEX NUV photometry. If the NUV flux is smoothly distributed, then 2700 seconds is required to achieve the minimum S/N. However, if the NUV flux is produced in clumps then the S/N in the same exposure time will be higher. This will map the presence of young stars at ∼ 30 pc metric resolution to high significance. The orbit will be split into at least four dithered sub-exposures to facilitate cosmic ray subtraction and to remove hot pixels or bad columns and avoid the effect of the droplets. The resulting NUV image will locate regions with recent star formation within the galaxy. 1 orbit for the NUV image. Deep near infrared images will be obtained with the WFC3 IR channel using the broad band F110W, F140W and F160W filters. Exposure times of ≈ 500 seconds yield a S/N per pixel of ∼ 90 for a flux density of 20 mag/sq. arcsec. Exposures are dithered to avoid bad/hot pixels, skip over the “blobs,” and minimize persistence. 1 orbit for WFC3/IR images. The single orbit in ACS/WFC will be divided between three optical filters: F435W (Johnson B), F555W (Johnson V), and F814W (Broad I). The exposure time will be divided between them so as to achieve roughly equal S/N per pixel in each filter. Exposures of 1800 seconds in F435W, 500 seconds in F555W, and 140 seconds in F814W will produce a S/N ∼ 15 per pixel in each of the three filters. As with the UVIS orbit, these exposures will be split into dithered sub-exposures to avoid cosmic rays, hot pixels, and bad columns. 1 orbit for optical imaging. The multi-band imaging will allow us to map the stellar morphology of the galaxy, as well as the detailed dust distribution both in the center of the galaxy and out near one effective radius. The diameter of NGC 1266 (D25 = 90′′) will fill most of the field of view of both instruments. The galaxy will be positioned off-center on each detector to avoid placing the critical central region of the galaxy over the gap between CCDs. AGN/QUASARS 12 false 0.0 0.0 false false false false SUPPORTED GALAXY BAR SEYFERT SPIRAL This object was generated by the targetselector and retrieved from the NED database. J2000 J2000 WFC3/UVIS Imaging No No F225W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F140W WFC3/IR Imaging No No F160W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 1 false POS-TARG DITHER DITHER 4 5.183 WFC3-IR-DITHER-BOX-MIN false 74.653 true 0.365 0.572 2 41.859 POS-TARG WFC3-IR-DITHER-BLOB 18.528 2 false POS-TARG DITHER 3.011 LINE false false 2 85.28 ACS-WFC-DITHER-LINE 3 false The scheduling data was generated by CASM 19.3. CASM was run in Phase II mode. 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