We have updated visits 02 and 09 changed PI in Phase II file as requested earlier ----- Submission 1 (Tue May 16 18:32:18 GMT 2006) ----- Phase II Proposal 10920 (uvlgp2) successfully submitted. ----- Submission 2 (Thu Jul 13 15:19:18 GMT 2006) ----- ----- Submission 3 (Thu Aug 24 18:28:13 GMT 2006) ----- ----- Attempting Submission 4 (Tue Apr 24 19:47:29 GMT 2007) ----- ----- Attempting Submission 5 (Tue Apr 24 19:51:29 GMT 2007) ----- The warnings only concern the ACS/WFC ramp filter exposures that were already executed in Cycle 15, and one pattern that is not being used anymore. Assigned ID: 285 ----- Submission 1 (Fri Jan 27 17:40:22 GMT 2006) ----- Phase I Proposal 285 (uvlg15) successfully submitted. ----- Submission 2 (Fri Jan 27 19:01:48 GMT 2006) ----- High-Resolution Imaging of Nearby Lyman Break Galaxy Analogs in the GALEX All-Sky Survey We have used the ultraviolet all-sky imaging survey currently being conducted by the Galaxy Evolution Explorer (GALEX) to identify for the first time a rare population of low-redshift starbursts with properties remarkably similar to high-redshift Lyman Break Galaxies. These compact UV luminous galaxies (UVLGs) resemble Lyman Break Galaxies in terms of size, UV luminosity, star-formation rate, surface brightness, mass, metallicity, kinematics, dust content, and color. They have characteristic ``ages'' (stellar mass/SFR) of only a few hundred Myr. This population of galaxies is thus worthy of study in its own right and as a sample of local analogs of Lyman Break Galaxies. We propose to image a sample of the 9 nearest and brightest compact UVLGs in the near-ultraviolet, near-infrared, and H-alpha using ACS. With these images we will 1) characterize their structure and morphology, 2) look for signs of interactions and mergers, 3) investigate the distribution and propogation of star formation over varying time scales, and 4) quantify the stellar populations and star formation history, in order to determine whether a previous generation of stars formed long before the current burst. These data will perfectly complement our existing Spitzer, GALEX, and SDSS data, and will provide important information on star-formation in the present-day universe as well as shed light on the earliest major episodes of star formation in high-redshift galaxies.
We propose to observe 9 UVLGs with the ACS in three bands, each of which probes the star formation history over a different characteristic timescale. We will use the ramp filters on the WFC to image the H-alpha emission, and thereby trace the distribution of current (< 10 Myr) star formation in each galaxy. We will use the F330W near-UV filter on the HRC to trace the star formation over longer (~100 Myr) timesales. Finally, we will use the WFC with the F850LP near-IR filter to search for an older, more smoothly distributed population of stars (if one exists). Using this set of three complementary images will allow us to measure the structure and star-formation history of these galaxies. We have chosen these specific filters to provide maximal sensitivity, while at the same time suffering from a minimal contribution from strong emission lines in the passbands of the F330W and F850LP filters (less than a few percent, based on SDSS spectra and standard nebular conditions). The ramp filters were chosen to encompass the H-alpha line at the redshift of the target galaxy. We chose the HRC for the F330W images to study the star formation distribution with the highest resolution possible. We chose the WFC for the H-alpha images in order to look for large scale ionized filaments from starburst outflows, and for the F850LP images we require the larger field-of-view of the WFC to look for evidence of tidal tails or faint companion galaxies which may have trigggered the current burst of star formation. It is important to note that there is good evidence that the extinction in these galaxies is modest, ensuring that even the F330W near-UV images will provide reliable information about the distribution of star formation. First, the emission-line Balmer decrements imply only modest amounts of dust reddening, with E(B-V) values of 0 to 0.3. Second, the star formation rates derived from the extinction-corrected Balmer emission-lines typically agree to within a factor of ~2 with those derived from the observed far-UV luminosity (with no extinction correction). Third, the UV colors are relatively blue, strongly suggesting only modest UV extinction. Fourth, the weakness of the far-IR emission indicates that a significant fraction (typically > 50%) of the intrinsic near-UV light escapes the galaxies. These images will resolve structures as small as ~0.2 kpc at the median redshift of our sample (z~0.16). These galaxies have typical half-light diameters of about 2 kpc so they will cover many resolution elements, allowing us to map the distribution of star-forming regions in each galaxy. Feasibility H-alpha: For the detection of the HII regions, we take a typical total H-alpha flux of 7x10^-15 erg s^-1 cm^-2 from the SDSS spectra. We assume that this emission is distributed in ten star forming knots (point sources), each of which produces 10% of the total. We assume that the equivalent width of the H-alpha emission for each knot is 100 Angstroms (as it typically is in the spectra). The ACS ETC yields a S/N ratio per knot of 50 in an orbit (2 CR-split exposures). For the detection of fainter filamentary emission associated with a galactic outflow, we use the surface brightnesses of the filaments seen in starbursts with star formation rates similar to the UVLGs. These surface brightnesses are typically 10^-15 erg s^-1 cm^-2 arcsec^-2 at a radius of 2 kpc (corresponding to 0.7 arcsec for the ULVGs). In a single orbit (2 CR-split exposures) we would achieve a S/N of 4 per 2x2 pixel region. The large H-alpha equivalent width indicates that the image will be primarily line-emission, so we can use the F850LP image to remove the continuum from the narrow-band image. F330W: The faintest galaxy in our sample has a mean surface brightness interior to the half light radius in the F330W band of 6.0x10^-17 erg s^-1 cm^-2 Angstroms^-1 arcsec^-2 (derived from the SDSS-measured u-band flux and half-light radius). The ACS ETC gives a time of 35 minutes for 2 CR-Split observations (1 orbit with overhead) to achieve a S/N of 10 in a 2x2 pixel region. F850LP: The faintest galaxy in our sample has a mean surface brightness interior to the half light radius in the F850LP band of 2.0x10^-17 erg s^-1 cm^-2 Angstroms^-1 arcsec^-2 (derived from the SDSS-measured z-band flux and half-light radius). In two CR-Split exposures occupying one orbit we can reach a S/N of 10 per 2x2 pixel region at a surface brightness of 2x10^-18 erg s^-1 cm^-2 Angstroms^-1 arcsec^-2 (ten times fainter than the galaxy mean surface brightness interior to the half-light radius). This will allow us to search for a smoothly distributed spatially-extended population of redder (older) stars. We will also use these images to search for tidal tails and close companion galaxies. 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