We have noted the diagnostic warnings in the Phase II proposal. We have compared the coordinates of GSC2.2 field objects with the coordinates from the NOAO Deep Wide-Field Survey in the vicinity of our target and find that they agree to better than 0.1 arcsec. We are therefore confident that the coordinates are accurate enough for target acquisition for the planned observations. ----- Submission 1 (Fri Apr 29 21:17:37 GMT 2005) ----- ----- Submission 2 (Thu May 26 18:20:54 GMT 2005) ----- Phase II Proposal 10591 (10591_2) successfully submitted. ----- Submission 3 (Fri May 27 22:11:20 GMT 2005) ----- Phase II Proposal 10591 (10591_2) successfully submitted. ----- Submission 4 (Tue May 31 19:01:53 GMT 2005) ----- We are aware that the current Phase II has diagnostic messages which relate to the source of coordinates for our target. This is because our target coordinates have been derived from the NOAO Deep Wide-Field Survey rather than the GSC. We have compared the GSC2.2 coordinates of 98 field objects with the coordinates from the NOAO Deep Wide-Field Survey in the vicinity of our target and find that they agree to better than 0.1 arcsec. We are therefore confident that the coordinates are accurate enough for target acquisition for the planned observations. Assigned ID: 575 ----- Submission 1 (Sat Jan 22 00:00:14 GMT 2005) ----- ACS Observations of the Galaxies in A Giant Ly-alpha Nebula at z~2.7 Giant Ly-alpha nebulae appear to be sites of ongoing massive galaxy formation, as evidenced by their association with very luminous, young, star-forming galaxies and large galaxy overdensities. However the origin of the extended gas and the source of ionization remain mysterious. We have discovered a ~200 kpc size nebula which appears to contain a number of embedded sources, including a very obscured, luminous mid-infrared source and a Lyman break galaxy. We propose to obtain deep ACS and NICMOS images of this nebula in order to: (i) determine the spatial morphology of the Ly-alpha emission on sub-kpc scales; (ii) precisely locate the known continuum sources within the nebula; (ii) determine their morphologies; (iii) detect the source of ionizing photons at the very center of the nebula; (iv) constrain the ionizing luminosity contributed by a possible distributed population of faint, compact continuum sources in the nebula; and (v) by SED fitting of population synthesis models, constrain the ages of the ionizing sources with the aim of determining the timescale of the galaxy formation process in the nebula.
We will be observing a large Lya nebula with HST for 23 orbits. Our observations are split into 11 orbits with ACS WFC (3 orbits for a broad-band observation through the F606W filter, 5 orbits through the narrow-band FR462N ramp filter centered at 4448A and 3 orbits through the narrow-band FR601N ramp filter centered at 5998A) and 12 orbits with NICMOS NIC2 (6 orbits each through the broad-band F110W and F160W filters). The primary goals of the ACS observations are to (i) precisely locate the bright continuum sources in the nebula relative to the peaks in the line emission, (ii) determine the number and distribution of the fainter ionizing sources, through a comparison of Ly-alpha, HeII and deep continuum imaging, and (iii) to measure the morphologies of the brighter objects in the field that are associated with the nebula. The primary goal of the NICMOS observations is to constrain the SED of the continuum sources detected in the ACS observations and provide confirmation that these faint sources truly are associated with the nebula. The details of the observing for each instrument and filter are below: 1. ACS/WFC Imaging F606W - 3 orbits We will take 6 exposures - 2 exposures per orbit (approximately 1300s per exposure). We will use the default ACS-WFC dither box for the first 4 exposures centered on aperture WFC1, and use similar offsets (in different directions) for the remaining 2 exposures. We have no orientation restrictions for these exposures. 2. ACS-WFC Ramp filter FR462N (center @ 4448A) - 5 orbits We will take 10 exposures - 2 exposures per orbit (approximately 1300s per exposure). We will use the compact ACS-WFC dither box for the 1st 4 exposures and then perform another 4 exposures with the same ditter pattern but with the pattern centered. The remaining 2 exposures are with similar positional offsets but in different directions. We require the orientation to be between 270 and 360 degrees. 3. ACS/WFC Ramp filter F601N (center at 5998A) - 3 orbits We will take 6 exposures (2 exposures per orbit). We will use the compact ACS-WFC dither box for the first 4 exposures and then offset by a similar amount in different directions for the remaining 2 exposures. We require the orientation to be between 270 and 360 degrees. 4. NIC2 Imaging F110W - 6 orbits We will obtain 6 exposures (1 exposure per orbit). We will use the NIC-spiral dither pattern with 0.6375 point spacing beginning at nic2-fix. We will run the instrument in MULTIACCUM mode with SPARS256 and Nsamp=13. We will restrict the orientation to 230-130 to ensure no part of our extended source falls on the coronagraphic hole. 5. NIC2 Imaging F160W - 6 orbits We will obtain 6 exposures (1 exposure per orbit). We will use the NIC-spiral dither pattern with 0.6375 point spacing beginning at nic2-fix. We will run the instrument in MULTIACCUM mode with SPARS256 and NSAMP=13. We will restrict the orientation to 230-130 degrees to ensure no part of our extended source falls on the coronagraphic hole. GALAXIES 12 false 0 0.0 false 0 false false false false SUPPORTED GALAXY LYMAN ALPHA CLOUD PROTOGALAXY STARBURST ULTRALUMINOUS IR GAL QSO We have carried out a comparison between the NDWFS coordinates and GSC2.2 coordinates for 98 stars in the field of the Lya nebula. We found the median offsets between the two frames to be (deltaRA, deltaDEC) = (0.022,-0.063) arcsec (in the sense that the NDWFS astrometric system is east and south of the GSC2.2 astrometric system. This difference is so small that we chose not to apply any correction to the NDWFS astrometry. 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