This is a post-ACS resubmission for the remainder of Proposal 10925. The remaining two targets have been reworked into WFPC2 observations. Please let me know (danforth@casa.colorado.edu) if you see any obvious problems. Remove quotes in the exposure label. ----- Submission 1 (Mon May 15 19:24:17 GMT 2006) ----- Phase II Proposal 133 (imageDLA) successfully submitted. ----- Submission 2 (Tue May 23 16:44:11 GMT 2006) ----- Phase II Proposal 10925 (imageDLA) successfully submitted. ----- Attempting Submission 4 (Thu Mar 15 16:39:34 GMT 2007) ----- ----- Attempting Submission 5 (Thu Mar 15 17:40:06 GMT 2007) ----- APT shows no warning or errors after running all tools (twice). I have no idea why it's having submission problems. Removed the quotes in the exposure label Assigned ID: 133 ----- Submission 1 (Thu Jan 26 20:41:02 GMT 2006) ----- Phase I Proposal 133 (imageDLA) successfully submitted. Imaging the Nearest Damped Lyman Alpha Absorbers We propose to acquire broad-band and H-alpha imaging of three bright, very nearby host galaxies for damped Ly-alpha absorbers (DLAs). Our targets are the only DLA hosts at z < 0.03 (i.e., spatial resolutions of < 1.2 kpc). The purpose of these observations is to discover the detailed morphology and kinematics and thus the origins of the gas giving rise to DLAs. While ground-based spectroscopy of DLAs is used to infer indirectly the evolution of galaxy metallicity and thick disk kinematics out to z > 4, only with HST imaging of the very lowest redshift DLA galaxies can we discover these relationships directly. In conjunction with H I 21-cm VLA emission maps, broad-band and H-alpha images of these DLAs will allow us to determine: (1) the sites of active star formation in the host galaxies and their relationship to the QSO sightline, (2) the presence of stellar streams, supernova shells, or bipolar "superwind" outflows in DLA host galaxies, and (3) the detailed spiral structure of the host galaxies, which will allow us to use the lower resolution H I 21-cm emission line images to determine unambiguous DLA kinematics with respect to the host galaxy (i.e., is the DLA rotating with the disk?). Thus, the high resolution imaging will allow us to correctly interpret the kinematics and metallicity information provided by the H I 21-cm VLA maps and HST UV spectroscopy to better inform the high-z results.
This program requires broadband and Halpha imaging of 3 bright nearby (V < 15:5; z < 0:03) galaxies. Whenever possible, we will use ACS/WFC for these observations in order to take advantage of the higher throughput and resolution of ACS as compared to WFPC2, as well as its larger FOV. We will CR-SPLIT and dither all broadband observations to more efficiently reject cosmic rays and improve sub-pixel resolution, but the narrowband observations will not be CR-SPLIT to minimize read-noise. Halpha imaging of our closest target, NGC3067 (cz=1465 km/s), will be acquired using ACS/WFC with the F660N filter. Two orbits will be required for H imaging of this target and one orbit for the broadband (1500 s each in F435W and F775W). This total Halpha integration time of 2 orbits will allow us to reach comparable depth to the Cecil et al. (2001) F658N image of NGC3079, whose Halpha integration time was 4 orbits with WFPC2. Thus, if the same ?superbubble? structures are present in NGC3067 as in NGC3079, we expect to detect them easily with the proposed images. Unfortunately, there is no narrowband filter in either ACS or WFPC2 that will allow us to image Halpha at its redshifted wavelength of 6680A for ESO1327?2041 (cz=5370 km/s); therefore, we will observe ESO 1327?2041 in 3 broadband filters (F435W, F625W, F775W) with ACS/WFC. Five orbits will be required for this broadband imaging (1 orbit in F435W and 2 orbits each in F625W and F775W) so that emission line gas present in the difference image (F625W-F775W) is detected with signal-to-noise >15 per resolution element. This signal-to-noise limit will allow us to clearly detect emission line filaments in the difference image and measure their surface brightness distribution. Ground-based H imaging at 1-arcsec resolution will be used to isolate the regions where H emission is expected in the HST images. Halpha imaging of our last target, Klemola 31A (cz=8605 km/s), will be obtained with WFPC2 and the F673N filter. We will also acquire a broadband F791W image for continuum subtraction and a broadband F439W image to locate the sites of active star formation in this galaxy. A total of five orbits will be required for this target, one orbit each for the F439W and F791W images and three orbits for Halpha. These integration times will allow us to detect unresolved H II regions with L(Halpha)>10^37 ergs/s and perform accurate (<0.1 mag) photometry on individual H II regionswith L(Halpha)>6x10^37 ergs/s, corresponding to a star formation rate of >0.001 M/yr. While the detectability of an individual filamentary structure depends critically on its geometry and spatial extent, these exposure times have been computed assuming a geometry intermediate between well-resolved at all redshifts (i.e., constant surface brightness for z<<1) and unresolved at all redshifts (surface brightness propto 1/r^2). Thus, we request a total of 13 orbits of ACS and WFPC2 imaging for our three target galaxies. QUASAR ABSORPTION LINES AND IGM 12 false 0 0.0 0 false false false false false false SUPPORTED GALAXY HALO LYMAN ALPHA CLOUD This object was generated by the targetselector and retrieved from the NED database. J2000 09 58 21.0000 +32 22 12.00 J2000 GALAXY HALO LYMAN ALPHA CLOUD SPIRAL This object was generated by the targetselector and retrieved from the NED database. J2000 13 30 5.3000 -20 55 59.00 J2000 GALAXY HALO LYMAN ALPHA CLOUD SPIRAL This object was generated by the targetselector and retrieved from the NED database. J2000 20 23 45.2000 -36 55 6.00 J2000 ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F660N ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W WFPC2 Imaging No F439W WFPC2 Imaging No F673N WFPC2 Imaging No F791W POS-TARG DITHER 2.121 15 WF pixel shift in both x and y LINE false false 2 45 LINE 1 false POS-TARG DITHER 2.121 15 WF pixel shift in both x and y LINE false false 3 45 LINE 2 false NGC3067 Continuum Obs (now WFPC2) (Tic-Visit :proposal-id 10925 :visit-id "01" :proposal-version -1 :trans-version "20070108" :date "13-Mar-2007 12:49:32.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 537792 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10925 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10925 :visit-id "01" :orbit-number 1 :pcs-time 355 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