Assigned ID: 356
----- Attempting Submission 1 (Fri Feb 25 13:56:41 GMT 2011) -----I have one worry with my submission namely that I could not find a solution where visit 4 was exectuted with a 180 degrees
rotation relative to visit 3. If such a solution exist (while still keeping the target between the diffraction spikes of the PSF) I
would be very grateful to know and modify accordingly.----- Attempting Submission 1 (Thu Jun 30 13:32:17 GMT 2011) -----Detecting the stellar continuum of the galaxy counterparts of three z>2 Damped Lyman-alpha AbsorbersDespite more than 20 years of study the Damped Lyman-alpha Absorbers (DLAs) have not yet found their place in the puzzle of galaxy formation and evolution. In particular, the nature of the DLA galaxy counterparts remain very poorly constrained even after substantial amounts of observing time both with HST and 8-m class telescopes. The reason for this is now understood: DLAs are due to their HI cross-section selection drawn from the faint end of the luminosity function. However, we have found evidence that DLAs fullfil luminosity-metallicity and mass-metallicity relations similar to local relations. We have therefore initiated a survey of the galaxy counterparts of metal rich Damped Lyman-alpha Absorbers at redshifts around 2.5 using the newly commissioned X-shooter spectrograph at the ESO Very Large Telescope. For the first 6 targets in the survey we have detected Lyman-alpha, [OIII] and/or H-alpha emission from three of the DLA absorbers. We here proposed to characterize the stellar content of the galaxy counterparts (age, extinction, morphology) and compare these properties with similar properties of emission selected galaxies at similar redshifts. This will be an important step in finding the proper place for DLAs in the puzzle of galaxy formation.The purpose of the observation is to detect galaxy counterparts of Damped Lyman-alpha Absorbers close to QSO sightlines. The challenge is to design the observation such that the PSF of the background QSO can be optimally subtracted. In order to optimize the PSF subtraction I rotate the field to place the position of the DLA galaxy between the diffraction spikes of the PSF. I follow the calculation in Fig. 7.1 in the Phase II proposal instructions for cycle 19:
Q2222-0946 (visits 1, 5 and 6): PA = 45 degrees EofN (impact parameter 0.8 arcsec). Hence, ORIENT should be 221.38 + 45. = 266.38 degrees.
Allow a +/- 5 degree range and also a 180 degree rotation.
261.38 to 271.38 degrees or 81.38 to 91.38 degrees
For IR add 4.8 degrees:
266.18 to 276.18 or 86.18 to 96.18 degrees
Q0918+1636 (visits 2, 7 and 8) : PA = 246 degrees EofN (impact parameter 2.0 arcec). Equivalent to 66 degrees EofN. Hence, ORIENT should be 221.38 + 66. = 287.38 degrees.
Allow a +/- 5 degree range and also a 180 degree rotation.
282.38 to 292.38 or 102.38 to 122.38 degrees.
For IR add 4.8 degrees: 287.18 to 297.18 or 107.18 to 117.18 degrees.
Q0338-0005 (visits 3 and 4): PA = -30.+/-10. degrees EofN (impact parameter 0.5 arcsec). Hence, ORIENT should be 221.38 - 30. = 191.38 degrees.
Allow a +/- 5 degree range and also a 180 degree rotation.
186.38 to 196.38 or 6.38 to 16.38 degrees.
For this target we only do UVIS. I would have preferred if visits 3 and 4 could have orientations rotated by 180 degree relative to eachother, but there seems to be no visibility if I rotate visit 4 by 180 degrees relative to visit 3.
Furthermore, to improve the sampling of the PSF we will use a four-point, half-pixel shift dither pattern for each visit.NANAQUASAR ABSORPTION LINES AND IGM12false0.00.0falsefalsefalsefalseSUPPORTEDGALAXYQSOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYQSOJ2000J2000GALAXYQSOJ2000J2000WFC3/UVISImagingNoNoF606WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF160WWFC3/UVISImagingNoNoF606WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF160WWFC3/UVISImagingNoNoF606WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falsePOS-TARGDITHER0.572LINE0.365falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN2falseThe scheduling data was generated by CASM 19.3.CASM was run in Phase II mode./private/var/folders/LL/LLompMhAGQmLL5AeTDWQK+++98Q/-Tmp-/OPVisit1773400323143956102.xmlI plan to place the target between the diffraction spikes (the two horisontal holes to also avoid troubles with bleeding cf. Fig. 7.1 in the Phase II instructions). The target is at a PA of 45. degrees EofN.(Tic-Visit
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