0Assigned ID: 439
----- Attempting Submission 1 (Fri Apr 11 12:23:58 GMT 2014) -----
HST Phase I Proposal 439 (sin1.apt) successfully submitted.0The Stellar Continuum Light from Damped Lyman-alpha Absorber Galaxies Detected with Integral Field SpectroscopyA new challenge in galaxy evolution studies is to understand how gas flows in and out of galaxies through their circumgalactic medium (CGM). The best way to tackle this is to bring together data on cold gas, metals and stellar content of the same galaxies. Galaxies selected via the absorption they produce in the spectra of background quasars are a powerful tool to study the cold gas play a crucial role in this respect, but characterising the stellar content of these absorbers has proved to be challenging until now. Our group has used 3D spectroscopy at near-infrared wavelengths made possible by the SINFONI instrument on VLT, aided with adaptive optics (AO), to successfully detect 5 galaxies responsible for DLAs/sub-DLAs. For this sample, we have retrieved and analyzed data from HST/STIS (for the neutral gas content), VLT/UVES, Keck/HIRES or Magellan/MIKE (for the metallicity and dust content of H I gas), VLT/SINFONI (for SFR and kinematics of H II gas) and VLT/X-Shooter (for metallicity of H II gas). However, none of the data currently in hand can probe the faint optical continuum of these objects. Here we propose to observe these DLA/sub-DLA galaxies at z~1-2 using WFC3/UVIS and IR channels, to characterize the stellar content (extinction, stellar mass, age) and environment. The proposed observations will allow us to better probe the flow of gas around these galaxies, directly testing models of cold gas accretion from filaments and thus current theories of galaxy formation and evolution.This proposal is aiming at detecting the continuum of faint Damped Lyman Alpha (DLA)-galaxies next to bright background quasars. We propose to obtain UVIS/F606W, IR/F105W and IR/F160W images of the DLA galaxies using the WFC3 optical and IR channels. We choose WFC3 UVIS channel to get a higher spatial resolution (by 20 %) over ACS WFC and higher throughput over ACS HRC. The high spatial resolution and stable PSF of the proposed WFC3 images will allow us to probe the absorbing galaxies at small impact parameters from the bright, background quasars, to resolve the two separate components in the case of Q0302 (<1") and to obtain accurate measurements of faint galaxy fluxes. Note that although, we have accurate flux determination in H-alpha for each target, we do not know their broad-band magnitudes since their continuum are not detected in either our VLT/SINFONI or VLT/X-Shooter observations.
For UVIS, we use the F606W filter to sample the blue end of the redshifted 4000-A break unless the equivalent is available in the archive. For IR, we request the F105W and F160W filters unless these are available in the archives (see Table 1 of the Phase 1 of the proposal). Priority should be given to the two systems where no information is currently available (Q1009 and Q2352).
We use a dithering pattern to help with removal of cosmic rays and hot pixels. The UVIS observation is taken using the WFC3-UVIS-DITHER-BOX pattern. The two observations with the IR detector are taken using the WFC3-IR-DITHER-BOX-MIN pattern providing an optimal 4-point sampling of the PSF. Our observations have no special scheduling constraints.
We aim at making sure that the faint DLA-galaxy falls in between the WFC3 diffraction spikes at 45 degrees and to avoid any possible bleeding of flux (from the bright quasar) on to the faint galaxy. Since flux bleeds along the detector-columns, aligning the CCD rows of UVIS (the X-axis in case of the IR) with the line joining the galaxy and the quasar would prevent flux-bleeding on to our target galaxy. Thus our orient ranges should ensure that: (1) the diffraction spikes are away from the galaxy-quasar line (preferably by ~45 degrees) and (2) The CCD rows (the X-axis) of UVIS (IR) are parallel with the galaxy-quasar line. In our calculations, the angles are measured from North and the we adopt the convention that angle is positive when measured in the counter-clockwise direction.
Q1009: PA = -85 degrees from North
For, UVIS observations, we want the CCD rows to align with the line joining the target galaxy and the bright quasar (i.e., the CCD rows should make an angle same as PA with North). From Table 7.4, the offset angle between UVIS CCD row and +U3 axis is 221.38 degress.
Therefore, +U3 will be making an angle -85+221.38 degrees = +136.38 degrees with North. With this orientation, the angle between the +V3/-V3 (-U3/+U3) axis and the galaxy-quasar line will be 41.38 degrees. The +V2/-V2 axis will make an angle of 48.62 degrees with this line. Thus, the diffraction spikes should be away from the target galaxy.
Therefore, for UVIS observations of Q1009, including +/- 5 degrees variance, ORIENT range should be: +131.38 to +141.38 degrees from North (and, with 180 degrees rotation, +311.38 to +321.38 degrees from North). However, for increase schedulability, we set the final orientation requirements to +130.38 to +142.38; +310.38 to +322.38.
For, IR observations, the X-axis needs to be aligned with the line joining the galaxy and quasar. Therefore, from Table 7.4, +U3 should be at -85+225.18 = +140.18 degrees from North. The angle between the galaxy-quasar line and the +V3/-V3 axis will be 45.18 degrees while the angle between the galaxy-quasar line and the V2/-V2 axis is 44.82 degrees (the spikes should be where we want them to be relative to the galaxy-quasar line).
Therefore, for IR observations of Q1009, including +/- 5 degrees variance, ORIENT range should be: +135.18 to +145.18 degrees from North (and, with 180 degrees rotation, +315.18 to +325.18 degrees from North).
Similarly, for Q2352, PA = +90 degrees from North
UVIS: (+U3 makes 90+221.38 = +311.38 degrees from North) ORIENT range: +306.38 to +316.38 degrees from North (and, with 180 degrees rotation,+126.38 to +136.38 degrees from North). However, this ORIENT range makes observations unschedulable. We, therefore are forced to relax the constraints and widen the ORIENT range to +271.38 to +351.38 degrees from North (and, with 180 degrees rotation, +91.38 to +171.38 degrees from North).
IR: (+U3 makes 90+225.18 = +315.18 degrees from North) ORIENT range: +310.18 to +320.18 degrees from North (and, with 180 degrees rotation, +130.18 to +140.18 degrees from North). However, this ORIENT range makes observations unschedulable. We, therefore are forced to relax the constraints and widen the ORIENT range to +275.18 to +355.18 degrees from North (and, with 180 degrees rotation, +95.18 to +175.18 degrees from North).
For Q0452, PA = -5 degrees from North
UVIS: (+U3 makes -5+221.38 = +216.38 degrees from North) ORIENT range: +211.38 to +221.38 degrees from North (and, with 180 degrees rotation, +31.38 to +41.38 degrees from North).
IR: (+U3 makes -5+225.18 = +220.18 degrees from North) ORIENT range: +215.18 to +225.18 degrees from North (and, with 180 degrees rotation, +35.18 to +45.18 degrees from North).
For Q0302, PA = +10 degrees from North
IR: (+U3 makes 10+225.18 = +235.18 degrees from North) ORIENT range: +230.18 to +240.18 degrees from North (and, with 180 degrees rotation, +50.18 to +60.18 degrees from North). However, for increase schedulability, we set the final orientation requirements to +40.18 to +70.18; +220.18 to +250.18.
-------- Realtime Justification --------
NA
------ Calibration Justification -------
NAQUASAR ABSORPTION LINES AND IGM12falsefalse0.00.0falsefalsefalseSUPPORTEDGALAXYQSOThe science goal is to observe the faint DLA-galaxy at z=0.887 with flux F(H-alpha)=17.1x10^17 erg/s/cm^2. The coordinates of the target entered are for the bright quasar next to it with V mag=17.43J2000J2000GALAXYQSOThe science goal is to observe the faint DLA-galaxy at z=1.032 with flux F(H-alpha)=4.9x10^17 erg/s/cm^2. The coordinates of the target entered are for the bright quasar next to it with V mag=18.41J2000J2000GALAXYQSOThe science goal is to observe the faint DLA-galaxy at z=1.007 with flux F(H-alpha)=14.5x10^17 erg/s/cm^2. The coordinates of the target entered are for the bright quasar next to it with V mag=17.00J2000J2000GALAXYQSOThe science goal is to observe the faint DLA-galaxy at z=1.009 with flux F(H-alpha)=7.7x10^17 erg/s/cm^2. The coordinates of the target entered are for the bright quasar next to it with V mag=16.40J2000J2000WFC3/UVISImagingNoNoF606WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF105WWFC3/UVISImagingNoNoF606WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF105WWFC3/UVISImagingNoNoF606WWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF105WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falsePOS-TARGDITHER0.572LINE0.365falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN2falseThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.The orientation requirements are set to avoid the faint DLA-galaxy target to fall on the diffraction spikes of the bright background quasar PSF. The target is at a PA of -85 degrees EofN.(Tic-Visit
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