0 Assigned ID: 356 ----- Attempting Submission 1 (Fri Apr 11 04:09:06 GMT 2014) ----- HST Phase I Proposal 356 (Tadpoles2014.apt) successfully submitted. ----- Attempting Submission 2 (Fri Apr 11 15:00:11 GMT 2014) ----- This is a single small head-tail galaxy with an expectation of diffuse Halpha emission coming from the north east intergalactic region, away from the main galaxy image but still in the field of view. Therefore we center the F657N filter in chip 1 and do a GAP-LINE pattern to fill in the chip gap and add an additional 2 point dither (4 exposures total) for cosmic rays and PSF purposes. This leaves chip 2 available to see the expected diffuse emission from that position off the galaxy. The two UV filters, F225W and F336W, are put in chip 2 because that is more sensitive in the UV. They are long exposures with 4 point dithers (dither box) to get a nice PSF. The other 4 filters (F438W, F547M, F606W, F814W) are given a "dither line" for cosmic ray purposes and the galaxies are centered on chip 2 with the gap pretty far away and not in an interesting place for these filters. Thus only the Ha+NII filter is given a GAP dither to fill in the GAP. The spectrum for F657N uses Orion II in the ETC because I got an error message for Orion I that the filter did not cover the same region as the spectrum, which seems not true. The S/N is high but that is for a fairly bright region and there are fainter regions we are interested in too. All ETC calculations include enough post flash electrons to bring the total electrons to just over 12. -1683586690 ----- Attempting Submission 1 (Thu Jul 24 03:28:17 GMT 2014) ----- We propose WFC3 broadband and Halpha observations of a local tadpole galaxy with a starburst and low metallicity in the head suggestive of ram pressure triggering from cosmological inflow. Such head-tail structure dominates local ultra-low metallicity Blue Compact Dwarfs and it represents 10% of resolved galaxies in the Hubble UDF. We will identify star clusters and measure their properties, including masses and ages, two-point correlations for position as a function of mass and age, and the cluster mass distribution as a function of age. We will also determine the star formation fraction in clusters. These measurements can suggest definite processes for star formation including the importance of turbulent fragmentation. The presence of a super star cluster, if found, will be a model for the formation of metal-poor globular clusters in high redshift dwarf galaxies, which could have formed in similar conditions. The Halpha observations will also show bright rims and nebular structures down to 10's of pc scales. Such structures can indicate pressure sources and nebular flow directions that allow us to understand gas motions inside the starburst head, including pressurized outflows and cosmological inflows. The head is so bright in Halpha that even if only 25% of the ionizing radiation escapes, an inflowing halo stream as far away as 1' will be ionized sufficiently on the surface for our observations to detect it. Thus the proposed galaxy, Kiso 5639, is a prime laboratory to study processes that may be related to cosmic accretion, starburst conditions in primitive galaxies, and the formation of metal-poor globular clusters. We will observe one source in two visits with seven total filters: FEC#/UVIS: F225W, F336W, F438W, F547M, F606W F814W and F657N This is an observation of an elongated galaxy with a bright region at one end. We call this bright region the head and the fainter rest of the galaxy, the tail. We expect Halpha emission from a region to the side of the galaxy, just off the bright head part. We expect there to be accreting cosmic gas at this place, and so bright emission of Halpha from the accreting gas. There is also a bright star near the galaxy which we don't care about but which needs to be placed so that neither the diffraction spikes nor the channel leakage will cross the galaxy image. Our constraints therefore are as follows: Visit 1: The uv observations with filters F225W F336W should place the galaxy on chip 2, which is the most sensitive chip for FUV. These filters will be observed with one orbit for each filter and two orbits total in this visit. Visit 2: The other observations can be on chip 1 and in particular, the Halpha observation with F657N, should be on chip 1 so that there is area available near the head part of the galaxy still on chip 2 to see the expected emission there. These filters will be observed with one orbit for F438W and F547M, another orbit for F606W and F814W, and a third orbit for F657N. There are 3 orbits total in this visit. The galaxy should be placed on chips 2 (Visit 1) and 1 (Visit 2), respectively, so that there are at least 2 guide stars in the guide star field of views. This requires the galaxy to be slightly offset from the center of the chip in each case. The orientation of the satellite should be such that the diffraction spikes from the nearby bright star and the channel leakage from the nearby bright star do not cross the galaxy image in any filter. These constrains require two visits, as indicated, and therefore it requires time removed from the beginning of the second visit, which is when filters F437W and F537W will be observed, in order to find the guide stars for a second time. The dithering strategy is as follows: For the FUV filters, F225W and F336W, we will dither in a box "Dither Box" without requiring that the chip gap be filled in. The galaxy avoids the chip gap so this filling in is not necessary. For the next 4 filters: F438W, F547M, F606W, and F814W, the exposure times are shorter for each filter and we will dither with 2 pointings "Dither Line". We cannot dither with more pointings because then the data dump cuts into the observing time. For the 7th filter, F657N, we need to fill in the chip gap since we are looking for extended emission in this region. Thus we want the "Gap Line" dithering pattern, which has 2 pointing with one point on each side of the gap spacing. ISM IN EXTERNAL GALAXIES Default false false false false false SUPPORTED GALAXY AMORPHOUS IRREGULAR IONIZATION FRONT STAR FORMING REGION STARBURST This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY AMORPHOUS IRREGULAR IONIZATION FRONT STAR FORMING REGION STARBURST This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F657N POS-TARG MOSAIC DITHER 2 2.414 WFC3-UVIS-DITHER-LINE false true 0.145 2 85.759 POS-TARG WFC3-UVIS-GAP-LINE 46.84 4 true POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 5 false POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 6 false 1411650277753 /Users/cmannfolk/Desktop/OP-cache/13723_edit-v01.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13723 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "25-Sep-2014 09:04:37.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2310000 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13723 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13723 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2921 :al-overhead-at-end 123 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13723 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3034 :al-overhead-at-end 122 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 2 0 1411650286086 /Users/cmannfolk/Desktop/OP-cache/13723_edit-v02.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13723 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "25-Sep-2014 09:04:45.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3465008 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13723 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13723 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2921 :al-overhead-at-end 119 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13723 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13723 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3034 :al-overhead-at-end 122 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 3 0