removed the on hold to make it more flexible 1015767389 ----- Attempting Submission 4 (Fri Apr 19 08:35:25 GMT 2013) ----- ----- Attempting Submission 5 (Wed Jun 12 17:25:03 GMT 2013) ----- Warnings refer to Visit 02, which has already been executed. Escape of Lyman photons from Tololo 1247-232 Tololo 1247-232 is a unique galaxy in the local universe in that it is the best Lyman continuum emitter candidate in the whole FUSE archive. Moreover, it has an unusually blue continuum in the spectral region just longwards of the Lyman limit, and it is a bright Lyman alpha emitter. Hence, this galaxy has an enourmous potential as an astrophysical laboratory where the fate and transport of ionizing and Hydrogen recombination line photons can be studied in detail. To substantiate these findings, HST follow up with COS spectroscopy, and imaging, is required. We propose to map the far UV morphology with ACS/SBC. By adding observations with WFC3/UVIS we can in addition map the near UV spectral slope, Lyman alpha, Halpha and Hbeta at HST resolution. We will use this information to properly position the COS aperture and the images will also be vital for the analysis of the COS spectra themselves. First the target should be imaged with ACS/SBC and WFC3/UVIS in a total of 7 filter settings. These images will be analysed in a timely manner to select the optimum pointing for the COS spectroscopy that will follow. For each imaging filter observation there will be 2 exposures with small POS-TARG shifts in between. The SBC imaging is straightforward and suses the sequence F140LP - F125LP - F125LP - F140LP in order to have the F125LP observations done in the shadow part of the orbit. In order to lower the dark current, the SBC should preferably not have been used in the preceeding visit (by another program). The target galaxy has a small angular size, approx 10 arcsec. In order to mitigate CTE effects the WFC3 imaging has therefore been designed to put the galaxy approx 20 arcsec from the readout of UVIS ccd 1. For the quad-filter images, this has been done by using the the FIX QUAD aperture followed by a small pos-targ. Due to the confused bandpass in the quadrant interfaces we here put the target at slightly higher y-coordinate. For the other filters we have selected the UVIS aperture which put the target approx 10 arcsec above the CCD1 readout, followed by a pos-targ of 10 arcsec in the Y-director to get the target at a more comfortable distance from the chip boundary. All WFC3 imaging has two filters per bandpass that are offset by 2.95 and 3.15 arcsec in X and Y, respetively, to dither over possible droplets. To further mitigate the CTE effects in the UVIS observations where all exposures are expected to have low background levels as judged by the ETC, we have inserted a postflash of 10 electrons. The COS spectroscopy will be performed with the G130M grating in two different wavelength regions, the first sampling the Lyman continuum and the second Lyman alpha as well as ISM absorption lines. Moreover, the COS spectroscopy will be obtained at 2 different orientations offsett by approximately 90 degrees to allow extraction of spatial information. The COS visits included in this version of the phase 2 file examples of what they may look like, but will be reworked once the imaging data has been processed. The COS visits have been put on hold for the execution of the SBC and UVIS imaging visits. NA NA ISM IN EXTERNAL GALAXIES 12 false false 0.0 0.0 false false false SUPPORTED GALAXY STARBURST This object was generated by the targetselector and retrieved from the NED database. J2000 J2000 GALAXY STARBURST This object was duplicated from Object 1, with coordinates modified based upon the 2MASS point source catelogue, for precise acquisition with the COS. Old coordinates from Target Selector : 12 50 18.9000, -23 33 57.60 New coordinates from 2MASS : 12 50 18.9019, -23 33 57.39 The difference is just 0.21 arcsec. J2000 J2000 ACS/SBC Imaging No No F125LP ACS/SBC Imaging No No F140LP WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F775W WFC3/UVIS Imaging No No F680N WFC3/UVIS Imaging No No FQ508N COS/FUV Spectroscopic No No G130M 1055 COS/FUV Spectroscopic No No G130M 1327 Timing link suitability includes constraints ([01 After 02 by 21.0 to 50.0 days]) The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. In order to minimize the dark current, this visit should not be scheduled immediately after another visit that uses SBC. 1363940538000 333.2612367380233 (Tic-Visit :proposal-id 13027 :visit-id "01" :proposal-version -1 :trans-version "20121031" :date "19-Apr-2013 10:33:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "28" :si-bright-earth-limb-angle 20.0 :data-volume 74064 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13027 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13027 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2682 :al-overhead-at-end 0 :internal-dur-at-end 117 :dark-offset 685 :dark-utilization 1331 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([01 After 02 by 21.0 to 50.0 days]) The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. 1359857801000 302.0187239065204 (Tic-Visit :proposal-id 13027 :visit-id "02" :proposal-version -1 :trans-version "20121031" :date "19-Apr-2013 10:33:17.0" :trans-errors '(:WARNINGS 1 :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 2887504 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13027 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13027 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2682 :al-overhead-at-end 122 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13027 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2799 :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 3015 :pcs-gap 0 ) true 2 1 Timing link suitability includes constraints ([12 After 11 by at least 60.0 days]) The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. First COS visit, 2 orbits, first ORIENT angle This visit must be executed BEFORE visit 12. The target is two star clusters, which are aligned ~0.3 arcsec N-S of each other. Both fit in the aperture and both are bright. In order to possibly extract them independently, and to work at the maximal spectral resolution even if we cannot, we would like to align the XDISP axis of COS in the N-S direction. Or P.A.=0=180. According to the PII instructions, table 7.4, the +Y (XDISP) axis is offset 135 degrees from the U3 axis, and the caption states that we should add this to the P.A. on sky. Thus we want to align the U3 axis at +135 (or 315 ) degrees. We then add a +- 20 degree tolerance upon this, giving a 40 degree allowed range. 1369855820000 115.0 (Tic-Visit :proposal-id 13027 :visit-id "11" :proposal-version -1 :trans-version "20121031" :date "19-Apr-2013 10:27:11.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 87168 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13027 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13027 :visit-id "11" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2640 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13027 :visit-id "11" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2793 :al-overhead-at-end 0 :internal-dur-at-end 376 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 2 0 In the ETC Run, the aim is to reach S/N>40 in the brightest star-cluster. This flux has been estimated by full multiband photometry with ACS/SBC and WFC3/UVIS, in 0.2 arcsec (radius) with quoted aperture corrections applied. Thus it is *NOT* the same spectrum as used for observtations LyC1-LyC4, which use photometry performed inside the full COS aperture (R=1.25 arcsec). Standard NUV image acquisiton with MIRRORB. Coordinates are well known (<0.4 arcsec) from 2MASS point-source catalogue, GSC2.3, and even 6dFGS. All these are consistent within 0.2 arcsec which agree (also within 0.2 arcsec) with the NED coordinates used with the targetselector for the ACS/SBC and WFC3/UVIS visits. Acquisition is with MIRRORB, since the predicted countrate is very close to the 50 e-/sec BOP limit with MIRROR A. The spectrum uploaded for the ETC Run is based upon full multiband photometry in ACS/SBC and WFC3/UVIS, and a fit to the SED. The aperture was a circle of 1.25 arcsec radius, centred upon the brightest cluster (at 1500 AA). Thus it is NOT the same as the spectrum used for the NUV Acquisition observation, which is based upon small aperture photometry of the individual clusters. Observations LyC1 and LyC2 have somewhat shorter Exposure than LyC3 and LyC4. Sequentially, observations increment the FP-POS setting by 1. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. The spectrum uploaded for the ETC Run is based upon full multiband photometry in ACS/SBC and WFC3/UVIS, and a fit to the SED. The aperture was a circle of 1.25 arcsec radius, centred upon the brightest cluster (at 1500 AA). Thus it is NOT the same as the spectrum used for the NUV Acquisition observation, which is based upon small aperture photometry of the individual clusters. Observations LyC1 and LyC2 have somewhat shorter Exposure than LyC3 and LyC4. Sequentially, observations increment the FP-POS setting by 1. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. The spectrum uploaded for the ETC Run is based upon full multiband photometry in ACS/SBC and WFC3/UVIS, and a fit to the SED. The aperture was a circle of 1.25 arcsec radius, centred upon the brightest cluster (at 1500 AA). Thus it is NOT the same as the spectrum used for the NUV Acquisition observation, which is based upon small aperture photometry of the individual clusters. Observations LyC1 and LyC2 have somewhat shorter Exposure than LyC3 and LyC4. Sequentially, observations increment the FP-POS setting by 1. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. The spectrum uploaded for the ETC Run is based upon full multiband photometry in ACS/SBC and WFC3/UVIS, and a fit to the SED. The aperture was a circle of 1.25 arcsec radius, centred upon the brightest cluster (at 1500 AA). Thus it is NOT the same as the spectrum used for the NUV Acquisition observation, which is based upon small aperture photometry of the individual clusters. Observations LyC1 and LyC2 have somewhat shorter Exposure than LyC3 and LyC4. Sequentially, observations increment the FP-POS setting by 1. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. Timing link suitability includes constraints ([12 After 11 by at least 60.0 days]) The scheduling data was generated by CASM 21.0. CASM was run in Phase II mode. Second COS visit, 3 orbits, same ORIENT angle This visit must be executed AFTER visit 11. The target is two star clusters, which are aligned ~0.3 arcsec N-S of each other. Both fit in the aperture and both are bright. In order to possibly extract them independently, and to work at the maximal spectral resolution even if we cannot, we would like to align the XDISP axis of COS in the N-S direction. Or P.A.=0=180. According to the PII instructions, table 7.4, the +Y (XDISP) axis is offset 135 degrees from the U3 axis, and the caption states that we should add this to the P.A. on sky. Thus we want to align the U3 axis at +135 (or 315 ) degrees. We then add a +- 20 degree tolerance upon this, giving a 40 degree allowed range. (Tic-Visit :proposal-id 13027 :visit-id "12" :proposal-version -1 :trans-version "20121031" :date "19-Apr-2013 10:27:00.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 191616 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13027 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13027 :visit-id "12" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2640 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13027 :visit-id "12" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2793 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13027 :visit-id "12" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2788 :al-overhead-at-end 0 :internal-dur-at-end 385 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 3 0 In the ETC Run, the aim is to reach S/N>40 in the brightest star-cluster. This flux has been estimated by full multiband photometry with ACS/SBC and WFC3/UVIS, in 0.2 arcsec (radius) with quoted aperture corrections. Thus it is *NOT* the same spectrum as used for observtations LyC1-LyC4, which use photometry performed inside the full COS aperture (R=1.25 arcsec). Standard NUV acquisiton with MIRRORB. Coordinates are well known (<0.4 arcsec) from 2MASS point-source catalogue, GSC2.3, and even 6dFGS. All these are consistent within 0.2 arcsec which agree (also within 0.2 arcsec) with the NED coordinates used with the targetselector for the ACS/SBC and WFC3/UVIS visiits. Acquisition is with MIRRORB, since the predicted countrate is very close to to the 50 e-/sec BOP limit. The spectrum uploaded for the ETC Run is based upon full multiband photometry in ACS/SBC and WFC3/UVIS, and a fit to the SED. The aperture was a circle of 1.25 arcsec radius, centred upon the brightest cluster (at 1500 AA). Thus it is NOT the same as the spectrum used for the NUV Acquisition observation, which is based upon small aperture photometry of the individual clusters. Observations LyC1 and LyC2 have somewhat shorter Exposure than LyC3 and LyC4. Subseqeunt observations increment the FP-POS setting by 1. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. For the ETC Run, the same spectrum as for the LyC runs is used, but with the 1327 setting and the central wavelength changed to 1275AA. All observations are the same length, and aim simply to iterate over all four FP-POS settings. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. For the ETC Run, the same spectrum as for the LyC runs is used, but with the 1327 setting and the central wavelength changed to 1275AA. All observations are the same length, and aim simply to iterate over all four FP-POS settings. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. For the ETC Run, the same spectrum as for the LyC runs is used, but with the 1327 setting and the central wavelength changed to 1275AA. All observations are the same length, and aim simply to iterate over all four FP-POS settings. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases. For the ETC Run, the same spectrum as for the LyC runs is used, but with the 1327 setting and the central wavelength changed to 1275AA. All observations are the same length, and aim simply to iterate over all four FP-POS settings. Buffer time is set to 2/3 the BT output by the ETC. We notice that when setting BT to Exposure Time, the overhead increases.