0Assigned ID: 1344
----- Attempting Submission 1 (Wed Feb 01 00:55:34 GMT 2017) -----
HST Phase I Proposal 1344 (tol1214.apt) successfully submitted.
Receipt: # 1344-1
----- Attempting Submission 2 (Wed Feb 01 01:28:53 GMT 2017) -----
HST Phase I Proposal 1344 (tol1214.apt) successfully submitted.
Receipt: # 1344-2POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.Tthe COS visit has been put on hold, with the intention to use the WFC3 and SBC images
for optimizing the target acquisition.
The APT is generating some warnings:
-For WFC3 it warns about the use pos targs for Quad filter observations. These pos targs are just small
movements to dither across detector artifacts.
-It did warns about the flash levels in some cases, but these we have verified against the ETC.
changes 19 april:
changed pos-targs, and updated FLASH levels. Corrected one error in filter selection.
22 april
slight changes to WFC3 orbit, pos-targ values
put in 0 explicitly in v.1, exp. 13
5 june
refined coordinates for COS visit (that was put on hold) with acquisition based on on UV imaging from visits 1 and 2.
changed visit number from 04 back to 031996152731----- Attempting Submission 1 (Tue Mar 28 14:57:20 GMT 2017) -----
HST Phase II Proposal 14923 (tol1214.apt) successfully submitted.
Receipt: # 14923-1
----- Attempting Submission 2 (Thu Mar 30 10:03:33 GMT 2017) -----
HST Phase II Proposal 14923 (tol1214.apt) successfully submitted.
Receipt: # 14923-2
----- Attempting Submission 4 (Wed Apr 19 15:22:21 GMT 2017) -----
----- Attempting Submission 5 (Fri Apr 21 22:46:58 GMT 2017) -----
----- Attempting Submission 6 (Mon Apr 24 17:09:03 GMT 2017) -----
----- Attempting Submission 7 (Sun Jun 04 23:43:59 GMT 2017) -----
----- Attempting Submission 8 (Mon Jun 05 13:12:35 GMT 2017) -----The list of Investigators does not match the STScI records for this program:
-We added collaborator Gneva Micheva from UMich. If this poses a problem, we will remove her, as she can still join us in the analysis.
SAME POS MAY NOT BE APPROPRIATE:
Applies to: #<exposure 009>
-This is to ensure the same pointing as for the preceeding observation that uses the QUAD-FIX aperture. Since exposure 9 uses full
UVIS field there is no risk it will miss the target.
Applies to: #<exposure 010>
- same explanation as for exposure 9
Warning (Form): POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field
of view or moving it to another quadrant.
- Indeed, we u only adopt a small shift (2.5 & 1.5 arcsec). The target is smaller than the QUAD aperture and will not be vignetted.
Warning (Form): If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
- as explained in the phase 2 file we propose to put the COS visit on hold until the UVIS and SBC data has been obtained.
Warning (Orbit Planner): REFERENCE-FRAME MUST BE ICRS OR GSC1 FOR SMALL APERTURE
- Once the WFC3/UVIS and ACS/SBC imaging is in hand we will use the astrometry of these frames and update the coordinates.
Warning (Form): COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
- We are aware of the limitationsLYCAT - LYman Continuum and Alpha in Tol1214-277In terms of understanding the output and escape of ionising (Lyman continuum) and Lyman alpha photons from galaxies, Tololo 1214-277 appears to be a unique object in the local universe, and possibly a Rosetta stone for our understanding of how dwarfish galaxies might have contributed to the reionisation of the universe. It is the only object known (from HST/GHRS observations) in the nearby universe to exhibit a symmetric Lyman alpha profile centered on the systemic velocity. This indicates that Lyman alpha has suffered very little scattering implying a low optical depth for Lyman continuum photons. Here we propose to obtain a new COS spectrum with higher spectral resolution, covering Lyman alpha as well as metal absorption lines to map the velocity and structure of the ISM, and imaging in Lyman alpha, Halpha, Hbeta, [OII], and [OIII]. The emission line maps will provide further diagnostics on the escape probability of Lyman continuum photons and pave way for a future direct detection experiment with COS.The program consists of 3 visist, one each with the following instruments: WFC3/UVIS, ACS/SBC and COS.
The purpose of the WFC3/UVIS visit is to do broad abnd imaging in the F336W, F439W and F775W filters, and to do emission line imaging in the narrow filters F502N (redshifted H-beta), FQ378N (redshifted[OII]), FQ508N (redshifted [OIII]) and FQ674N (redshifted Halpha). The latter 3 filters are quad filters. All filters use 2 dithered exposures, and post-flashing to reach the minimal recommended background of 12e/pixel.
The purpose of the ACS/SBC imaging is to do long-pass imaging in F125LP, F140LP, F150LP and F165LP. The F125LP is crucial as it contains the Lyman-alpha line and by taking the difference between F125LP and F140LP we form an effective narrowband filter for isolating the Lya-line. The F140LP, F150LP and F165LP images sample the continuum longwards of Lyman-alpha. The F125LP and F140LP images are split in two dithered exposures each, while one exposure will be obtained for F150LP and F165LP each. We ask the schedulers to make sure that the SBC was not used or turned on in the preceeding visit (by our or another program) in order to ensure a minimal dark current level.
The purpose of the COS visit is to obtain deep G130M spectroscopy. In order to enable an optimum target acquisition, we ask for the COS visit to be put on-hold until at least one week after the UVIS and SBC visits have been obtained. We will use the F140LP and F336W images to interpolate an approximate
COS NUV image. Following this, we will be able to use the normal ACQ/IMAGE mode, followed by 4 exposures with G130M at cenwave 1318, using all the 4 FP-POS settings. (Should it not be possible to put the COS visit on hold, the ACQ/IMAGE will have to be preceeded by an ACQ/SEARCH exposure).GalaxiesIntergalactic Medium and Cosmology3falsetruefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTYESThis object was generated by the target selector and retrieved from the NED database.J2000J2000FUV=19.3 magGALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOThis target was defined by imaging from this programmeJ2000J2000FUV=19.3 magACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoFQ378NWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoFQ674NCOS/FUVSpectroscopicNoNoG130M1300The scheduling data was generated by CASM 25.0.CASM was run in Phase II mode.149535827500093.34327831238897(Tic-Visit
:proposal-id 14923
:visit-id "01"
:proposal-version -1
:trans-version "20170109"
:date "22-Apr-2017 00:44:24.0"
: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 4042464
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 14923
:visit-id "01"
:obset-id "01"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 14923
:visit-id "01"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2896
:al-overhead-at-end 121
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3229
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 14923
:visit-id "01"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3007
: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 3229
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 14923
:visit-id "01"
:orbit-number 3
:pcs-time 222
:si-vis-utilization 3007
:al-overhead-at-end 125
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3229
:pcs-gap 0
)false30The scheduling data was generated by CASM 25.0.CASM was run in Phase II mode.Schedulers, please try to ascertain that the SBC was not used in the preceeding visit.149416259300081.85952192333781(Tic-Visit
:proposal-id 14923
:visit-id "02"
:proposal-version -1
:trans-version "20170109"
:date "05-Apr-2017 17:10:12.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "28"
:si-bright-earth-limb-angle 20.0
:data-volume 111088
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 14923
:visit-id "02"
:obset-id "02"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 14923
:visit-id "02"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2896
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset 866
:dark-utilization 1068
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3229
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 14923
:visit-id "02"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3007
:al-overhead-at-end 0
:internal-dur-at-end 158
:dark-offset 977
:dark-utilization 1068
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3229
:pcs-gap 0
)false20The scheduling data was generated by CASM 25.0.CASM was run in Phase II mode.Photometry that guides target acquisition and integration times is done with HST data from visits 01 and 02 from this program. Flux was measured on the brightest UV source in 0.2 arcsec (acquisition) and 1.25 arcsec (spectroscopic observation) apertures, using the F140LP and F336W filters. Then we interpolated (power-law) between the two, to lambda=2300 AA. Fluxes are quoted below. These numbers (and the beta slope) were entered into the acquisition and spectroscopic ETCs.
HST Imaging Datasets for Photometry:
F140LP 14923 jdew02030
F336W 14923 idew01020
FUV full = 44.741 adu/sec = 1.2138e-15 cgs/AA
FUV ACQ = 24.773 adu/sec = 6.7205e-16 cgs/AA
Uband full = 190.037 adu/sec = 2.702e-16 cgs/AA
Uband ACQ = 114.645 adu/sec = 1.63e-16 cgs/AA
Beta full = -1.9093
Beta ACQ = -1.8003
Resulting estimates for COS/NUV:
COS/NUV full = 6.386e-16 cgs/AA
COS/NUV ACQ = 3.6679e-16 cgs/AA
We use 4 different spectral settings to cover all lines of interest and cover the detector gap, but instead of using a single CENWAVE with 4 FP-POS we use two different CENWAVE, each with two FP-POS.(Tic-Visit
:proposal-id 14923
:visit-id "04"
:proposal-version -1
:trans-version "20170109"
:date "04-Jun-2017 22:51:28.0"
: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 121920
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 14923
:visit-id "04"
:obset-id "04"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 14923
:visit-id "04"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2896
:al-overhead-at-end 0
:internal-dur-at-end 57
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3229
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 14923
:visit-id "04"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3007
:al-overhead-at-end 0
:internal-dur-at-end 350
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3229
:pcs-gap 0
)false20We request to put COS observations on hold until a minimum of 1 week after delivery of the WFC3/UVIS and ACS/SBC images. These images will be used for optimal target acquisition.