0Assigned ID: 130
----- Attempting Submission 1 (Wed Apr 09 21:39:25 GMT 2014) -----POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.2014-12-16: 2nd update. should have been 14 e- in visit 33 instead of 13.
2014-12-16: updated number of postflash e- for the H-alpha images, [uneven illumination/reduced level at (x,y) of the ramp aperture].366749214----- Attempting Submission 1 (Wed Jul 23 08:47:34 GMT 2014) -----
----- Attempting Submission 2 (Tue Dec 16 10:02:11 GMT 2014) -----
HST Phase II Proposal 13655 (ulirg_pii_20141216.apt) successfully submitted.
----- Attempting Submission 3 (Tue Dec 16 10:07:37 GMT 2014) -----Every problem relates to using a POS-TARG with a ramp filter on ACS/WFC. However the dithers are particularly small, and so the spatial variation of the bandpass has a negligible impact.How Lyman alpha bites/beats the dustThe bulk of high redshift star formation occurs in IR-bright objects. At similar epochs the de facto spectroscopic tracer of galaxies is the Lyman-alpha line, which is used almost ubiquitously with a diverse range of applications in galaxy evolution. Ly-alpha is also very sensitive to dust absorption, however, and a challenging emergent result of recent years is that an overwhelming fraction of IR-bright galaxies are also luminous Ly-alpha emitters. How is this possible given the mammoth dust contents? We will take advantage of the unique capabilities of HST and the Cycle 22 UV initiative to find out.
Ly-alpha observations are infamously difficult to interpret because of the resonant nature of the transition. This has motivated detailed studies of nearby galaxies with space-based platforms, that have aided in unleashing the power of Ly-alpha for high-z studies. Only HST provides the UV access and resolution to do this, and hundreds of orbits have been devoted to studying UV-selected galaxies. Yet the UV reveals a small fraction of high-z star formation and no study has ever imaged the IR-bright systems in Ly-alpha. The proposed ACS observations will do this in five Ultraluminous Infrared Galaxies (ULIRGs), sampling spatial scales of just 50 pc. We will test sophisticated new models of Ly-alpha escape, study morphologies in comparison to the stars and nebular gas, measure global Ly-alpha quantities for the first time, and probe the relevant structures in the ISM in minute detail. We will finally push nearby Ly-alpha studies to the highest possible bolometric luminosities.We will take images of 5 ultraluminous infrared galaxies with the Advanced Camera for Surveys. For each galaxy we will observe in 4 ultraviolet filters with the SBC, and 2 optical filters with WFC. We require four orbits for each galaxy: 3 for SBC and 1 for WFC.
Since we use >2 hours of SBC, these observations become sensitive to the rising dark current (DC), so we break the SBC observations into two visits. SBC visits of 2 and 1 orbits are submitted for each target. WFC observations are obtained in their own visit.
*** As with our other programmes, we request that the SBC amplifiers have been turned off for the three orbits prior to our visits. This allows the SBC to cool and 'reset' the thermal DC before our observations begin. ***
In the numbering of Visits, the first number (1-5) describes the target, the second number (1-3) describes the observation where 1=2orbits with SBC, 2=1 orbit with SBC, and 3=1 orbit with WFC.
The four orbits break down as follows:
First visit per galaxy:
Orbit1: F165LP - F125LP - F140LP - F150LP
Orbit2: [ POS-TARG ] F150LP - F140LP - F125LP - F165LP
Second visit per galaxy:
Orbit1: [ POS-TARG ] F165LP - F125LP - F140LP - F150LP
Third orbit per galaxy:
Orbit1: FR782N - F775W [ POS-TARG ] F775W - FR782N
One of the targets (#3 in the target list) will be observed in the CVZ, and thus the description above is modified with more exposures, treating each CVZ orbit as similar to 1 normal orbit.
SBC ETC runs are computed from the GALEX FUV and NUV magnitudes, and the measured continuum colour (beta) between them. FUV magnitude is entered into the ETC for each galaxy, together with the beta slope. Illustrative EXPTIMES are 400s (F125LP), 500s (F140LP), 700s (F150LP), 1000s (F165LP).
The ACS/WFC observations include a NB (ramp filter) observation and use a 13 or 11 post-flash electrons. The F775W filter becomes background limited within the exposure and does not require flashing.ISM IN EXTERNAL GALAXIES12RegularfalsetruefalsefalsefalseSUPPORTEDGALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=19.8 (AB); L_FIR = 10**12.24 Lsun [ z=0.158 ]GALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=20.3 (AB): L_FIR = 10**12.06 Lsun [ z=0.158 ]GALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=21.2 (AB): L_FIR = 10**12.15 Lsun [ z=0.157 ]GALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.8 (AB): L_FIR = 10**12.39 Lsun [ z=0.159 ]GALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.9 (AB); L_FIR = 10**12.19 Lsun [ z=0.131 ]ACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPACS/WFCRampFilterNoNoFR782NACS/WFCImagingNoNoF775WACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPACS/WFCRampFilterNoNoFR782NACS/WFCImagingNoNoF775WACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPACS/WFCRampFilterNoNoFR782NACS/WFCImagingNoNoF775WACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPACS/WFCRampFilterNoNoFR782NACS/WFCImagingNoNoF775WACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPACS/WFCRampFilterNoNoFR716NACS/WFCImagingNoNoF775WThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.SBC; 2 orbits1428904842000137.0239097314133(Tic-Visit
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:max-dark-utilization 1920
:low-sky "N"
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)true10The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.WFC; 1 orbit1429422482000239.302409380801(Tic-Visit
:proposal-id 13655
:visit-id "53"
:proposal-version -1
:trans-version "20140605"
:date "16-Dec-2014 11:05:05.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "27"
:si-bright-earth-limb-angle 20.0
:data-volume 1136896
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13655
:visit-id "53"
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:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13655
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:internal-dur-at-end 347
:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3241
:pcs-gap 0
)true10