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.In this re-submission, we have added BLADE=A to all of the exposures (all of them are 1.4 sec) in order to
reduce the effects of shutter jitter. -- CoI H. E. Bond 9/17/13
We are submitting a repeat of the failed Visits 01 and 02, as authorized by the TTRB. The BEFORE
has been changed to 15-oct-2014, and we have added more ORIENTs to allow the observations to be
scheduled. Also, based on the exposures obtained in March 2014, the exposure times have been
changed to 1.5 sec. We moreover are now grouping the observations as SEQ NON-INT to make sure
that all of the observations are done in the same orbit for each star.
--CoI H. E. Bond on behalf of PI Nancy Evans, 6/3/14.-264519746----- Attempting Submission 2 (Wed Sep 18 00:42:36 GMT 2013) -----
----- Attempting Submission 3 (Tue Jun 03 23:51:02 GMT 2014) -----The warnings are about use of Patterns and POS TARG with quad filters. We believe we understand correct usage.The Dynamical Mass of Polaris, the Nearest CepheidCepheid variables are the primary standard candles for measuring extragalactic distances, and they provide critical tests of stellar-evolution theory. Thus it is important to understand them astrophysically. Polaris (alpha UMi) is the nearest and brightest of all Cepheids. It offers a unique opportunity to measure the dynamical mass of a Cepheid, because it is in a 30-year binary system for which a single-lined spectroscopic orbit is already available. In Cycle 14, we resolved the system for the first time, using ACS/HRC in the UV, and followed up in Cycle 15. These observations established the sense of the orbital motion, as well as a first approximation to the dynamical mass. An observation with WFC3 in Cycle 17 again revealed the companion, in spite of the larger pixels than ACS/HRC, after deconvolution. This further refined our mass determination.
We propose an additional WFC3 observation in Cycle 21, which will extend the coverage of the orbit substantially. We estimate that this new observation will reduce the uncertainty in the mass of Polaris from 26% to 10%. The window for this observation is rapidly closing since the two stars are heading for periastron. This is a UV Initiative proposal since making the observations in the UV enhances the relative brightness of the companion, which is warmer than Polaris, by about 2 magnitudes relative to the visible. Because of the degradation of the PSF in short WFC3 exposures due to "shutter jitter," we also request one orbit to observe a nearby bright single star, Beta Cas, using identical exposure times, to serve as a PSF reference star in the specialized FQ232N filter that we will use.The aim of the observations is to resolve the very close, faint companion of Polaris, and measure its separation and position angle as part of a solution for the dynamical mass of Polaris. We will take a series of dithered 1.4-sec exposures on Polaris in the FQ232N filter, which makes unsaturated images of Polaris possible, and reduces the magnitude difference between the two stars. We will also take a set of identical exposures on Gamma Cas, in order to determine the PSF in this very rarely used WFC3 filter for a single star, observed with the same amount of shutter jitter as for Polaris. For all of the exposures, because of very faint backgrounds, we added FLASH=12.COOL STARS12falsetrue0.00.0falsefalsefalseAVAILABLESTARCEPHEIDF3-F9PULSATING VARIABLEALPHA-UMIJ2000J2000STARF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.J2000WFC3/UVISImagingNoNoFQ232NWFC3/UVISImagingNoNoFQ232NPOS-TARGDITHER0.173LINE0.112falsetrue81.785423.884WFC3-UVIS-DITHER-BOX1falseTiming link suitability includes constraints ([Group (01 02) Within 2.0 days])The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.ORIENT is chosen to place the faint companion Polaris Ab at between "noon" and "1 o'clock" in the image frame relative to Polaris A, which appears to be the optimal location for the FQ232N PSF to avoid diffraction spikes and filter ghosts. A small window around "2 o'clock" is also allowed. The BEFORE 15-jun-2014 is included to assure that the observation is done in Cycle 21, so as to cover this important part of the binary orbit.139502104600019.132879638954904(Tic-Visit
:proposal-id 13369
:visit-id "01"
:proposal-version -1
:trans-version "20130722"
:date "17-Sep-2013 20:34:36.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 985408
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13369
:visit-id "01"
:obset-id "01"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13369
:visit-id "01"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3158
:al-overhead-at-end 174
:internal-dur-at-end 498
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3646
:pcs-gap 0
)false10Timing link suitability includes constraints ([Group (03 04) Within 2.0 days])The scheduling data was generated by CASM 22.0.CASM was run in Phase II mode.ORIENT is chosen to place the faint companion Polaris Ab at between "noon" and "1 o'clock" in the image frame relative to Polaris A, which appears to be the optimal location for the FQ232N PSF to avoid diffraction spikes and filter ghosts. A small window around "2 o'clock" is also allowed. The BEFORE 15-Oct-2014 is included to assure that the observation is done in Cycle 21, so as to cover this important part of the binary orbit.
Note that this is a repeat of Visit 01 which failed in March 2014. We also added orients differing by 180 deg from the originals, and changed the exposure times from 1.4 to 1.5 sec.(Tic-Visit
:proposal-id 13369
:visit-id "03"
:proposal-version -1
:trans-version "20131031"
:date "03-Jun-2014 19:30:39.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 985408
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13369
:visit-id "03"
:obset-id "03"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13369
:visit-id "03"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3004
:al-overhead-at-end 174
:internal-dur-at-end 652
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3646
:pcs-gap 0
)false10Timing link suitability includes constraints ([Group (01 02) Within 2.0 days])The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.This is a PSF reference star for the analysis of the Polaris images. Set of exposures is identical to those for Polaris. Should be taken within a few HST orbits of the Polaris observation.1395033194000298.6690894904091(Tic-Visit
:proposal-id 13369
:visit-id "02"
:proposal-version -1
:trans-version "20130722"
:date "17-Sep-2013 20:34:40.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 844640
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13369
:visit-id "02"
:obset-id "02"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13369
:visit-id "02"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2774
:al-overhead-at-end 174
:internal-dur-at-end 344
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3333
:pcs-gap 0
)false10Timing link suitability includes constraints ([Group (03 04) Within 2.0 days])The scheduling data was generated by CASM 22.0.CASM was run in Phase II mode.This is a PSF reference star for the analysis of the Polaris images. Set of exposures is identical to those for Polaris. Should be taken within a few HST orbits of the Polaris observation.
Note that this is a repeat of Visit 02 which failed in March 2014.(Tic-Visit
:proposal-id 13369
:visit-id "04"
:proposal-version -1
:trans-version "20131031"
:date "03-Jun-2014 19:39:00.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 844640
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:obset-id "04"
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)
(Tic-Orbit
:proposal-id 13369
:visit-id "04"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2620
:al-overhead-at-end 174
:internal-dur-at-end 498
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3333
:pcs-gap 0
)true10