0Assigned ID: 831
----- Attempting Submission 1 (Fri Apr 11 21:09:46 GMT 2014) -----
HST Phase I Proposal 831 (Gennaro_imf_JH.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 22:28:47 GMT 2014) -----
HST Phase I Proposal 831 (Gennaro_imf_JH.apt) successfully submitted.PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIME
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIME
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIME
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIMEWe have only changed the description of observations, which was completely lacking.-1777423438----- Attempting Submission 1 (Thu Jul 17 18:43:03 GMT 2014) -----
HST Phase II Proposal 13860 (adhoc_split.apt) successfully submitted.
----- Attempting Submission 2 (Thu Jul 17 21:34:48 GMT 2014) -----
HST Phase II Proposal 13860 (adhoc_split.apt) successfully submitted.
----- Attempting Submission 3 (Tue Sep 02 18:51:12 GMT 2014) -----The warnings issued by the APT are due to the fact that we have extended the exposures times
for the ACS parallel observations beyond those of the WFC3/IR primary ones.
This is due to the "quantized" nature of WFC3/IR exposure times which forces us to have
some unused orbit time in the primary observations, which we can still use for the parallels.Investigating the low-mass slope and possible turnover in the LMC IMFWe propose to derive the Initial Mass Function (IMF) of the field population of the Large Magellanic Cloud (LMC) down to 0.2 solar masses, probing the mass regime where the characteristic IMF turnover is observed in our Galaxy. The power of the HST, using the WFC3 IR channel, is necessary to obtain photometric mass estimates for the faint, cool, dwarf stars with masses below the expected IMF turnover point. Only by probing the IMF down to such masses, it will be possible to clearly distinguish between a bottom-heavy or bottom-light IMF in the LMC. Recent studies, using the deepest available observations for the Small Magellanic Cloud, cannot find clear evidence of a turnover in the IMF for this galaxy, suggesting a bottom-heavy IMF in contrast to the Milky Way. A similar study of the LMC is needed to confirm a possible dependence of the low-mass IMF with galactic environment. Studies of giant ellipticals have recently challenged the picture of a universal IMF, and suggest an enviromental dependence of the IMF, with the most massive galaxies having a larger fraction of low mass stars and no IMF turnover. A study of possible IMF variations from resolved stellar populations in nearby galaxies is of great importance in sheding light on this issue. Our simple approach, using direct evidence from basic star counts, is much less prone to systematic errors with respect to studies of more distant objects which have to rely on the observations of integrated properties.Our observations are designed to reach the low-mass main sequence of the field population in the Large Magaellanic Cloud, using WFC3/IR, down to about 0.25 Msun at SNR=10. The aim is to constrain the slope and possible turnover of the IMF in the LMC. The target magnitudes in F110W and F160W are equivalent to V=30 mag (Vega) for the appropriate stellar spectral type. We have designed parallel ACS observations in F606W and F814W that, while not reaching the same depth, will add constraints to the star formation history of the chosen region.
The 12 allocated orbits are grouped into 6 visits of 2 orbits each.
The primary observations of the first 4 visits (8 orbits) are executed using the F160W filter, while for the other 2 visits (4 orbits) we use F110W. We use the SAMP-SEQ=STEP200 WFC3/IR sampling sequence, which allow us to maximize both the effective observing time, and the number of read samples (14 or 15).
The parallel observations are divided into short, medium and long exposures, to capture the dynamical range of the observed stars with ACS; 5 (2 for short + medium, 3 for long exposures) parallel orbits are dedicated to F814W and 7 (2 for short + medium, 5 for long exposures) to F606W. In the short ACS exposures we use post-flash (FLASH=75) illumination to improve the CTE.
Each visit consists of 4 primary exposures in a box dithering pattern, to better sample the PSF.
The pattern matches the default pattern in the WFC3 Handbook. Between visits we execute additional small offsets (few pixels) to ensure that no star falls repeatedly on the same position, thus minimizing the impact of detector artifacts.RESOLVED STELLAR POPULATIONSDefaultfalsefalsefalsefalsefalseSUPPORTEDGALAXYMAGELLANIC IRREGULARJ2000J2000WFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF160W/Users/gennaro/Desktop/APT_phaseII_b/OP-cache/adhoc_split-v01.xmlHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.Two orbits visit.
The primary will be WFC3/IR with the F160W filter and in parallel we will have ACS/F606W
We will execute a 4-point dither pattern to improve PSF sampling.
Between visits we will execute an additional offset. This will ensure that no star is observed at the same chip location twice, thus avoiding bad pixels.
The parallel orbits are dedicated to short and medium ACS exposures(Tic-Visit
:proposal-id 13860
:visit-id "01"
:proposal-version -1
:trans-version "20140605"
:date "17-Jul-2014 16:28:38.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 3370544
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13860
:visit-id "01"
:obset-id "01"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13860
:visit-id "01"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3102
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 13860
:visit-id "01"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3302
:al-overhead-at-end 0
:internal-dur-at-end 524
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)true20/Users/gennaro/Desktop/APT_phaseII_b/OP-cache/adhoc_split-v02.xmlHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.Two orbits visit.
The primary will be WFC3/IR with the F160W filter and in parallel we will have ACS/F606W
We will execute a 4-point dither pattern to improve PSF sampling.
Between visits we will execute an additional offset. This will ensure that no star is observed at the same chip location twice, thus avoiding bad pixels.(Tic-Visit
:proposal-id 13860
:visit-id "02"
:proposal-version -1
:trans-version "20140605"
:date "11-Jul-2014 17:02:08.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 2233648
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13860
:visit-id "02"
:obset-id "02"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13860
:visit-id "02"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3231
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 13860
:visit-id "02"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3302
:al-overhead-at-end 0
:internal-dur-at-end 524
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)true20/Users/gennaro/Desktop/APT_phaseII_b/OP-cache/adhoc_split-v03.xmlHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.Two orbits visit.
The primary will be WFC3/IR with the F160W filter and in parallel we will have ACS/F606W
We will execute a 4-point dither pattern to improve PSF sampling.
Between visits we will execute an additional offset. This will ensure that no star is observed at the same chip location twice, thus avoiding bad pixels.(Tic-Visit
:proposal-id 13860
:visit-id "03"
:proposal-version -1
:trans-version "20140605"
:date "11-Jul-2014 17:02:10.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 2233648
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13860
:visit-id "03"
:obset-id "03"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13860
:visit-id "03"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3231
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 13860
:visit-id "03"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3302
:al-overhead-at-end 0
:internal-dur-at-end 524
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)true20/Users/gennaro/Desktop/APT_phaseII_b/OP-cache/adhoc_split-v04.xmlHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.Two orbits visit.
The primary will be WFC3/IR with the F160W filter and in parallel we will have ACS/F606W for 1 orbit and ACS/814W for the other orbit.
We will execute a 4-point dither pattern to improve PSF sampling.
Between visits we will execute an additional offset. This will ensure that no star is observed at the same chip location twice, thus avoiding bad pixels.(Tic-Visit
:proposal-id 13860
:visit-id "04"
:proposal-version -1
:trans-version "20140605"
:date "17-Jul-2014 14:13:12.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 2233648
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13860
:visit-id "04"
:obset-id "04"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13860
:visit-id "04"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3231
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 13860
:visit-id "04"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3302
:al-overhead-at-end 0
:internal-dur-at-end 524
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)true20/Users/gennaro/Desktop/APT_phaseII_b/OP-cache/adhoc_split-v05.xmlHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.Two orbits visit.
The primary will be WFC3/IR with the F110W filter and in parallel we will have ACS/F814W
We will execute a 4-point dither pattern to improve PSF sampling.
Between visits we will execute an additional offset. This will ensure that no star is observed at the same chip location twice, thus avoiding bad pixels.
The parallel orbits are dedicated to short and medium ACS exposures(Tic-Visit
:proposal-id 13860
:visit-id "05"
:proposal-version -1
:trans-version "20140605"
:date "17-Jul-2014 16:28:54.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 3370544
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13860
:visit-id "05"
:obset-id "05"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13860
:visit-id "05"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3102
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 13860
:visit-id "05"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3302
:al-overhead-at-end 0
:internal-dur-at-end 524
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)true20/Users/gennaro/Desktop/APT_phaseII_b/OP-cache/adhoc_split-v06.xmlHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.Two orbits visit.
The primary will be WFC3/IR with the F110W filter and in parallel we will have ACS/F814W
We will execute a 4-point dither pattern to improve PSF sampling.
Between visits we will execute an additional offset. This will ensure that no star is observed at the same chip location twice, thus avoiding bad pixels.(Tic-Visit
:proposal-id 13860
:visit-id "06"
:proposal-version -1
:trans-version "20140605"
:date "11-Jul-2014 17:02:14.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 2233648
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13860
:visit-id "06"
:obset-id "06"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13860
:visit-id "06"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 3231
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 13860
:visit-id "06"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3302
:al-overhead-at-end 0
:internal-dur-at-end 524
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3572
:pcs-gap 0
)true20