The total number of Primary Orbits used in all Cycles must equal the total number of Primary Orbits specified on all the Observations. (Compare totals reported on the first and second pages of the PDF Preview.)
Cannot find file /home/imants/APT_25.0.4/dwarfgal.pdf
0
Assigned ID: 931
----- Attempting Submission 1 (Fri Apr 07 20:21:29 GMT 2017) -----
0
----- Attempting Submission 1 (Tue Jul 18 16:35:51 GMT 2017) -----
----- Attempting Submission 2 (Wed Jul 26 19:54:02 GMT 2017) -----
----- Attempting Submission 3 (Thu Jul 27 13:42:15 GMT 2017) -----
----- Attempting Submission 4 (Tue Aug 08 19:39:54 GMT 2017) -----
----- Attempting Submission 5 (Wed Apr 18 14:32:48 GMT 2018) -----
----- Attempting Submission 6 (Mon Apr 23 18:28:14 GMT 2018) -----
----- Attempting Submission 7 (Mon Jan 07 17:59:19 GMT 2019) -----
The Low-Mass Stellar Initial Mass Function: Ultra-Faint Dwarf Galaxies Revisited
The stellar Initial Mass Function plays a critical role in the evolution of the baryonic content of the Universe. The form of the low-mass IMF - stars of mass less than the solar mass - determines the fraction of baryons locked up for a Hubble time, and thus indicates how gas and metals are cycled through galaxies. Inferences from resolved stellar populations, where the low-mass luminosity function and associated IMF can be derived from direct star counts, generally favor an invariant and universal IMF. However, a recent study of ultra-faint dwarf galaxies Hercules and Leo IV indicates a "bottom-lite" IMF, over a narrow range of stellar mass (only 0.55-0.75 M_sun), correlated with the internal velocity dispersion and/or metallicity. We propose to obtain ultra-deep imaging for a significantly closer ultra-faint dwarf, Bootes I, which will allow us to construct the luminosity function down to M_v=+10 (equivalent to ~0.35 solar mass). We will also re-analyze the HST archival observations for the Hercules and Leo IV dwarfs using the same updated techniques as for Bootes I. The combined datasets should provide a reliable answer to the question of how variable is the low-mass stellar IMF.
We request all observations of the Bootes-I ultra-faint dwarf galaxy to be obtained at Orientation angles ranging from 128 to 129 degrees in accordance with the archival observations of GO-12549 upon which our science case is built. The timing of each visit can be arbitrary.
Stellar Populations
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SUPPORTED
GALAXY
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NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
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NO
J2000
J2000
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NO
J2000
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:orbit-number 1
:pcs-time 333
:si-vis-utilization 2823
: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 3156
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 15317
:visit-id "13"
:orbit-number 2
:pcs-time 302
:si-vis-utilization 2853
:al-overhead-at-end 0
:internal-dur-at-end 347
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3156
:pcs-gap 0
)
true
2
0