Morphologies of the Most UV luminous Lyman Break Galaxies at z~3
We propose to carry out WFC3/F160W high spatial resolution imaging of a sample of eighteen extremely UV luminous Lyman Break Galaxies (LBGs) at z=2.2-3.2 to study their morphologies and to constrain models of the formation and evolution of the most massive and luminous galaxies at high-redshift. Studies of high-redshift LBGs in recent years have provided key insight into the history of galaxy assembly at the peak of cosmic star formation activity. However, most previous studies have been limited by small survey volume and could not select the rarest systems. We have carried out wide-field multicolor surveys of LBGs covering >300 deg^2, increasing the survey volume by ~2 orders of magnitude. Our initial observations have revealed eighteen extremely UV luminous galaxies with r~21-22.5, more than 2 magnitudes brighter than typical LBGs. At L > 6L*, they represent some of the rarest and most intensive star forming systems in the early Universe. With the proposed observations, we will look for signatures of major merger activities, measure the relative contribution of nuclear point source to the total luminosity, and carry out detailed quantitative morphological measurements. These analyses will help us understand the triggering mechanism of the intense star formation in these galaxies, constrain their star formation and assembly histories, and reveal their evolutionary stage in the overall sequence of galaxy formation. Together with other observations, our study will place these newly discovered galaxies in the context of galaxy growth through merger and cold flow accretion at the peak era of cosmic star formation, and provide a unique laboratory for galaxy formation theory.
The main purpose of the proposed observations is to obtain high spatial resolution rest-frame optical images of a sample of extremely UV luminous Lyman Break Galaxies (LBGs) to study their morphological properties. We proposed to observe18 UV luminous LBGs with WFC3/F160W filter. Our purpose is to get high S/N WFC3/F160 image to sample the rest-frame optical emission (~4000A) and trace old stellar populations and stellar structure.
Total 18 individal visits (one orbit per visit) are create for the 18 galaxies. For each visit, we use a four pointing dithering partern (WFC3-IR-DITHER-BOX-MIN ) to fill the one-orbit observing time. For each pointing, the sampling sequence with NSAMP=14, SAMP-SEQ=SAPAR50 is used. With this setup, the exposure time on each of the galaxy will reach 2600s. Based on the ETC, the observation will provide enough S/N (S/N>7 for 0.1"x0.1" region) to perform both parametric and non-parametric analysis on the morphology of these galaxies.
UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE
12
false
0.0
0.0
false
false
false
false
SUPPORTED
GALAXY
DISK
J2000
J2000
r = 21.0
GALAXY
DISK
J2000
J2000
r = 20.9
GALAXY
DISK
STARBURST
J2000
J2000
r = 21.6
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.3
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.1
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.0
GALAXY
DISK
STARBURST
J2000
J2000
r = 21.7
GALAXY
DISK
SPIRAL ARM
J2000
J2000
r = 22.3
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.3
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.5
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.5
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.4
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.5
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.4
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.3
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.4
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.5
GALAXY
DISK
STARBURST
J2000
J2000
r = 22.5
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
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No
F160W
WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
POS-TARG
DITHER
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LINE
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 12861
:visit-id "18"
:proposal-version -1
:trans-version "20120604"
:date "03-Jul-2012 13:53:23.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 974896
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 12861
:visit-id "18"
:obset-id "18"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 12861
:visit-id "18"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2640
:al-overhead-at-end 0
:internal-dur-at-end 481
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)
true
1
0