Characterizing the Stellar Populations in Lyman-Alpha Emitters and Lyman Break Galaxies at 5.7<z<7 in the Subaru Deep Field
The epoch of reionization marks a major phase transition of the Universe, during which the intergalactic space became transparent to UV photons. Determining when this occurred and the physical processes involved represents the latest frontier in observational cosmology. Over the last few years, searches have intensified to identify the population of high-redshift (z>6) galaxies that might be responsible for this process, but the progress is hampered partly by the difficulty of obtaining physical information (stellar mass, age, star formation rate/history) for individual sources. This is because the number of z>6 galaxies that have both secure spectroscopic redshifts and high-quality infrared photometry (especially with Spitzer/IRAC) is still fairly small. Considering that only several photometric points are available per source, and that many model SEDs are highly degenerate, it is crucial to obtain as many observational constraints as possible for each source to ensure the validity of SED modeling. To better understand the physical properties of high-redshift galaxies, we propose here to conduct HST/NICMOS (72 orbits) and Spitzer/IRAC (102 hours) imaging of spectroscopically confirmed, bright (z<26 mag (AB)) Ly-alpha emitters (LAEs) and Lyman-break galaxies (LBGs) at 5.7<z<7 selected from the Subaru Deep Field. Spectroscopic redshifts remove one critical free parameter from SED modeling while bright source magnitudes ensure high-quality photometric data. By making accurate determinations of stellar masses, ages, and star-formation histories, we will specifically address the following major questions: (1) Do LAEs and LBGs represent physically different galaxy populations at z>6 as suggested recently? (2) Is Ly-alpha emission systematically suppressed at z>6 with respect to continuum emission? (i.e., are we reaching the epoch of incomplete reionization?), and (3) Do we see any sign of abnormally young stellar population in any of the z>6 galaxies?
We will image each source in the sample with a combination of
NICMOS/F110W and NICMOS/F160W pointings, using the NIC3 camera. The
NIC3 camera is used to achieve the best sensitivity since the target
sources are faint. The two-filter observations are necessary to
measure the rest-frame UV continuum slope. For K-band photometry,
we will use ground-based 8m-class telescopes, which are more
sensitive. Because our sources are isolated, there is no need for
specific constraints on the orientation of the NIC3 camera.
We used the latest version of the ETC to derive the limiting magnitude
reached by each NICMOS pointing, assuming 38 minutes of science
integration time per orbit in low-sky (LOW) background. We achieve a
S/N of 5 for a limiting point source sensitivity of 26.1 (AB) in a
single NICMOS/F110W orbit, computed within a 0.6"-diameter
aperture. Similarly, a single NICMOS/F160W orbit will reach a
5-sigma sensitivity of 25.9.
The z{AB} magnitudes provided in the proposal are pure continuum
values, and if the target galaxies have a flat f_nu spectrum, the
near-infrared continuum magnitudes will be similar (i.e., constant AB
magnitudes). However, the rest-frame UV continuum could be quite blue
if the underlying stellar population is young and contains very
massive stars. In this case, the near-infrared continuum becomes
fainter than the z-band continuum.
Considering the uncertainties with the expected near-infrared
continuum magnitudes, not only due to the unknown slope of the
rest-frame UV continuum but also due to the z-band photometry
themselves (for z>6 galaxies, observed z magnitudes had to be
corrected for the IGM absorption and Ly-alpha emission), it is
desirable to achieve NICMOS F110W and F160W detection limits one
magnitude deeper than the z magnitudes listed. We can achieve this
goal by integrating for 2 orbits (1 F110W; 1 F160W) for the 4 targets
with z magnitudes of 24.5--25.0 mag and for 4 orbits (2 F110W; 2
F160W) for 7 targets with z=25.0-25.5 mag. For the remaining 9
galaxies with z>25.5 mag, we will also integrate for 4 orbits (2
F110W; 2 F160W). This depth will allow detections if the rest-frame
UV continuum is fairly flat in f_nu.
In total, we request 72 orbits for this program (2 orbits x 4 sources
+ 4 orbits x 16 sources).
COSMOLOGY
12
false
0.0
0.0
false
false
false
false
false
false
SUPPORTED
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=26.4
J2000
13 23 59.8000
+27 24 56.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.57
J2000
13 25 22.3000
+27 35 20.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.17
J2000
13 23 57.1000
+27 24 48.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.81
J2000
13 25 18.1000
+27 30 43.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=24.94
J2000
13 24 8.3000
+27 15 43.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.13
J2000
13 24 10.8000
+27 19 28.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=24.73
J2000
13 24 15.7000
+27 30 58.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.57
J2000
13 23 53.1000
+27 16 31.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.66
J2000
13 24 40.6000
+27 36 7.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.24
J2000
13 23 45.6000
+27 17 1.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.88
J2000
13 24 0.3000
+27 32 38.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.74
J2000
13 24 42.5000
+27 24 23.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.36
J2000
13 24 26.5000
+27 16 0.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.89
J2000
13 24 31.5000
+27 15 9.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.42
J2000
13 25 19.4000
+27 18 29.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.75
J2000
13 24 18.4000
+27 16 33.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=24.73
J2000
00 00 0.0000
+00 00 0.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.34
J2000
13 25 23.4000
+27 17 1.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=24.84
J2000
13 24 16.1000
+27 44 11.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
z(AB)=25.37
J2000
13 24 16.4000
+27 19 7.00
J2000
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F110W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
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No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
NIC3
Imaging
No
No
F160W
POS-TARG
DITHER
DITHER
5.0
NIC-XSTRIP-DITH
false
false
4
22.5
POS-TARG
NIC-SPIRAL-DITH
0.0
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false
POS-TARG
DITHER
0.572
LINE
0.365
false
false
74.653
4
18.528
WFC3-IR-DITHER-BOX-MIN
2
false
POS-TARG
DITHER
0.636
LINE
false
false
2
41.788
WFC3-IR-DITHER-LINE
3
false
The scheduling data was generated by CASM 17.5.
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true
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The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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true
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The scheduling data was generated by CASM 17.5.
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false
2
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For this target, we are now using F125W instead of F110W.
The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 17.5.
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true
4
0
The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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true
4
0
The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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true
2
0
The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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true
4
0
The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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true
2
0
The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
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true
2
0
The scheduling data was generated by CASM 17.5.
CASM was run in Phase II mode.
Although this target was already observed in Visit 01, our reduction of this data set shows that the achieved depth is inadequate. The source is seen in the images, but it is too faint to perform accurate photometry. Therefore, we have allocated one extra orbit of WFC3 time to reobserve this target.
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:low-sky "N"
:pcs-visibility 3149
:pcs-gap 0
)
true
1
0
For this target, we are now using F125W instead of F110W.