0
Assigned ID: 138
----- Attempting Submission 1 (Wed Apr 09 23:04:32 GMT 2014) -----
HST Phase I Proposal 138 (HST_HyLIRGs.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 04:52:00 GMT 2014) -----
0
----- Attempting Submission 1 (Thu Jul 24 23:17:26 GMT 2014) -----
Probing the Most Luminous Galaxies in the Universe at the Peak of Galaxy Assembly
What drives the most luminous galaxies in the universe at z~2, the peak of galaxy assembly? Is it the major merger of two gas rich disk systems as is the case in the local universe or can these extreme luminosities be driven by secular processes, such as the steady accretion of cold gas along filaments thought to play an important role in the early universe? Recent studies on the structure of high redshift luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs, respectively) have stirred up this controversy but have found a range of results leading to a confused picture of star formation in the early universe. In order to solve this question, we will search for unambiguous merger signatures (i.e., pairs, double nuclei, and tidal features) among a large sample of the more rare, extremely luminous HyLIRGs (L_IR > 10^13 L_sun) and the highest luminosity ULIRGs with a wide range of properties and separate them from galaxies that are clearly not mergers (e.g., structured disks). For those objects that remain ambiguous, particularly irregular clumpy systems, we will obtain ground-based IFU follow up observations to add detailed velocity information to the observed morphologies. The large volume probed by the COSMOS field at these high redshifts is an excellent complement to the smaller area fields covered by the CANDELS survey. While CANDELS imaging is excellent for studying the properties of less luminous but more common LIRGs and ULIRGs, it completely misses the more rare, extreme sources. Combined, these data will allow the detailed study of IR galaxies across a range of luminosities spanning over two orders of magnitude.
We propose to obtain rest-frame optical imaging for 101 extremely luminous infrared galaxies
selected at 100 and 160 micron in the COSMOS field at 1.5 < z < 3.0. All of these sources have
accurate photometric redshifts derived from the extensive multiwavelength dataset within
COSMOS (Ilbert et al. 2009; Salvato et al. 2009, 2011) and ~ 10% have reliable spectroscopic
redshifts from optical spectroscopy. Additionally, SPIRE observations in COSMOS
(PI: S. Oliver) will allow us to better constrain LIR and the dust temperature of our sample.
We are in the process of obtaining NIR spectroscopy for this sample as part of a large effort
using FMOS on Subaru (Kartaltepe et al., in prep.) and MOSFIRE on Keck. These spectra
will allow us to measure accurate redshifts and luminosities as well as use standard optical
line diagnostics to study the relative contributions from starbursts and AGN in our sample.
The 101 objects in our sample were carefully chosen to require the fewest number of
WFC3 pointings by observing sources where more than one target can be obtained in a
single WFC3 FOV. None of our targets have existing WFC3 or NICMOS imaging. We can
image all 101 of these sources in 30 pointings. For each of these 30 pointings, we request
single orbit integrations with WFC3 in F160W, roughly equivalent to the CANDELS wide
area depth (CANDELS is 4/3 orbit in F160W Grogin et al. 2011) that will provide the
imaging for the sources with LIR < 10^12.5 L_sun. The choice of the F160W filter ensures that
we will obtain rest-frame optical images for our entire sample with maximum sensitivity,
thus enabling us to detect faint emission from features such as tidal debris and faint disks.
Each orbit will be split into four equal length exposures giving us a total integration time
of 2600 sec and the four exposures will be dithered to obtain the best PSF. In one orbit we
expect to achieve a 5sigma sensitivity of 26.95 mag (AB) for a point source and 25.63 for an
extended source using the ETC with average background. All of our targets are detected
in the Spitzer-IRAC imaging at 3.6 micron and at J and K band, therefore we expect that
all of our targets will easily be detected at high S/N to allow for detailed measurements
of their morphology (including low-surface brightness features) with WFC3-F160W at the
requested depth. CANDELS imaging degraded to the integration times proposed here show
no significant difference from the original CANDELS imaging.
Sample Size: The size of our sample will allow us to combine our data with the sample
of (U)LIRGs observed by CANDELS and study trends as a function of LIR in bins of ~ 0.5
dex over two orders of magnitude in luminosity with ~ 40-60 objects per bin. This sample
size will provide statistics on the presence or absence of mergers and allow us to divide the
sources in other ways, such as into starburst/main sequence categories (2 bins of sSFR)
or as a function of the presence/strength of an AGN identified via rest-frame optical line
diagnostics, X-ray imaging, and SED analysis.
We propose parallel observations with ACS in F606W. About half of our 30 pointings
can be oriented such that these parallels will cover the targets in this proposal. The remaining
will cover additional (U)LIRGs and HyLIRGs in the field and will supplement existing HST
coverage of the COSMOS field.
UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE
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true
1
0
The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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(Tic-Visit
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true
1
0
The scheduling data was generated by CASM 22.2.
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false
1
0
The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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false
1
0
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
1
0
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
1
0
The scheduling data was generated by CASM 22.2.
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(Tic-Visit
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true
1
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The scheduling data was generated by CASM 22.2.
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true
1
0
The scheduling data was generated by CASM 22.2.
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(Tic-Visit
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false
1
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The scheduling data was generated by CASM 22.2.
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(Tic-Visit
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true
1
0
The scheduling data was generated by CASM 22.2.
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(Tic-Visit
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true
1
0
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
1
0