Low-z Analogs of High Redshift Lyman Alpha Emitters
Lyman-alpha emitting galaxies with luminosities comparable to those
of the highest redshift galaxies are first seen at z ~ 1. Unlike higher
redshift Lyman-alpha emitters, the Lyman-alpha emission from these
galaxies is hardly modified by the intergalactic medium, which makes it possible
to study the galaxies' intrinsic properties. We propose to develop a sample
of 100-200 such galaxies in the GOODS-N field lying in the redshift range
z = 0.7 - 1.8. This requires 24 1-orbit exposures with the G280L grism on the
WFC3-UVIS. The sample will allow us to construct Lyman-alpha luminosity
functions in this poorly studied redshift range and to determine how the Lyman-alpha
emitters are drawn from the general galaxy population at these redshifts.
We will determine how the Lyman-alpha lines correlate with Balmer line fluxes,
star formation rates, extinctions, and metallicities using the wealth of imaging and
spectroscopic information available for the intensively studied GOODS-N region.
These templates will be valuable for studying what controls the escape of
Lyman-alpha photons in the more luminous star forming galaxies, in
interpreting the highest redshift Lyman-alpha emitters, and in understanding how
their properties are modified by the intergalactic gas.
We propose to obtain spectral images
at 24 positions covering the GOODS-N field with the G280
grism on WFC3 to find a substantial sample of z=0.7-1.8 Ly alpha emitters
over the wavelength range from 2100 to 3400A.
WFC3+G280 provides the unique combination of wavelength
coverage, sensitivity, and field needed for this project.
We have chosen the field positions to cover the deepest
portions of the GOODS-N region. We have slightly overlapped
the fields to allow for edge effects. The 24 pointings
will cover a total area of approximately 140 square arcminutes.
They are at a PA of 45 degs E of N to match the orientation of the GOODS-N field.
At each position we will obtain a short 120 s imaging exposure
with the F2000LP filter prior to the spectroscopic
exposures to calibrate the spectroscopic wavelengths by
establishing the positions and shapes of the galaxies
relative to the grism images.
We will then obtain an approximately 2400s grism image
broken into 5 475s dithered sub-exposures to remove
artifacts, as well as cosmic rays.
COSMOLOGY
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