Predicting the redshift 2 Halpha luminosity function using [OIII] emission line galaxies

Understand

Upcoming space-based surveys such as Euclid and WFIRST-AFTA plan to measure Baryonic Acoustic Oscillations (BAOs) in order to study dark energy.

• These surveys will use IR slitless grism spectroscopy to measure redshifts of a large number of galaxies over a significant redshift range.
• In this paper, we use the WFC3 Infrared Spectroscopic Parallel Survey (WISP) to estimate the expected number of Halpha (Ha) emitters observable by these future surveys.
• WISP is an ongoing HST slitless spectroscopic survey, covering the 0.8-1.65micron wavelength range and allowing the detection of Ha emitters up to z~1.5 and [OIII] emitters to z~2.3.