WFIRST

WFIRST Simulations


Wide-Field Infrared Survey Telescope

Simulations using GULLS

WFI Direct Imaging Simulations in Support of Exoplanet Microlensing

Summary

The WFIRST microlensing survey is designed to discover cold, low-mass exoplanets with semimajor axes beyond about 1 AU through the microlensing effect (Spergel et al. 2015). The goal of the GULLS simulation (Penny et al. 2018) is to predict the yield of the WFIRST microlensing survey. For the nominal baseline WFIRST design, the overall prediction is for ∼1400 bound exoplanets with mass greater than 0.1 M. Given in the tables below is the baseline design — WFIRST Cycle 7, including telescope, instrument and other parameters — assumed for the simulation. Note that the parameters given below were the ones used for the simulations, but they may not necessarily accurately reflect the most recent changes in the conceived WFIRST telescope, instrument and survey parameters.


Generating the Sky Scene

The simulation is performed using the GULLS code, which produces simulated images for each microlensing event it simulates. GULLS was first introduced and described in Penny et al. (2013), where it was called MaBĪ¼LS, and has then been renamed to disambiguate it from the www.mabuls.net online tools (Awiphan et al. 2016). GULLS uses a smooth background plus stars from the Besançon Galactic model (see below). At each epoch a new realization of the counts is made. Counts from stars, smooth backgrounds and instrumental backgrounds (thermal background and dark current) are Poisson realized, and fluctuations from readout noise are Gaussian realized. See the table below for the assumptions about telescope and instrument parameters used in the simulations. For point source simulation, GULLS uses well sampled numerical PSFs generated using the WebbPSF tool (Perrin et al. 2012) with parameters from Cycle 5. Then unweighted relative aperture photometry is performed in a three pixel by three pixel square. GULLS uses user-supplied functions to compute microlensing magnification, including any effects that the user wants to model (e.g., binary lens, parallax).

WFIRST Cycle 7
Name Value
Orbit L2
Mirror diameter (m) 2.36
Obscured fraction (area) 13.9%
Detectors 6 × 3 H4RG-10
Plate scale (arc-sec/pix) 0.11
Field of view (deg2) 0.282
Baseline duration (years) 5

WFIRST Microlensing Survey
Name Value
Total survey duration (d) 432
Seasons 6
Season duration (d) 72
Survey area (deg2) 1.96
Fields 7
Average slew and settle time (s) 83.1
Primary bandpass (μm) 0.93–2.00 (W149)
Secondary bandpass (μm) 0.76–0.98 (Z087)
Photometric precision 0.01 mag @ W149 ∼ 21.15 mag

Name W149 Z087
Zeropoint (mag) 27.615 26.387
Exposure time (s) 46.8 286
Cadence 15.16 min 12.0 hr
Exposures per field ∼ 41000 ∼ 860
Saturation (mag) ∼ 14.8 ∼ 13.9
Bias (counts/pix) 1000 1000
Readout noise (counts/pix) 12.12 12.12
Thermal + dark (counts/pix/s) 1.072 0.130
Sky background (mag/arcsec2) 21.48 21.55
Sky background (counts/pix/s) 3.43 1.04
Error floor (mmag) 1.0 1.0
Saturation§ (103 counts/pix) 679 679

Notes

Magnitude that produces 1 count per second in the detector.

Effective readout noise after multiple non-destructive reads.

Sum of thermal backgrounds (caused by infrared emission of the telescope and its support structures etc.) and dark current.

Evaluated using a zodiacal light model at a season midpoint.

§ Effective saturation level after full exposure time. For WFIRST it is assumed that thanks to multiple reads, useful data can be measured from pixels that saturate after two reads, so for a constant full-well depth, the saturation level increases with exposure time.


GULLS Yield Microlensing Simulator

GULLS uses a modified version of the Besançon Galactic model (Kerins et al. 2009, Robin et al. 2003), with source star counts normalized to HST star counts from Clarkson et al. (2008) and Calamida et al. (2015), and the microlensing event rates are normalized to corrected event rates (Sumi & Penny 2016) from the MOA-II survey (Sumi et al. 2013). Information on similar Euclid simulations is available in Penny et al. (2013) where the simulator was first discussed and referred to as MaBμLS, Manchester-Besançon microLensing Simulator, and the general information in that paper is applicable to WFIRST observations as well. GULLS has also been used for an analysis for the predictions for the detection and characterization of a population of free-floating planets with K2 Campaign 9 (Penny et al. 2017).


Output From the Simulations

Shown at the right is a comparison of a simulated WFIRST infrared color image of a Galactic bulge scene to a simulated optical image of the same scene taken from the ground with a typical PSF FWHM of 0.9 arcsec. The images are 110 arcsec × 110 arcsec. Exposure times were 290s, 52s, and 145s for the WFIRST Z087, W149, and F184 bands, respectively, while the ground-based image used exposure times of 150s, 120s, and 100s in V, R, and I bands, respectively, for a 1.3-m telescope (i.e., similar to the OGLE survey). See https://github.com/mtpenny/wfirst-ml-figures for more plots and tables from Penny et al. (2018).

WFIRST Microlensing Survey - Expected Signal
Name Value
Stars (W149 < 21) ∼ 38 × 106
Stars (W149 < 25) ∼ 240 × 106
Microlensing events ∼ 27000
Planet Detection (0.1 – 104 M) ∼ 1400
Planet Detection (< 3 M) ∼ 200