Microlensing Observations in Astrophysics (MOA) Survey Information

Here we present the publicly available data from the Microlensing Observations in Astrophysics (MOA) collaboration, which operates a joint Japanese/New Zealand ground-based microlensing survey. In total, this data release includes approximately 6,000 photometric light curves, acquired from 2006–2014, using the 1.8m MOA telescope located at Mount John Observatory in New Zealand. These data span 22 target fields, the locations of which are shown in the observational coverage map below, were selected using the methodology described below, and have been made available to the public via the NASA Exoplanet Archive with help from the MOA collaboration.

NASA Exoplanet Archive MOA Resources

The NASA Exoplanet Archive hosts photometric light curves for approximately 6,000 microlensing events detected by the ground-based MOA microlensing survey, totaling roughly 17 GB of data. See the links below to download these data, either as a complete data set (first link in table below), or by specific observational field (subsequent links in table below). Full column descriptions for each light curve are given in the Data Columns page.

Additionally we provide tables with positional information as well as microlensing fit parameter values, derived by the MOA collaboration, for each of the presented light curves (final set of links in table below).

Observational Coverage Map

This figure identifies the 22 target fields observed by the MOA survey, from which the approximately 6,000 microlensing events were selected. (Click for larger image)

Data Selection Criteria

Here we describe the criteria used by the MOA collaboration to identify and select as microlensing events the approximately 6,000 objects presented here. This methodology is a slight variation of what is described in the Supplementary Information section of Sumi, T., et al. (2011) Nature, 473, 349. Please refer to that manuscript for additional details.

1. Cut-0:

On a subtracted image, variable objects can be seen as positive or negative point spread function (PSF) profiles depending on whether the target star is brighter or fainter than in the reference image. We use a custom implementation of the IRAF task DAOFIND to detect these variable objects (like microlensing events), with the modification that both positive and negative PSF profiles are searched for simultaneously. This algorithm finds difference image peaks with a signal to noise ratio (S/N) > 5 and then applies several additional criteria to avoid the detection of spurious variations that are not associated with stellar variability, such as cosmic ray hits, satellite tracks and electrons leaked from the saturated images of bright stars. The positions of detected objects are checked against those obtained in previous reductions of the field. When no object is cross-referenced, the object is classified as new and added to the list of variable object positions. If an object has previously been detected within 8 days, the number of continuous detections for this object, N_{detect,continue}, is incremented. We require that maximum of N_{detect,continue} to be > 2.

2. Cut-1:

Light curves of the candidates passing Cut-0 were then created using PSF fitting photometry on the difference images. The photometric error bars were calibrated with constant stars in each sub-field. We place a 1400-day moving window on each light curve and define the baseline flux to be the weighted average flux outside of that window. We require the baseline to have more than 100 data points and calculated χ²_out/dof for a constant flux fit. We then search for positive light curve "bumps" inside the 1400-day window, with a "bump" defined as a brightening episode with more than 3 consecutive measurements with excess flux > 3σ' above the baseline flux, F_base. We define a statistic χ₃₊ = Σ_i (F_i - F_base) /σ_i' summed over consecutive points with F_i - F_base > 3σ_i'. We cut the objects if χ₃₊ < 40 or ( χ₃₊ < 75 && χ²_out/dof > 3).

3. The candidates were selected by eye inspection of these objects.

This sample include candidates which may be cut by microlensing light curve fitting in the detailed analysis.

MOA Data Acknowledgement

If you make use of data from this archive, please include the following acknowledgement:

This paper makes use of data obtained by the MOA collaboration with the 1.8 metre MOA-II telescope at the University of Canterbury Mount John Observatory, Lake Tekapo, New Zealand. The MOA collaboration is supported by JSPS KAKENHI grant and the Royal Society of New Zealand Marsden Fund. These data are made available using services at the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.

Last updated: 4 April 2019