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Table 1.
Features used in this work.
| Feature | Description | Reference |
|---|---|---|
| ASF | rms magnitude difference of the SF, computed over a 1 yr timescale | Schmidt et al. (2010) |
| γSF | Logarithmic gradient of the mean change in magnitude | Schmidt et al. (2010) |
| GP_DRW_τ | Relaxation time τ (i.e., time necessary for the time series to become uncorrelated), | Graham et al. (2017) |
| from a DRW model for the light curve | ||
| GP_DRW_σ | Variability of the time series at short timescales (t ≪ τ), | Graham et al. (2017) |
| from a DRW model for the light curve | ||
| ExcessVar | Measure of the intrinsic variability amplitude | Allevato et al. (2013) |
| Pvar | Probability that the source is intrinsically variable | McLaughlin et al. (1996) |
| IARϕ | Level of autocorrelation using a discrete-time representation of a DRW model | Eyheramendy et al. (2018) |
| Amplitude | Half of the difference between the median of the maximum 5% and of the minimum | Richards et al. (2011) |
| 5% magnitudes | ||
| AndersonDarling | Test of whether a sample of data comes from a population with a specific distribution | Nun et al. (2015) |
| Autocor_length | Lag value where the autocorrelation function becomes smaller than ηe | Kim et al. (2011) |
| Beyond1Std | Percentage of points with photometric mag that lie beyond 1σ from the mean | Richards et al. (2011) |
| ηe | Ratio of the mean of the squares of successive mag differences to the variance | Kim et al. (2014) |
| of the light curve | ||
| Gskew | Median-based measure of the skew | – |
| LinearTrend | Slope of a linear fit to the light curve | Richards et al. (2011) |
| MaxSlope | Maximum absolute magnitude slope between two consecutive observations | Richards et al. (2011) |
| Meanvariance | Ratio of the standard deviation to the mean magnitude | Nun et al. (2015) |
| MedianAbsDev | Median discrepancy of the data from the median data | Richards et al. (2011) |
| MedianBRP | Fraction of photometric points within amplitude/10 of the median mag | Richards et al. (2011) |
| MHAOV Period | Period obtained using the P4J Python package (https://github.com/phuijse/P4J) | Huijse et al. (2018) |
| PairSlopeTrend | Fraction of increasing first differences minus the fraction of decreasing first differences | Richards et al. (2011) |
| over the last 30 time-sorted mag measures | ||
| PercentAmplitude | Largest percentage difference between either max or min mag and median mag | Richards et al. (2011) |
| Q31 | Difference between the third and the first quartile of the light curve | Kim et al. (2014) |
| Period_fit | False-alarm probability of the largest periodogram value obtained with LS | Kim et al. (2011) |
| Ψcs | Range of a cumulative sum applied to the phase-folded light curve | Kim et al. (2011) |
| Ψη | ηe index calculated from the folded light curve | Kim et al. (2014) |
| Rcs | Range of a cumulative sum | Kim et al. (2011) |
| Skew | Skewness measure | Richards et al. (2011) |
| Std | Standard deviation of the light curve | Nun et al. (2015) |
| StetsonK | Robust kurtosis measure | Kim et al. (2011) |
| class_star | HST stellarity index | Koekemoer et al. (2007), |
| Scoville et al. (2007b) | ||
| u − B | CFHT u magnitude – Subaru B magnitude | Laigle et al. (2016) |
| B − r | Subaru Suprime-Cam B mag – Subaru Suprime-Cam r+ mag | Laigle et al. (2016) |
| r − i | Subaru Suprime-Cam r+ mag – Subaru Suprime-Cam i+ mag | Laigle et al. (2016) |
| i − z | Subaru Suprime-Cam i+ mag – Subaru Suprime-Cam z++ mag | Laigle et al. (2016) |
| z − y | Subaru Suprime-Cam z++ mag – Subaru Hyper-Suprime-Cam y mag | Laigle et al. (2016) |
| ch21 | Spitzer 4.5 μm (channel2) mag – 3.6 μm (channel1) mag | Laigle et al. (2016) |
Notes. The first two blocks of the table report variability features; class_star is the only morphology feature used. The bottom part of the table reports the color features used, where ch21 is the only MIR color used, while the others are optical or NIR colors.
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