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CBF = | Close binary, full period. These stars are contact or near-contact eclipsing binaries for which the Fourier fit has found the correct period and hence fit the primary and secondary eclipses separately; |

CBH = | Close binary, half period. These stars are contact or near-contact eclipsing binaries for which the Fourier fit has settled on half the correct period and hence has overlapped the primary and secondary eclipses. Physically, the CBF and CBH stars are expected to differ in that the primary and secondary eclipses are likely to be more similar in depth in the latter class; |

DBF = | Distant binary, full period. These stars are detached eclipsing binaries for which the Fourier fit has found the correct period and hence fit the primary and secondary eclipses separately; |

DBH = | Distant binary, half period. These stars are fully detached eclipsing binaries for which the Fourier fit has settled on half the correct period and hence has overlapped the primary and secondary eclipses; |

IRR/LPV = | The acronyms stand for "long-period" and "irregular" variables. These classes serve as "catch-all" bins for objects that do not seem to fit into any of our more specific categories. The LPV class contains objects whose variations appear to be dominated by low frequencies, corresponding to P≳5 days, while the IRR class contains objects whose dominant frequencies are higher. Most of the stars classified as LPV or IRR (especially the latter) do not show coherent variations that can be folded cleanly with a single period. Hence, both classes are in some sense "irregular," though the characteristic timescales are different. Among the objects that cannot be cleanly phased to a single period, the LPV class surely includes many semiregular red giant variables, while the IRR class has a large number of cataclysmic binaries; |

MIRA = | Mira variables. These stars are a subset of the LPV's that have photometric amplitudes exceeding 2.0 mag in either the cyan or orange filter. They generally show coherent periodicity, but the two-year temporal baseline of our data may in many cases be insufficient to solve for the period accurately; |

MPULSE = | Stars showing modulated pulsation, such that the Fourier fit has settled on a period double or triple the actual pulsation, in order to render multiple pulses of different amplitudes or shapes. These objects could be multimodal or Blazhko-effect stars, or stars exhibiting some other kind of variability in addition to their pulsations; |

MSINE = | Stars showing modulated sinusoids. These are exactly analogous to the MPULSE stars, except that instead of a classic sawtooth pulse light curve, the fundamental waveform being modulated is a simple sinusoid. Thus, MSINE stars may show two, three, four, five, or even six cycles through the Fourier fit. Each cycle appears to be a good approximation to a sine wave, but the amplitude and/or mean magnitude varies from one to the next. Physically, the MSINE stars may include spotted ellipsoidal variables, rotating stars with evolving spots, and sinusoidal pulsators such as RR Lyrae (RRC) stars that have multiple modes or multiple types of variability; |

NSINE = | Sinusoidal variables with much residual noise or with evidence of additional variability not captured in the fit. Many spotted rotators with evolving spots likely fall into this class, as well as faint or low-amplitude δ Scuti stars and ellipsoidal variables; |

PULSE = | Pulsating stars showing the classic sawtooth light curve, regardless of period. They are expected to include both RR Lyrae and δ Scuti stars, and some Cepheids. These classes are resolvable based on period, color, amplitude, and the phase offsets of the various Fourier terms; |

SHAV = | These are the slow high-amplitude variables, an extremely rare class with long periods and Mira-like amplitudes, but with color insufficiently red for a true Mira. Only 17 of these were identified in our entire catalog. They include AGNs, R Coronae Borealis stars, and at least one apparent nova; |

SINE = | Sinusoidal variables. These stars exhibit simple sine-wave variability with little residual noise. Ellipsoidal variables likely dominate this class; |

STOCH = | These are the variables that do not fit into any coherent periodic class, not even IRR. They would be classified as "dubious" except that they have ddcSTAT=1, meaning that detections on the difference images demonstrate their genuine variability. Their physical nature is unclear, but many of them do appear to exhibit highly significant stochastic variations with very little coherence on the timescales probed by ATLAS; |

dubious = | Star might not be a real variable. |

http://cdsannotations.u-strasbg.fr/annotations/vizierTable//

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