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Table 3.
Candidate objects for mid-IR variability.
| # | Name |  |
 |
Δtmax, corr (yr) | Δtmax, total (yr) | σrel, corr | σrel, total | Ncorr | Ntotal | Comment |
|---|---|---|---|---|---|---|---|---|---|---|
| 50 | EX Lup | 90.4 | 16.5 | 4.9 | 4.9 | 1.5 | 1.1 | 20 | 17 | Young eruptive star. |
| 5 | T Tau S | 76.1 | 7.6 | 8.2 | 8.2 | 0.7 | 0.5 | 4 | 3 | T Tauri star, a close binary system. Known IR variable (Ghez et al. 1991; Duchêne et al. 2002). |
| 69 | HD 150193 | 40.3 | 2.8 | 6.9 | 6.9 | 7.0 | 0.1 | 13 | 11 | Herbig Ae star. Interferometric spectra are also modulated by an apparent binary signal. A comparison of ISOPHOT-S, ISO-SWS, and UKIRT/CGS3 spectra indicate significant variations both in flux level and shape of the silicate feature (Kóspál et al. 2012). |
| 75 | SVS20N | 37.7 | 0.7 | 3.7 | 3.7 | 0.5 | 0.2 | 6 | 6 | Embedded Herbig Ae star. A gapped model may also fit the data without the need for time variability. |
| 82 | HD 179218 | 31.7 | 4.4 | 5.3 | 5.3 | 2.0 | 0.1 | 21 | 6 | Herbig Ae star. |
| 30 | V1647 Ori | 30.9 | 2.6 | 0.9 | 0.6 | 0.7 | 0.4 | 9 | 3 | Young eruptive star. MIDI observations were taken during its 20037#x2013;2006 outburst. |
| 3 | RY Tau | 29.5 | 29.1 | 9.3 | 9.2 | 0.2 | 0.4 | 7 | 6 | T Tauri star. |
| 78 | S CrA N | 26.6 | 4.2 | 1.1 | 1.1 | 0.9 | 0.3 | 6 | 4 | T Tauri star. Mid-IR variability, with an amplitude of ∼30% was also observed with Spitzer IRS and ISOPHOT-S (Kóspál et al. 2012). |
| 68 | V346 Nor | 25.2 | 9.9 | 1.9 | 1.9 | 0.4 | 0.4 | 19 | 14 | Young eruptive star. |
| 41 | CV Cha | 20.7 | 1.0 | 0.8 | 0.8 | 0.4 | 0.2 | 3 | 3 | T Tauri star. Dispersion also can be due to disk inclination. Variability was marginally observed by Kóspál et al. (2012). |
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