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Table 1.

Multiple stellar systems in the atlas.

# Name Type Separation (″) Modulation of MIDI phases Comment References
1 SVS 13A1 eruptive 0.3 no Only one star (VLA 4B) in the close binary system has mid-IR emission associated with it. 1
4 T Tau N TT 0.7 no Triple system: T Tau N and S is a wide binary, T Tau Sab is a close binary sytem. 2
5 T Tau S TT 0.1 yes Sa, Sb: a close binary system itself. 3
7 Haro 6-10N TT 1.2 no Both components are embedded in a common envelope. The disks of the components are highly misaligned. 4,5
8 Haro 6-10S TT 1.2 no Both components are embedded in a common envelope. The disks of the components are highly misaligned. 4,5
9 HBC 393 eruptive 0.32 n/a Binary protostar, listed also as a FUor, (N, S components), both components have disks. 6
11 GG Tau Aab TT 0.25 yes Quadruple system: Aab–Bab 10″ separation, Aa–Ab 0.25″ separation, Ba–Bb 1.48″ separation, having a circumbinary disk. MIDI observed GG Tau Aab pair. 7,8
14 UY Aur B TT 0.88 no Both components have circumstellar disks, and a circumbinary ring. 9
15 UY Aur A TT 0.88 no Both components have circumstellar disks, and a circumbinary ring. 9
17 AB Aur HAe yes At the longest baselines phases show binary signal.
21 CO Ori HAe 2 no The primary (CO Ori A) shows UX Ori-type variability. CO Ori B is a K2–K5 type star, which also has circumstellar material. 10,11
22 GW Ori TT/HAe 0.02 yes Triple system, containing a spectroscopic binary and a tertiary component at ∼20 mas from the primary. The components of the spectroscopic binary are separated by ∼1 au (∼3.5 mas), based on radial velocity measurements. At the longest baselines phases show weak modulation, probably caused by the tertiary component. 12,13
29 FU Ori eruptive 0.4 no FU Ori N: main component, FU Ori S is embedded is (AV = 8) and 5–6 mag fainter in J and H. 14,15
32 Z CMa eruptive 0.1 yes The NW component is a Herbig Be star, which shows EXor-like outbursts, the SE component exhibits broad double-peaked optical absorption lines that are typical of a FU Ori object. 16,17
34 HD 72106 HAe 0.8 yes The primary (A) is a late B-type magnetic star, secondary (B) is a Herbig A. The weak modulation is possibly not the signal of the companion, but may be due to asymmetric disk structure. 18,19
37 DI Cha TT 0.2 no It is a quadruple system with a hierachical structure, consisting of two binaries: a G2/M6 pair (A and D, separation: 0.2″) and a pair of two M5.5 dwarfs (B and C, separation: 0.06″). Separation of A and B is 4.6″. MIDI observed source A. Source D is possibly a brown dwarf. 20
38 Glass I TT 2.4 no Multiple system: Glass Ia is binary with K (WTTS) and M star components. Glass Ib is a G-type young star, which dominates the mid-IR emission of the system. MIDI observed Glass Ib. 21,22
44 HD 135344B HAe 21 no Visual binary, the companion (HD 135344 or HD 135344A) is well separated. 23,24
46 HD 141569 HAe 7.5 no Triple system in a comoving group, the primary (HD 141569A) was observed with MIDI. The companions (B and C, separation: 1.4″) form a binary pair 7.5″ from A. 25
47 HD 142527 HAe 0.088 yes Faint companion HD 142527 B 13 au from the primary (A). Modulation can be seen at the longest baselines. 26
51 HD 144432 HAe 1.47 no Hierarchical triple system. The components B and C are located 1.47″ north of the primary star (A). B and C are separated by 0.1″. MIDI observed component A. 27
53 AS 205 N TT 1.3 no This is the A (North) component. 28
54 AS 205 S TT 1.3 no This is the B (South) component. 28
57 HBC 639 TT 2 no Aka. DoAr 24E. The primary (DoAr 24E A) is a weak line T Tauri star. The secondary (DoAr 24E B) is an infrared companion, an active class I object, a binary itself. MIDI observed the primary component. 28,29
60 SR 24N TT 0.197 yes North component of the triple system, itself a binary. 30
61 SR 24S TT 5.2 no South component of the triple system, located 5.2″ from SR 24N. 31
63 SR 21A TT/HAe 6.7 no SR 21A and SR 21B are classified as a binary, however it does not appear to be a bound, co-eval system. 32,33
69 HD 150193 HAe 1.1 yes HD 150193A is physically associated with a K4 star (HD 150193B). The disk of component A (which was observed with MIDI) has an asymmetric structure due to the interaction with HD 150193B, where no disk was detected. 34,35
71 AK Sco HAe 0.001 no Spectroscopic binary with a semimajor axis of 0.16 au. It has a circumbinary disk. 36
75 SVS20N TT 1.58 no Triple system: SVS20N and S is a wide binary, SVS20S is a close binary sytem. 37,38
76 SVS20S embHAe 0.32 no SVS20S is a close binary sytem itself. 37,38
77 S CrA S TT 1.4 no 31,39,40
78 S CrA N TT 1.4 no 31,39,40
80 VV CrA NE TT 2 no 31,40
81 VV CrA SW TT 2 no 31,40
82 HD 179218 HAe 2.5 yes The modulation is possibly not caused by the known companion. 41

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