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 |
References. (1) Fujiyoshi et al. (2015); (2) Dyck et al. (1982); (3) Ratzka et al. (2009); (4) Leinert & Haas (1989); (5) Roccatagliata et al. (2011); (6) Rodríguez et al. (1998); (7) Leinert et al. (1991); (8) Dutrey et al. (2016); (9) Tang et al. (2014); (10) Correia et al. (2006); (11) Davies et al. (2018); (12) Berger et al. (2011); (13) Fang et al. (2014); (14) Wang et al. (2004); (15) Pueyo et al. (2012); (16) Hartmann et al. (1989); (17) Szeifert et al. (2010); (18) ESA (1997); (19) Folsom et al. (2008); (20) Schmidt et al. (2013); (21) Chelli et al. (1988); (22) Kruger et al. (2013); (23) Coulson & Walther (1995); (24) Dunkin et al. (1997); (25) Weinberger et al. (2000); (26) Biller et al. (2012); (27) Müller et al. (2011); (28) Ghez et al. (1993); (29) Koresko (2002); (30) Simon et al. (1995); (31) Reipurth & Zinnecker (1993); (32) Barsony et al. (2003); (33) Prato et al. (2003); (34) Bouvier & Corporon (2001); (35) Garufi et al. (2014); (36) Janson et al. (2016); (37) Eiroa et al. (1987); (38) Duchêne et al. (2007); (39) Baier et al. (1985); (40) Sicilia-Aguilar et al. (2011); (41) Thomas et al. (2007).
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