Interferometric study on the temporal variability of the brightness distributions of protoplanetary disks

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Volume 642 (October 2020)

A&A, 642 (2020) A104

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Table C.1

Overview of the sample.

Name	RA (J2000)	Dec (J2000)	d	Separation	Multi-epoch			Variability	Classification
	(h ms s)	(° ′ ′′)	(pc)	(′′)	data
RY Tau	04 21 57.4	+28 26 35.5			–	A	M

T Tau S	04 21 59.4	+19 32 05.9	144 ± 2 ⁽¹⁾	0.12 ⁽³⁾	–	–	M
T Tau N	04 21 59.4	+19 32 06.4	144 ± 2⁽¹⁾	0.7 ⁽⁴⁾	–	–	M
DG Tau	04 27 04.7	+26 06 16.0	121 ± 2 ⁽¹⁾		–	–	M
Haro 6-10N	04 29 23.7	+24 33 00.9		1.2 ⁽⁵⁾	–	–	M

Haro 6-10S	04 29 23.7	+24 32 59.7		1.2 ⁽⁵⁾	–	–	M

GG Tau	04 32 30.3	+17 31 40.8		0.032 ⁽⁶⁾	–	–	M

DR Tau	04 47 06.2	+16 58 42.8	195 ± 2 ⁽¹⁾		–	–	M
AB Aur	04 55 45.8	+30 33 04.3			–	A	M

HD 31648	04 58 46.3	+29 50 36.0	161 ± 2 ⁽¹⁾		–	–	M
UX Ori	05 04 29.0	–03 47 14.3	322 ± 5 ⁽¹⁾		P	–	M
CO Ori	05 27 38.3	+11 25 38.9	399 ± 7 ⁽¹⁾	2 ⁽⁷⁾	P	–	M
GW Ori	05 29 08.4	+11 52 12.7		0.003 ⁽⁸⁾	P	–	M

HD 36112	05 30 27.5	+25 19 57.1	160 ± 2 ⁽¹⁾		–	–	M
CQ Tau	05 35 58.5	+24 44 54.1	162 ± 2 ⁽¹⁾		P	–	–
V1247 Ori	05 38 05.3	–01 15 21.7	394 ± 10 ⁽¹⁾		P	–	–
HD 37806	05 41 02.3	–02 43 00.7			P	–	–

FU Ori	05 45 22.4	+09 04 12.3		0.4 ⁽⁹⁾	P	–	M

V1647 Ori	05 46 13.1	–00 06 04.9			–	–	M

HD 45677	06 28 17.4	–13 03 11.1			–	A	–

HD 259431	06 33 05.2	+10 19 19.0			–	A	–

HD 50138	06 51 33.4	–06 57 59.4	377 ± 9 ⁽¹⁾		P	A	–	A1(P), A3(A)	a
Z CMa	07 03 43.2	–11 33 06.2		0.1 ⁽¹⁰⁾	–	–	M

HD 72106	08 29 34.9	–38 36 21.1		0.8 ⁽¹¹⁾	–	–	M
HD 85567	09 50 28.5	–60 58 02.9			–	A	–

Hen 3-545	10 59 06.0	–77 01 40.3	186 ± 1 ⁽¹⁾		–	–	M
TW Hya	11 01 51.9	–34 42 17.0	60 ± 0 ⁽¹⁾		P	–	M
DI Cha	11 07 20.7	–77 38 07.3	190 ± 1 ⁽¹⁾	0.2 ⁽¹²⁾	P	–	M
HP Cha	11 08 15.1	–77 33 53.2	200 ± 8 ⁽¹⁾		–	–	M
Ass Cha T 1-23	11 09 53.4	–76 34 25.7	201 ± 6 ⁽¹⁾		–	–	M
WW Cha	11 10 00.1	–76 34 57.0	191 ± 1 ⁽¹⁾		P	–	M
CV Cha	11 12 27.7	–76 44 22.3	192 ± 1 ⁽¹⁾		P	–	M
HD 100453	11 33 05.6	–54 19 28.5	104 ± 0 ⁽¹⁾		–	A	–
DX Cha	12 00 05.1	–78 11 34.6	108 ± 1 ⁽¹⁾	0.002 ⁽¹³⁾	P	A	M	A1(P,A), A3(P)	s, a
CPD-36 6759	15 15 48.4	–37 09 16.0	135 ± 1 ⁽¹⁾		P	A	M
HD 139614	15 40 46.4	–42 29 53.5	134 ± 1 ⁽¹⁾		P	–	M
HD 141569	15 49 57.7	–03 55 16.3	110 ± 1 ⁽¹⁾		P	–	M
HD 142666	15 56 40.0	–22 01 40.0	148 ± 1 ⁽¹⁾		–	A	–
HD 142527	15 56 41.9	–42 19 23.2	157 ± 1 ⁽¹⁾	0.08 ⁽¹⁴⁾	P	A	M	A1(P,A)	–
RU Lup	15 56 42.3	–37 49 15.5	159 ± 2 ⁽¹⁾		P	–	M
HD 143006	15 58 36.9	–22 57 15.2	165 ± 4 ⁽¹⁾		P	–	–
HD 325367	16 03 05.5	–40 18 25.4	157 ± 1 ⁽¹⁾		–	–	M
HD 144432	16 06 57.0	–27 43 09.8	155 ± 1 ⁽¹⁾	1.47 ⁽¹⁵⁾	P	–	M
V856 Sco	16 08 34.3	–39 06 18.3	160 ± 2 ⁽¹⁾		P	A	M	A1(P,A), A3(P,A)	s, a
AS 205 N	16 11 31.4	–18 38 26.3	127 ± 2 ⁽¹⁾	1.3 ⁽¹⁶⁾	P	–	–
SR 4	16 25 56.2	–24 20 48.2	134 ± 1 ⁽¹⁾		–	–	M
Haro 1-6	16 26 03.0	–24 23 36.2	134 ± 1 ⁽¹⁾		–	–	M
GSS 31	16 26 23.4	–24 20 59.6	137 ± 2 ⁽¹⁾		–	–	M
Elia 2-24	16 26 24.1	–24 16 13.5	136 ± 2 ⁽¹⁾		–	–	M
SR 24A	16 26 58.5	–24 45 36.7		5.2 ⁽⁷⁾	P	–	–

SR 21A	16 27 10.3	–24 19 12.6	138 ± 1 ⁽¹⁾	6.7 ⁽¹⁷⁾	P	–	M
SR 9	16 27 40.3	–24 22 04.1	130 ± 1 ⁽¹⁾		P	–	–
Haro 1-16	16 31 33.5	–24 27 37.3	145 ± 1 ⁽¹⁾		P	–	M
V346 Nor	16 32 32.2	–44 55 30.7	620 ⁽²⁾		–	–	M

HD 150193	16 40 17.9	–23 53 45.2	150 ± 2 ⁽¹⁾	1.1 ⁽¹⁸⁾	P	A	M
AS 209	16 49 15.3	–14 22 08.6	121 ± 1 ⁽¹⁾		–	–	M
AK Sco	16 54 44.8	–36 53 18.6	140 ± 1 ⁽¹⁾	0.001 ⁽¹⁹⁾	P	–	–	A3(P)	a
HD 163296	17 56 21.3	–21 57 21.9	101 ± 1 ⁽¹⁾		P	A	M	A1(A), A3(P,A)	s
HD 169142	18 24 29.8	–29 46 49.3	114 ± 1 ⁽¹⁾		P	–	M
MWC 297	18 27 39.5	–03 49 52.1	372 ± 12 ⁽¹⁾		–	A	–
VV Ser	18 28 47.9	+00 08 39.9	415 ± 8 ⁽¹⁾		P	–	–
SVS20N	18 29 57.7	+01 14 05.7		1.58 ⁽²⁰⁾	–	–	M

SVS20S	18 29 57.7	+01 14 05.7		0.32 ⁽²⁰⁾	–	–	M

S CrA N	19 01 08.6	–36 57 19.9	152 ± 2 ⁽¹⁾	1.3 ⁽⁷⁾	P	–	M
R CrA	19 01 53.7	–36 57 08.1		0.012 ⁽²¹⁾	–	A	–	A1(A), A3(A)	–

VV CrA NE	19 03 06.7	–37 12 49.7	149 ± 2 ⁽¹⁾	1.9 ⁽⁷⁾	–	–	M
VV CrA SW	19 03 06.7	–37 12 49.7	149 ± 2 ⁽¹⁾	1.9 ⁽⁷⁾	–	–	M
HD 179218	19 11 11.3	+15 47 15.6	264 ± 3 ⁽¹⁾		P	–	M

Notes. The separations of known binaries are listed in the fifth column, whereas for multiple systems we only give the distance to the companion nearest to the observed object. Separations smaller than the field of view of the VLTI (~0.16′′, Hummel et al. 2016)are indicated in bold face. The flag in the sixth column indicates the availability of multi-epoch observations obtained with PIONIER (P), AMBER (A), and MIDI (M). The seventh column indicates whether evidence for temporal variability is found based on the two approaches described in Sect. 4.1 (A1, direct comparison of interferometric observations obtained using equal baselines) and Sect. 4.3 (A3, comparison of interferometric observations obtained with different baselines). In the last column, the variable objects are classified according to the symmetry of the found variations (s: supposedly symmetric, a: asymmetric, –: unclassified; compare Sect. 5.3).

References. ⁽¹⁾ Bailer-Jones et al. (2018), ⁽²⁾ Evans et al. (1994), ⁽³⁾ Ratzka et al. (2009), ⁽⁴⁾ Dyck et al. (1982), ⁽⁵⁾ Leinert & Haas (1989), ⁽⁶⁾ Di Folco et al. (2014), ⁽⁷⁾ Reipurth & Zinnecker (1993), ⁽⁸⁾ Mathieu et al. (1991), ⁽⁹⁾ Wang et al. (2004), ⁽¹⁰⁾ Koresko et al. (1991), ⁽¹¹⁾ Dommanget & Nys (2000), ⁽¹²⁾ Schmidt et al. (2013), ⁽¹³⁾ Garcia et al. (2013), ⁽¹⁴⁾ Close et al. (2014); Biller et al. (2012), ⁽¹⁵⁾Müller et al. (2011), ⁽¹⁶⁾Ghez et al. (1993), ⁽¹⁷⁾Barsony et al. (2003), ⁽¹⁸⁾Monnier et al. (2017), ⁽¹⁹⁾Jensen et al. (1996), ⁽²⁰⁾Duchêne et al. (2007), ⁽²¹⁾Sissa et al. (2019).

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