A 1.3 mm SMA survey of 29 variable young stellar objects

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Volume 612 (April 2018)

A&A, 612 (2018) A54

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Table D.1

Summary for individual target sources.

Source name	RNO 1B (V710 Cas)	RNO 1C	SVS 13A(Per-emb-44 A/B)	PP 13S
Evolutionary Class	Class I/II (cluster)	Class I (cluster)	Class I (binary)	Class I
Stellar RA (J2000)	00^h36^m46^s.05	00^h36^m46^s.65	03^h29^m03^s.759	04^h10^m41^s.119
Stellar Dec (J2000)	+63°28′53. ′′29	+63°28′57. ′′90	+31°16′03. ′′99	+38°07′54. ′′41
Spectral type	F8	M (?)	late-F to early-G (unknown type companion separated from ~0. ′′3)	mid-K (?)
Onset (yr)	1978	FUor-like	>1988, <1990	FUor-like
Outburst duration (yr)	≳40	⋯	≳30	⋯
Assumed distance (pc)	929	929	235	350

Synthesized beam	1. ′′3 × 1. ′′1; –25°	1. ′′3 × 1. ′′1; –25°	1. ′′5 × 0. ′′88; 43°	1. ′′7 × 1. ′′0; 54°
(θ_maj ×θ_min; PA)			[31–140 kλ]
Image RMS (mJy beam⁻¹)	1.2	1.2	10.6	7.0

mm RA (J2000)	confused	confused	03^h29^m03^s.75	04^h10^m41^s.12
mm Dec (J2000)	confused	confused	+31°16′03. ′′7	+38°07′54. ′′5
Image component size	⋯	⋯	1. ′′7 ×1. ′′1; 39°	1. ′′8 ×1. ′′1; 49°
(FWHMmaj ×FWHMnmin; PA)			lightly confused
Peak intensity (mJy beam⁻¹)	≲6	≲12	162 ± 16	200 ± 20
Peak S/N	≲5	≲10	15	29
Integrated 1.3 mm Flux (mJy)	⋯	⋯	225 ± 23	229 ± 23

Source name	L1551 IRS5	XZ Tau A	VY Tau	V1118 Ori

Evolutionary Class	Class I (binary)	Class III (binary)	Class III (binary)	Class II (binary)
Stellar RA (J2000)	04^h31^m34^s.08	04^h31^m40^s.095	04^h39^m17^s.412	05^h34^m44^s.747
Stellar Dec (J2000)	+18°08′04. ′′90	+18°13′56. ′′71	+22°47′53. ′′40	−05°33′42. ′′26
Spectral type	Both mid-K ? (separated by 0. ′′3)	M3 (one M0 companion at ~42 AU separation, and potentially an unknown type one at 13 AU separation)	M0 (with a M2-M4 companion, orbital period >350 yr)	M2-M3 (with a companion of unclear spectral type, separation ~76 AU)
Onset (yr)	FUor-like	many	many (1900–1970, 2013–present)	many
Outburst duration (yr)	⋯	a few	0.5–2	~1.2
Assumed distance (pc)	140	140	140	420

Synthesized beam	1. ′′2 × 0. ′′90; –85°	0. ′′54 × 0. ′′39; 86°	0. ′′59 ×0. ′′40; 75°	0. ′′61 ×0. ′′47; 70°
(θ_maj ×θ_min; PA)
Image RMS (mJy beam⁻¹)	3.0	17.0	0.55	0.6

mm RA (J2000)	04^h31^m34^s.16	⋯	⋯	05^h34^m44^s.75
mm Dec (J2000)	+18°08′04. ′′6	⋯	⋯	−05°33′42. ′′3
Image component size	1. ′′3 ×1. ′′1; 137°	⋯	⋯	0. ′′7 ×0. ′′37; 17°
(FWHMmaj ×FWHMmin; PA)
Peak intensity (mJy beam⁻¹)	488 ± 49	3σ < 51	3σ < 1.7	2.3 ± 0.6
Peak S/N	150	⋯	⋯	3.8
Integrated 1.3 mm Flux (mJy)	780 ± 78	3σ < 51	3σ < 1.7	2.3 ± 0.6

Source name	Haro 5a/6a IRS	NY Ori	V1143 Ori	V883 Ori

Evolutionary Class	Class I	Class II	Class II	Class I/II
Stellar RA (J2000)	05^h35^m26^s.560	05^h35^m36^s.011	05^h38^m03^s.896	05^h38^m18^s.1
Stellar Dec (J2000)	−05°03′55. ′′08	−05°12′25. ′′32	−04°16′42. ′′85	−07°02′26″
Spectral type	uncertain	mid-G to early-K	M2	F5
Onset (yr)	FUor-like	many	many	FUor-like
Outburst duration (yr)	⋯	>0.3	~1	⋯
Assumed distance (pc)	450	420	420	460

Synthesized beam	1. ′′2 × 0. ′′88; 90°	2. ′′0 ×0. ′′86; 64°	0. ′′58 ×0. ′′47; 65°	2. ′′4 × 2. ′′2; –55°
(θ_maj ×θ_min; PA)				[271 GHz]
Image RMS (mJy beam⁻¹)	2.4	1.7	0.62	7.6

mm RA (J2000)	05^h35^m26^s.56	05^h35^m36^s.01	⋯	05^h38^m18^s.11
mm Dec (J2000)	−05°03′55. ′′2	−05°12′25. ′′3	⋯	−07°02′25. ′′9
Image component size	1. ′′3 ×1. ′′08; 78°	2. ′′0 ×0. ′′94; 66°	⋯	2. ′′5 ×2. ′′3; 123°
(FWHMmaj ×FWHMmin; PA)
Peak intensity (mJy beam⁻¹)	132 ± 13	29 ± 2.9	⋯	664 ± 66
Peak S/N	55	17	⋯	87
Integrated 1.3 mm Flux (mJy)	171 ± 17	32 ± 3.2	3σ < 1.9	704 ± 70

Source name	V2775 Ori ([ctf93] 216-2)	FU Ori	V1647 Ori	NGC 2071 MM3

Evolutionary Class	Class I	Class I/II	Class I/II	Class I
Stellar RA (J2000)	05^h42^m48^s.488	05^h45^m22^s.368	05^h46^m13^s.135	05^h47^m36^s.6
Stellar Dec (J2000)	−08°16′34. ′′74	+09°04′12. ′′25	−00°06′04. ′′82	+00°20′06
Spectral type	M5	early-K to mid-M (with a ~1 M_⊙ companion, ~0. ′′5 separation)	M0	uncertain
Onset (yr)	>2005, <2007	1936	many	FUor-like
Outburst duration (yr)	>5	>80	a few	⋯
Assumed distance (pc)	420	353	400	400

Synthesized beam	1. ′′1 × 1. ′′0; 73°	1. ′′7 × 0. ′′77; 67°	1. ′′2 × 1. ′′0; −82°	3. ′′9 × 2. ′′9; 86°
(θ_maj ×θ_min; PA)
Image RMS (mJy beam⁻¹)	1.9	1.8	0.66	4.0

mm RA (J2000)	05^h42^m48^s.49	05^h45^m22^s.38	05^h46^m13^s.14	05^h47^m36^s.59
mm Dec (J2000)	−08°16′34. ′′7	+09°04′12. ′′3	−00°06′04. ′′9	+00°20′06. ′′1
Image component size	1. ′′1 ×1. ′′1; 76°	1. ′′3 ×0. ′′83; 69°	1. ′′3 ×1. ′′1; 98°	4. ′′2 ×3. ′′4; 78°
(FWHMmaj ×FWHMmin; PA)				confused
Peak intensity (mJy beam⁻¹)	99 ± 10	18 ± 1.8	69 ± 6.9	55 ± 5.5
Peak S/N	52	9.3	105	14
Integrated 1.3 mm Flux (mJy)	115 ± 12	18 ± 1.8	74 ± 7.4	≲70

Source name	AR 6A/6B	Z CMa NW/SE	Parsamian 21 (HBC 687)	V1515 Cyg

Evolutionary Class	Class I (binary)	Class I (binary)	Class I	Class II
Stellar RA (J2000)	06^h40^m59^s.31/59^s.31	07^h03^m43^s.164	19^h29^m00^s.86	20^h23^m48^s.010
Stellar Dec (J2000)	+09°35′52. ′′0/49. ′′2	−11°33′06. ′′22	+09°38′42.9	+42°12′25. ′′70
Spectral type	early-G to late-K/ Unknown (separated by 2. ′′8)	B8-outbursting / F5-FUor-like (separation ~0. ′′1)	A5e	G2-G5
Onset (yr)	FUor-like/FUor-like	many (1987, 2000, 2004, 2008, etc.)/⋯	FUor-like	1950
Outburst duration (yr)	⋯ /⋯	a few/⋯	⋯	~30
Assumed distance (pc)	800	930	400	1000

Synthesized beam	4. ′′2 × 1. ′′4; 37°	1. ′′1 × 0. ′′93; 42°	1. ′′2 × 0. ′′83; 40°	1. ′′7 × 1. ′′3; 78°
(θ_maj ×θ_min; PA)		[35–162 kλ]	[266 GHz]	[220–277 GHz]
Image RMS (mJy beam⁻¹)	1.3	1.3	1.1	1.0

mm RA (J2000)	⋯	07^h03^m43^s.16	19^h29^m00^s.86	20^h23^m48^s.02
mm Dec (J2000)	⋯	−11°33′06. ′′0	+09°38′42. ′′5	+42°12′25. ′′8
Image component size	⋯	1. ′′4 ×0. ′′90; 38°	1. ′′1 ×0. ′′78; 37°	1. ′′7 ×1. ′′3; 77°
(FWHMmaj ×FWHMmin; PA)		confused
Peak intensity (mJy beam⁻¹)	3σ < 3.9	21 ± 2.1	37 ± 3.7	6.0 ± 1.0
Peak S/N	⋯	16	34	6
Integrated 1.3 mm Flux (mJy)	3σ < 3.9	27 ± 2.7	37 ± 3.7	6.0 ± 1.0

Source name	HBC 722 (V2493 Cyg or PTF 10qpf)	V2494 Cyg (HH 381 IRS)	V1057 Cyg	IRAS 20588+5215N

Evolutionary Class	Class II	Class I/II	Class I/II (binary)	Class I
Stellar RA (J2000)	20^h58^m17^s.029	20^h58^m21^s.09	20^h58^m53^s.72	21^h00^m21^s.40
Stellar Dec (J2000)	+43°53′43. ′′29	+52°29′27. ′′70	+44°15′28. ′′3	+52°27′09. ′′40
Spectral type	K7-M0	G	F7-G3 I-II (with a M-type companion, separation ~30 AU)	uncertain
Onset (yr)	2010	>1983, <1989	1970	Actively accreting,
Outburst duration (yr)	>6	≳20	10-30	but not necessarily a FUor or EXor
Assumed distance (pc)	520	800	600	800

Synthesized beam	3. ′′3 × 3. ′′0; −14°	0. ′′86 × 0. ′′53; 74°	0. ′′87 × 0. ′′50; 76°	1. ′′2 × 1. ′′0; 85°
(θ_maj ×θ_min; PA)
Image RMS (mJy beam⁻¹)	2.4	1.0	0.7	2.1

mm RA (J2000)	⋯	20^h58^m21^s.10	20^h58^m53^s.73	⋯
mm Dec (J2000)	⋯	+52°29′27. ′′5	+44°15′28. ′′4	⋯
Image component size	⋯	0. ′′87 ×0. ′′53; 75°	1. ′′0 ×0. ′′59; 84°	⋯
(FWHMmaj ×FWHMmin; PA)		variable
Peak intensity (mJy beam⁻¹)	3σ < 7.2	117 ± 15	15 ± 2.0	3σ < 6.3
Peak S/N	⋯	117	21	⋯
Integrated 1.3 mm Flux (mJy)	3σ < 7.2	117 ± 15	19 ± 2.0	3σ < 6.3

Source name	V2495 Cyg	V1735 Cyg (Elias 1-12)	V733 Cep (Persson’s star)

Evolutionary Class	Class I/II	Class I/II	Class II
Stellar RA (J2000)	21^h00^m25^s.25	21^h47^m20^s.65	22^h53^m33^s.24
Stellar Dec (J2000)	+52°30′17. ′′0	+47°32′03. ′′8	+62°32′23. ′′8
Spectral type	K5-M1 (uncertain)	F0 II-G0 II	early- to mid-G
Onset (yr)	~1999	>1957 and <1965	>1953 and <1984
Outburst duration (yr)	>8	≳30	≳30
Assumed distance (pc)	800	900	800

Synthesized beam	0. ′′78 × 0. ′′46; 74°	1. ′′2 × 0. ′′97; 85°	3. ′′3 × 2. ′′9; −84°
(θ_maj ×θ_min; PA)
Image RMS (mJy beam⁻¹)	1.0	2.6	0.59

mm RA (J2000)	21^h00^m25^s.24	⋯	⋯
mm Dec (J2000)	+52°30′16. ′′9	⋯	⋯
Image component size	0. ′′78 ×0. ′′49; 75°	⋯	⋯
(FWHMmaj ×FWHMmin; PA)	variable
Peak intensity (mJy beam⁻¹)	73 ± 15	3σ < 7.8	3σ < 1.7
Peak S/N	73	⋯	⋯
Integrated 1.3 mm Flux (mJy)	89 ± 15	3σ < 7.8	3σ < 1.7

Notes: ^b Except for FU Ori of which the parallax distance has been provided by Gaia data releases (Gaia Collaboration 2016), we quoted the target source distances mostly from Audard et al. (2014). We note that the distance of Z CMa may be as high as 1800 pc, which is approximately two times higher than the value we quote here. ^b Spectral types of our target sources may be uncertain. We quote them mainly based on the discussion in Gramajo et al. (2014), Audard et al. (2014), and references therein. We provide the list of references for the sake of crediting the original works, on the other hand not duplicating the related description given that we are not providing any better observational constraints. The protostellar mass of V883 Ori has been constrained by the observations of Keplerian rotation curve with ALMA (Cieza et al. 2016). We do not find dedicated discussion about the protostellar masses of Haro 5a/6a IRS, NGC 2071 MM3, and IRAS 20588+5215N. ^b We specify whether a target source is a confirmed visual or spectroscopic binary or multiple systems in this table. However, we cannot rule out the possibility that some unspecified sources are not yet resolved close binaries. We refer to Reipurth & Aspin (2004b) and references therein for more discussion about multiplicity of these objects.

References: 1)Ábrahám et al. (2004); 2) Andrews et al. (2004); 3) Anglada et al. (2004); 4) Antoniucci et al. (2016); 5) Aspin & Sandell (1994); 6) Aspin & Reipurth (2003); 7) Aspin et al. (2008); 8) Aspin et al. (2009); 9) Beck & Aspin(2012); 10) Beljawsky (1928); 11) Bonnefoy et al. (2017); 12) Briceño et al. (2004); 13) Caratti o Garatti et al. (2011); 14) Caratti o Garatti et al. (2012); 15) Carrasco-González et al. (2009); 16) Chen et al. (2016); 17) Cieza et al. (2016); 18) Cohen & Kuhi (1979); 19) Dibai (1969); 20) Dodin et al. (2016); 21) Eisloeffel et al. (1991); 22) Elias (1978); 23) Fischer et al. (2012); 24) Forgan et al. (2014); 25) Gramajo et al. (2014); 26) Green et al. (2006); 27) Green et al. (2013); 28) Green et al. (2016a); 29) Haas et al. (1990); 30) Hartmann et al. (1989); 31) Hartmann & Kenyon (1996); 32) Herbig (1977); 33) Herbig et al. (2003); 34) Herbig (2008); 35) Hillenbrand (1997); 36) Hodapp & Chini (2014); 37) Kenyon et al. (1988); 38) Kenyon et al. (1989); 39) Kenyon et al. (1991); 40) Kenyon et al. (1993); 41) Kolotilov & Petrov (1983); 42) Koresko et al. (1991); 43) Kospal et al. (2005); 44) Kopatskaya et al. (2013); 45) Krist et al. (1997); 46) Lim et al. (2016); 47) Lodato & Bertin (2001); 48) Lodato & Bertin (2003); 49) Magakian et al. (2013); 50) Miller et al. (2011); 51) Movsessian et al. (2006); 52) Munari et al. (2010); 53) Peneva et al. (2010); 54) Persson (2004); 55) Pueyo et al. (2012); 56) Quanz et al. (2007a); 57) Reipurth & Aspin (1997); 58) Reipurth et al. (2004); 59) Reipurth & Aspin (2004a); 60) Reipurth & Aspin (2004b); 61) Reipurth et al. (2007a); 62) Reipurth et al. (2007b); 63) Reipurth & Aspin (2010); 64) Rodríguez et al. (2003); 65) Sandell & Aspin (1998); 66) Semkov et al. (2010); 67) Semkov et al. (2012); 68) Staude & Neckel (1991); 69) Staude & Neckel (1992); 70) Strom & Strom (1993); 71) Szeifert et al. (2010); 72) de Winter et al. (1994); 73) van den Ancker et al. (2004); 74) Wang et al. (2004); 75) Welin (1971); 76) Zhu et al. (2007); 77) Hillenbrand (1997); 78) Kóspál et al. (2016).

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