The (w)hole survey: An unbiased sample study of transition disk candidates based on Spitzer catalogs

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Table A.1

Sample of transition disk candidates.

ID	Target	RA	Dec	Reg^a	d^b	Color^c	Origin	Prev.^d	Ref
					(pc)		data

1	TCha	11 57 13.53	–79 21 31.5	ϵ Cha	108	[L]	Other	Imag.	1,2
2	RECX11	08 47 01.80	–78 59 35.2	η Cha	97	–	Other	TD	3,4
3	RECX5	08 42 27.09	–78 57 47.9	η Cha	97	[A]	Other	PF	5,4
4	CHXR22E	11 07 13.30	–77 43 49.9	ChaI	160	–	Other	TD	6,7
5	ISO52	11 04 42.58	–77 41 57.1	ChaI	160	[B]	GB	V	8
...

Notes. The full table is available at the CDS.

^(a)

Full names of the regions: Cha = Chamaeleon, Lup = Lupus, CrA = Corona Australis, Oph = Ophiuchus, UppS = Upper Sco, Oph = Ophiuchus, Tau = Taurus, Aur = Auriga, Per = Perseus, TWH = TW Hydrae, Isol. = Isolated.

^(b)

Distances were adopted from the literature as follows: 120 pc for Oph (Loinard et al. 2008), 150 pc for Lup I, IV, V, and VI and 200 pc for LupIII (Comerón 2008; Comerón et al. 2009), 250 pc for Per (Jørgensen et al. 2006), 140 pc for Tau (Kenyon et al. 2008), 450 pc for Aur (Broekhoven-Fiene et al. 2014), 145 pc for Upp Sco (Carpenter et al. 2008), 150 pc for Corona Australis (Sicilia-Aguilar et al. 2008), 109 pc for ϵ Cha (Torres et al. 2008), 160 pc for ChaI (Kim et al. 2009), 180 pc for ChaII (Alcalá et al. 2008), 97 pc for η Cha (Mamajek et al. 1999), and 415 pc for Ser (Dzib et al. 2010).

^(c)

An asterix (*) indicates this target was part of the M10 sample.

^(d)

The full explanation of previous classifications is as follows, according to their recording papers. 1) Cieza et al. (2010): "PF"=Planet-forming disk, "GG"=Grain-growth dominated disk, "PE"=Photoevaportive disk. 2) Merín et al. (2008), Harvey et al. (2007): "L"=low-infrared excess or anemic disk, "H"=high-infrared excess, "T"=T Tauri-like infrared excess. 3) Others: "PTD" = pretransitional disk, "V" = seesaw variability.

Reference. 1) Wahhaj et al. (2010), 2) Huélamo et al. (2015), 3) Megeath et al. (2005), 4) Sicilia-Aguilar et al. (2009), 5) Bouwman et al. (2010), 6) Kim et al. (2009), 7) Luhman et al. (2008), 8) Espaillat et al. (2011).

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