Understanding the water emission in the mid- and far-IR from protoplanetary disks around T Tauri stars

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Table D.1

Line and continuum observations of the targets discussed in the main paper.

Object	d [pc]	12.407 μm blend flux^**	13.5/30 μm continuum	538.29 μm line flux	850 μm continuum⁵
		[10^-17 W/m²]	flux ratio¹	[10^-20 W/m0²]	[Jy]

AA Tau	140	<1.33	0.663 ± 0.027	n.a.	n.a.
DM Tau	140	n.a.	n.a.	<1.15⁴	0.237 ± 0.012
DG Tau	140	<10.63	0.388 ± 0.008	67.00 ± 7.00²	1.180 ± 0.118
RW Aur	144	<13.51^*	0.702 ± 0.010^*	n.a.	n.a.
TW Hya	56	n.a.	n.a.	2.72 ± 0.12^3,^*	0.182 ± 0.018^*

Notes.

⁽¹⁾

Ratios have been computed from c2d IRS spectra (Evans et al. 2009);

⁽²⁾

from Podio et al. (2013);

⁽³⁾

scaled to 140 pc from Hogerheijde et al. (2011);

⁽⁴⁾

from Bergin et al. (2010);

⁽⁵⁾

scaled to 140 pc from Di Francesco et al. (2008);

^(*)

flux scaled to 140 pc;

^(**)

12.407 μm fluxes extraction procedure is described in the text of this Appendix.

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