| Issue |
A&A
Volume 538, February 2012
|
|
|---|---|---|
| Article Number | L3 | |
| Number of page(s) | 5 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361/201118448 | |
| Published online | 09 February 2012 | |
Online material
Appendix A: Non detections
GASPS is a flux-limited survey. All sources have detection limits for the o-H2O line at 63.32 μm around 10-17 W/m2, with an uncertainty of a factor of two both ways. The list of non detections is given in Table A.1.
Source list, spectral types, and 63.32 μm o-H2O line fluxes.
Appendix B: Location of emission for H2O lines
 |
Fig. B.1
Location of the H2O emission for a typical disc model (M∗ = 0.8 M⊙, L∗ = 0.7 L⊙, Teff = 4400 K, UV excess fUV = 0.01, X-ray luminosity LX = 1030 erg s-1, Rin = 0.1 AU, Rout = 300 AU, Mdisc = 0.01 M⊙, dust/gas = 0.01, ϵ = −1, scale height H0 = 1 AU at r0 = 10 AU, flaring β = 1.1, astronomical silicate with uniform dust size distribution amin = 0.05 μm, amax = 1 mm, and index = 3.5). The 15.738 μm line is used as a typical H2O line detected by Spitzer. We have marked the radii where the cumulative line flux reaches 15% and 85% with vertical lines, for the four selected H2O lines. In addition, the horizontal lines mark the heights above the midplane where 15% and 85% of the line flux, from every vertical column, originate in. The encircled regions are hence responsible for 70% × 70% = 49% of the total line flux (for a pole-on disc). |
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© ESO, 2012
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