Discovery of carbon monoxide emission from five debris disks around young A-type stars

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Table 5

Stirring of spatially resolved debris disks in our sample.

Target name	M_{disk,self–stir} (M_⊕)	M_pl,stir (M_Jup)
HD 9985	$600_{- 300}^{+ 200}$ $\[600_{-300}^{+200}\]$	${0.10}_{- 0.13}^{+ 0.11}$ $\[0.10_{-0.13}^{+0.11}\]$
HD 112532	$40_{- 40}^{+ 40}$ $\[40_{-40}^{+40}\]$	${0.04}_{- 0.13}^{+ 0.13}$ $\[0.04_{-0.13}^{+0.13}\]$
HD 141960	$100_{- 100}^{+ 100}$ $\[100_{-100}^{+100}\]$	${0.07}_{- 0.14}^{+ 0.14}$ $\[0.07_{-0.14}^{+0.14}\]$
HD 152989^a	$2100_{- 400}^{+ 400}$ $\[2100_{-400}^{+400}\]$	${0.13}_{- 0.06}^{+ 0.06}$ $\[0.13_{-0.06}^{+0.06}\]$
HD 152989^b	$2000_{- 600}^{+ 600}$ $\[2000_{-600}^{+600}\]$	${0.10}_{- 0.08}^{+ 0.08}$ $\[0.10_{-0.08}^{+0.08}\]$
HD 155853	$3000_{- 600}^{+ 600}$ $\[3000_{-600}^{+600}\]$	${1.63}_{- 1.07}^{+ 1.07}$ $\[1.63_{-1.07}^{+1.07}\]$
HD 159595	$800_{- 200}^{+ 300}$ $\[800_{-200}^{+300}\]$	${0.37}_{- 0.32}^{+ 0.34}$ $\[0.37_{-0.32}^{+0.34}\]$
HD 170116	$11 000_{- 4000}^{+ 4000}$ $\[11~000_{-4000}^{+4000}\]$	${0.58}_{- 0.50}^{+ 0.49}$ $\[0.58_{-0.50}^{+0.49}\]$
HD 176497	$600_{- 400}^{+ 400}$ $\[600_{-400}^{+400}\]$	${0.17}_{- 0.30}^{+ 0.30}$ $\[0.17_{-0.30}^{+0.30}\]$

Notes. Minimum disk mass (M_{disk,self–stir}) and minimum planet mass (M_pl,stir) required to excite the disk by self-stirring or secular stirring by an eccentric planet over the life of the system (for details see Sect. 6.6). In the case of HD 152989, both available continuum models (a: Gaussian ring; b: double ring) were considered in the calculations.

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