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

Open Access

Table 1

Overview of the sample.

Target name	SpT	Distance (pc)	v_rad (km s⁻¹)	Group	T_eff (K)	L_* (L_⊙)	M_* (M_⊙)	Age (Myr)	Mult.	Ref.	Label
HD 9985	A2	${158.2}_{- 1.0}^{+ 1.0}$ $\[158.2_{-1.0}^{+1.0}\]$	+10.2±3.7	. . .	8900±200	14.18±0.61	1.88±0.04	$44_{- 16}^{+ 31}$ $\[44_{-16}^{+31}\]$	. . .	3	1
HD 31305	A3	${142.6}_{- 2.7}^{+ 2.6}$ $\[142.6_{-2.7}^{+2.6}\]$	−2.1±3.3	TAU	8600±170	16.95±0.64	${1.97}_{- 0.07}^{+ 0.06}$ $\[1.97_{-0.07}^{+0.06}\]$	${2.5}_{- 1.5}^{+ 3.8}$ $\[2.5_{-1.5}^{+3.8}\]$	Y	1	. . .
HD 112532	A2	${119.5}_{- 0.4}^{+ 0.4}$ $\[119.5_{-0.4}^{+0.4}\]$	+12.4±4.4	LCC	8850±200	13.87±0.62	1.87±0.04	15±3	. . .	2	2
HD 131960	F1	${146.6}_{- 0.5}^{+ 0.5}$ $\[146.6_{-0.5}^{+0.5}\]$	+2.58±1.47	UCL	7000±150	4.22±0.18	1.41±0.04	16±2	. . .	2	. . .
HD 141960	A9	${142.5}_{- 0.4}^{+ 0.5}$ $\[142.5_{-0.4}^{+0.5}\]$	+0.90±0.72	US	7400±130	6.46±0.23	1.57±0.04	10±3	. . .	2	3
HD 144277	A3	${143.4}_{- 0.7}^{+ 0.6}$ $\[143.4_{-0.7}^{+0.6}\]$	+1.72±0.49	UCL	8550±170	11.83±0.47	1.80±0.05	16±2	Y	2	. . .
HD 145101	A6	${137.7}_{- 0.9}^{+ 0.8}$ $\[137.7_{-0.9}^{+0.8}\]$	−5.07±0.35	US	7950±200	18.58±0.68	${1.89}_{- 0.05}^{+ 0.14}$ $\[1.89_{-0.05}^{+0.14}\]$	6.7±0.5	. . .	2	4
HD 152989	A6	${114.9}_{- 0.5}^{+ 0.4}$ $\[114.9_{-0.5}^{+0.4}\]$	−7.49±0.80	UCL	7950±150	7.21±0.22	${1.59}_{- 0.03}^{+ 0.02}$ $\[1.59_{-0.03}^{+0.02}\]$	16±2	Y	4	5
HD 155853	A4	${136.1}_{- 0.6}^{+ 0.7}$ $\[136.1_{-0.6}^{+0.7}\]$	+0.39±1.51	UCL	8250±150	11.24±0.41	${1.79}_{- 0.04}^{+ 0.03}$ $\[1.79_{-0.04}^{+0.03}\]$	16±2	. . .	2	6
HD 159595	A3	${93.0}_{- 0.2}^{+ 0.3}$ $\[93.0_{-0.2}^{+0.3}\]$	−9.08±0.65	BPMG?	8450±140	10.58±0.35	1.75±0.03	$21_{- 5}^{+ 4}$ $\[21_{-5}^{+4}\]$	. . .	2	7
HD 170116	A4	${187.8}_{- 0.8}^{+ 0.8}$ $\[187.8_{-0.8}^{+0.8}\]$	−17.83±1.33	. . .	8250±250	11.63±0.60	1.79±0.04	$31_{- 7}^{+ 9}$ $\[31_{-7}^{+9}\]$	. . .	3	8
HD 176497	A4	${153.3}_{- 0.6}^{+ 0.6}$ $\[153.3_{-0.6}^{+0.6}\]$	−5.14±1.64	UCRA	8200±170	8.90±0.37	1.68±0.03	10	. . .	2	9

Notes. Distance estimates are from Bailer-Jones et al. (2021) using their geometric approach that is based only on the Gaia EDR3 parallaxes. Where available, the listed heliocentric radial velocity (v_rad) data were taken from the Gaia DR3 catalogue. For HD 9985 the quoted v_rad is from Gontcharov (2006), while for HD 31305 and HD 112532 we list the optimal radial velocities provided by the BANYAN Σ tool (Gagné et al. 2018), assuming that the star is indeed a member of the stellar association determined from astrometric data alone (Appendix A.3). For a more detailed description of how the listed stellar properties (T_eff, L_*, M_*, group membership, age, and multiplicity) were determined, see Appendix A. Abbreviations in the group column are as follows – COL: Columba moving group; LCC: Lower Centaurus Crux association; TAU: Taurus; UCRA: Upper CrA; UCL: Upper Centaurus Lupus association; US: Upper Scorpius association. Spectral type are derived from the obtained T_eff estimates using the updated online table¹ of stellar parameters compiled by Pecaut & Mamajek (2013). The listed references show those studies in which the infrared excess of the stars was first reported: (1) Clark (1991); (2) Cotten & Song (2016); (3) McDonald et al. (2012); (4) this work. The last column shows which label we use to mark the given object in Figs. 7–9.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.