The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) - I. Motivation, sample, data reduction, and results overview

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Volume 705 (January 2026)

A&A, 705 (2026) A195

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Table 1

Main system parameters of the ARKS sample.

								Expected from REASONS
Name	Dist	Spt	L_⋆	M_⋆	Age	L_cold/L_⋆	a_p	F_belt	i	PA	R	Δ R/R
	[pc]		[L_⊙]	[M_⊙]	[Myr]	[×10⁻⁴]	[au]	[mJy]	[°]	[°]	[au]
Moderately inclined belts (i<75°)
HD 15257	49.0	F1V	14	1.75	$1000_{- 800}^{+ 800}$ $1000^{+800}_{-800}$	0.61		7.5	40	60	270	0.81
HD 76582	48.9	A7V	9.9	1.61	$1200_{- 900}^{+ 900}$ $1200^{+900}_{-900}$	2.0		8.0	72	104	219	0.96
HD 84870	88.8	A9V	7.9	1.66	$300_{- 200}^{+ 200}$ $300^{+200}_{-200}$	4.3		4.8	50	10	260	1.00
HD 92945	21.5	K0V	0.37	0.85	$200_{- 100}^{+ 100}$ $200^{+100}_{-100}$	6.6	PMa: 2−30	10.1	67	100	96	0.83
HD 95086	86.5	A9V	6.4	1.54	${13.3}_{- 0.6}^{+ 1}$ $13.3^{+1}_{-0.6}$	16	52(1)	8.1	29	93	206	0.87
HD 107146	27.5	G0V	1.00	1.04	$150_{- 50}^{+ 100}$ $150^{+100}_{-50}$	9.8	PMa: 2.5−20	39.3	22	149	107	1.03
HD 121617^g	118	A1V	14	1.90	$16_{- 2}^{+ 2}$ $16^{+2}_{-2}$	51		4.8	37	60	78	0.77
HD 131835^g	130	A8V	8.9	1.70	$16_{- 2}^{+ 2}$ $16^{+2}_{-2}$	23		5.5	74	60	84	1.04
HD 145560	121	F5V	3.3	1.35	$16_{- 2}^{+ 2}$ $16^{+2}_{-2}$	20		4.1	47	28	76	0.66
HD 161868	29.7	A1V	24	2.11	$300_{- 200}^{+ 200}$ $300^{+200}_{-200}$	0.65	PMa: 3−25	6.3	68	57	124	0.89
HD 170773	36.9	F4V	3.6	1.40	$200_{- 100}^{+ 100}$ $200^{+100}_{-100}$	4.9		15.8	33	114	194	0.35
HD 206893	40.8	F5V	2.8	1.33	$160_{- 20}^{+ 20}$ $160^{+20}_{-20}$	2.7	3.5,9.7(2)	2.9	24	60	108	0.93
TYC 9340-437-1	36.7	K7V	0.19	0.75	$23_{- 3}^{+ 3}$ $23^{+3}_{-3}$	10		11.0	40	130	130	0.77
HD 218396 (HR 8799)	40.9	A9V	5.5	1.50	$33_{- 10}^{+ 7}$ $33^{+7}_{-10}$	2.5	15,27,41,72(3)	11.2	39	51	290	0.86

Highly inclined belts (i > 75°)
HD 9672 (49 Ceti)^g	57.2	A2V	15	2.00	$45_{- 5}^{+ 5}$ $45^{+5}_{-5}$	7.2		15.2	79	107	136	1.08
HD 10647 (q¹ Eri)	17.3	F8V	1.6	1.12	$1700_{- 600}^{+ 600}$ $1700^{+600}_{-600}$	2.6	2.0(4)	12.8	77	57	100	0.70
HD 14055	35.7	A1V	29	2.19	$300_{- 200}^{+ 200}$ $300^{+200}_{-200}$	0.89		8.5	81	163	180	0.89
HD 15115	48.8	F3V	3.7	1.43	$45_{- 5}^{+ 5}$ $45^{+5}_{-5}$	4.7		5.8	88	98	93	0.23
HD 32297^g	130	A8V	7.0	1.57	$30_{- 10}^{+ 10}$ $30^{+10}_{-10}$	61		9.9	87	48	122	0.51
HD 39060 (β Pic)^g	19.6	A4V	8.7	1.72	$23_{- 3}^{+ 3}$ $23^{+3}_{-3}$	25	2.7,10(5)	56.2	87	30	105	0.88
HD 61005	36.5	G6V	0.62	0.95	$45_{- 5}^{+ 5}$ $45^{+5}_{-5}$	25		16.4	86	70	73	0.52
HD 109573 (HR 4796)	70.8	B9.5V	25	2.14	$10_{- 3}^{+ 3}$ $10^{+3}_{-3}$	42	PMa: 4−38	15.4	76	27	78	0.19
HD 131488^g	152	A3V	12	1.80	$16_{- 2}^{+ 2}$ $16^{+2}_{-2}$	26		8.1	84	96	92	0.50
HD 197481 (AU Mic)	9.71	M1V	0.098	0.61	$23_{- 3}^{+ 3}$ $23^{+3}_{-3}$	3.9	0.070,0.12(6)	17.4	88	129	35	0.36

Notes. Column 2 indicates the distance according to Gaia DR3 (Gaia Collaboration 2023). The approximate spectral types are shown in Column 3, estimated using the stellar effective temperatures of REASONS and the main sequence from Pecaut & Mamajek (2013). The stellar luminosity and fractional luminosity of the cold dust component (Columns 4 and 7) were taken from spectral energy distribution fits using the same methodology as in REASONS (Matrà et al. 2025), but with updated disc fluxes based on ARKS (see Appendix D). The stellar age (Column 6) was taken from REASONS (Matrà et al. 2025). The stellar masses in Column 5 were inferred as described in Appendix C. Column 8 shows the semi-major axes of known planets in these systems. Systems with unknown planets but with a significant (>3σ) proper motion anomaly are labelled as PMa (Kervella et al. 2022), with the values originating from Milli et al. (2026). The last five columns show the expected belt flux at 0.88 mm, the belt inclination, position angle, central radius and fractional width from REASONS. Systems with archival data only and not observed by ARKS are highlighted in grey, and systems with CO gas are flagged ^‘g’. (1): Chauvin et al. (2018); (2): Hinkley et al. (2023); (3): Zurlo et al. (2022); (4): Marmier et al. (2013); (5): Brandt et al. (2021); (6): Mallorquín et al. (2024).

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