The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) - V. Comparison between scattered light and thermal emission

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Volume 705 (January 2026)

A&A, 705 (2026) A199

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Table A.1

List of the 24 ARKS targets, with the main system parameters from Marino et al. (2026b, see there for uncertainties) and their detection or non-detection in scattered light.

Name	Distance [pc]	Spectral type	L_⋆ [L_⊙]	Age [Myr]	L_cold/L_⋆ [×10⁻⁴]	Incl.^(a) [°]	Detected in scattered light ? if yes: Instrument / Filter / Mode^(b)/Ref^(c)
Moderately inclined belts (i < 75°)
HD 15257	49.0	F1V	14	$1000_{- 800}^{+ 800}$ $\[1000_{-800}^{+800}\]$	0.61	59.4 ± 4.9	No
HD 161868	29.7	A1V	24	$300_{- 200}^{+ 200}$ $\[300_{-200}^{+200}\]$	0.65	66.1 ± 1.5	No
HD 76582	48.9	A7V	9.9	$1200_{- 900}^{+ 900}$ $\[1200_{-900}^{+900}\]$	2.0	72.6 ± 0.7	No
HD 206893	40.8	F5V	2.8	$160_{- 20}^{+ 20}$ $\[160_{-20}^{+20}\]$	2.7	45.2 ± 2.5	No
HD 218396 (HR 8799)	40.9	A9V	5.5	$33_{- 10}^{+ 7}$ $\[33_{-10}^{+7}\]$	2.5	28.8 ± 3.3	No^(d)
HD 84870	88.8	A9V	7.9	$300_{- 200}^{+ 200}$ $\[300_{-200}^{+200}\]$	4.3	47.1 ± 2.6	No
HD 170773	36.9	F4V	3.6	$200_{- 100}^{+ 100}$ $\[200_{-100}^{+100}\]$	4.9	32.9 ± 1.9	No
HD 92945	21.5	K0V	0.37	$200_{- 100}^{+ 100}$ $\[200_{-100}^{+100}\]$	6.6	65.4 ± 0.6	ACS / F606W and F814W / I / Golimowski et al. (2011); Ren et al. (2017)
HD 107146	27.5	G0V	1.0	$150_{- 50}^{+ 100}$ $\[150_{-50}^{+100}\]$	9.8	19.3 ± 0.6	ACS / F606W and F814W / I / Ardila et al. (2004); Ertel et al. (2011)
TYC 9340-437-1	36.7	K7V	0.19	$23_{- 3}^{+ 3}$ $\[23_{-3}^{+3}\]$	10	18.0 ± 8.0	NICMOS / F160W / I / this work
HD 95086	86.5	A9V	6.4	$13_{- 0.6}^{+ 1}$ $\[13_{-0.6}^{+1}\]$	16	31.6 ± 3.5	No^(e)
HD 145560	121	F5V	3.3	$16_{- 2}^{+ 2}$ $\[16_{-2}^{+2}\]$	20	47.6 ± 0.6	GPI / H / pI / Hom et al. (2020)
HD 131835	130	A8V	8.9	$16_{- 2}^{+ 2}$ $\[16_{-2}^{+2}\]$	23	74.2 ± 0.2	SPHERE / H / I / Feldt et al. (2017); Jankovic et al. (2026)
HD 121617	118	A1V	14	$16_{- 2}^{+ 2}$ $\[16_{-2}^{+2}\]$	51	44.1 ± 0.6	SPHERE / J / pI / Perrot et al. (2023)

Highly inclined belts (i > 75°)
HD 14055 (γ Tri)	35.7	A1V	29	$300_{- 200}^{+ 200}$ $\[300_{-200}^{+200}\]$	0.89	80.7 ± 0.2	No ^(f)
HD 10647 (q¹ Eri)	17.3	F8V	1.6	$1700_{- 600}^{+ 600}$ $\[1700_{-600}^{+600}\]$	2.6	77.8 ± 0.1	ACS / F606W / I / Lovell et al. (2021)
HD 197481 (AU Mic)	9.71	M1V	0.098	$23_{- 3}^{+ 3}$ $\[23_{-3}^{+3}\]$	3.9	88.3 ± 0.1	SPHERE / H / I and pI / Boccaletti et al. (2015, 2018)
HD 15115	48.8	F3V	3.7	$45_{- 5}^{+ 5}$ $\[45_{-5}^{+5}\]$	4.7	86.7 ± 0.0	SPHERE / J / I (Engler et al. 2019)
HD 9672 (49 Ceti)	57.2	A2V	15	$45_{- 5}^{+ 5}$ $\[45_{-5}^{+5}\]$	7.2	78.7 ± 0.2	SPHERE / H / I / Choquet et al. (2017)
							NICMOS / F110W / I / (Choquet et al. 2017)
HD 39060 (β Pic)	19.6	A4V	8.7	$23_{- 3}^{+ 3}$ $\[23_{-3}^{+3}\]$	25	86.4 ± 0.2	SPHERE / H / pI / van Holstein et al. (2021)
HD 61005	36.5	G6V	0.62	$45_{- 5}^{+ 5}$ $\[45_{-5}^{+5}\]$	25	85.9 ± 0.1	SPHERE / H / I and pI / Olofsson et al. (2016)
HD 131488	152	A3V	12	$16_{- 2}^{+ 2}$ $\[16_{-2}^{+2}\]$	26	85.0 ± 0.1	SPHERE, H, I Pawellek et al. (2024)
HD 109573 (HR 4796)	70.8	B 9.5 V	25	$10_{- 3}^{+ 3}$ $\[10_{-3}^{+3}\]$	42	76.6 ± 0.1	SPHERE / H / I / Milli et al. (2017)
							SPHERE / J / pI / Bonduelle et al. (in prep)
HD 32297	130	A8V	7.0	$30_{- 10}^{+ 10}$ $\[30_{-10}^{+10}\]$	61	88.3 ± 0.0	SPHERE / H / I and pI / Bhowmik et al. (2019)

Notes. The list is grouped into moderately and highly inclined discs, and within each group, the discs are listed in increasing fractional luminosity L_cold/L_⋆. The discs detected in scattered light and analysed in this paper are highlighted in grey. The discs in bold face have been detected in CO with ALMA.

^(a)Inclination of the disc, as estimated from the ARKS ALMA image (Marino et al. 2026b). ^(b)I stands for total intensity while pI stands for polarised intensity. ^(c)Reference corresponding to the scattered light dataset used in this work. Additional scattered light dataset may exist. ^(d)Engler et al. (2025) detected the inner warm disc with SPHERE in polarisation, but the outer cold disc remains elusive. ^(e)A marginal detection in polarised light with SPHERE in the J band is claimed in Chauvin et al. (2018, see their Fig. 15). However, our reanalysis of the data does not recover the signal. ^(f)HD 14055 was observed with IRDIS in the H band in polarised light on 2023-10-14 (PI: Moor) but not detected (private com.).

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