Table 1
Debris discs, ranked by increasing fractional luminosity fd, with resolved halos in scattered light, for which a power-law fit of the outer radial profile of either the SB, the volumic number density n, or the surface density σ is available in the literature.
| Name | fd = (Ldisc/L*)IR | r0 (au) | rmax (au) | SB (−3.5) | n (−2.5) | σ (−1.5) | i (deg) | Reference |
|---|---|---|---|---|---|---|---|---|
| HD139664 | 9 × 10−5 | 83.1 | 109.4 | −2.5 | 87 | Kalas et al. (2006) | ||
| HD 141943 (d) | 1.2 × 10−4 | 115 | 145 | −4 | 87 | Boccaletti et al. (2019) | ||
| HD160305 | 1.2 × 10−4 | 86 | 106 | −7.1 | 82.3 | Perrot et al. (2019) | ||
| HD202628 | 1.4 × 10−4 | 175 | 200;250 | −4.5;−3.9/−12.9;−2.8 | 61 | Schneider et al. (2016) | ||
| HIP 67497 | 1.4 × 10−4 | 60.7 | 70 | −8.5 or −1.3 (c) | 80 | Bonnefoy et al. (2017) | ||
| HD 53143 | 2.5 × 10−4 | 82 | 110 | −3 | −1 | 45 | Kalas et al. (2006) | |
| AU Mic | 3.9 × 10−4 | 33 | 60 | −3.8 | 90 | Fitzgerald et al. (2007) | ||
| HD 15115 | 5 × 10−4 | 98 | 340/580 | −4.7/−3 | −5.5/−3.5 | 86 | Engler et al. (2019) | |
| HD143675 | 5.6 × 10−4 | 48.1 | 55.6 | −3 | 87.2 | Esposito et al. (2020) | ||
| HD192758 | 5.7 × 10−4 | 95 | 170(?) | −2 | 58 | Choquet et al. (2018) | ||
| HD104860 | 6.3 × 10−4 | 114 | 160 | −3.9 | 54 | Choquet et al. (2018) | ||
| HD172555 | 7.2 × 10−4 | 10.9 | 15 | −9.8 | 103.5 | Engler et al. (2018) | ||
| HD157687 | 7.9 × 10−4 | 78.9 | 211 | −2.2 | 68.3 | Millar-Blanchaer et al. (2016) | ||
| Fomalhaut | 9 × 10−4 | 154 | 209 | −3.3 | 66 | Kalas et al. (2013) | ||
| 49Cet | 9 × 10−4 | 129 | 270 | −2.1 | 79 | Choquet et al. (2017) | ||
| HD107146 | 1.2 × 10−3 | 135.5 | 185 | −4.8 | −2.8 | 18 | Ardila et al. (2004) | |
| HD145560 | 1.27 × 10−3 | 85.3 | 108 | −3 | 44 | Esposito et al. (2020) | ||
| HD 106906 (b) | 1.3 × 10−3 | 67.6 | 110 | −4 | 85 | Lagrange et al. (2016) | ||
| HD35841 | 1.3 × 10−3 | 56 | 110 | −3.55 | 84.9 | Esposito et al. (2018) | ||
| HD 191089 (d) | 1.4 × 10−3 | 45 | 60;400 | −6.1;−2.68 | 59 | Ren et al. (2019) | ||
| HD131835 | 1.4 × 10−3 | 96 | 140 | −2.3 | 75.1 | Feldt et al. (2017) | ||
| TWA 7 (a) | 1.7 × 10−3 | 25 | 70 | −1.5 | 13 | Olofsson et al. (2018) | ||
| HD115600 | 1.7 × 10−3 | 48 | 60 | −7.5 | 79.5 | Currie et al. (2015) | ||
| HD181327 | 2 × 10−3 | 90 | 150;250 | −3.7;−1.7 | 32 | Stark et al. (2014) | ||
| HD15745 | 2.2 × 10−3 | 165 | 450 | −3.5 | 65 | Kalas et al. (2007) | ||
| β Pic | 2.4 × 10−3 | 127 | 193;258 | −4;−3/−4.5;−3.5 | 90 | Golimowski et al. (2006) | ||
| HD117214 | 2.67 × 10−3 | 60.2 | 97.2 | −4.5 | 71 | Esposito et al. (2020) | ||
| HD 32297 (e) | 2.7 × 10−3 | 130 | 400 | −3.2 or −5.3 | −4 or −6 | 90 | Bhowmik et al. (2019) | |
| HD114082 | 3 × 10−3 | 29.6 | ? | −3.9 | 83 | Wahhaj et al. (2016) | ||
| HD61005 | 3 × 10−3 | 60 | ? | −2.7 | 84.1 | Olofsson et al. (2016) | ||
| HD36546 | 4 × 10−3 | 82 | 110 | −2.5 | −1.5 | 78.9 | Lawson et al. (2021) | |
| HD111161 | 4.2 × 10−3 | 72.4 | 98.1 | −3 | 62 | Esposito et al. (2020) | ||
| HD156623 | 4.3 × 10−3 | 80 | 94 | −3.5 | 30 | Esposito et al. (2020) | ||
| HD121617 | 4.8 × 10−3 | 78.3 | 128 | −5.6 | 43.1 | Perrot et al. (2023) | ||
| HR4796 | 5 × 10−3 | 81.4 | 330/123;330 | −5.1/−7.8;−3.8 | 76 | Schneider et al. (2018) | ||
| HD129590 | 5 × 10−3 | 59.3 | 141 | −1.3 | 74.6 | Matthews et al. (2017) | ||
| HIP79977 | 5.21 × 10−3 | 73 | 225 | −2.5 | 84.6 | Engler et al. (2017) |
Notes. r0 is the location of the density peak in the main belt, rmax the radial distance out to which the radial slope of the halo has been constrained. When two different profiles have been obtained for opposite sides of the disc, a forward slash is inserted between the two fits. When the fitted radial slope has the form of a broken power law, two rmax values are given, separated by a semicolon, the first value being the distance at which the slope changes. Likewise, two radial-index values are also given, also separated by a semicolon. The values in parenthesis given at the top of the SB, n, and σ columns correspond to the expected radial-index values in the simplified scenario of STCH and TBWU. Notes: (a) There is a tentative detection of a second ring at 52 au that could be the cause of the apparently shallow profile. (b) Disc around a central binary. Imaged planet at a projected separation of 650 au. (c) The two indices correspond to two separate fits: one with a single belt and one with a double belt (Bonnefoy et al. 2017). (d) (NZ Lup) The slope given here is that beyond the outer ring in the “2 belt” scenario considered (Boccaletti et al. 2019). (e) The values for the SB slopes are derived by eye from Fig. 10 of Bhowmik et al. (2019).
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