Table 1.
Open in new tab

Properties of gapped discs and the planets hypothesized to reside within them (confirmed in the case of PDS 70). Column headings: (1) System name. For systems with multiple gaps, we append ‘G#’ to distinguish between different gaps. (2) Stellar mass (Blondel & Djie 2006; Ducourant et al. 2014; Andrews et al. 2018; Keppler et al. 2019; Oberg et al. 2021) (3) Stellar age (Ducourant et al. 2014; Pohl et al. 2017; Andrews et al. 2018; Müller et al. 2018) (4) Planet orbital radius (Dong & Fung 2017; Keppler et al. 2018; Zhang et al. 2018) (5) Planet mass. For the non-PDS 70 planets (first 22 entries), the quoted range in Mp corresponds to disc viscosities α = 10−5–10−3, scaled from the gap-fitting, two-fluid, planet–disc simulations of Zhang et al. (2018) and Dong & Fung (2017) (see Section 2.4.1). The ranges on Mp for PDS 70b and c roughly cover values inferred from infrared photometry and cooling models (Keppler et al. 2018; Müller et al. 2018; Wang et al. 2020). (6) Gas surface density at the planet’s location, as inferred from C18O emission (Isella et al. 2016; Fedele et al. 2017; Favre et al. 2019; Facchini et al. 2021; Nomura et al. 2021; Zhang et al. 2021). The quoted ranges on Σgas in AS 209, IM Lup, HD 163296, and TW Hya accommodate the possibility that the CO:H2 abundance ratio in these discs is lower than in the ISM (Zhang et al. 2019; Calahan et al. 2021; Zhang et al. 2021). (7) Dust surface density at the planet’s location (Fedele et al. 2017; Huang et al. 2018; Benisty et al. 2021; Nomura et al. 2021) accounting for an assumed factor of 7 uncertainty in opacity. Because most gaps are only marginally resolved in mm continuum emission we are likely overestimating Σdust (see Section 2.2). Daggers (†) mark the five gaps which Jennings et al. (2021) found to have lower dust continuum intensities and hence lower Σdust than Huang et al. (2018) found. (8) Disc aspect ratio, mostly taken from Zhang et al. (2018) except for those marked with an asterisk (see Section 2.3). The values for tage, Mp, Σgas, Σdust, and h/r are uncertain and quoted to only one significant figure.

    (1)(2)  (3)(4)(5)(6)(7)  (8)
NameM⋆ (M⊙)tage (Myr)r (au)Mp (M⊕)Σgas (g cm−2)Σdust (g cm−2)h/r
Sz 1140.171393–6N/A0.08–0.60.1
GW Lup0.462742–10N/A0.03–0.2†0.08
Elias 200.48≤ 0.8258–20N/A0.1–0.70.08
Elias 270.490.8693–20N/A0.05–0.30.09
RU Lup0.630.52910–20N/A0.2–10.07
SR 40.680.81160–700N/A0.03–0.2†0.05
Elias 240.780.25730–300N/A0.003–0.020.09
TW Hya-G10.808218–800.04–30.06–0.40.08*
TW Hya-G20.808855–500.008–0.20.002–0.020.09*
Sz 1290.834415–10N/A0.2–10.06
DoAr 25-G10.9529820–30N/A0.05–0.30.07
DoAr 25-G20.9521255–10N/A0.08–0.60.07
IM Lup1.10.511710–300.1–100.03–0.20.1*
AS 209-G11.21960–700N/A0.05–0.3†0.04
AS 209-G21.219930–2000.04–0.40.008–0.060.06*
HD 1426661.58101610–100N/A0.2–10.05
HD 1691421.65105130–3000.1–0.2≤0.010.07*
HD 143006-G11.78422400–6000N/A0.003–0.02†0.04
HD 143006-G21.7845120–100N/A0.02–0.20.05
HD 163296-G12.0101030–200N/A0.2–10.07*
HD 163296-G22.0104890–7001–400.003–0.02†0.08*
HD 163296-G32.0108610–3000.1–200.01–0.090.08*
PDS 70b0.88522300–30000.0008–0.08≤0.020.07*
PDS 70c0.88534300–30000.0008–0.08≤0.020.08*
    (1)(2)  (3)(4)(5)(6)(7)  (8)
NameM⋆ (M⊙)tage (Myr)r (au)Mp (M⊕)Σgas (g cm−2)Σdust (g cm−2)h/r
Sz 1140.171393–6N/A0.08–0.60.1
GW Lup0.462742–10N/A0.03–0.2†0.08
Elias 200.48≤ 0.8258–20N/A0.1–0.70.08
Elias 270.490.8693–20N/A0.05–0.30.09
RU Lup0.630.52910–20N/A0.2–10.07
SR 40.680.81160–700N/A0.03–0.2†0.05
Elias 240.780.25730–300N/A0.003–0.020.09
TW Hya-G10.808218–800.04–30.06–0.40.08*
TW Hya-G20.808855–500.008–0.20.002–0.020.09*
Sz 1290.834415–10N/A0.2–10.06
DoAr 25-G10.9529820–30N/A0.05–0.30.07
DoAr 25-G20.9521255–10N/A0.08–0.60.07
IM Lup1.10.511710–300.1–100.03–0.20.1*
AS 209-G11.21960–700N/A0.05–0.3†0.04
AS 209-G21.219930–2000.04–0.40.008–0.060.06*
HD 1426661.58101610–100N/A0.2–10.05
HD 1691421.65105130–3000.1–0.2≤0.010.07*
HD 143006-G11.78422400–6000N/A0.003–0.02†0.04
HD 143006-G21.7845120–100N/A0.02–0.20.05
HD 163296-G12.0101030–200N/A0.2–10.07*
HD 163296-G22.0104890–7001–400.003–0.02†0.08*
HD 163296-G32.0108610–3000.1–200.01–0.090.08*
PDS 70b0.88522300–30000.0008–0.08≤0.020.07*
PDS 70c0.88534300–30000.0008–0.08≤0.020.08*
Table 1.
Open in new tab

Properties of gapped discs and the planets hypothesized to reside within them (confirmed in the case of PDS 70). Column headings: (1) System name. For systems with multiple gaps, we append ‘G#’ to distinguish between different gaps. (2) Stellar mass (Blondel & Djie 2006; Ducourant et al. 2014; Andrews et al. 2018; Keppler et al. 2019; Oberg et al. 2021) (3) Stellar age (Ducourant et al. 2014; Pohl et al. 2017; Andrews et al. 2018; Müller et al. 2018) (4) Planet orbital radius (Dong & Fung 2017; Keppler et al. 2018; Zhang et al. 2018) (5) Planet mass. For the non-PDS 70 planets (first 22 entries), the quoted range in Mp corresponds to disc viscosities α = 10−5–10−3, scaled from the gap-fitting, two-fluid, planet–disc simulations of Zhang et al. (2018) and Dong & Fung (2017) (see Section 2.4.1). The ranges on Mp for PDS 70b and c roughly cover values inferred from infrared photometry and cooling models (Keppler et al. 2018; Müller et al. 2018; Wang et al. 2020). (6) Gas surface density at the planet’s location, as inferred from C18O emission (Isella et al. 2016; Fedele et al. 2017; Favre et al. 2019; Facchini et al. 2021; Nomura et al. 2021; Zhang et al. 2021). The quoted ranges on Σgas in AS 209, IM Lup, HD 163296, and TW Hya accommodate the possibility that the CO:H2 abundance ratio in these discs is lower than in the ISM (Zhang et al. 2019; Calahan et al. 2021; Zhang et al. 2021). (7) Dust surface density at the planet’s location (Fedele et al. 2017; Huang et al. 2018; Benisty et al. 2021; Nomura et al. 2021) accounting for an assumed factor of 7 uncertainty in opacity. Because most gaps are only marginally resolved in mm continuum emission we are likely overestimating Σdust (see Section 2.2). Daggers (†) mark the five gaps which Jennings et al. (2021) found to have lower dust continuum intensities and hence lower Σdust than Huang et al. (2018) found. (8) Disc aspect ratio, mostly taken from Zhang et al. (2018) except for those marked with an asterisk (see Section 2.3). The values for tage, Mp, Σgas, Σdust, and h/r are uncertain and quoted to only one significant figure.

    (1)(2)  (3)(4)(5)(6)(7)  (8)
NameM⋆ (M⊙)tage (Myr)r (au)Mp (M⊕)Σgas (g cm−2)Σdust (g cm−2)h/r
Sz 1140.171393–6N/A0.08–0.60.1
GW Lup0.462742–10N/A0.03–0.2†0.08
Elias 200.48≤ 0.8258–20N/A0.1–0.70.08
Elias 270.490.8693–20N/A0.05–0.30.09
RU Lup0.630.52910–20N/A0.2–10.07
SR 40.680.81160–700N/A0.03–0.2†0.05
Elias 240.780.25730–300N/A0.003–0.020.09
TW Hya-G10.808218–800.04–30.06–0.40.08*
TW Hya-G20.808855–500.008–0.20.002–0.020.09*
Sz 1290.834415–10N/A0.2–10.06
DoAr 25-G10.9529820–30N/A0.05–0.30.07
DoAr 25-G20.9521255–10N/A0.08–0.60.07
IM Lup1.10.511710–300.1–100.03–0.20.1*
AS 209-G11.21960–700N/A0.05–0.3†0.04
AS 209-G21.219930–2000.04–0.40.008–0.060.06*
HD 1426661.58101610–100N/A0.2–10.05
HD 1691421.65105130–3000.1–0.2≤0.010.07*
HD 143006-G11.78422400–6000N/A0.003–0.02†0.04
HD 143006-G21.7845120–100N/A0.02–0.20.05
HD 163296-G12.0101030–200N/A0.2–10.07*
HD 163296-G22.0104890–7001–400.003–0.02†0.08*
HD 163296-G32.0108610–3000.1–200.01–0.090.08*
PDS 70b0.88522300–30000.0008–0.08≤0.020.07*
PDS 70c0.88534300–30000.0008–0.08≤0.020.08*
    (1)(2)  (3)(4)(5)(6)(7)  (8)
NameM⋆ (M⊙)tage (Myr)r (au)Mp (M⊕)Σgas (g cm−2)Σdust (g cm−2)h/r
Sz 1140.171393–6N/A0.08–0.60.1
GW Lup0.462742–10N/A0.03–0.2†0.08
Elias 200.48≤ 0.8258–20N/A0.1–0.70.08
Elias 270.490.8693–20N/A0.05–0.30.09
RU Lup0.630.52910–20N/A0.2–10.07
SR 40.680.81160–700N/A0.03–0.2†0.05
Elias 240.780.25730–300N/A0.003–0.020.09
TW Hya-G10.808218–800.04–30.06–0.40.08*
TW Hya-G20.808855–500.008–0.20.002–0.020.09*
Sz 1290.834415–10N/A0.2–10.06
DoAr 25-G10.9529820–30N/A0.05–0.30.07
DoAr 25-G20.9521255–10N/A0.08–0.60.07
IM Lup1.10.511710–300.1–100.03–0.20.1*
AS 209-G11.21960–700N/A0.05–0.3†0.04
AS 209-G21.219930–2000.04–0.40.008–0.060.06*
HD 1426661.58101610–100N/A0.2–10.05
HD 1691421.65105130–3000.1–0.2≤0.010.07*
HD 143006-G11.78422400–6000N/A0.003–0.02†0.04
HD 143006-G21.7845120–100N/A0.02–0.20.05
HD 163296-G12.0101030–200N/A0.2–10.07*
HD 163296-G22.0104890–7001–400.003–0.02†0.08*
HD 163296-G32.0108610–3000.1–200.01–0.090.08*
PDS 70b0.88522300–30000.0008–0.08≤0.020.07*
PDS 70c0.88534300–30000.0008–0.08≤0.020.08*
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