Table 1.
Open in new tab

Key parameters of the sources. The Herbig Ae/Be discs with and without flaring, respectively, are listed first, followed by the T Tauri discs. Within each group, the ordering is by spectral type from early to late.

Object name (alternative)Spectral[ref.]Cat.(a)Distance[ref.]Disc diameter [ref.](b)Flaring(c)
type(pc)(au)(y/n)
HD 100546B9 Ve[1]HAeBe103±6[1]700submm [2]y
HD 179218B9e[3]HAeBe240|$^{+70}_{-40}$|[1]240±40model [4]y
HD 97048 (CU Cha)B9/A0e[1]HAeBe180|$^{+30}_{-20}$|[1]∼750mid-IR [5]y
AB Aur (HD 31293)A0 Ve[1]HAeBe139±19[6]900submm [7]y
HD 36112 (MWC 758)A5 IVe[3]HAeBe205[6]∼330submm [8]y
HD 169142 (MWC 925)A5 Ve[3]HAeBe∼145[3]470±10mm [9]y
HD 100453A9 Ve[3]HAeBe122±10[6]∼100optical [10]y
HD 142527F6 IIIe[11]HAeBe145±15[12]∼600submm [13]y
HD 50138 (MWC 158)B6-7 III-Ve[14]HAeBe(d)500±150[6]>30mid-IR [15]n
HD 163296 (MWC 275)A1-3 Ve[16]HAeBe119|$^{+13}_{-10}$|[6]∼1000submm [17]n
HD 104237 (DX Cha)A4 IVe[3]HAeBe115±5[6]-n
HD 144432A9/F0 Ve[18]HAeBe160|$^{+36}_{-25}$|[6]120±40model [4]n
RNO 90G5[19]T Tauri125[20]--
RY TauK1[19]T Tauri140[21]∼140mm [22]-
DR TauK5[23]T Tauri140[21]180–380(sub)mm [24]-
TW HyaK7[25]T Tauri51±4[26]400(sub)mm [27]-
FZ TauM0[28]T Tauri140[21]200–600mm [24]-
VW ChaM0.5[29]T Tauri180[30]≲ 30near-IR [31]-
Object name (alternative)Spectral[ref.]Cat.(a)Distance[ref.]Disc diameter [ref.](b)Flaring(c)
type(pc)(au)(y/n)
HD 100546B9 Ve[1]HAeBe103±6[1]700submm [2]y
HD 179218B9e[3]HAeBe240|$^{+70}_{-40}$|[1]240±40model [4]y
HD 97048 (CU Cha)B9/A0e[1]HAeBe180|$^{+30}_{-20}$|[1]∼750mid-IR [5]y
AB Aur (HD 31293)A0 Ve[1]HAeBe139±19[6]900submm [7]y
HD 36112 (MWC 758)A5 IVe[3]HAeBe205[6]∼330submm [8]y
HD 169142 (MWC 925)A5 Ve[3]HAeBe∼145[3]470±10mm [9]y
HD 100453A9 Ve[3]HAeBe122±10[6]∼100optical [10]y
HD 142527F6 IIIe[11]HAeBe145±15[12]∼600submm [13]y
HD 50138 (MWC 158)B6-7 III-Ve[14]HAeBe(d)500±150[6]>30mid-IR [15]n
HD 163296 (MWC 275)A1-3 Ve[16]HAeBe119|$^{+13}_{-10}$|[6]∼1000submm [17]n
HD 104237 (DX Cha)A4 IVe[3]HAeBe115±5[6]-n
HD 144432A9/F0 Ve[18]HAeBe160|$^{+36}_{-25}$|[6]120±40model [4]n
RNO 90G5[19]T Tauri125[20]--
RY TauK1[19]T Tauri140[21]∼140mm [22]-
DR TauK5[23]T Tauri140[21]180–380(sub)mm [24]-
TW HyaK7[25]T Tauri51±4[26]400(sub)mm [27]-
FZ TauM0[28]T Tauri140[21]200–600mm [24]-
VW ChaM0.5[29]T Tauri180[30]≲ 30near-IR [31]-

Notes:aCategory based on spectral type of central star. bDisc diameter is taken from resolved imaging at millimetre or submillimetre wavelengths, if available; otherwise from other wavelengths or inferred from model fits. A ‘-’ symbol indicates an unknown disc diameter. cThe division of Herbig Ae/Be objects into ‘flaring’ and ‘non-flaring’ (flat) disc geometries is the same as in Meeus et al. (2013, table 1), based on the mid-infrared dust SED shape (Meeus et al. 2001). A similar classification has not yet emerged for T Tauri objects, because their dust SEDs have a less pronounced dichotomy and they are typically more embedded in surrounding material. dAlthough usually classified as a pre-main-sequence Herbig star, HD 50138 could also be an evolved B[e] star (e.g. Borges Fernandes et al. 2012). References — [1] Van den Ancker, De Winter & Tjin A Djie (1998); [2] Pineda et al. (2014); [3] Van Boekel et al. (2005); [4] Dent et al. (2005, disc diameter from model fit to unresolved data); [5] Lagage et al. (2006); [6] revised Hipparcos parallaxes (Van Leeuwen 2007); [7] Lin et al. (2006); [8] Isella et al. (2010b); [9] Raman et al. (2006); [10] Collins et al. (2009, who infer the disc size of HD 100453 from various observations, including scattered light images from Hubble); [11] (Verhoeff et al. 2011); [12] Acke & Van den Ancker (2004); [13] Fukagawa et al. (2013); [14] Borges Fernandes et al. (2009); [15] Borges Fernandes et al. (2011); [16] Tilling et al. (2012); [17] Isella et al. (2007); [18] Dunkin, Barlow & Ryan (1997); [19] Chen et al. (1995); [20] Pontoppidan, Blake & Smette (2011); [21] Associated with the Taurus star-forming region, typically assumed to be at a distance of 140 pc (Torres et al. 2009); [22] Isella, Carpenter & Sargent (2010a); [23] Mora et al. (2001); [24] Ricci et al. (2010); [25] Webb et al. (1999); [26] Mamajek (2005); [27] Qi et al. (2004); [28] Rebull et al. (2010); [29] Guenther et al. (2007); [30] Pontoppidan et al. (2010); [31] Brandeker et al. (2001, who infer a limit to VW Cha's disc size from near-infrared subarcsecond imaging).

Table 1.
Open in new tab

Key parameters of the sources. The Herbig Ae/Be discs with and without flaring, respectively, are listed first, followed by the T Tauri discs. Within each group, the ordering is by spectral type from early to late.

Object name (alternative)Spectral[ref.]Cat.(a)Distance[ref.]Disc diameter [ref.](b)Flaring(c)
type(pc)(au)(y/n)
HD 100546B9 Ve[1]HAeBe103±6[1]700submm [2]y
HD 179218B9e[3]HAeBe240|$^{+70}_{-40}$|[1]240±40model [4]y
HD 97048 (CU Cha)B9/A0e[1]HAeBe180|$^{+30}_{-20}$|[1]∼750mid-IR [5]y
AB Aur (HD 31293)A0 Ve[1]HAeBe139±19[6]900submm [7]y
HD 36112 (MWC 758)A5 IVe[3]HAeBe205[6]∼330submm [8]y
HD 169142 (MWC 925)A5 Ve[3]HAeBe∼145[3]470±10mm [9]y
HD 100453A9 Ve[3]HAeBe122±10[6]∼100optical [10]y
HD 142527F6 IIIe[11]HAeBe145±15[12]∼600submm [13]y
HD 50138 (MWC 158)B6-7 III-Ve[14]HAeBe(d)500±150[6]>30mid-IR [15]n
HD 163296 (MWC 275)A1-3 Ve[16]HAeBe119|$^{+13}_{-10}$|[6]∼1000submm [17]n
HD 104237 (DX Cha)A4 IVe[3]HAeBe115±5[6]-n
HD 144432A9/F0 Ve[18]HAeBe160|$^{+36}_{-25}$|[6]120±40model [4]n
RNO 90G5[19]T Tauri125[20]--
RY TauK1[19]T Tauri140[21]∼140mm [22]-
DR TauK5[23]T Tauri140[21]180–380(sub)mm [24]-
TW HyaK7[25]T Tauri51±4[26]400(sub)mm [27]-
FZ TauM0[28]T Tauri140[21]200–600mm [24]-
VW ChaM0.5[29]T Tauri180[30]≲ 30near-IR [31]-
Object name (alternative)Spectral[ref.]Cat.(a)Distance[ref.]Disc diameter [ref.](b)Flaring(c)
type(pc)(au)(y/n)
HD 100546B9 Ve[1]HAeBe103±6[1]700submm [2]y
HD 179218B9e[3]HAeBe240|$^{+70}_{-40}$|[1]240±40model [4]y
HD 97048 (CU Cha)B9/A0e[1]HAeBe180|$^{+30}_{-20}$|[1]∼750mid-IR [5]y
AB Aur (HD 31293)A0 Ve[1]HAeBe139±19[6]900submm [7]y
HD 36112 (MWC 758)A5 IVe[3]HAeBe205[6]∼330submm [8]y
HD 169142 (MWC 925)A5 Ve[3]HAeBe∼145[3]470±10mm [9]y
HD 100453A9 Ve[3]HAeBe122±10[6]∼100optical [10]y
HD 142527F6 IIIe[11]HAeBe145±15[12]∼600submm [13]y
HD 50138 (MWC 158)B6-7 III-Ve[14]HAeBe(d)500±150[6]>30mid-IR [15]n
HD 163296 (MWC 275)A1-3 Ve[16]HAeBe119|$^{+13}_{-10}$|[6]∼1000submm [17]n
HD 104237 (DX Cha)A4 IVe[3]HAeBe115±5[6]-n
HD 144432A9/F0 Ve[18]HAeBe160|$^{+36}_{-25}$|[6]120±40model [4]n
RNO 90G5[19]T Tauri125[20]--
RY TauK1[19]T Tauri140[21]∼140mm [22]-
DR TauK5[23]T Tauri140[21]180–380(sub)mm [24]-
TW HyaK7[25]T Tauri51±4[26]400(sub)mm [27]-
FZ TauM0[28]T Tauri140[21]200–600mm [24]-
VW ChaM0.5[29]T Tauri180[30]≲ 30near-IR [31]-

Notes:aCategory based on spectral type of central star. bDisc diameter is taken from resolved imaging at millimetre or submillimetre wavelengths, if available; otherwise from other wavelengths or inferred from model fits. A ‘-’ symbol indicates an unknown disc diameter. cThe division of Herbig Ae/Be objects into ‘flaring’ and ‘non-flaring’ (flat) disc geometries is the same as in Meeus et al. (2013, table 1), based on the mid-infrared dust SED shape (Meeus et al. 2001). A similar classification has not yet emerged for T Tauri objects, because their dust SEDs have a less pronounced dichotomy and they are typically more embedded in surrounding material. dAlthough usually classified as a pre-main-sequence Herbig star, HD 50138 could also be an evolved B[e] star (e.g. Borges Fernandes et al. 2012). References — [1] Van den Ancker, De Winter & Tjin A Djie (1998); [2] Pineda et al. (2014); [3] Van Boekel et al. (2005); [4] Dent et al. (2005, disc diameter from model fit to unresolved data); [5] Lagage et al. (2006); [6] revised Hipparcos parallaxes (Van Leeuwen 2007); [7] Lin et al. (2006); [8] Isella et al. (2010b); [9] Raman et al. (2006); [10] Collins et al. (2009, who infer the disc size of HD 100453 from various observations, including scattered light images from Hubble); [11] (Verhoeff et al. 2011); [12] Acke & Van den Ancker (2004); [13] Fukagawa et al. (2013); [14] Borges Fernandes et al. (2009); [15] Borges Fernandes et al. (2011); [16] Tilling et al. (2012); [17] Isella et al. (2007); [18] Dunkin, Barlow & Ryan (1997); [19] Chen et al. (1995); [20] Pontoppidan, Blake & Smette (2011); [21] Associated with the Taurus star-forming region, typically assumed to be at a distance of 140 pc (Torres et al. 2009); [22] Isella, Carpenter & Sargent (2010a); [23] Mora et al. (2001); [24] Ricci et al. (2010); [25] Webb et al. (1999); [26] Mamajek (2005); [27] Qi et al. (2004); [28] Rebull et al. (2010); [29] Guenther et al. (2007); [30] Pontoppidan et al. (2010); [31] Brandeker et al. (2001, who infer a limit to VW Cha's disc size from near-infrared subarcsecond imaging).

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