Table 1: Parameters of Herbig Ae/Be candidates. Evidence for a flared disk and disk outer radius from spectral energy distribution modeling and millimeter interferometry observations. Presence of AIBs and silicate bands. Crystalline signatures.
Object d Sp. type $T_{\rm {eff}}$ $L_\star $ $\chi $a Flared $R_{\rm disk}$b AIBs Sil. Cryst. Ref.
  [pc]   [K] $L_\odot $   disk [AU]        
AB Aur 144 B9/A0Ve 9750 47 105 $\surd$ 140 $\surd$ $\surd$ - (1)
HD 100 546 103 B9Ve 11 000 36 105 $\surd$ 300(150b1) $\surd$ $\surd$ $\surd$ (1)
HD 142 527 200 F7IIIe 6250 31 $4 \times 10^3$ $\surd$   $\surd$ $\surd$ $\surd$c (1)
HD 179218 240 B9e 10 000 80 $2 \times 10^5$ $\surd$ (<600b2) $\surd$ $\surd$ $\surd$c (1)
HD 100453 114 A9Ve 7500 9 $5 \times 10^3$ $\surd$   $\surd$ - - (1)
HD 135344 84 F4Ve 6750 3 $6 \times 10^2$ $\surd$   ? - - (1)
HD 139614 157 A7Ve 8000 12 104 $\surd$   - - - (1)
HD 169142 145 A5Ve 10 500 32 105 $\surd$ 220 $\surd$ - - (1)
HD 104237 116 A4Ve 10 500 40 105 No   - $\surd$ ? (1)
HD 142666 116 A8Ve 8500 11 104 No   $\surd$ $\surd$ $\surd$c (1)
HD 144432 200 A9Ve 8000 32 $3 \times 10^4$ No   - $\surd$ ? (1)
HD 150193 150 A1Ve 10 000 40 105 No   - $\surd$ $\surd$ (1)
HD 163296 122 A3Ve 10 500 30 105 No 360 - $\surd$ $\surd$ (1)
HD 97048 180 B9-A0 10 000 31 105   (300b1-900b2) $\surd$ - - (2)
Elias 1 150 A0-A6 8000 21 $2 \times 10^4$   70 (<200b3) $\surd$ $\surd$ ?d (2)
Lk H$\alpha $ 25 800 A0 9800 9 $2 \times 10^4$   (<1200) $\surd$     (3)
HK Ori 460 A5 8300 12 104   (70) $\surd$ -   (3)
HD 245185 400 A2 9100 17 $3 \times 10^4$   (110) $\surd$     (3)
Lk H$\alpha $ 198 600 A5 8300 6 $6 \times 10^3$   (900) - $\surd$   (3)
BD+61$^{\circ}$154 650 B8 11 200 330 106   (900) -     (3)
T Ori 460 B9 10 700 83 $3 \times 10^5$   (88) - -   (3)
V380 Ori 460 B9 10 700 85 $3 \times 10^5$   (150) - $\surd$   (3)
HD 250550 700 B7 12 300 240 106   (410) - -   (3)
Lk H$\alpha $ 208 1000 B7 12 300 210 106   (1600) -     (3)
VV Ser 440 B9 10 700 100 $4 \times 10^5$   (410) - -   (3)
WW Vul 700 A3 8700 20 $3 \times 10^4$   (88) -     (3)
BD+46$^{\circ}$3471 1000 A0 9800 508 106   (190) -     (3)
Lk H$\alpha $ 233 880 A5 8300 30 $3 \times 10^4$   (320) - $\surd$   (3)
WL 16 125 B8-A7 9000 240 $4 \times 10^5$   (450) $\surd$ - - (4)
$\surd$ : detection, ?: possible detection, -: no detection.
a Far-ultraviolet (FUV, 6 $<h\nu<$ 13.6 eV) flux at 150 AU from the star expressed in units of the average interstellar radiation field, $1.6\times 10^{-6}$ W m-2 (Habing 1968).
b In parenthese we give estimate of the PAH emission extension. References: (b1) van Boekel et al. (2004); (b2) Siebenmorgen et al. (2000); (b3) Brooke et al. (1993).
c Possible blend with the PAH 11.2(3) $\mu $m band.
d Hanner et al. (1994).
References: (1) Meeus et al. (2001) and references therein; (2) Van Kerckhoven et al. (2002) and references therein; (3) for astrophysical parameters Hillenbrand et al. (1992) (except for BD+46$^{\circ}$3471 see Berrilli et al. (1992) and for VV Ser see Testi et al. (1998)); for PAH emission extension and AIBs detection Brooke et al. (1993); for silicate emission features detection Berrilli et al. (1992); (4) Ressler & Barsony (2003) and references therein.

Source LaTeX | All tables | In the text