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Table 1:

Stellar parameters and known fluxes of our target sample.
Object Class Spectral type $T_{{\rm adopted}}$ (log g) $_{{\rm adopted}}$ V $F_{{\rm 12~\mu m}}$ Age Ref. d Ref. Av Ref. Sep. Ref.

    [K]   [mag] [Jy] [Myr]   [pc]   [mag]   ['']  
HD 3003 Vega A0V 11 000 4.5 5.07 0.48 $\rm 50 _{- ...}^{+ 197}$ (1) 47 (9) ...   0.1 (?) (26)

HD 34 700 A

TTS G0IVe 6000 4.5 9.15 0.60 ...   ... (10) 0.68 (19) SB / 5.2 / 9.2 (27)

HD 80 951 A

Vega A1V 9500 4.5 6.00 0.44 ...   220 (9) ...   0.3 / 7.1 / 48.2 (26)

HD 109 085

Vega F2V 7000 4.5 4.31 2.18 $\rm 1000_{- 300}^{+ 300}$ (2) 18 (11) 0.12 (20) ...  

HD 123 356 AB

Vega G1V / M? 6000 / 4000 4.5 10.0 / 12.2 1.36 ...   ... (12) 0.16 (20) 2.5 (28)

HD 143 006

TTS G5Ve 5750 4.5 10.21 0.86 $\sim$1 (3) 82 (13) 0.62 (21) ...  

HD 155 555 ABC

TTS G5IV / K0IV-V / M4.5 5750 / ... 4.5 6.88 / 13.0 0.69 $\rm 12_{- 4}^{+ 8}$ (4) 32 (9) ...   SB / 33.0 (26)

HD 181 296 A

Vega A0Vn 9500 4.5 5.03 0.54 $\rm 12_{- 4}^{+ 8}$ (4) 48 (9) 0.12 (20) 4.1 (29)

HD 190 073

HAeBe A2IIIpe 9500 4.5 7.82 7.16 $\rm 1.2_{- 0.6}^{+ 0.6}$ (5) >290 (14) 0.19 (19) ...  

HD 319 139

TTS K5Ve / K7Ve 4250 4.5 10.44 0.45 $\rm 5.5_{- 1.5}^{+ 1.5}$ (6) 83 (15) $\leq$0.12 (22) SB (30)

CD-43 344

TTS (?) M2 4500 4.5 9.42 3.73 ...   ... (10) 0.0 (20) ...  

FU Ori A

FUOR G0II ... 4.5 8.94 5.95 <0.3 (7) 450 (16) 2.2 (23) 0.5 (31)

KK Oph A

HAeBe A6Ve 8750 4.5 9.4 - 12.9 9.87 $\rm 7_{- 0.5}^{+ 1.0}$ (8) 160 (17) 1.6 (24) 1.6 (32)

PDS 144 N

HAeBe A2IV 8750 4.5 14.2 ... ...   $\sim$1000 (18) 3.0 (25) $\sim$5.0 (33)

PDS 144 S

HAeBe A5V 8750 4.5 13.1 ... ...   $\sim$1000 (18) 1.1 (25) $\sim$5.0 (33)

References: Spectral types are obtained either from SIMBAD or one of the cited papers, if a more accurate classification is available in the literature. $T_{{\rm adopted}}$ and (log g) $_{{\rm adopted}}$ list the temperature and surface gravity which we used for the Kurucz atmosphere models. V-band magnitudes and IRAS 12 $\mu $m fluxes are taken from the SIMBAD database. KK Oph shows variability in the visual. PDS 144 is not resolved by IRAS; its V-band fluxes were given by Perrin et al. (2006). Stellar ages: (1) Song et al. (2001), (2) Wyatt et al. (2005) and references therein, (3) Dunkin et al. (1997) and references therein, (4) mean age of the $\beta$ Pic moving group as given in Zuckerman & Song (2001), (5) Catala et al. (2007), (6) Quast et al. (2000), (7) e.g. D'Angelo et al. (2000), (8) Carmona et al. (2007). Errors in the age determinations are quite heterogeneous, depending on the cited work. Distances are taken from (9) Hipparcos parallax, (10) uncertain Hipparcos parallax, (11) Wyatt et al. (2005), (12) The Hipparcos parallax was recently removed from SIMBAD and is likely not firm, (13) Sylvester et al. (1996), (14) van den Ancker et al. (1998), (15) Quast et al. (2000), (16) e.g. Wang et al. (2004), (17) Hillenbrand et al. (1992), (18) Perrin et al. (2006) and references therein. Extinctions: (19) van den Ancker et al. (1998), (20) Sylvester & Mannings (2000), (21) Malfait et al. (1998), (22) Hutchinson et al. (1990), (23) Kenyon et al. (1988), (24) Carmona et al. (2007), (25) Perrin et al. (2006). Stellar separations in multiple systems: (26) Dommanget & Nys (2002), (27) Sterzik et al. (2005), (28) Worley & Douglass (1997), (29) Lowrance et al. (2000), (30) Quast et al. (2000), (31) Wang et al. (2004), (32) Leinert et al. (1997), (33) Perrin et al. (2006). ``SB'' denotes a spectroscopic binary. Note on the multiplicity of HD 155 555: Although the SB components are not spatially resolved, we label them as A and B, since this naming convention existed already in the literature.


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