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Home All issues Volume 497 / No 2 (April II 2009) A&A, 497 2 (2009) 409-421 Full HTML
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Table 1:

The stellar properties, e.g. spectral type, temperature, luminosity and age range are reported in the first columns (from Meyer et al. 2006, 2008, Hillenbrand et al. 2008). CSO 350 $\mu $m and IRAM 1.2 mm measured fluxes and upper limits are reported in the sixth and seventh column. The detected sources are highlighted in bold. In the ninth column are the references to the stellar distances (listed in the eighth column).
Source Spectral $T_{\rm eff}$ log $(L_{\star}/L_{\hbox{$\odot$ }}$) log(Age) $S_{350~\mu{\rm m}}^{\star}$ $S_{1.2~{\rm mm}}^{\star\star}$ Distance Ref.
  Type [$^{\rm o}$K]     [mJy] [mJy] [pc]  

FEPS sources older than 10 Myr		  

(Obj)HD 60737(Obj)		 G0 5895 0.01 8.0-8.5   <4.5 $38\pm2$ (2)
(Obj)HII1101(Obj) G0V 5988 0.08 8.0-8.5   <2.3 $133\pm4$ (5)
(Obj)HII152(Obj) G5V 5823 -0.10 8.0-8.5   <2.7 $133\pm4$ (5)
(Obj)HII1200(Obj) F6V 6217 0.35 8.0-8.5   <2.3 $133\pm4$ (5)
(Obj)HD 90905(Obj) G1V 6028 0.16 8.0-8.5   <3 $32\pm1$ (2)
(Obj)HII514(Obj) -- 5727 0.11 8.0-8.5   <2.6 $133\pm4$ (5)
(Obj)HD 104860(Obj) F8 5950 0.12 8.0-8.5 $50.1\pm9.3$ $4.4 \pm1.1$ $48\pm2$ (2)
(Obj)HD 377(Obj) G2V 5852 0.09 8.0-8.5   $4.0 \pm1.0$ $40\pm2$ (2)
(Obj)HD 61005(Obj) G8V 5456 -0.25 8.0-8.5 $95\pm12$   $35\pm1$ (2)
(Obj)HD 107146(Obj) G2V 5859 0.04 8.0-8.5 $319\pm6$   $29\pm1$ (2)
(Obj)HD 72687(Obj) G5V 5738 -0.05 8.0-8.5 <54   $46\pm2$ (2)
(Obj)HII250(Obj) -- 5767 -0.04 8.0-8.5   <3.28 $133\pm4$ (5)
(Obj)HD 219498(Obj) G5 5671 0.69 8.5-9.0   <4.8 $150\pm13$ (3)
(Obj)HD 61994(Obj) G6V 5538 0.01 8.5-9.0   <2.6 $28\pm2$ (2)
(Obj)HD 145229(Obj) G0 5893 -0.02 8.5-9.0 <22.5 <2.8 $33\pm1$ (2)
(Obj)HD 150706(Obj) G3(V) 5883 -0.02 8.5-9.0   <3.2 $27\pm1$ (2)
(Obj)HD 204277(Obj) F8V 6190 0.29 8.5-9.0   <2.1 $34\pm1$ (2)
(Obj)HD 85301(Obj) G5 5605 -0.15 8.5-9.0 <17.4 <2.7 $32\pm1$ (2)
(Obj)HD 69076(Obj) K0V 5405 -0.28 9.0-9.7 <42 <2.1 $34\pm1$ (2)
(Obj)HD 205905(Obj) G2V 5925 0.04 9.0-9.7   < 4.6 $26\pm1$ (2)
(Obj)HD 201219(Obj) G5 5604 -0.16 9.0-9.7   <4.1 $36\pm2$ (2)
(Obj)HD 206374(Obj) G6.5V 5580 -0.17 9.0-9.7   <3.9 $27\pm1$ (2)
(Obj)HD 38529(Obj) G8III/IV 5361 0.82 9.0-9.7   <3.2 $42\pm2$ (2)
(Obj)HD 136923(Obj) G9V 5343 -0.29 9.0-9.7   <3.2 $20\pm1$ (2)
(Obj)HD 6963(Obj) G7V 5517 -0.26 9.0-9.7   <4.2 $27\pm1$ (2)
(Obj)HD 122652(Obj) F8 6157 0.18 9.0-9.7 <19.5 3.2 $37\pm1$ (2)
(Obj)HD 187897(Obj) G5 5875 0.12 9.0-9.7   <2.4 $33\pm1$ (2)

FEPS sources older than 10 Myr not included in the statistical analysis		  
(Obj)HD 134319(Obj) G5(V) 5660 -0.14 7.5-8.0 <25.2 <8.5 $44\pm1$ (2)
(Obj)HD 191089(Obj) F5V 6441 0.50 8.0-8.5 $54\pm15$ <3.6 $54\pm3$ (2)
(Obj)HD 25457(Obj) F7V 6172 0.32 8.0-8.5   <2.2 $19\pm1$ (2)
(Obj)HD 8907(Obj) F8 6250 0.32 8.5-9.0   $3.2\pm0.9$ $34\pm1$ (2)

FEPS sources younger than 10 Myr		  

(Obj)[PZ99] J161411.0-230536(Obj)		 K0 4963 0.50 6.5-7.0 <21.9 $3.5\pm1.1$ $145\pm2$ (1)
(Obj)RXJ1612.6-1859a(Obj) K0IV 5372 0.38 6.5-7.0 $43\pm8.7$ $5.9 \pm1.4$ $145\pm2$ (1)
(Obj)HD 143006(Obj) G6/8 5884 0.39 6.5-7.0 $1400 \pm39$   $145\pm2$ (1)
(Obj)SCOPMS214(Obj) K0IV 5318 0.26 6.5-7.0 <72   $145\pm2$ (1)
(Obj)RX J1842.9-3532(Obj) K0IV 4995 -0.01 6.5-7.0 $650\pm29$   $130\pm10$ (3)
(Obj)RX J1852.3-3700(Obj) K3 4759 -0.23 6.5-7.0 $1200 \pm45$   $130\pm10$ (3)
(Obj)HD 35850(Obj) F7/8V 6047 0.25 7.0-7.5   <3.7 $27\pm1$ (2)
(Obj)HE848(Obj) F9V 6309 0.47 7.5-8.0   <3.1 $176\pm5$ (4)
(Obj)HD 77407(Obj) G0(V) 5986 0.08 7.5-8.0   <3.45 $30\pm1$ (2)
(Obj)HD 22179(Obj) G0 5986 0.36 7.5-8.0   <3.3 $100\pm20$ (3)
(Obj)HD 12039(Obj) G3/5V 5688 -0.05 7.5-8.0   <2.7 $42\pm2$ (2)
(Obj)HD 70573(Obj) G1/2V 5896 0.14 7.5-8.0   <2.73 $46\pm15$ (3)
(Obj)HE750(Obj) F5 6421 0.28 7.5-8.0   <4.60 $176\pm5$ (4)
(Obj)HD 135363(Obj) G5(V) 4728 -0.48 7.5-8.0   <2.22 $29\pm1$ (2)

Not in the FEPS list		  

(Obj)HD 82943(Obj)		           <27.9    
(Obj)HD 38207(Obj) F2V 6769 0.72 8.0-8.5   <0.33 $127\pm25$ (3)
(Obj)HD 117176(Obj)           <14.1    
(Obj)HD 218738(Obj)         <21.9 <3.3    
$^{\star}$ The errors and the upper limits refer to the statistical errors (flux rms) and do not include the calibration uncertainty (between 12 and 22% of the flux). $^{\star\star}$ The errors and the upper limits refer to the statistical errors (flux rms) and do not include the calibration uncertainty (between 11 and 16% of the flux). Distance references: 1 de Zeeuw et al. (1999); 2 Perryman et al. (1997); 3 Hillenbrand et al.(2008); 4 Pinsonneault et al. (1998); 5 based on recent Pleiades distances: de Zeeuw et al. (1999), Zwahlen et al. (2004), Soderblom et al. (2004) and Pan et al. (2004).


Source LaTeX | All tables | In the text

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