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Table 3:

Mid-IR, far-IR, and submm photometry of all BPMG members that have been observed at submm wavelengths. A $3\sigma $ upper limit on the flux density is given for non-detections.

Star
Other name Instrument $\lambda$ $F_{\nu}$ Reference
      ($\mu $m) (Jy)  
HD 15115   MIPS 24 $0.054\pm0.006$ 1
    IRAS 60 $0.473\pm0.052$ 1
    ISOPHOT 60 $0.415\pm0.020$ 1
    ISOPHOT 90 $0.427\pm0.030$ 1
    SCUBA 850 $0.0049\pm0.0016$ 2
    LABOCA 870 <0.0153 3
HD 35850 AF Lep MIPS 24 $0.0790\pm0.00316$ 4
    MIPS 70 $0.0447\pm0.00447$ 4
    MIPS 160 <0.077 4
    IRAS 12 $0.4900\pm0.0588$ 5, 6
    IRAS 25 $0.080\pm0.008$ 5, 6
    IRAS 60 <0.180 5, 6
    IRAS 100 <1.930 5, 6
    ISOPHOT 60 $0.049\pm0.014$ 5, 6
    ISOPHOT 90 $0.050\pm0.012$ 5, 6
    SCUBA 850 <0.0045 7
HD 39060 $\beta $ Pic MIPS 24 $7.276\pm0.29104$ 4
    MIPS 70 $12.990\pm1.299$ 4
    MIPS 160 $3.646\pm0.43752$ 4
    IRAS 12 $2.38\pm0.10$ 1
    IRAS 25 $10.29\pm0.41$ 1
    IRAS 60 $18.92\pm0.76$ 1
    IRAS 100 $9.32\pm0.37$ 1
    ISOPHOT 60 $14.7\pm0.346$ 8
    ISOPHOT 120 $6.680\pm1.010$ 1
    ISOPHOT 150 $4.390\pm0.670$ 1
    ISOPHOT 170 $3.807\pm0.143$ 1
    ISOPHOT 200 $2.030\pm0.340$ 1
    SCUBA 850 $0.0583\pm0.0065$ 9
    LABOCA 870 $0.0636\pm0.0067$ 3
    SIMBA 1200 $0.0243\pm0.003$ 10
    SEST 1300 $0.0249\pm0.0026$ 16
HD 164249   MIPS 24 $0.076\pm0.0304$ 4
    MIPS 70 $0.624\pm0.0624$ 4
    MIPS 160 $0.104\pm0.01248$ 4
    IRAS 12 $0.280\pm0.028$ 11
    IRAS 25 ${<}0.158\pm$ 11
    IRAS 60 $0.669\pm0.094$ 1
    IRAS 100 <2.63 11
    ISOPHOT 60 $0.761\pm0.0380$ 1
    ISOPHOT 90 $0.560\pm0.0390$ 1
    LABOCA 870 <0.012 3
HD 172555   MIPS 24 $0.766\pm0.03064$ 4
  MIPS 70 $0.197\pm0.0197$ 4
    IRAS 12 $1.34\pm0.05$ 1
    IRAS 25 $0.91\pm0.05$ 1
    IRAS 60 $0.241\pm0.036$ 1
    LABOCA 870 $0.07\pm0.01$ 3
HD 181296 $\eta$ Tel MIPS 24 $0.382\pm0.01528$ 4
    MIPS 70 $0.409\pm0.0409$ 4
    MIPS 160 $0.068\pm0.00816$ 4
    IRAS 12 $0.351\pm0.018$ 1
    IRAS 25 $0.496\pm0.025$ 1
    IRAS 60 $0.449\pm0.040$ 1
    ISOPHOT 60 $0.433\pm0.022$ 1
    ISOPHOT 90 $0.286\pm0.021$ 1
    LABOCA 870 <0.0144 3
HD 181327   MIPS 24 $0.195\pm0.0078$ 4
    MIPS 70 $1.468\pm0.1468$ 4
    MIPS 160 $0.658\pm0.07896$ 4
    IRAS 12 $0.164\pm0.016$ 11
    IRAS 25 $0.286\pm0.023$ 1
    IRAS 60 $1.93\pm0.08$ 1
    IRAS 100 $1.69\pm0.20$ 1
    ISOPHOT 60 $1.730\pm0.170$ 1
    ISOPHOT 90 $1.410\pm0.140$ 1
    ISOPHOT 170 $0.736\pm0.192$ 1
    LABOCA 870 $0.0517\pm0.0062$ 3
HD 191089   MIPS 24 $0.1856\pm0.0076$ 12
    MIPS 70 $0.5443\pm0.0401$ 12
    MIPS 160 $0.2046\pm0.0446$ 12
    IRAS 25 $0.387\pm0.058$ 1
    IRAS 60 $0.729\pm0.058$ 1
    ISOPHOT 60 $0.781\pm0.081$ 1
    ISOPHOT 90 $0.370\pm0.038$ 1
    LABOCA 870 <0.018 3
HD 196982 AT Mic MIPS 24 $0.1160\pm0.00464$ 4
    MIPS 70 <0.018 4
    SCUBA 850 <0.009 7
HD 197481 AU Mic MIPS 24 $0.1430\pm0.00572$ 4
    MIPS 70 $0.2050\pm0.0205$ 4
    MIPS 160 $0.1680\pm0.0202$ 4
    IRAS 60 $0.252\pm0.043$ 1
    SHARC 350 $0.072\pm0.020$ 13, 15
    SCUBA 450 $0.085\pm0.042$ 7
    SCUBA 850 $0.0144\pm0.0018$ 7
HD 199143   MIPS 24 $0.0350\pm0.00014$ 4
    MIPS 70 <0.022 4
    MIPS 160 <0.031 4
    SCUBA 850 <0.0075 7
HD 358623 AZ Cap MIPS 24 $0.0130\pm0.00052$ 4
    MIPS 70 <0.0012 4
    SCUBA 850 <0.0069 7

References. (1) Moór et al. (2006); (2) Williams & Andrews (2006); (3) this paper; (4) Rebull et al. (2008); (5) Spangler et al. (2001); (6) Silverstone (2000); (7) Liu et al. (2004); (8) Habing et al. (2001); (9) Holland et al. (1998); (10) Liseau et al. (2003); (11) Moshir et al. (1993); (12) Hillenbrand et al. (2008); (13) Chen et al. (2005); (14) Di Francesco et al. (2008); (15) Augereau & Beust (2006); (16) Chini et al. (1991).


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