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Table 1

Source properties.

Name RA (J2000) Dec (J2000) F 890 μm rms d M L SpT T eff
(mJy) (mJy/beam) (pc) (M) (L) (K)

Sz 65 15:39:27.75 –34:46:17.56 64.49 0.32 150 0.76 0.832 K7 4060
J15450887-3417333 15:45:08.85 –34:17:33.81 46.27 0.5 150 0.14 0.058 M5.5 3060
Sz 68 15:45:12.84 –34:17:30.98 150.37 0.46 150 2.13 5.129 K2 4900
Sz 69 15:45:17.39 –34:18:28.66 16.96 0.28 150 0.19 0.088 M4.5 3197
Sz 71 15:46:44.71 –34:30:36.05 166.04 0.63 150 0.42 0.309 M1.5 3632
Sz 73 15:47:56.92 –35:14:35.15 30.43 0.55 150 0.82 0.419 K7 4060
IM Lup 15:56:09.18 –37:56:06.12 600.0 0.13 150 1.0 1.65 M0 3850
Sz 83 15:56:42.29 –37:49:15.82 426.9 0.72 150 0.75 1.313 K7 4060
Sz 84 15:58:02.50 –37:36:03.08 32.64 0.4 150 0.18 0.122 M5.0 3125
Sz 129 15:59:16.45 –41:57:10.66 181.12 0.52 150 0.8 0.372 K7 4060
J16000236–4222145 16:00:02.34 –42:22:14.99 119.85 0.63 150 0.24 0.148 M4 3270
MY Lup 16:00:44.50 –41:55:31.27 176.81 0.76 150 1.02 0.776 K0 5100
Sz 133 16:03:29.37 –41:40:02.14 69.05 0.77 150 0.63 0.07 K2 4900
Sz 90 16:07:10.05 –39:11:03.64 21.83 0.46 200 0.79 0.661 K7 4060
Sz 98 16:08:22.48 –39:04:46.81 237.29 1.42 200 0.74 2.512 K7 4060
Sz 100 16:08:25.74 –39:06:1.63 54.85 0.58 200 0.18 0.169 M5.5 3057
Sz 108B 16:08:42.86 –39:06:15.04 26.77 0.34 200 0.19 0.151 M5 3125
J16085324–3914401 16:08:53.22 –39:14:40.53 19.57 0.28 200 0.32 0.302 M3 3415
Sz 113 16:08:57.78 –39:02:23.21 22.35 0.27 200 0.19 0.064 M4.5 3197
Sz 114 16:09:01.83 –39:05:12.79 96.41 0.41 200 0.23 0.312 M4.8 3175
J16102955–3922144 16:10:29.53 –39:22:14.83 7.14 0.35 200 0.22 0.158 M4.5 3200
J16124373–3815031 16:12:43.73 –38:15:03.40 29.88 0.49 200 0.47 0.617 M1 3705

Notes. F890 μm is the integrated flux and rms is the root mean square noise from Ansdell et al. (2016). d is the distance to the source: for sources in the Lupus I, II and IV clouds d = 150 pc, while for stars in the Lupus III cloud d = 200 pc (see Comerón 2008). We note that recent measurements from the Gaia space telescope might suggest a distance of 150 pc for the Lupus III cloud. M is the stellar mass as in Ansdell et al. (2016), obtained using evolutionary tracks by Siess et al. (2000). Stellar bolometric luminosity L, effective temperature Teff and spectral type SpT are derived from X-shooter measurements by (Alcalá et al. 2014, 2017).

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