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Home All issues Volume 572 (December 2014) A&A, 572 (2014) A62 Full HTML
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Table 2

Observed Serpens targets and their main properties.

ID Name RA Dec Other names L∗ a Teff a M ∗ a A V L disk b Lbol Ref.
. . (2000) (2000) . L⊙ K M⊙ mag L⊙ L⊙
01 [WMW2007]103 18:29:41.472 01:07:37.90 ... 1.37 4832 1.39 6.2 0.13 1.5 1,2
02 [WMW2007]65 18:29:43.932 01:07:20.80 ... 0.21 4060 0.77 8.0 0.08 0.29 1,2
03 [WMW2007]7 18:29:49.602 01:17:05.83 EC76 1.90 3400 0.32 9.6 -0.8c 1.1 1,4
04 [WMW2007]81 18:29:53.608 01:17:01.73 EC67 0.48 3560 0.38 7.4 0.31 0.79 1,2
05 [WMW2007]38 18:29:55.711 01:14:31.50 GEL4,EC74 1.00 3199 0.24 18.5d 0.2 1.2 1,3
06 [WMW2007]80 18:29:56.553 01:12:59.65 GEL5,SVS4-2,EC79 0.49 ... ... 14.2 0.1 0.59 1,3
07 [WMW2007]85 18:29:56.967 01:12:47.83 EC84 2.00 2965 0.18 19.4d ... ... 2,3
08 [WMW2007]35 18:29:57.737 01:14:05.69 GEL10,EC90 0.27 3270 0.26 9.6 47.73 48 1,5
09 [WMW2007]83 18:29:57.816 01:15:31.86 CK13,EC93 4.40 4900 2.00 24.4d -1.6c 2.8 1,2
10 [WMW2007]70 18:29:57.819 01:12:28.05 [ACA2003]SerA4,EC91 1.00 3600 0.40 40.0d 0.8 1.8 1,4
11 [WMW2007]37 18:29:57.849 01:12:37.90 EC94 4.30 4000 0.70 40.0d 1.8 6.1 1,4
12 [WMW2007]2 18:29:57.858 01:12:51.40 EC92 ... ... ... 9.6 ... 4.8 1
13 [WMW2007]27 18:29:58.205 01:15:21.68 GEL12,CK4,EC97 0.96 3997 0.69 12.8 1.64 2.6 1,2
14 [WMW2007]4 18:29:58.765 01:14:25.78 EC103 ... ... ... 9.6 ... 1.6 1
15 [WMW2007]10 18:30:02.747 01:12:28.06 EC129 9.50 3872 0.68 24.0d -3.7c 5.8 1,3
16 [WMW2007]78 18:30:03.413 01:16:19.14 EC135 0.54 3850 0.57 5.9 0.2 0.74 1,2
17 [WMW2007]73 18:30:07.708 01:12:04.32 ... 0.78 3487 0.35 7.4 0.42 1.2 1,2

Notes. All parameters are taken from the literature, except for M∗, which was recomputed (see text). Assumed distance is 259 pc (Straižys et al. 1996).

(a)

Typical relative uncertainties for the parameters are as follows (see text): L∗ 40%, Teff 20%, M∗ 40%.

(b)

Ldisk is computed as Lbol – L∗ (see Sect. 2.2).

(c)

Ldisk is assumed to be 0 in these sources because Lbol – L∗ gives a negative value.

(d)

For these high-extinction objects the stellar parameters must be considered to be less reliable.

Reference. 1: Evans et al. (2009), 2: Winston et al. (2007, 2009), 3: Gorlova et al. (2010), 4: Doppmann et al. (2005), 5: Oliveira et al. (2009).

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