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Table 12

Stellar parameters and X-ray upper limits for probable and possible members of Collinder 69 (taken from D&M1999, ByN2004 and Morales 2008) that are undetected in X-rays (western pointing –Col69 W).

Designation RA Dec Catalog XMM- Rate log Lx IRAC Disk? T eff Lum(bol) Mass
field class type Model Logg = 4 5 Myr [L] [M]

(1) [10-3 cts/s] [erg/s] (2) (3) (4) (5) (6)

C69WI1-09288 5:34:03.910 +09:52:12.30 1 sq. deg W  <0.91  <29.2  <−3.63 II Thin NG 3000 3615 0.1757 0.0016 0.396
C69WI1-14892 5:33:21.960 +10:02:02.00 1 sq. deg W  <1.31  <29.3  <−3.12 II Thick Ku 4250 3196 0.0685 0.0005 0.184
LOri005 5 33 53.65 +09 43 7.97 CFHT1999 W  <1.94  <29.5  <−4.03 III Diskless Ku 4000 4360 0.8880 0.0089 1.140
LOri007 5 34 29.55 +09 48 58.70 CFHT1999 W  <1.72  <29.5  <−3.88 III Diskless Ku 4000 4188 0.6309 0.0082 0.935
LOri011 5 34 44.66 +09 53 57.50 CFHT1999 W  <3.64  <29.8  <−3.62 III Diskless Ku 3750 4227 0.6807 0.0075 0.980
LOri015 5 34 21.84 +10 4 14.50 CFHT1999 W  <1.33  <29.4  <−3.97 III Diskless Ku 4250 4168 0.6054 0.0061 0.911
LOri046 5 34 26.08 +09 51 49.70 CFHT1999 W  <1.30  <29.3  <−3.48 III Diskless Ku 3750 3556 0.1583 0.0017 0.366
LOri053 5 34 36.71 +09 52 58.10 CFHT1999 W  <2.50  <29.6  <−3.12 III Diskless NG 3700 3482 0.1365 0.0016 0.327
LOri071 5 34 15.78 +10 6 54.44 CFHT1999 W  <1.79  <29.5  <−2.96 III Diskless NG 3300 3224 0.0746 0.0008 0.195
LOri081 5 33 56.64 +10 6 14.70 CFHT1999 W  <1.12  <29.3  <−2.91 II Thick NG 3600 3075 0.0422 0.0006 0.133
LOri086 5 34 11.56 +09 49 15.61 CFHT1999 W  <1.28  <29.3  <−2.89 III Diskless NG 3600 3066 0.0402 0.0006 0.129
LOri087 5 34 33.72 +09 55 33.44 CFHT1999 W  <1.72  <29.5  <−2.77 III Thin NG 3400 3106 0.0488 0.0007 0.145
LOri091 5 34 35.82 +09 54 25.99 CFHT1999 W  <1.66  <29.5  <−2.76 II Thin NG 3100 3098 0.0472 0.0006 0.142
LOri093 5 34 41.19 +09 50 16.34 CFHT1999 W  <5.57  <30.0  <−2.18 III Diskless NG 3400 3062 0.0393 0.0006 0.127
LOri094 5 34 43.18 +10 1 59.92 CFHT1999 W b b b III Diskless NG 3200 3067 0.0403 0.0005 0.129
LOri105 5 34 17.57 +09 52 30.14 CFHT1999 W  <1.23  <29.3  <−2.68 III Diskless NG 3200 2996 0.0248 0.0004 0.099
LOri109 5 34 8.54 +09 50 43.57 CFHT1999 W  <1.10  <29.3  <−2.63 III Diskless NG 3200 2985 0.0224 9.1E-5 0.094
LOri113 5 33 47.92 +10 1 39.62 CFHT1999 W  <0.90  <29.2  <−2.67 II Thick NG 3300 2967 0.0194 7.8E-5 0.087
LOri120 5 34 46.20 +09 55 36.90 CFHT1999 W  <3.67  <29.8  <−2.00 II Thick NG 3000 2936 0.0166 0.0004 0.077
LOri122 5 34 35.43 +09 51 18.71 CFHT1999 W  <1.77  <29.5  <−2.27 II Thin NG 3000 2921 0.0153 0.0004 0.072
LOri124a 5 34 14.24 +09 48 26.97 CFHT1999 W  <1.37  <29.4  <−2.28 III Diskless NG 3200 2877 0.0126 0.0004 0.060
LOri132 5 34 29.18 +09 47 7.70 CFHT1999 W  <1.87  <29.5  <−2.14 II Thin NG 2900 2841 0.0114 0.0004 0.054
LOri136 5 34 38.31 +09 58 13.10 CFHT1999 W  <2.56  <29.6  <−2.10 III Thin NG 2900 2886 0.0131 0.0004 0.063
LOri138 5 33 43.44 +09 45 22.81 CFHT1999 W  <1.67  <29.4  <−2.20 Thin NG 2900 2811 0.0104 0.0003 0.049
LOri140 5 34 19.29 +09 48 28.02 CFHT1999 W  <1.62  <29.4  <−2.18 II Thick NG 2800 2792 0.0098 0.0003 0.046
LOri142 5 34 17.00 +10 6 16.42 CFHT1999 W  <1.71  <29.5  <−1.93 NG 3000 2685 0.0070 2.8E-5 0.035
LOri154 5 34 19.78 +09 54 20.84 CFHT1999 W  <1.13  <29.3  <−1.92 Du 2200 2558 0.0043 0.0003 0.026
LOri156 5 34 36.28 +09 55 32.18 CFHT1999 W  <2.06  <29.5  <−1.59 III Thick Du 2200 2503 0.0032 2.4E-5 0.023
LOri160 5 34 11.27 +09 45 10.72 CFHT1999 W  <1.88  <29.5  <−1.29 NG 2800 2356 0.0016 1.6E-5 0.017
LOri166 5 34 0.35 +09 54 22.45 CFHT1999 W  <1.14  <29.3  <−1.24 Du 2300 2207 0.0009 9.0E-6 0.014

Notes. (1) First listed in Morales-Calderón (2008) –1 sq. deg with Spitzer et al. (1999, DM1999) – or Barrado y Navascués et al. (2004) – CFHT1999. (2) Based on Spitzer/IRAC color–color diagram. (3) IRAC slope, after Lada et al. (2007). (4) Temperatures from VOSA fitting with logg = 4.0 dex or from a 5 Myr isochrone. (5) Bolometric luminosity from VOSA and logg = 4.0 dex. (6) Mass from a 5 My isochrone.

a

LOri124 = LOri125.

b

LOri094 was located very close to the XMM-Newton edge. It is a non-detection, but no reliable upper limit was derived.

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