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Table 3

Driving sources and properties of molecular hydrogen outflows in Ophiuchus.

Outflow source [EDJ2009]a RAa Deca α a MHOb 850 μmc 1100 μmd L e θ f PAg DAh VVi CO outflowj
(J2000) (J2000) core? core? (′) (deg) (deg) (103 yr) (km s-1 100 AU-1) associated?
[EDJ2009]800 800 +16 26 14.6 –24 25 07.5 ... 2102 Y N 0.9 1 141 2.9 ... N
YLW31 806 +16 26 18.9 –24 28 19.6 –1.30 2103–2104 Y N 3.1 4 62 ... ... N
CRBR2317.5–1729 807 +16 26 19.0 –24 24 14.2 –0.33 2150 N N 0.6 6 48 0.9 ... N
GSS32 820 +16 26 24.0 –24 24 48.0 –0.96 2151 N N 0.7 ... 252 2.0 ... N
[GY92]30 822 +16 26 25.5 –24 23 01.3 0.64 2137 N Y 0.7 5 120 0.5 ... N
VLA1623–243 825 +16 26 26.4 –24 24 30.0 ... 2105–2106 Y N 6.2 23 123 2.7 –0.1 ± 0.2; –0.04 ± 0.03 Y
[GY92]93 833 +16 26 41.2 –24 40 17.9 –1.35 2115a,c N N 9.4 1 40 9.8 –46 ± 131 N
WL18 841 +16 26 49.0 –24 38 25.1 –1.27 2108 N N 0.4 ... 297 ... ... N
YLW5 857 +16 27 02.3 –24 37 27.2 0.58 2109 N Y 0.9 ... 297 1.9 ... N
BBRCG24 869 +16 27 09.1 –24 34 08.0 –1.26 2115d,e,b,f,g N N 1.1 51 167 0.7 0.5 ± 0.6 N
[GY92]232 875 +16 27 13.3 –24 41 33.4 –3.24 2114 N N 2.5 ... 163 3.6 ... N
[GY92]235 877 +16 27 13.8 –24 43 31.6 –0.85 2113 N N 0.6 ... 225 1.3 ... N
[GY92]239 880 +16 27 15.4 –24 26 39.6 –1.20 2153 N N 1.1 ... 77 1.1 ... N
YLW14 891 +16 27 21.8 –24 29 53.1 0.98 2116 N N 0.4 ... 40 0.3 ... N
WSB49 893 +16 27 23.0 –24 48 07.1 –1.19 2111 N N 1.1 5 183 1.8 –0.2 ± 0.4 N
YLW16 901 +16 27 28.0 –24 39 33.4 1.96 2118–2119 Y Y 2.0 34 18 0.6 ... Y
YLW47 916 +16 27 38.3 –24 36 58.4 –1.06 2122,2123c N N 2.5 12 195 6.2 − 0.1 ± 0.3 N
[GY92]344 932 +16 27 45.8 –24 44 53.8 0.10 2126 N N 0.3 4 20 0.4 ... N
YLW52 937 +16 27 51.8 –24 31 45.4 –0.26 2128–2131 N N 4.9 17 81 8.8 0.2 ± 0.2; –0.8 ± 0.3 N
YLW58 950 +16 28 16.5 –24 36 57.9 –0.92 2154 N N 2.0 ... 357 ... ... N
MMS126 954 +16 28 21.6 –24 36 23.4 1.14 2132 N Y 2.6 22 37 1.2 –0.8 ± 0.2 N

Notes.

(a)

Name, position and de-reddened spectral index of driving sources from Evans et al. (2009).

(b)

The MHOs, which are driven by the driving sources. MHO names are from Davis et al. (2010).

(c)

“Y” or “N” indicates whether or not a 850 μm dust core is associated with the driving source. The details on the 850 μm dust cores can be found in Johnstone et al. (2000).

(d)

Same as for the 850 μm cores, but for the 1100 μm dust cores. Details can be found in Evans et al. (2009) and Young et al. (2006).

(e)

The entire length (L) of the outflow. This length is the distance from the emission feature to the source projected to the bisector of the opening angle in cases where more than one feature is identified in the outflow. In case there is only one feature identified in the outflow, this length is just the distance from the source to the feature.

(f)

The opening angle (θ) of the outflow. This angle is measured from a cone with the smallest vertex angle centered on the driving source that includes all MHO features in the outflow. Note that the opening angle can not be calculated if there is only one feature in the outflow.

(g)

The position angle (PA) of the outflow measured east of north as computed from the bisector of the opening angle. Note that for bipolar outflows we select the angle smaller than 180 degrees as the position angle.

(h)

The dynamic age (DA) of the outflow, which is the maximum dynamic age of the features with proper motions.

(i)

Variation in velocity (VV) along the outflow. This parameter is calculated through fitting the tangential velocity of MHO features vs. the distance from MHO features to the driving source using a linear least square method. VV equals 1 means that the MHO features will speed up by 1 km s-1 after they propagate 100 AU along the outflow. Note that for the bipolar outflows, we calculated the VVs for each lobe.

(j)

“Y” or “N” indicates whether or not a CO molecular outflow is associated with the MHO. The CO molecular outflows are identified by Nakamura et al. (2011) based on the CO (J = 3–2) and CO (J = 1–0) mapping observations.

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