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Table 1

Radial velocities of the individual observed sources (in Col. 3) as found in the literature (references are given in Col. 4).

Source Type Radial velocity References vLSR of a local absorption
(km s−1) (km s−1)
IRS 1W Red 35 ± 20 Paumard et al. (2006) 35 ± 15 in R(0)
50 ± 15 in P(1)
IRS 2S Cool 107 ± 20 Genzel et al. (2000) − 110 ± 15 in R(0) P(1) and P(2)
IRS 2L Red 60 ± 15 in R(0), P(1), P(2) and P(3)
105 ± 15 in R(0), P(1) and P(3)
IRS 3 Red 60 ± 15 in R(0), P(1), P(2), P(3), P(4), P(6) and P(7)
IRS 5 Cool 110 ± 60 Tanner et al. (2005) (flow) 70 ± 15 in P(1), P(2), and P(3)
IRS 6W Hot 63 ± 3 Zhu et al. (2008), Herbst et al. (1993) − 20 ± 15 in P(1), P(2), P(4) and P(5)
65 ± 15 in P(1), P(2), P(4) and P(5)
IRS 10W Cool 80 ± 60 Tanner et al. (2005) (source) 50 ± 15 in P(1) and P(2)
− 105 ± 15 in R(0), P(1), P(2) and P(3)
Cool 195 ± 150 Tanner et al. (2005) (flow) 110 ± 15 in P(3)
210 ± 15 in P(3)
IRS 12N Cool − 69 ± 2 Zhu et al. (2008) − 85 ± 15 in R(0), P(1), P(3), P(4), P(6), P(7) and P(9)
− 61 ± 1 Figer et al. (2003)
IRS 13E Hot 45 ± 60 Genzel et al. (2000) 60 ± 15 in R(0), P(1), P(2) and P(3)
IRS 16C Hot 125 ± 30 Paumard et al. (2006)
IRS 16SW Hot 453 ± 4 Martins et al. (2006)
IRS 21 Hot − 90 ± 20 Genzel et al. (2000) − 60 ± 15 in P(3)
55 ± 15 in R(0), P(1), P(2) and P(3)
IRS 29S Hot − 93 ± 20 Genzel et al. (2000) −60 ± 15 in P(3)
Hot − 164 ± 2 Zhu et al. (2008)

Notes. The second column shows the spectral type of the sources listed in Col. 1. Most of the radial velocities clearly lie beyond the 20–50 km s−1 cloud velocities. For sources IRS 5 and IRS 10W, Tanner et al. (2005) give separate values for the source and the corresponding minispiral flow (see e.g., velocity field given by Zhao et al. 2010). For IRS 10W, two “flow” values are given (175 ± 130 and 215 ± 160 km s−1) of which we list the average in the table. Sources IRS 1W, IRS 2L, and IRS 3 are enshrouded in dust and are therefore labeled as “red”. For IRS 2L and IRS 3 we found no quoted velocity. For IRS 6W, we classify this source as “hot” using the information by Herbst et al. (1993) that the Brγ line emission is present in its spectrum. The radial velocity given by Herbst et al. (1993) has not been tabulated in their paper but can be read off their Fig. 5 as −166 ± 30 km s−1 and may be associated with the gas flow in the minispiral bar. In Col. 5, we present the assumed local gas velocities measured in our spectra in the CO transition lines indicated. The values in bold are the first determinations of the radial velocities of IRS 2L and IRS 3 that we derive from the present work (see Sect. 4).

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