Hot ammonia around young O-type stars - II. JVLA imaging of highly excited metastable NH3 masers in W51-North

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Table 1

Parameters of JVLA observations toward W51.

Transition^a	ν_rest	E_u/k^b	Date	JVLA	Beamwidth^c	rms^d
(J,K)	(MHz)	(K)	(yyyy-mmm-dd)	Receiver	θ_M(′′) × θ_m(′′); PA(°)	(mJy/beam)

(6, 6)	25 055.96	408	2012-May-31	K	0.29 × 0.23; −21	1.3
(7, 7)	25 715.14	539	2012-May-31	K	0.28 × 0.23; −2	1.4
(9, 9)	27 477.94	853	2012-Jun.-21	Ka	0.24 × 0.22; +53	1.3
(10, 10)	28 604.75	1035	2012-Aug.-07	Ka	0.23 × 0.21; +61	2.9
(13, 13)	33 156.84	1691	2012-Jun.-21	Ka	0.20 × 0.18; +52	1.9

Notes.

^(a)

Transitions include ortho-NH₃ (K = 3n) and para-NH₃ (K ≠ 3n).

^(b)

Energy above the ground reported from the JPL database.

^(c)

Synthesized beams in images made with the CASA task CLEAN with a robust parameter set to 0.5.

^(d)

rms noise in a ~0.4 km s^-1 channel without primary beam correction. After primary beam correction, the noise level increases by up to 25%.

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