Upgraded antennas for pulsar observations in the Argentine Institute of Radio astronomy

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Table 2.

Observable MSPs from IAR with the current setup (top) and with future upgrades (bottom).

J name	P₀	S₁₄₀₀	W₅₀^(a)	S/N^(b)	D	DM
	[ms]	[mJy]	[ms]		[kpc]	[pc cm⁻³]
J0437−4715	5.757	150.2	0.141	336 ^(c)	0.16	2.64
J1744−1134	4.075	3.2	0.137	15.1	0.15	3.14
J2241−5236	2.187	1.95	0.07	9.4	0.96	11.41

J1643−1224	4.622	4.68	0.314	15.26	0.79	62.41
J1600−3053	3.598	2.44	0.094	13.1	2.53	52.33
J2124−3358	4.931	4.5	0.524	11.5	0.36	4.60
J1603−7202	14.84	3.5	1.206	10.4	1.13	38.05
J1730−2304	8.123	4.00	0.965	9.6	0.51	9.62
J0900−3144	11.11	3.00	0.8	9.5	0.38	75.71
J0711−6830	5.491	3.7	1.092	6.5	0.11	18.41
J1933−6211	3.543	2.30	0.36	6.0	0.65	11.52
J1652−48	3.785	2.70	*	*	4.39	187.8

Notes. P₀ is the barycentric period of the pulsar, S₁₄₀₀ the mean flux density at 1400 MHz, W₅₀ the pulse width at 50% of peak, S/N the expected signal-to-noise with 220′ of observation with A1, D the distance based on the Yao et al. (2017) electron density model, and DM the dispersion measure.

^(a)

Quoted values are indicative only, as the width of pulse at 50% of peak is a function of both observing frequency and time resolution.

^(b)

Estimated according to Eq. (1) and the values of A1 given in Table 1. We note that Eq. (1) involves the equivalent width of the pulse W which we do not know, but for a gaussian pulse it is valid to approximate W ≈ W₅₀.

^(c)

The pulse of J0437−4715 significantly differs from gaussian, so in this case we use the equivalent width of the pulse that we measure, W ≈ 0.77 ms.

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