A search for radio pulsars in five nearby supernova remnants

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Table 1.

Supernova remnants targeted in this survey without compact objects and with distances less than 3 kpc.

SNR	Dist (kpc)	Size (′)	Age (10³ yr)	Number of pointings	Total observation time (h)	T_sky (K)	S_SNR (Jy beam⁻¹)	Average S_min (mJy)	Required 2D velocity (km s⁻¹)	Previous S_min (mJy)
G53.6−2.2	2.8 ^(a)	33	7 ^(b)	2	4.5	14.11	1.92	0.11	1900	0.2
G78.2+2.1	1.5 ^(c)	60	7 ^(d)	5	6.8	39.56	22.13	0.15	1800	2.4
G89.0+4.7	1.7 ^(e)	105	16 ^(f)	10	7.0	16.41	3.71	0.14	1600	1.0
G116.9+0.2	1.6 ^(g)	34	7 ^(h)	7	2.3	10.58	1.76	0.19	1100	0.8
G156.2+5.7	1.3 ⁽ⁱ⁾	110	15 ^(j)	27	7.3	7.31	0.10	0.16	1300	0.7

Notes. Ages are from Sedov-phase approximations using X-ray temperatures. The size is the diameter of the remnants. The total observation time is the time each remnant has been observed. T_sky is the sky temperature calculated from Haslam et al. (1982) assuming a spectral index of −2.6 and an 820 MHz observing frequency. The S_SNR is the flux of the SNR per pointing calculated using data from Green (2017). Also shown are the average flux density thresholds of the remnants, the required velocity of the pulsar to escape the field of view studied in the survey, and the previous recorded minimum flux densities. All the SNRs except G53.6−2.2 were observed by Lorimer et al. (1998) down to the minimum flux densities given in the column ‘Previous S_min’. SNR G53.6−2.2 was observed by Gorham et al. (1996) down to a sensitivity limit of 0.2 mJy.

References.

^(a)

Giacani et al. (1998),

^(b)

Goss et al. (1975),

^(c)

Landecker et al. (1980),

^(d)

Leahy et al. (2013),

^(e)

Byun et al. (2006),

^(f)

Lazendic & Slane (2006),

^(g)

Yar-Uyaniker et al. (2004),

^(h)

Hailey & Craig (1994),

⁽ⁱ⁾

Pfeffermann et al. (1991), and

^(j)

Borkowski et al. (2001).

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