TY - JOUR
T1 - 1E 1207.4-5209
T2 - The puzzling pulsar at the center of the supernova remnant PKS 1209-51/52
AU - Pavlov, G. G.
AU - Zavlin, V. E.
AU - Sanwal, D.
AU - Trümper, J.
N1 - Funding Information:
We thank Glenn Allen and Allyn Tennant for the helpful advice on the ACIS timing issues. We are grateful to Marcus Teter and Fernando Camilo for useful discussions. This work was partly supported by SAO grant GO2-3088X and NASA grant NAG5-10865.
PY - 2002/4/20
Y1 - 2002/4/20
N2 - A second Chandra observation of 1E 1207.4-5209, the central source of the supernova remnant (SNR) PKS 1209-51/52, allowed us to confirm the previously detected period of 424 ms and, assuming a uniform spin-down, estimate the period derivative, Ṗ ∼ (0.7-3) × 10-14 s s -1. The corresponding characteristic age of the pulsar, P/2Ṗ ∼ 200-900 kyr, is much larger than the estimated age of the SNR, ∼ 7 kyr. The values of the spin-down luminosity, Ė ∼ (0.4-1.6) × 1034 ergs s-1, and conventional magnetic field, B ∼ (2-4) × 1012 G, are typical for a middle-aged radio pulsar, although no manifestations of pulsar activity have been observed. If 1E 1207.4-5209 is indeed the neutron star formed in the same supernova explosion that created PKS 1209-51/52, such a discrepancy in ages could be explained either by a long initial period, close to its current value, or, less likely, by a very large braking index of the pulsar. Alternatively, the pulsar could be a foreground object unrelated to the SNR, but the probability of such a coincidence is very low.
AB - A second Chandra observation of 1E 1207.4-5209, the central source of the supernova remnant (SNR) PKS 1209-51/52, allowed us to confirm the previously detected period of 424 ms and, assuming a uniform spin-down, estimate the period derivative, Ṗ ∼ (0.7-3) × 10-14 s s -1. The corresponding characteristic age of the pulsar, P/2Ṗ ∼ 200-900 kyr, is much larger than the estimated age of the SNR, ∼ 7 kyr. The values of the spin-down luminosity, Ė ∼ (0.4-1.6) × 1034 ergs s-1, and conventional magnetic field, B ∼ (2-4) × 1012 G, are typical for a middle-aged radio pulsar, although no manifestations of pulsar activity have been observed. If 1E 1207.4-5209 is indeed the neutron star formed in the same supernova explosion that created PKS 1209-51/52, such a discrepancy in ages could be explained either by a long initial period, close to its current value, or, less likely, by a very large braking index of the pulsar. Alternatively, the pulsar could be a foreground object unrelated to the SNR, but the probability of such a coincidence is very low.
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U2 - 10.1086/340640
DO - 10.1086/340640
M3 - Article
AN - SCOPUS:0009704831
SN - 0004-637X
VL - 569
SP - L95-L98
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 II
ER -