Issue |
A&A
Volume 525, January 2011
|
|
---|---|---|
Article Number | A106 | |
Number of page(s) | 7 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/201014982 | |
Published online | 06 December 2010 |
HST and VLT observations of the neutron star 1E 1207.4–5209⋆
1
Istituto Universitario di Studi Superiori,
Viale Lungo Ticino Sforza 56,
27100
Pavia,
Italy
e-mail: deluca@lambrate.inaf.it
2
INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano,
via Bassini 15,
20133
Milano,
Italy
3
Istituto Nazionale di Fisica Nucleare, Sez. di Pavia,
via Bassi 6,
27100
Pavia,
Italy
4
Mullard Space Science Laboratory, University College London,
Holmbury St. Mary,
Dorking, Surrey,
RH5 6NT,
UK
5
Università degli Studi di Pavia, Dipartimento di Fisica Nucleare e
Teorica, via Bassi
6, 27100
Pavia,
Italy
6
European Southern Observatory, Karl Schwarzschild-Str. 2, 85748
Garching,
Germany
Received:
12
May
2010
Accepted:
20
June
2010
The peculiar central compact object 1E 1207.4−5209 in the G296.5+10.0 supernova remnant has been proposed to be an “anti-magnetar” – a young neutron star born with a weak dipole field. Accretion, possibly of supernova fallback material, has also been invoked to explain a large surface temperature anisotropy as well as the generation of peculiar cyclotron absorption features superimposed on its thermal spectrum. Interestingly enough, a faint optical/infrared source was proposed as a possible counterpart to 1E 1207.4−5209, but later questioned, based on coarse positional coincidence. On the basis of the large offset of 1E 1207.4−5209 with respect to the center of its host supernova remnant, the source should move at ~70 mas yr-1. Thus, we tested the association by measuring the proper motion of the proposed optical counterpart. Using Hubble Space Telescope (HST) observations spanning 3.75 years, we computed a 3σ upper limit of 7 mas yr-1. Absolute astrometry on the same HST data set also places the optical source significantly off the 99% confidence Chandra position. This allows us to safely rule out the association. Using the HST data set, coupled to ground-based observations collected at the ESO/Very Large Telescope (VLT), we set the deepest limits ever obtained on the optical/infrared emission from 1E 1207.4−5209. By combining these limits with the constraints derived from X-ray timing, we rule out accretion as the source of the thermal anisotropy of the neutron star.
Key words: stars: neutron / pulsars: individual: 1E 1207.4−5209
© ESO, 2010
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