VLT observations of the middle-aged pulsar PSR B1055-52

Details VLT observations of the middle-aged pulsar PSR B1055-52 VLT observations of the middle-aged pulsar PSR B1055-52

Sep 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010a%26a...520a..21m&link_type=abstract

Astronomy and Astrophysics, Volume 520, id.A21

Astronomy and Astrophysics

Astrophysics

1

Pulsars: Individual: Psr B1055-52

Scientific paper

Context. The 535 kyear old radio pulsar B1055-52 is the oldest of the “Three Musketeers”, the group of the middle-aged pulsars (the other two being PSR B0656+14 and Geminga) with bright soft X-ray and high-energy γ-ray emission. The identification of its optical counterpart has been only recently confirmed through observations performed with the Hubble Space Telescope (HST), which provided a first characterisation of the pulsar spectrum. Aims: We aim at measuring the pulsar flux in the B band for which only an upper limit has been obtained with the HST. Methods: We used the deepest ground-based observations of the PSR B1055-52 field obtained with Very Large Telescope (VLT), available in the ESO archive. Results: Due to the non-optimal image quality of the VLT data (~1.2 arcsec) we could not resolve the faint pulsar emission against the higher sky background induced by the presence of a bright star (Star A; mV = 14.6) ~4.4 arcsec away from the pulsar position. We determined a 3 σ upper limit of mB ~ 25.3 on the pulsar brightness. This corresponds to an extinction-corrected flux ⪉0.391 μJy which is consistent with the HST spectrum and comparable with the HST flux upper limit at a similar wavelength. Conclusions: The presence of Star A makes it improbable to detect PSR B1055-52 in the optical bands through ground-based observations, unless performed under exceptional seeing conditions. The situation might be more promising through adaptive optics high-spatial resolution observations in the near-infrared, where the HST spectrum hints at a steep power-law which predicts an higher flux at longer wavelengths.
Based on observations collected at the European Southern Observatory (ESO), La Silla and Paranal, Chile under programme ID 68.D-0407(A).

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