On the PSR B1133+16 optical counterpart

TL;DR

This study confirms the optical counterpart of pulsar PSR B1133+16 by analyzing multi-epoch deep optical images, demonstrating the counterpart's proper motion consistent with radio measurements.

Contribution

The paper provides the first confirmation of the optical counterpart of PSR B1133+16 through multi-epoch imaging and proper motion analysis, refining previous candidate identifications.

Findings

Detected an optical object consistent with the pulsar's proper motion

Confirmed the optical counterpart moved from the 2003 position

Supported the identification with proper motion-corrected radio coordinates

Abstract

The aim of this work is confirming the optical identification of PSR B1133+16, whose candidate optical counterpart was detected in Very Large Telescope (VLT) images obtained back in 2003. We used new deep optical images of the PSR B1133+16 field obtained with both the 10.4 m Gran Telescopio Canarias (GTC) and the VLT in the g' and B bands, respectively, to confirm the detection of its candidate optical counterpart and its coincidence with the most recent pulsar's radio coordinates. We did not detect any object at the position of the pulsar candidate counterpart (B~28), measured in our 2003 VLT images. However, we tentatively detected an object of comparable brightness in both the 2012 GTC and VLT images, whose position is offset by ~3.03" from that of the pulsar's candidate counterpart in the 2003 VLT images and lies along the pulsar's proper motion direction. Accounting for the time span of ~9 years between the 2012 quasi-contemporary GTC and VLT images and the 2003 VLT one, this offset is consistent with the yearly displacement of the pulsar due to its proper motion. Therefore, both the flux of the object detected in the 2012 GTC and VLT images and its position, consistent with the proper motion-corrected pulsar radio coordinates, suggest that we have detected the candidate pulsar counterpart that has moved away from its 2003 discovery position.