Archival radio observations of XTE J1810-197
ATel #207; B. M. Gaensler (Harvard-Smithsonian CfA), C. L. Brogan (IfA, U Hawaii)
on 18 Nov 2003; 11:00 UT
Credential Certification: Bryan Gaensler (bgaensler@cfa.harvard.edu)
Subjects: Radio, A Comment, Neutron Star, Soft Gamma-ray Repeater, Supernova Remnant, Transient, Variables, Pulsar
We report on deep radio observations made with the Very Large
Array (VLA) of the field of the newly discovered anomalous X-ray pulsar
(AXP) XTE J1810-197 (also known as CXOU J180951.1-194351; IAUC 8168 ,
IAUC 8190 , ATEL #188, ATEL #193, ATEL #195, ATEL #203, Gotthelf et al,
astro-ph/0309745; Ibrahim et al, astro-ph/0310665).
We have examined archival VLA data at frequencies of 330 and 1420 MHz,
to search for both a supernova remnant (SNR) potentially associated with
XTE J1810-197, and to look for radio emission from the source itself.
The 330 MHz data consist of observations in A, B, C and D arrays, observed
throughout 2001 and 2002 (see Brogan et al, astro-ph/0310109). The
one-sigma RMS sensitivity in the vicinity of XTE J1810-197 is 3.5 mJy/beam
at a resolution of 25 arcsec; our image has complete sensitivity up to
scales of 70 arcmin. The 1420 MHz data consist of observations taken in
the DnC configuration on 2003 Feb 03 and 2003 Feb 10. The RMS sensitivity
is 3.5 mJy/beam at a resolution of 62x35 arcsec; this image is sensitive
to scales up to 15 arcmin in extent.
Down to the sensitivities quoted above, we see no evidence for an
associated SNR in either data-set, nor do we see any unresolved radio
emission at the position of the neutron star. The lack of a detected
SNR is not particularly constraining, because of the complex nature
of radio emission in this region, behind which a faint remnant could
easily be hidden. As is the case for other AXPs and SGRs, the upper
limits on emission from the neutron star itself are well above those
for the faintest radio pulsars.
