XTE J1814-338 is likely the EXOSAT slew source EXMS B1810-337
ATel #166; Rudy Wijnands (University of St Andrews) & Alastair Reynolds (ESTEC)
on 18 Jun 2003; 16:41 UT
Credential Certification: Rudy Wijnands (rudy@space.mit.edu)
Subjects: X-ray, A Comment, Binary, Neutron Star, Transient, Pulsar
We report that the new X-ray transient and accretion-driven
millisecond X-ray pulsar XTE J1814-338 (IAUC 8144 , ATEL #164 and #165)
is at a position consistent with the source EXMS B1810-337 listed in
the EXOSAT medium-energy slew survey catalogue (Reynolds et al. 1999,
A&AS 134, 287, Table 5). The error box of EXMS B1810-337 fully
encompasses the error circle quoted for XTE J1814-338 in IAUC 8144 and
ATEL #164, indicating that EXMS B1810-337 is most likely the same
source as XTE J1814-338. The coordinates for the corners of the EXOSAT
error box of EXMS B1810-337 are given by: 273.679, -34.456; 273.507,
-32.963; 273.242, -32.983; 273.410, -34.477 (decimal R.A. and Dec. for
epoch J2000; we note that the corner coordinates given in Table 5 of
Reynolds et al. 1999 are for B1950 and not for J2000 as stated in the
same paper). The
figure shows the ROSAT All Sky Survey image (in J2000 coordinates)
of the region around XTE J1814-338 with the RXTE error circle and the
EXOSAT error box over-plotted (note that XTE J1814-338 is not detected
in the ROSAT data). EXMS B1810-337 was detected on 2 September 1984
with an absorbed 2-10 keV flux of ~5E-11 erg/s/cm/cm. If XTE
J1814-338 can indeed be identified with EXMS B1810-337, then the
recurrence time of this source can be inferred to be less than 19
years but more than 4.5 years (the time since the RXTE/PCA bulge scan
observations started in February 1999; Swank & Markwardt 2001,
astro-ph/0109240), unless the recurrence time of the source varies
significantly.
