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 groj1744-28_accepted.tex MNRAS in press
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%astro-ph/0703692
%http://www-astro.physics.ox.ac.uk/~ajg/papers/groj.pdf

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\newcommand{\groj}{GRO~J\,1744-28}

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\title[GRO J1744-28, search for the counterpart]{GRO J1744-28, search
for the counterpart: infrared photometry and spectroscopy}

\author[A. J. Gosling et al.]{A.J. Gosling,$^{1}$\thanks{e-mail:
ajg@astro.ox.ac.uk} R.M. Bandyopadhyay,$^{2}$ J.C.A.
Miller-Jones$^{3}$ and S.A. Farrell,$^{4,5}$ \\
$^{1}$Department of Astrophysics, University of Oxford, Keble Road,
Oxford, OX1 3RH, UK \\
$^{2}$Department of Astronomy, University of Florida, Gainesville, FL
32611, USA\\
$^{3}$Astronomical Institute `Anton Pannekoek', University of
Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands\\
$^{4}$School of PEMS, UNSW@ADFA, Northcott Drive, Canberra, ACT 2600,
Australia\\
$^{5}$Centre d'Etude Spatiale des Rayonnements, 9 Avenue du Colonel
Roche, 31028 Toulouse Cedex 4, France CNRS/UPS}

\begin{document}

\date{\today}

\pagerange{\pageref{firstpage}--\pageref{lastpage}} \pubyear{2007}

\maketitle

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

\label{firstpage}

\begin{abstract}
\noindent

Using VLT/ISAAC, we have detected 2 candidate counterparts to the
bursting pulsar \groj, one bright and one faint, both within the X-ray
error circles found using {\it XMM-Newton} and {\it Chandra}. In
determining the spectral types of the counterparts we applied 3
different extinction corrections; one for an all-sky value, one for a
Galactic Bulge value and one for a local value. We find that the local
value, with an extinction law of $\alpha = 3.23 \pm 0.01$ is the only
correction that results in colours and magnitudes for both the bright
and faint counterparts that are consistent with a small range of
spectral types, and in the case of the bright counterpart are also
consistent with the spectroscopic identification.  Photometry of the
fainter candidate then indicates it is a K7/M0~V star at a distance of
$3.75\pm1\,{\rm kpc}$. Such a star would require a very low
inclination angle ($i<9^{\circ}$) to satisfy the mass-function
constraints; however this source cannot be excluded as the counterpart
without follow-up spectroscopy to detect emission signatures of
accretion.  Photometry and spectroscopy of the bright candidate
indicate that it is most likely a G/K~III star. The spectrum does not
show \brg\ emission, a known indicator of accretion. The bright star's
magnitudes are in agreement with the constraints placed on the
probable counterpart by the calculations of \citet{rapp97} for an
evolved star that has had its envelope stripped.  The mass-function
indicates the most likely counterpart has $M < 0.3\,\Msol$ for an
inclination of $i \geq 15\degr$; a stripped giant, or a main
sequence M3+~V star would be consistent with this mass-function
constraint.  In both cases mass-transfer, if present, will be by
wind-accretion as the counterpart will not fill its Roche lobe given
the observed orbital period. In this case, the derived magnetic field
strength of $2.4 \times 10^{11}$ G is sufficient to inhibit accretion
of captured material by the propeller effect, hence the quiescent
state of the system.

\end{abstract}

\begin{keywords}
pulsars: individual (\groj) -- X-rays: binaries -- infrared: stars
\end{keywords}



-- 
---------------------------------------------------------------------
www-astro.physics.ox.ac.uk/~ajg
Andrew Gosling        ajgosling@gmail.com
Hertford College       ajg@astro.ox.ac.uk
Oxford                      andrew.gosling@hertford.ox.ac.uk