---
author:
- 'V. Doroshenko, S. Suchy, A. Santangelo, R. Staubert, I. Kreykenbohm, R. Rothschild, K. Pottschmidt, J. Wilms'
bibliography:
- 'auto\_clean.bib'
title: '*RXTE* observations of the 1A 1118$-$61 in an outburst, and the discovery of a cyclotron line.' 
---

Introduction {#sec:introduction}
============

The hard X-ray transient 1A 1118$-$61 was first discovered during an outburst in 1974 by the *Ariel-5* satellite [@Eyles:1975p3466].  The outburst lasted for $\sim$10 days and no flux could be observed afterwards.  Pulsations with a period of 405.6s were observed by @Ives:1975p3476 and were initially interpreted as the orbital period of two compact objects.  It was suggested by [@fabian75] that the observed period was due to a slow rotation of the neutron star.  The optical counterpart was identified as the Be-star He 3$-$640/Wray 793 by @Chevalier:1975p3481 and classified as an O9.5IV-Ve star with strong Balmer emission lines and an extended envelope by @JanotPacheco:1981p3486.  The distance was estimated to be $5\pm2$kpc [@JanotPacheco:1981p3486].  The classification and distance was confirmed by @Coe:1985p3489 by UV observations of the source.  The X-ray spectrum of the pulsar was fitted with a power law with a photon index of $\Gamma \sim 1 $, with a possible spectral softening to $\Gamma \sim 0.9$ during the peak of the outburst (significant at $1\sigma$ confidence level). 

A second outburst occurred in 1992 and was observed by *CGRO*/BATSE [@Coe:1994p3488].  The measured peak pulsed flux was $\sim
150$ mCrab for the 20–100keV energy range, similar to the 1974 outburst [@Coe:1994p3488; @maraschi].  It was followed by a period of elevated emission $\sim 25$ days after the main outburst.  This lasted for $\sim
30$ days [see @Coe:1994p3488 Fig.1].  Pulsations with a period of 406.5s were detected up to 100keV and the pulse profile showed a single, broad peak, asymmetric at lower (20–40keV) energies.  A spin-up of 0.016s/day was observed during the decay of the outburst.  The pulsed spectrum was described with a single-temperature optically-thin, thermal bremsstrahlung model with a temperature of ($15.1 \pm 0.5$)keV for the main outburst and ($18.5 \pm0.9$)keV during the elevated emission.  Multi-wavelength observations revealed a strong correlation between the $H_\alpha$ equivalent width and the X-ray flux, which allowed [@Coe:1994p3488] to conclude that expansion of the circumstellar disk of the optical companion was mainly responsible for the increased X-ray activity.  The periastron passage would then trigger an outburst if enough matter had accumulated in the system.  This conclusion was supported by the pulsations with a period of $\sim409$s, which were also detected in quiescence [@quescence]. 

The source remained in quiescence until 2009 January 4, when a third outburst was detected by *Swift* [@Mangano09_GCN8777].  Pointed observations with *Swift*/XRT allowed the detection of pulsations with a period of $407.68\pm0.02$s reported later by [@swift_atel].  The complete outburst was regularly monitored with *RXTE*.  INTEGRAL observed the source after the main outburst and observed flaring activity $\sim 30$ days after the main burst [@intatel]. * Suzaku* observed 1A 1118$-$61 twice, once during the peak of the outburst and also $\sim
20$days later when the flux returned to its previous level (S. Suchy, in preparation). 

We report here on the monitoring observations by *RXTE*.  A timing analysis to determine the pulse period of the source and the rate of the observed strong spin-up was carried out.  Pulse phase averaged spectral analysis revealed an absorption feature at $\sim55$keV, confirmed independently with *Suzaku* (S. Suchy, in preparation).  We interpret this feature as a cyclotron resonance scattering feature (CRSF), which is observed for the first time in this source. 

Observations
============

The outburst was observed by multiple X-ray missions.  The source light-curve as observed by *Swift/BAT* with marked observation times by various satellites is presented in Fig.\[fig:bat\].  The source flux peaked on 2009 January 14, (*Swift/BAT* countrate 0.12 counts/s corresponding to $\sim500$mCrab in the 15–50keV energy range) and slowly decreased afterwards.  The source was regularly monitored with *RXTE* between January 10 and 2009 February 4, with a total exposure of 86ks (PCA) and dead-time-corrected live time of 29ks (HEXTE-B).  The data from the HEXTE-A detector were not used as it was not rocking during the entire observation and the background could not be properly estimated.  The data were reduced with the HEASOFT version 6.8 and a set of calibration files version 20091202.  The spectral modeling was performed with the *XSPEC* package version 12.5.1n.  The energy range 3.5–25keV was used for the PCA and 18–120keV for the HEXTE spectra.  Based on an analysis of recent Crab observations performed during the same time frame (2008 December 16, – 2009 March 11, proposal ID P94802), a systematic of 0.5% was determined for the PCA data.  No systematic error was required for the HEXTE data. 

![* Swift/BAT* daily light-curve of the outburst in 2009 January (dotted line).  Observation times by various missions are indicated with vertical lines.[]{data-label="fig:bat"}](./19629fg1.eps)

Timing analysis
===============

To determine the pulse period of 1A 1118$-$61 the PCA light-curve covering the complete observation in the 3–50keV energy range was used.  We searched for the pulse period and pulse period derivative using the phase connection technique [@staubert2009].  Our best-fit results give $P_\mathrm{spin}$=407.719(9)s, $\dot{P}_\mathrm{spin}=-4.6(2)\times10^{-7}\,\rm{s}\,\rm{s}^{-1}$, at a folding epoch of MJD54841.62 (the uncertainties given in parenthesis are at $1\sigma$ confidence level and refer to the last digit given).  The best-fit residuals for pulse arrival times are presented in Fig.  \[fig:toa\].  Note that the obtained parameters characterize the pulse period evolution during the *RXTE* observations only and are not consistent with the pulse period value provided by [@swift_atel].  This inconsistence is anticipated, because the luminosity and hence the accretion rate were significantly higher during the *RXTE* observations.  The spin-up rate of the neutron star depends on the accretion rate, and therefore extrapolating the timing solution obtained close to the peak of the outburst (with a stronger spin-up) to the beginning of the outburst (where the spin-up rate is expected to be significantly lower) gives a longer pulse period than can be directly measured at the time.  Note also that our solution does not account for the Doppler delays caused by orbital motion, because the parameters of the orbit are unknown and our data do not allow us to find an unambiguous solution for the orbit.  The estimated value for an orbital period from “pulse period”–“orbital period” diagram [@corbet] lies in the 400–800d range, which is much longer than the span of our data.  The intrinsic spin-period evolution is expected to be complicated, so it is difficult to separate it from the effects of the orbital motion.  Moreover, [@Coe:1994p3488] suggested that the orbit may be almost circular, and the outbursts may occur at any orbital phase, so a possible orbital period value derived from the comparison of outburst times is also potentially ambiguous. 

Both the spin-up rate $\sim0.04$sd$^{-1}$ and flux are somewhat higher (by a factor of $\sim$2–3) than reported by @Coe:1994p3488 for the previous outburst observed with *CGRO*/BATSE.  The stronger spin-up measured for the current outburst is likely caused by the higher flux and consequently higher accretion rate (although it is difficult to directly compare BAT and BATSE fluxes, because BATSE measured only pulsed flux and the energy ranges are slightly different).  A potential difference in the orbital phase during the two observations may also be responsible for the difference in the observed spin-up rate. 

![ Best-fit residuals for the pulse arrival times determined using *RXTE* PCA lightcurve (i.e. difference between pulse arrival times as observed (O) and as calculated (C) with an assumed pulse period and derivative).  Solid, dashed and dotted lines correspond to fits including the pulse period derivatives up to second, first and none (constant period) respectively.[]{data-label="fig:toa"}](./19629fg2.eps)

![ image](./19629fg4.eps)

A set of pulse profiles in several energy ranges was constructed with the determined period.  The pulse profile significantly changes with energy as shown in Fig.  \[fig:enphase\].  At energies below 10keV the pulse profile has two peaks.  The secondary peak amplitude decreases towards higher energies, disappearing above 10keV. A shoulder appears on the other side of the main peak at about the same energy.  The pulse profile becomes single peaked and gradually more symmetric and narrow at higher energies.  A similar behavior was observed previously with *CGRO*/BATSE [@Coe:1994p3488].  The pulse fraction, defined as $(A_{max}-A_{min})/(A_{max}+A_{min})$ increases with energy in a similar way to other accreting pulsars, except for a drop at around 8keV, where the second peak disappears (see Fig.\[fig:enphase\]). 

Spectral analysis
=================

![ image](./19629fg5.eps)

  Parameter                            `FDCUT`                               `NPEX`                             `CompTT`$_\mathrm{fix23}$   `CompTT`
  ------------------------------------ ------------------------ ------------ ------------------------- -------- --------------------------- ------------------------
  $N_\mathrm{H}$                       $4.9_{-0.6}^{+0.6}$                   $3.5_{-0.4}^{+0.4}$                $0.0_{-0.0}^{+0.4}$         $0.2_{-0.2}^{+0.5}$
  $E_{22}$                             *22.76*                               *22.76*                            *22.76*                     $23.5_{-0.8}^{+1.5}$
  $\sigma_{22}$                        *1.8*                                 *1.8*                              *1.8*                       $4.6_{-1.1}^{+1.9}$
  $\tau_{22}$                          $0.02_{-0.01}^{+0.01}$                $0.032_{-0.01}^{+0.01}$            $0.05_{-0.01}^{+0.01}$      $0.09_{-0.02}^{+0.04}$
  $E_{\mathrm{cyc}}$                   $55.1_{-1.5}^{+1.6}$                  $55.2_{-1.5}^{+1.6}$               $52.9_{-1.4}^{+1.7}$        $55.5_{-2.1}^{+2.5}$
  $\sigma_{\mathrm{cyc}}$              $10.4_{-1.0}^{+1.1}$                  $11.8_{-1.1}^{+1.2}$               $10.2_{-1.2}^{+1.5}$        $13.3_{-2.0}^{+2.2}$
  $\tau_{cyc}$                         $0.8_{-0.1}^{+0.1}$                   $0.9_{-0.1}^{+0.2}$                $0.6_{-0.1}^{+0.1}$         $0.9_{-0.2}^{+0.3}$
  $\Gamma$                             $0.73_{-0.06}^{+0.05}$   $\Gamma_1$   $0.16_{-0.03}^{+0.03}$                                         
  $E_{\mathrm{cut}}$                   $16.5_{-2.9}^{+2.5}$     $\Gamma_2$   $-2.0$                    $\tau$   $6.0_{-0.1}^{+0.1}$         $6.0_{-0.2}^{+0.2}$
  $E_{\mathrm{fold}}$                  $12.0_{-0.5}^{+0.5}$     $A_2$        $0.16_{-0.02}^{+0.02}$    $T_0$    $1.47_{-0.03}^{+0.02}$      $1.44_{-0.05}^{+0.04}$
                                                                $kT$         $7.9_{-0.3}^{+0.3}$                $7.2_{-0.2}^{+0.2}$         $7.7_{-0.3}^{+0.4}$
  $E_{\mathrm{Fe}}$                    $6.5_{-0.1}^{+0.1}$                   $6.45_{-0.08}^{+0.07}$             $6.4_{-0.09}^{+0.02}$       $6.4_{-0.09}^{+0.02}$
  $\sigma_{\mathrm{Fe}}$               $\le0.4$                              $\le0.3$                           $\le0.3$                    $\le0.3$
  $A_{\mathrm{Fe}}$                    $3_{-1}^{+3}$                         $3.2_{-0.7}^{+0.7}$                $2.7_{-0.3}^{+0.3}$         $2.7_{-0.3}^{+0.3}$
  $A_{\mathrm{Cu}}$                    $2_{-2}^{+2}$                         $1_{-0.3}^{+0.3}$                                              
  $A_{\Gamma,1,\texttt{CompTT}}$       $22_{-1}^{+2}$                        $10.7_{-0.7}^{+0.7}$               $10.1_{-0.2}^{+0.2}$        $9.8_{-0.3}^{+0.3}$
  $\chi_{\mathrm{red}/\mathrm{dof}}$   1.04/83                               0.85/83                            1.08/84                     0.72/82

\[tab:phav\]

The longest observations were obtained during the maximum of the outburst, accordingly we focused on this data for the spectral analysis (observations 94032-04-02-03 to 94032-04-02-10).  The spectra of 1A 1118$-$61 in different energy ranges were previously described by power law and bremsstrahlung models [@maraschi; @Coe:1994p3488], but we found that these models do not describe our data adequately.  Our results show that the broadband continuum of 1A 1118$-$61 can be well described by the `FDCUT`, `NPEX`, and `CompTT` models [@Coburn:2002p158; @mihara; @comptt] with qualitatively similar goodness of the fit, modified by photoelectric absorption and iron emission line at $\sim6.4$keV.

All used continuum models in their best-fit residuals show a prominent absorption feature at $\sim55$keV. The inclusion of an absorption line with a Gaussian optical depth profile leads to a significant reduction of $\chi^2$ in all models (see Table \[tab:phav\]).  We interpret this absorption feature as a CRSF, which is detected in the spectrum of 1A 1118$-$61 for the first time.  The observed energy of the feature is one of the highest known and corresponds to a magnetic field B$\sim4.8\times10^{12}$G [@harding] in the scattering region.  Preliminary phase-resolved analysis shows that the energy of the CRSF is not likely to change significantly with the pulse phase (see Fig.\[fig:enphase\]). 

The best-fit residuals of `FDCUT` and `NPEX` models show also a prominent emission line-like feature at $\sim8$keV. Similar features at different energies were reported for a number of sources (@Coburn:2002p158 [@rroca] and references therein). [ @Coburn:2002p158] suggested that the employed phenomenological models for the continuum may be oversimplified for the real sources and hence may be responsible for this effect.  On the other hand, [@Rothschild06] suggested that the feature may be associated with the fluorescence copper line from the *Be/Cu* collimator of the PCA instrument.  To clarify the situation a more detailed analysis of the *Suzaku* data is currently made and will be presented as a separate paper (S. Suchy et al, in preparation). 

We found that the inclusion of an emission line with Gaussian profile may help to account for this feature and does not significantly affect other model parameters.  The $\chi^2$ substantially improves for fits with `FDCUT` and `NPEX` models, accordingly we included the line in all fits with those models.  The energy and the width of the line were fixed at 8.04keV and 0.01keV, corresponding to the copper $K_\alpha$ line, as proposed by [@Rothschild06]. 

The fit may be slightly improved by the inclusion of an additional absorption feature at $\sim23$keV for PCA data only.  The investigation of the Crab residuals (proposal P94802) shows that a similar feature is also present in the PCA Crab spectrum (more than 99% significance with maximum likelihood ratio (MLR) and F tests (@protassov, p-value $\sim0.006$).  This is consistent with our 1A 1118$-$61 data, because the line is not required by HEXTE data.  On the other hand, a shallow fundamental line at 22keV (with a first harmonic at 55 keV) could be more difficult to detect due to this instrumental feature using PCA data.  A comparison of our *RXTE* results with the *Suzaku* observations will help to clarify the picture (S. Suchy et al, in preparation). 

Conclusions
===========

For the first time since 1992 a major outburst of the Be/X-ray binary 1A 1118$-$61 was observed in 2009 January with *RXTE*, following the trigger of *Swift/BAT*.  Strong pulsations with a period of 407.72s and a spin up of $-4.6\times10^{-7}$ss$^{-1}$ were detected.  A similar temporal behavior was observed with *CGRO*/BATSE during the previous outburst.  A broadband spectrum of the source was obtained for a first time, and an absorption feature at $\sim55$keV, interpreted as a CRSF was detected.  The inclusion of the feature significantly improves fit results with all applied continuum models and its energy does not depend significantly on the model used.  More detailed spectral analysis is ongoing and the results will be published elsewhere. 

VD thanks DLR for financial support (grant 50OR0702).