Discovery of the optical counterpart to the X-ray pulsar SAX J2103.5+4545

Reig, P.; Negueruela, I.; Fabregat, J.; Chato, R.; Blay, P.; Mavromatakis, F.

doi:10.1051/0004-6361:20035786

Cited by 45 publications

(67 citation statements)

References 39 publications

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“…Although the number of optical observations of SAX J2103.5+4545 is scarce, the information available indicates a correlation between the long-term optical and X/γ-ray variability. The optical observations (August and September 2003) reported by Reig et al (2004) coincided with the transition to an X-ray faint state (see Fig. 8).…”

Section: Discussionsupporting

confidence: 63%

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INTEGRAL observations of the peculiar BeX System SAX J2103.5+4545

Blay

Reig

Martínez-Núñez

et al. 2004

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Abstract. We present an INTEGRAL data analysis of the X-ray transient SAX J2103.5+4545 during two outbursts detected in December 2002. The INTEGRAL coordinates and error circle agree with the position of the recently proposed optical counterpart. A power-law plus cut-off model provided a good fit to the 4-150 keV spectrum yielding a photon index of 1.0± 0.1, a cut-off energy E cut = 7.6 ± 2.0 keV and a folding energy E fold = 30.9 ± 2.5 keV. The X-ray luminosity in the 4-150 keV energy range was found to be 6.0 × 10 36 erg s −1 , assuming a distance of 6.5 kpc. This luminosity, together with the derived photon index, indicate that the source is in a bright state. A 354.9 ± 0.5 second pulse period is measured. This value is significantly smaller than previous measurements, indicating a long-term spin-up episode.

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Section: Discussionsupporting

confidence: 63%

“…Recently, Reig et al (2004) has reported the first optical and infrared observations of this system leading to the identification of the optical counterpart with a B0V star.…”

Section: Introductionmentioning

confidence: 99%

INTEGRAL observations of the peculiar BeX System SAX J2103.5+4545

Blay

Reig

Martínez-Núñez

et al. 2004

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“…We observe that shortly before the disappearance of the disc and during the first instances of the formation of a new disc, the Hα line profile is symmetric and double peaked. None of the Be/X-ray binaries that have gone through disc-loss phases and for which there is a good optical follow-up coverage exhibited asymmetric profiles during the initial stages of disc formation: X Per in 1990 (Clark et al 2001), 4U 0115+63 in 1997 ) and in 2002 (Reig et al 2007), 1A 0535+262 in 1999 (Haigh et al 1999;Grundstrom et al 2007) and RX J0440.9+4431 in 2001 (Reig et al 2004). That is, the effects of the density perturbation do not show up until the disc is fully developed.…”

Section: Discussionmentioning

confidence: 99%

“…5 in Grundstrom et al (2007) for 1A 0535+262. Only a lower limit, >2 R * , can be given for RX J0440.9+4431 (Reig et al 2004).…”

Section: Discussionmentioning

confidence: 99%

The optical counterpart to IGR J06074+2205: a Be/X-ray binary showing disc loss andV/Rvariability

Reig

Zezas

Gkouvelis

2010

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Context. Current X-ray missions are regularly discovering new X/γ-ray sources, so identifying the counterparts of these high-energy sources at other wavelengths is important for determining their nature. In particular, optical observations are crucial in the study of X-ray binary populations in our Galaxy. Aims. The main goal of this work is to determine the properties of the optical counterpart to the INTEGRAL source IGR J06074+2205 and study its long-term optical variability. Although its nature as a high-mass X-ray binary has been suggested, little is known about its physical parameters. Methods. We have been monitoring IGR J06074+2205 since 2006 in the optical band. We present optical photometric BVRI and spectroscopic observations covering the wavelength band 4000−7000 Å. The blue spectra allow us to determine the spectral type and luminosity class of the optical companion and the red spectra, together with the photometric magnitudes, were used to derive the colour excess E(B − V) and estimate the distance. Results. We have carried out the first detailed optical study of the massive component in the high-mass X-ray binary IGR J06074+2205. We find that the optical counterpart to IGR J06074+2205 is a V = 12.3 B0.5Ve star located at a distance of ∼4.5 kpc. Monitoring of the Hα line reveals V/R variability and an overall decline in its equivalent width. The Hα line has been seen to revert from an emission to an absorption profile. We attribute this variability to global changes in the structure of the Be star's circumstellar disc that eventually led to the complete loss of the disc. The density perturbation that gives rise to the V/R variability vanishes when the disc becomes too small.

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“…The optical counterpart is a B0Ve star (V = 14.2) at a distance between 3.2 and 6.5 kpc (Baykal et al 2002;Reig et al 2004). Baykal et al (2002) found a correlation between spinup rate and X-ray flux during the 1999 outburst.…”

Section: Introductionmentioning

confidence: 99%

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

Camero

Zurita

Gutiérrez‐Soto

et al. 2014

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Aims. We present a multiwavelength study of the Be/X-ray binary system SAX J2103.5+4545 with the goal of better characterizing the transient behaviour of this source. Methods. SAX J2103.5+4545 was observed by Swift/XRT four times in 2007 from April 25 to May 5, and during quiescence in 2012 August 31. In addition, this source has been monitored from the ground-based astronomical observatories of El Teide (Tenerife, Spain), Roque de los Muchachos (La Palma, Spain), and Sierra Nevada (Granada, Spain) since 2011 August, and from the TÜBİTAK National Observatory (Antalya, Turkey) since 2009 June. We performed spectral and photometric temporal analyses to investigate the different states exhibited by SAX J2103.5+4545. Results. In X-rays, an absorbed power-law model provided the best fit for all the XRT spectra. An iron-line feature at ∼6.42 keV was present in all the observations except for that taken during quiescence in 2012. The photon indexes are consistent with previous studies of SAX J2103.5+4545 in high/low-luminosity states. Pulsations were found in all the XRT data from 2007 (2.839(2) mHz; MJD 54 222.02), but not during quiescence. The two optical outbursts in 2010 and 2012 lasted for about eight or nine months (as the one in 2007 probably did and the current one in 2014 might do) and were most probably caused by mass-ejection events from the Be star that eventually fed the circumstellar disc. All of these outbursts started about three months before the triggering of the X-ray activity, and at about the same period before the maximum of the Hα line equivalent width (in emission) was reached at only ∼-5 Å. The global correlation between the BV variability and the X-ray intensity was also observed at longer wavelengths in the IR domain.

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Discovery of the optical counterpart to the X-ray pulsar SAX J2103.5+4545

Cited by 45 publications

References 39 publications

INTEGRAL observations of the peculiar BeX System SAX J2103.5+4545

INTEGRAL observations of the peculiar BeX System SAX J2103.5+4545

The optical counterpart to IGR J06074+2205: a Be/X-ray binary showing disc loss andV/Rvariability

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

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