The nature of the X-ray binary IGR J19294+1816 fromINTEGRAL,RXTE, andSwiftobservations

Rodríguez, J.; Tomsick, John A.; Bodaghee, A.; Heras, J. A. Zurita; Chaty, S.; Paizis, A.; Corbel, S.

doi:10.1051/0004-6361/200912739

Cited by 18 publications

(17 citation statements)

References 24 publications

(31 reference statements)

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“…The source lies in the Galactic plane where flux from the Galactic ridge needs to be included in the spectral modeling (Valinia & Marshall 1998). We have strictly followed the recipe of Rodriguez et al (2009a) while adding the Galactic ridge spectrum to the instrumental background spectrum. The data reduction and analysis was carried out using HEASOFT 3 , which consists of (chiefly) FTOOLS for general data extraction and analysis, XRONOS (Stella & Angelini 1992) for the timing analysis and XSPEC (Arnaud 1996) for the spectral analysis.…”

Section: Discussionmentioning

confidence: 99%

Timing and Spectral Study of IGR J19294+1816 with the RXTE: The Discovery of Cyclotron Features

Roy

Choudhury

Agrawal

2017

ApJ

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Gauss. This is also detected at a lower significance in two other observations. In addition an Fe line emission at 6.4 keV is prominently detected during the highest flux.X-ray pulsations are detected in 9 out of 10 observations; no pulsations were found in the observation with the lowest flux level. During this observation with the lowest flux the pulsation phenomenon becomes detectable only at the soft X-ray bands.

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Section: Discussionmentioning

confidence: 99%

Timing and Spectral Study of IGR J19294+1816 with the RXTE: The Discovery of Cyclotron Features

Roy

Choudhury

Agrawal

2017

ApJ

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“…Following previous works (e.g. Prat et al 2008;Rodriguez et al 2009), we estimated its level according to the Valinia & Marshall (1998) model, and by assuming that Chandra and RXTE/PCA are perfectly cross-calibrated. After removing the Galactic X-ray contribution, we found that a power-law fit to the 3-20 keV PCA spectrum gives a N H similar to that found for the three Chandra components, though not well constrained, (2.25 ± 1.1) × 10 22 cm −2 .…”

Section: Spectral Analysismentioning

confidence: 99%

Discovery of a Highly Energetic Pulsar Associated With Igr J14003–6326 in the Young Uncataloged Galactic Supernova Remnant G310.6–1.6

Renaud

Marandon

Gotthelf

et al. 2010

ApJ

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We report the discovery of 31.18 ms pulsations from the INTEGRAL source IGR J14003−6326 using the Rossi Xray Timing Explorer (RXTE). This pulsar is most likely associated with the bright Chandra X-ray point source lying at the center of G310.6−1.6, a previously unrecognized Galactic composite supernova remnant (SNR) with a bright central non-thermal radio and X-ray nebula, taken to be the pulsar wind nebula (PWN). PSR J1400−6325 is amongst the most energetic rotation-powered pulsars in the Galaxy, with a spin-down luminosity ofĖ = 5.1 × 10 37 erg s −1 . In the rotating dipole model, the surface dipole magnetic field strength is B s = 1.1 × 10 12 G and the characteristic age τ c ≡ P /2Ṗ = 12.7 kyr. The high spin-down power is consistent with the hard spectral indices of the pulsar and the nebula of 1.22 ± 0.15 and 1.83 ± 0.08, respectively, and a 2-10 keV flux ratio F PWN /F PSR ∼ 8. Followup Parkes observations resulted in the detection of radio emission at 10 and 20 cm from PSR J1400−6325 at a dispersion measure of ∼560 cm −3 pc, which implies a relatively large distance of 10 ± 3 kpc. However, the resulting location off the Galactic plane of ∼280 pc would be much larger than the typical thickness of the molecular disk, and we argue that G310.6−1.6 lies at a distance of ∼7 kpc. There is no gamma-ray counterpart to the nebula or pulsar in the Fermi data published so far. A multi-wavelength study of this new composite SNR, from radio to very high-energy gamma rays, suggests a young ( 10 3 yr) system formed by a sub-energetic ( 10 50 erg), low ejecta mass (M ej ∼ 3 M ) supernova explosion that occurred in a low-density environment (n 0 ∼ 0.01 cm −3 ).

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“…A summary of all these results and an in-depth inspection of all available INT EGRAL observations performed in the direction of the source was provided by Rodriguez et al (2009a). The authors reported on the discovery of relatively short flares (few thousands of seconds) from this source with INT EGRAL, and concluded that, even though the orbital and Send offprint requests to: E. Bozzo spin period of IGR J19294+1816 would nicely place the source in the region of the P spin -P orb diagram populated by the Be Xray binaries, a possible supergiant fast X-ray (SFXTs, see e.g., Walter & Zurita Heras 2007) nature of this source could not be ruled out.…”

Section: Introductionmentioning

confidence: 99%

INTEGRAL and Swift observations of IGR J19294+1816 in outburst

Bozzo

Ferrigno

Falanga

et al. 2011

A&A

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Context. IGR J19294+1816 was discovered by INT EGRAL in 2009 during a bright X-ray outburst and was classified as a possible Be X-ray binary or supergiant fast X-ray transient. Aims. On 2010 October 28, the source displayed a second X-ray outburst and a two months-long monitoring with Swift was carried out to follow the evolution of the source X-ray flux during the event.Methods. We report on the INT EGRAL and Swift observations of the second X-ray outburst observed from IGR J19294+1816. Results. We detected pulsations in the X-ray emission from the source at ∼12.5 s up to 50 keV. The source X-ray flux decreased smoothly during the two months of observation, displaying only marginal spectral changes. Owing to the relatively rapid decay of the source X-ray flux, no significant variations of the source spin period across the event could be measured. This prevented a firm confirmation of the previously suggested orbital period of the source at 117 d. This periodicity was also searched for in archival Swift /BAT data. We detected a marginally significant peak in the periodogram and determined the best period at 116.2±0.6 days (estimated chance probability of a spurious detection 1%).Conclusions. The smooth decline of the source X-ray flux across the two months of observations after the onset of the second outburst, together with its relatively low value of the spin period and the absence of remarkable changes in the spectral parameters (i.e., the absorption column density), suggests that IGR J19294+1816 is most likely another member of the Be X-ray binaries discovered by INT EGRAL and not a supergiant fast X-ray transient.

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The nature of the X-ray binary IGR J19294+1816 fromINTEGRAL,RXTE, andSwiftobservations

Cited by 18 publications

References 24 publications

Timing and Spectral Study of IGR J19294+1816 with the RXTE: The Discovery of Cyclotron Features

Timing and Spectral Study of IGR J19294+1816 with the RXTE: The Discovery of Cyclotron Features

Discovery of a Highly Energetic Pulsar Associated With Igr J14003–6326 in the Young Uncataloged Galactic Supernova Remnant G310.6–1.6

INTEGRAL and Swift observations of IGR J19294+1816 in outburst

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