New high energy γ-ray sources observed by COS B

Hermsen, W.; Swanenburg, B. N.; Bignami, G. F.; Boella, G.; Buccheri, R.; Scarsi, L.; Kanbach, G.; Mayer‐Hasselwander, H. A.; Masnou, J. L.; Paul, J.; Bennett, K.; Higdon, J. C.; Lichti, G.; Taylor, B. G.; Wills, R. D.

doi:10.1038/269494a0

Cited by 124 publications

(65 citation statements)

References 5 publications

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“…X-Ray Data X-ray source 1E 1547.0À5408 was discovered by Einstein during a search for X-ray counterparts of unidentified -ray sources (Lamb & Markert 1981)-in this case, the -ray source 1C G327-0 detected by COS-B ( Hermsen et al 1977). This detection was confirmed by the Advanced Satellite for Cosmology and Astrophysics (ASCA) Galactic plane survey, in which the source AX J155052À5418 was detected at the same position (Sugizaki et al 2001).…”

Section: Observations Of 1e 15470à5408mentioning

confidence: 59%

“…Quiescent emission from magnetars has been detected at energies as high as $100 keV by the INTEGRAL satellite (Götz et al 2006;Kuiper et al 2004), but not in the >100 MeV range detected by COS-B from 1C G327-0 (Hermsen et al 1977). Although magnetars have been known to be the source of intense -ray flares (Hurley et al 2005), these events are rare (only three have been detected in the past 30 years), and the maximum photon energy detected from these flares ($1 MeV; Hurley et al 2005) is significantly less than the photon energies detected from 1C G327-0.…”

Section: Discussionmentioning

confidence: 99%

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The Compact X‐Ray Source 1E 1547.0−5408 and the Radio Shell G327.24‐0.13: A New Proposed Association between a Candidate Magnetar and a Candidate Supernova Remnant

Gelfand

Gaensler

2007

ApJ

116

150

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We present new observations of the field centered on X-ray source 1E 1547.0À5408. Analysis of a new Chandra observation shows that it is unresolved at arcsecond resolution, and analysis of a new XMM-Newton observation shows that its X-ray spectrum is best described by an absorbed power-law and blackbody model. A comparison of the X-ray flux observed from 1E 1547.0À5408 between 1980 and 2006 reveals that its absorbed 0.5Y10 keV X-ray flux decreased from $2 ; 10 À12 to $3 ; 10 À13 ergs cm À2 during this period. The most recent XMM-Newton observation detected no pulsations from 1E 1547.0À5408, allowing us to put a 5 confidence upper limit of 14% for the 0.5Y10 keV peak-to-peak pulsed fraction for sinusoidal pulses with periods slower than 1.8 s. A near-infrared observation shows a magnitude K s ¼ 15:9 AE 0:2 source near 1E 1547.0À5408, but the implied X-ray to infrared flux ratio indicates that it is an unrelated field source, limiting the IR magnitude of any counterpart to 1E 1547.0À5408 to k17.5. Archival radio observations reveal that 1E 1547.0À5408 sits at the center of a faint, small radio shell, G327.24-0.13, possibly a previously unidentified supernova remnant. The X-ray properties of 1E 1547.0À5408 suggest that it is a magnetar, and the spatial coincidence between this source and G327.24-0.13 suggests that 1E 1547.0À5408 is associated with a young supernova remnant, supporting a neutron star interpretation. If both the nature of 1E 1547.0À5408 and G327.24-0.13 and their physical association are confirmed, this pair will be an important addition to the small number of known associations between magnetars and supernova remnants.

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Section: Observations Of 1e 15470à5408mentioning

confidence: 59%

Section: Discussionmentioning

confidence: 99%

The Compact X‐Ray Source 1E 1547.0−5408 and the Radio Shell G327.24‐0.13: A New Proposed Association between a Candidate Magnetar and a Candidate Supernova Remnant

Gelfand

Gaensler

2007

ApJ

116

150

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“…It was first detected as a strong γ-ray source by the COS B satellite (Hermsen et al 1977). More recently, it has also been reported as a source of high-energy (HE) and very highenergy (VHE) γ-rays by the Fermi Large Area Telescope (LAT, Abdo et al 2009), the MAGIC Cherenkov Telescope (Albert et al 2006), and by the VERITAS Collaboration (Maier et al 2012).…”

Section: Ls I+61mentioning

confidence: 99%

Connection between orbital modulation of Hαand gamma-rays in the Be/X-ray binary LS I+61°303

Zamanov

Martı́

Stoyanov

et al. 2013

A&A

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We studied the average orbital modulation of various parameters (γ-ray flux, Hα emission line, optical V band brightness) of the radioand γ-ray emitting Be/X-ray binary LS I+61 • 303. Using the Spearman rank correlation test, we found highly significant correlations between the orbital variability of the equivalent width of the blue hump of the Hα and Fermi-LAT flux with a Spearman p-value ∼2 × 10 −5 , and the equivalent widths ratio EW B /EW R and Fermi-LAT flux with p-value ∼9 × 10 −5 . We also found a significant anticorrelation between Fermi-LAT flux and V band magnitude with a p-value ∼7 × 10 −4 . All these correlations refer to the average orbital variability, and we conclude that the Hα and γ-ray emission processes in LS I+61 • 303 are connected. The possible physical scenario is briefly discussed.

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“…• 303 has been attracting a lot of attention (and observing time) owing to its putative link with the gammaray source 2CG 135+01, discovered by COS-B (Hermsen et al 1977;Swanenburg et al 1981;Bignami & Hermsen 1983) 30 years ago and later confirmed by CGRO/EGRET, as 3EG J0241+6103 (Hartman et al 1999), with observations spanning the period 1991-2000. In spite of relentless efforts (Tavani et al 1996;Kniffen et al 1997), no conclusive evidence for the orbital modulation was found in the gamma-ray data, thus hampering the source identification.…”

Section: Ls I +61mentioning

confidence: 99%

Swift/XRT monitoring of five orbital cycles of LS I +61° 303

Esposito

Caraveo

Luca

et al. 2007

A&A

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Context. LS I +61• 303 is one of the most interesting high-mass X-ray binaries owing to its spatially resolved radio emission and its TeV emission, generally attributed to non-thermal particles in an accretion-powered relativistic jet or in the termination shock of the relativistic wind of a young pulsar. Also, the nature of the compact object is still debated. Only LS 5039 and PSR B1259−63 (which hosts a non-accreting millisecond pulsar) have similar characteristics. Aims. We study the X-ray emission from LS I +61 • 303 covering both short-term and orbital variability. We also investigate the source spectral properties in the soft X-ray (0.3-10 keV) energy range. Methods. Twenty-five snapshot observations of LS I +61 • 303 were collected in 2006 with the XRT instrument on-board the Swift satellite over a period of four months, corresponding to about five orbital cycles. Since individual data sets have too few counts for a meaningful spectral analysis, we extracted a cumulative spectrum. Results. The count rate folded at the orbital phase shows a clear modulation pattern at the 26.5 days period and suggests that the X-ray peak occurs around phase 0.65. Moreover, the X-ray emission appears to be variable on a timescale of ∼1 ks. The cumulative spectrum is well described by an absorbed power-law model, with hydrogen column density N H = (5.7 ± 0.3) × 10 21 cm −2 and photon index Γ = 1.78 ± 0.05. No accretion disk signatures, such as an iron line, are found in the spectrum.

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New high energy γ-ray sources observed by COS B

Cited by 124 publications

References 5 publications

The Compact X‐Ray Source 1E 1547.0−5408 and the Radio Shell G327.24‐0.13: A New Proposed Association between a Candidate Magnetar and a Candidate Supernova Remnant

The Compact X‐Ray Source 1E 1547.0−5408 and the Radio Shell G327.24‐0.13: A New Proposed Association between a Candidate Magnetar and a Candidate Supernova Remnant

Connection between orbital modulation of Hαand gamma-rays in the Be/X-ray binary LS I+61°303

Swift/XRT monitoring of five orbital cycles of LS I +61° 303

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