The Einstein Slew Survey

Elvis, M.; Plummer, David A.; Schachter, J. F.; Fabbiano, G.

doi:10.1086/191665

Cited by 226 publications

(212 citation statements)

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“…1ES 1210-646 is a poorly studied X-ray source, which was found during the Einstein Slew Survey (Elvis et al, 1992). Based on optical spectroscopy the system was classified as a HMXB ).…”

Section: Discussionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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“…1ES 1210-646 is a poorly studied X-ray source, which was found during the Einstein Slew Survey (Elvis et al, 1992). Based on optical spectroscopy the system was classified as a HMXB ).…”

Section: Discussionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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“…The BL Lac object 1ES 2344+514, at a redshift of 0.044, was detected in the Einstein Slew Survey ( Elvis et al 1992) in the energy range 0.2-4 keV. The survey was constructed from data collected during the High Energy Astronomical Observatory 2 (HEAO 2) mission from 1978 to 1981.…”

Section: Observational Status Of 1es 2344+514mentioning

confidence: 99%

A Very High Energy Gamma‐Ray Spectrum of 1ES 2344+514

Schroedter

Badran

Buckley

et al. 2005

ApJ

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The BL Lacertae ( BL Lac) object 1ES 2344+514 (1ES 2344), at a redshift of 0.044, was discovered as a source of very high energy ( VHE) gamma rays by the Whipple collaboration in 1995 (Catanese et al.). This detection was recently confirmed by the HEGRA collaboration (Tluczykont et al.). As is typical for high-frequency-peaked blazars, the VHE gamma-ray emission is highly variable. On the night of 1995 December 20, a gamma-ray flare of 5.3 significance was detected, the brightest outburst from this object to date. The emission region is compatible with a point source. The spectrum between 0.8 and 12.6 TeV can be described by a power law, If we compare the spectral index with that of the other five confirmed TeV blazars, the spectrum of 1ES 2344 is similar to that of 1ES 1959+650, which is located at almost the same distance. The spectrum of 1ES 2344 is steeper than the brightest flare spectra of Markarian 421 ( Mrk 421) and Markarian 501 ( Mrk 501), both of which are located at a distance about two-thirds that of 1ES 2344, and harder than the spectra of PKS 2155À304 and H1426+428, which are located almost 3 times as far away. This trend is consistent with attenuation caused by the infrared extragalactic background radiation.

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“…It has not been studied in detail in spite of being observed on many occasions (Fairall 1988;Wisotzki et al 1996;Karachentsev & Makarov 1996). It was previously observed in X-rays with the ROSAT (1990 August; Voges et al 1999; Thomas et al 1998) and Einstein (Elvis et al 1992) satellites, as part of the study of the general properties of objects with X-ray emission (Simcoe et al 1997;Grupe et al 2001;Jahnke & Wisotzki 2003;Fuhrmeister & Schmitt 2003). More recently, it has been observed by Swift (2008 October) as part of a sample of 92 bright soft X-ray selected AGNs (Grupe et al 2010).…”

Section: Introductionmentioning

confidence: 97%

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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Aims. We seek a comprehensive analysis of all the information provided by the XMM-Newton satellite of the four Seyfert 1 galaxies ESO 359-G19, HE 1143-1810, CTS A08.12, and Mrk 110, including the UV range, to characterize the different components that are emitting and absorbing radiation in the vicinity of the active nucleus. Methods. The continuum emission was studied through the EPIC spectra by taking advantage of the spectral range of these cameras. The high-resolution RGS spectra were analyzed to characterize the absorbing and emission line features that arise in the spectra of the sources. All these data, complemented by information in the UV, are analyzed jointly in order to achieve a consistent characterization of the observed features in each object. Results. The continuum emission of the sources can be characterized either by a combination of a power law and a black body for the weakest objects or by two power law components for the brightest ones. The continuum is not absorbed by neutral or ionized material in the line of sight to any of these sources. In all of them we have identified a narrow Fe-Kα line at 6.4 keV. In ESO 359-G19 we also find an Fexxvi line at about 7 keV. In the soft X-rays band, we identify only one Ovii line in the spectra of HE 1143-1810 and CTS A08.12, and two Ovii-Heα triplets and a narrow Oviii-Lyα emission line in Mrk 110. Conclusions. Not detecting warm material in the line of sight to the low state objects is due to intrinsically weaker or absent absorption in the line of sight and not to a low signal-to-noise ratio in the data. Besides this, the absence of clear emission lines cannot be fully attributed to dilution of those lines by a strong continuum.

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The Einstein Slew Survey

Cited by 226 publications

References 0 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

A Very High Energy Gamma‐Ray Spectrum of 1ES 2344+514

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

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