<i>BeppoSAX</i>Observations of the Maser Seyfert 2 Galaxy ESO 103‐G35

Wilkes, B. J.; Mathur, S.; Fiore, F.; Antonelli, L. A.; Nicastro, F.

doi:10.1086/319063

Cited by 18 publications

(23 citation statements)

References 55 publications

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“…Such high values of R are possible, as suggested by Guainazzi (2001), if the intrinsic flux is variable, since the observed reflection component is produced by radiation emitted at a different time with respect to the observed primary emission. ESO 103-G35: The BeppoSAX data of this source have been analyzed by Wilkes et al (2000). Even if the models used in our work are slightly different, the basic results are in agreement with these authors.…”

Section: Discussionsupporting

confidence: 86%

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The BeppoSAX view of bright Compton-thin Seyfert 2 galaxies

Risaliti

2002

A&A

129

145

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Abstract. We present the analysis of 31 observations (17 of which are published here for the first time) of 20 bright Compton thin Seyfert 2 s, in the 0.1-200 keV band, performed with the BeppoSAX satellite. The sample consists of all Seyfert 2 s in the BeppoSAX public archive, with a 2-10 keV flux higher than 5 × 10 −12 erg cm −2 s −1 . The good statistics available and the broad energy band permit a detailed study of the main continuum components of these sources, i.e. the primary power-law, the reflected component, the soft emission and the high-energy cut-off. The main results of our analysis are: (1) the 3-200 keV intrinsic power-law has a mean photon index Γ = 1.79 ± 0.01, with a dispersion of σ = 0.23. (2) The high-energy exponential cut-off at E ∼ 100−300 keV is not an ubiquitous property of Seyfert galaxies: in ∼30% of the objects the continuum power-law does not drop up to energies of 300 keV or more. (3) A reflected component is present in almost all the sources (17 out of 21). The small variations of this component with respect to the intrinsic continuum, in objects with multiple observations, suggests that the reflector is not the accretion disk, but must be located much farther from the nucleus. (4) The range of ratios between the reflected and intrinsic components suggests that the circumnuclear medium is not homogeneous, and a significant fraction of the solid angle is covered by a gas thicker than that along the line of sight. (5) The iron Kα line is present is all but one the sources. The equivalent width is in the typical range of Seyfert 1 s (EW = 100−300 eV) in sources with low absorption (NH < 3 × 10 23 cm −2 ), and increases in more absorbed objects, as expected according to unified models. (6) The energy resolution of BeppoSAX is in general too low to measure the iron line width. However, in 6 cases we measured a significant line broadening.

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Section: Discussionsupporting

confidence: 86%

“…In the first observation we find E C = 84 +134 −33 keV. This is the lowest measured cut-off energy in our sample, but it is significantly higher than that found by Wilkes et al (2000) (E C = 29 ± 10 keV).…”

Section: Discussioncontrasting

confidence: 62%

The BeppoSAX view of bright Compton-thin Seyfert 2 galaxies

Risaliti

2002

A&A

129

145

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“…However we note that a stronger constraint is found from the 1996 October and 1997 BeppoSAX observations of ESO 103-G35, in which a reÑection component is indicated in a spectrum that extends up to D200 keV (Wilkes et al 1999). …”

Section: No Reñection Continuum In Ngc 4388 or Eso 103-g35mentioning

confidence: 72%

“…One of these sources can be identiÐed with a star with a proper motion of k \ 0.165^0.022 m B \ 11.5 arcsec yr~1 (Wroblewski & Torres 1994), and the other remains unidentiÐed. The Ñux from the PSPC observation of the weak, unresolved nuclear soft X-ray source identiÐed with ESO 103-G35 is consistent with that seen during the 1994 ASCA observation, although slightly low compared to that observed in the 1996 observation.…”

Section: T He Asca Spectra Of Eso 103-g35mentioning

confidence: 99%

The X‐Ray Spectra and Spectral Variability of Intermediate‐Type Seyfert Galaxies:ASCAObservations of NGC 4388 and ESO 103‐G35

Leighly¹,

Kay²

1999

ApJ

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The X-ray spectra of two intermediate-type Seyfert galaxies are investigated using ASCA observations separated by more than 1 yr. Both NGC 4388 and ESO 103-G35 exhibit strong, narrow Fe Ka line emission and absorption by cold neutral gas with a column density D1023 cm~2, characteristic of the X-ray spectra of type 2 Seyfert galaxies. The power-law continuum Ñux has changed by a factor of 2 over a timescale of D2 yr for both objects, declining in the case of NGC 4388 and rising in ESO 103-G35. No variation was observed in the equivalent width of the Fe Ka line in the spectra of NGC 4388, implying that the line Ñux declined with the continuum. We Ðnd that the strength of the line cannot be accounted for by Ñuorescence in line-of-sight material with the measured column density unless a "" leaky-absorber ÏÏ model of the type favored for IRAS 04575[7537 is employed. The equivalent width of the Fe Ka emission line is seen to decrease between the observations of ESO 103-G35 while the continuum Ñux increased. The 1996 observation of ESO 103-G35 can also be Ðtted with an absorption edge at 7.4^0.2 keV due to partially ionized iron, and when an ionized absorber model is Ðtted to the data it is found that the equivalent column of neutral hydrogen rises to 3.5 ] 1023 cm~2. The Fe Ka line Ñux can be accounted by Ñuorescence in this material alone, and this model is also a good representation of the 1988 and 1991 Ginga observations. There is then no requirement for a reÑection component in the ASCA spectra of ESO 103-G35 or NGC 4388.

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“…Mattson & Weaver (2004) for MCG-05-23-16, Guainazzi et al (2000) for NGC 4945, Grandi et al (2003) for Centaurus A, Matt et al (1999) and Guainazzi et al (1999) for the Circinus galaxy, Guainazzi (2002) for NGC 6300 and Wilkes et al (2001) for ESO 103-G35.…”

Section: Comparison With Bepposax/pds Resultsmentioning

confidence: 96%

INTEGRAL observations of six AGN in the Galactic Plane

Soldi

Beckmann

Bassani

et al. 2005

A&A

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We present results on approximately one year of INTEGRAL observations of six AGN detected during the regular scans of the Galactic Plane. The sample is composed by five Seyfert 2 objects (MCG -05-23-16, NGC 4945, the Circinus galaxy, NGC 6300, ESO 103-G35) and the radio galaxy Centaurus A. The continuum emission of each of these sources is well represented by a highly absorbed (N H > 10 22 cm −2 ) power law, with average spectral index Γ = 1.9 ± 0.3. A high energy exponential cut-off at E c ∼ 50 keV is required to fit the spectrum of the Circinus galaxy, whereas a lower limit of 130 keV has been found for NGC 4945 and no cut-off has been detected for NGC 6300 in the energy range covered by these INTEGRAL data. The flux of Centaurus A was found to vary by a factor of ∼2 in 10 months, showing a spectral change between the high and low state, which can be modelled equally well by a change in the absorption (N H from 17 to 33 × 10 22 cm −2 ) or by the presence of a cut-off at > ∼ 120 keV in the low state spectrum. A comparison with recently reprocessed BeppoSAX/PDS data shows a general agreement with INTEGRAL results. The high energy cut-off in the hard X-ray spectra appears to be a common but not universal characteristic of Seyfert 2 and to span a wide range of energies.

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BeppoSAXObservations of the Maser Seyfert 2 Galaxy ESO 103‐G35

Cited by 18 publications

References 55 publications

The BeppoSAX view of bright Compton-thin Seyfert 2 galaxies

The BeppoSAX view of bright Compton-thin Seyfert 2 galaxies

The X‐Ray Spectra and Spectral Variability of Intermediate‐Type Seyfert Galaxies:ASCAObservations of NGC 4388 and ESO 103‐G35

INTEGRAL observations of six AGN in the Galactic Plane

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