The Parkes half-jansky flat-spectrum sample

Drinkwater, Michael J.; Webster, R. L.; Francis, Paul; Condon, J. J.; Ellison, Sara L.; Jauncey, D. L.; Lovell, J. E. J.; Peterson, Bruce A.; Savage, A.

doi:10.1093/mnras/284.1.85

Cited by 163 publications

(159 citation statements)

References 28 publications

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“…These characteristics correspond to a normal AGN radiating at sub-Eddington luminosities, at 3× 10 −7 below the Eddington limit. They suggest that ADAF solutions can explain the X-ray spectrum, but these models failed to explain the high radio power of its compact source (Drinkwater et al 1997). The fitting parameters from GM+06 are in remarkably good agreement with theirs (Γ = 1.89, kT = 0.30 keV and L(2-10 keV) = 3.6× 10 40 erg s −1 ).…”

Section: Ic 1459 (Ic 5265)mentioning

confidence: 59%

An X-ray view of 82 LINERs with Chandra and XMM-Newton data

González‐Martín¹,

Masegosa

Márquez

et al. 2009

A&A

175

226

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We present the results of a homogeneous X-ray analysis for 82 nearby low-ionisation, narrow emission-line regions (LINERs) selected from the catalogue of Carrillo et al. (1999, Rev. Mex. Astron. Astrofis., 35, 187). All sources have available Chandra (68 sources) and/or XMM-Newton (55 sources) observations. This is the largest sample of LINERs with X-ray spectral data (60 out of the 82 objects), and it significantly improves our previous analysis based on Chandra data for 51 LINERs (Gonzalez-Martin et al. 2006b, A&A, 460, 45). It both increases the sample size and adds XMM-Newton data. New models permit the inclusion of double absorbers in the spectral fits. Nuclear X-ray morphology is inferred from the compactness of detected nuclear sources in the hard band (4.5-8.0 keV). Sixty per cent of the sample shows a compact nuclear source and are classified as active galactic nucleus (AGN) candidates. The spectral analysis indicates that best fits involve a composite model: 1) absorbed primary continuum and 2) soft spectrum below 2 keV described by an absorbed scatterer and/or a thermal component. The resulting median spectral parameters and their standard deviations are Γ = 2.11 ± 0.52, kT = 0.54 ± 0.30 keV, log(NH1) = 21.32 ± 0.71 and log(NH2) = 21.93 ± 1.36. We complement our X-ray results with an analysis of HST optical images and literature data on emission lines, radio compactness, and stellar population. After adding all these multiwavelength data, we conclude that evidence supports the AGN nature of their nuclear engine for 80% of the sample (66 out of 82 objects).

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Section: Ic 1459 (Ic 5265)mentioning

confidence: 59%

An X-ray view of 82 LINERs with Chandra and XMM-Newton data

González‐Martín¹,

Masegosa

Márquez

et al. 2009

A&A

175

226

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“…Perley Stickel et al (1993) for all sources but 0138−097 and 0454+844 (Stocke & Rector 1997), 0814+425 (Falomo et al 1997) and 2131−021 (Drinkwater et al 1997 Murphy et al (1993).…”

Section: −097mentioning

confidence: 97%

Extended radio emission in BL Lac objects

Cassaro

Stanghellini

Bondì

et al. 1999

Astron. Astrophys. Suppl. Ser.

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Abstract.We have observed 28 sources selected from the 1Jy sample of BL Lac objects (Stickel et al. 1991) with the Very Large Array (VLA) in A, B and D configurations at 1.36, 1.66 and 4.85 GHz, and/or with the Westerbork Synthesis Radio Telescope (WSRT) at 1.40 GHz. In this paper we present high sensitivity images at arcsecond resolution of the 18 objects showing extended structure in our images, and of another source from the FIRST (Faint Images of the Radio Sky at Twenty-cm) survey (Becker et al. 1995). In general our high sensitivity images reveal an amount of extended emission larger than previously reported. In some objects the luminosity of the extended structure is comparable with that of FR II radio sources. A future paper will be devoted to the interpretation of these results.

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“…For this reason, added to the fact that this region of the sky is poorly sampled by large X-ray surveys, it is difficult to find the possible responsible for this excess. After having checked in the literature, we found as a tentative candidate a QSO at z = 1.335 (Drinkwater et al 1997;Venturi et al 2000), located at α 2000 = 13 h 30 m 19 s and δ 2000 = −31 • 22 59 , i.e. North-East with respect to the position of SC 1327-312.…”

Section: Pds Datamentioning

confidence: 98%

SC 1327–312 & SC 1329–313: Two galaxy groups in-between a major merging event observed with Beppo–SAX

Bardelli

Grandi

Ettori

et al. 2002

A&A

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Abstract. We present the results of two Beppo-SAX observations of the poor clusters SC 1327-312 and SC 1329-313: these objects are located in a huge structure, formed by three ACO clusters, which is probably the remnant of one of the largest and best studied major mergings known. Given the fact that these poor clusters are in between two interacting ACO clusters, the aim of this work is to study the physics of the intracluster medium and to look for the possible presence of shocks. We derived the gas distribution profiles, the global (i.e. within 0.3 h −1 Mpc) temperatures and abundances and the temperature profiles and maps for SC 1327-312 and SC 1329-313. Also the presence of soft excess in LECS and hard excess in PDS have been examined. We do not find evidence of regions where the gas is shocked or significantly heated. The image of SC 1327-312 seems rather symmetric, while the gas profile of SC 1329-313 shows disturbed, "comet-like" shaped isophotes, with the tail pointing toward A3562 and a compression toward SC 1327-312. The presence of multiphase gas in SC 1329-313, as claimed by Hanami et al. (1999) based on ASCA data, has been found only at the 2σ confidence level. The lack of heating supports the hypothesis that the merging is at a late stage, after the first core-core encounter, when the main shock front had the time to travel to the external regions of the main clusters.

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The Parkes half-jansky flat-spectrum sample

Cited by 163 publications

References 28 publications

An X-ray view of 82 LINERs with Chandra and XMM-Newton data

An X-ray view of 82 LINERs with Chandra and XMM-Newton data

Extended radio emission in BL Lac objects

SC 1327–312 & SC 1329–313: Two galaxy groups in-between a major merging event observed with Beppo–SAX

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