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J/A+AS/131/303 GHz-Peaked-Spectrum radio sources (Stanghellini+ 1998) ================================================================================ A complete sample of GHz-Peaked-Spectrum radio sources and its radio properties Stanghellini C., O'Dea C.P., Dallacasa D., Baum S.A., Fanti R., Fanti C.=1998A&AS..131..303S (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Radio sources Keywords: galaxies: active - quasars: general - radio continuum: galaxies Abstract: We define a complete sample of thirty-three GHz-Peaked-Spectrum (GPS) radio sources based on their spectral properties. We present measurements of the radio spectra and polarization of the complete sample and a list of additional GPS sources which fail one or more criteria to be included in the complete sample. The majority of the data have been obtained from quasi-simultaneous multi-frequency observations at the Very Large Array (VLA) during 3 observing sessions. Low frequency data from the Westerbork Synthesis Radio Telescope (WSRT) and from the literature have been combined with the VLA data in order to better define the spectral shape. The objects presented here show a rather wide range of spectral indices at high and low frequencies, including a few cases where the spectral index below the turnover is close to the theoretical value of 2.5 typical of self-absorbed incoherent synchrotron emission. Faint and diffuse extended emission is found in about 10% of the sources. In the majority of the GPS sources, the fractional polarization is found to be very low, consistent with the residual instrumental polarization of 0.3%. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table4.dat 30 378 Flux densities for the complete sample table5.dat 30 162 Flux densities for the additional objects tables.tex 90 984 LaTeX version of the tables -------------------------------------------------------------------------------- See also: VIII/42 : Texas Survey of radio sources at 365MHz (Douglas+ 1996) VIII/16 : Molonglo Reference Catalogue of Radio Sources (Large+ 1991) VIII/5 : Bright Extragalactic Radio Sources (1Jy) (Kuehr+, 1981) VIII/37 : The Third Bologna Survey (B3) (Ficarra+ 1985) VIII/18 : 6C Survey of radio sources I. (Baldwin+ 1985) VIII/21 : 6C Survey of radio sources II. (Hales+ 1988) VIII/22 : 6C Survey of Radio Sources III. (Hales+ 1990) VIII/23 : 6C Survey of radio sources IV. (Hales+ 1991) VIII/24 : 6C Survey of Radio Sources V. (Hales+ 1993) VIII/25 : 6C Survey of radio sources VI. (Hales+ 1993) Byte-by-byte Description of file: table4.dat table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Name Source Name (1) 10- 15 F6.3 GHz nu Frequency 17- 21 F5.3 Jy Snu Flux density 23- 27 F5.3 Jy e_Snu rms uncertainty on S (2) 29- 30 I2 --- r_Snu References (3) -------------------------------------------------------------------------------- Note (1): Individual notes: 0108+388: the flux density at 608 MHz and higher frequencies refers to the core only, while the flux density measure at 325 MHz likely includes the extended structure found close to the main compact component (Baum et al. 1990). 0552+398: the flux density at 37 GHz is the average of the data taken in 1990 (Terasranta et al., 1992A&AS...94..121T), and the error is the r.m.s of the distribution. The flux density at 90GHz is the average of the data taken in 1990 (Steppe et al., 1992A&AS...96..441S), and the error is the r.m.s of the distribution. 2134+004: The flux density at 87 GHz is the average of the data taken between 1985 and 1988 (Terasranta et al., 1992A&AS...94..121T), the error is the r.m.s of the distribution. Note (2): The errors are taken as 3% if they were found in literature to be less then 3%. Note (3): 1: VLA first session 2: VLA second session 3: VLA third session 4: WSRT 5: Northern Cross 6: Ratan 600 7: Douglas et al., 1996AJ....111.1945D, Cat. 8: Large et al., 1981MNRAS.194..693L, Cat. 9: Kuhr et al., 1981A&AS...45..367K, Cat. 10: Baum et al., 1990A&A...232...19B 11: de Bruyn, private communication 12: de Bruyn, 1990, in Proc. Dwingeloo Workshop, Compact Steep Spectrum and GHz Peaked Spectrum Radio Sources, ed. C. Fanti, R.Fanti, C.P. O'Dea, & R.T. Schilizzi, (Bologna: Istituto di Radioastronomia), p.105 13: Steppe et al., 1988A&AS...75..317S 14: Chandler, 1995, VLA Test Memo 192 15: Ficarra et al., 1985A&AS...59..255F, Cat. 16: Esko, private communication 17: Gower et al., 1967MmRAS..71...49G, Pilkington et al., 1965MmRAS..69..183P 18: Dennison et al., 1981AJ.....86.1604D 19: Edelson, 1987AJ.....94.1150E 20: Terasranta et al., 1992A&AS...94..121T 23: Fiedler et al., 1987ApJS...65..319F 24: Steppe et al., 1992A&AS...96..441S 25: Baldwin et al., 1985MNRAS.217..717B, Cat. 26: Hales et al., 1988MNRAS.234..919H, Cat. 27: Hales et al., 1990MNRAS.246..256H, Cat < VIII/22> 28: Hales et al., 1991MNRAS.251...46H, Cat. 29: Hales et al., 1993MNRAS.262.1057H, Cat. 30: Hales et al., 1993MNRAS.263...25H, Cat. 31: Khabrakhmanov, private communication. -------------------------------------------------------------------------------- Acknowledgements: Carlo Stanghellini ================================================================================ (End) Patricia Bauer [CDS] 19-Mar-1998