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J/A+A/471/1105      XMM-LSS at 240MHz and 610MHz             (Tasse+, 2007)

GMRT observations of the XMM Large Scale Structure Survey field. Tasse C., Roettgering H.J.A., Best P.N., Cohen A.S., Pierre M., Wilman R. <Astron. Astrophys. 471, 1105 (2007)> =2007A&A...471.1105T
ADC_Keywords: Surveys ; Active gal. nuclei ; Radio sources Keywords: techniques: interferometric - methods: statistical - surveys - galaxies: active - radio continuum: galaxies - cosmology: large-scale structure of Universe Abstract: The low-frequency radio survey of the XMM-Large Scale Structure (XMM-LSS) field aims to study the connection between the extragalactic radio source populations and their environment as traced by X-ray and optical emission. In this paper we present new radio observations of the XMM-LSS field carried out using the Giant Meterwave Radio Telescope at 240 and 610MHz. These observations complement the observations presented by Cohen at al. (2003, Cat. J/ApJ/591/640) and Tasse et al. (2006, Cat. J/A+A/456/791) at 74 and 325MHz with the Very Large Array. At 240 and 610MHz, we reach noise levels of ∼2.5 and ∼0.3mJy/beam, leading to the detection of 466 and 769 sources over 18.0 and 12.7 degree2 with resolutions of 14.7arcsec and 6.5arcsec respectively. Combining these data with the available source lists at 74, 325 (Tasse et al., 2006, Cat. J/A+A/456/791) and 1400MHz (NVSS), we build a multifrequency catalogue containing 1611 radio sources. We check for consistency of the astrometry and flux density estimates. We fit a simple synchrotron radiation model to the flux density measurements of the 318 radio sources being detected in at least 4 bands. While ∼26% of them show signature of spectral ageing, ∼6% show self absorption. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 118 571 The 240MHz source list table4.dat 118 1037 The 610MHz source list table5.dat 131 318 Fitting parameters
See also: J/ApJ/591/640 : XMM-LSS low-frequency radio counterparts (Cohen+, 2003) J/A+A/439/413 : XMDS/VVDS 4σ catalogue (Chiappetti+, 2005) J/A+A/456/791 : XMM-LSS field at 74 and 325MHz (Tasse+, 2006) Byte-by-byte Description of file: table[34].dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Source Name (JHHMM.m+DDMM) 14- 15 I2 h RAh Right ascension (J2000) 17- 18 I2 min RAm Right ascension (J2000) 20- 24 F5.2 s RAs Right ascension (J2000) 26- 29 F4.2 arcsec e_RAs rms uncertainty on RA 31 A1 --- DE- Declination sign (J2000) 32- 33 I2 deg DEd Declination (J2000) 35- 36 I2 arcmin DEm Declination (J2000) 38- 42 F5.2 arcsec DEs Declination (J2000) 44- 47 F4.2 arcsec e_DEs rms uncertainty on DE 49 A1 --- Type [SMC] Source type: (S)ingle, (M)ultiple or (C)omponent of multiple source 51- 57 F7.1 mJy Sint ? Total integrated flux density at 240MHz (table3) or 610MHz (table4) 59- 64 F6.1 mJy e_Sint ? rms uncertainty on Sint 65 A1 --- n_Sint [*] *: flux calculated with pixel based method 66- 72 F7.1 mJy Scomp Integrated flux density of individual Gaussian fitting component at 240MHz (table3) or 610MHz (table4) 74- 79 F6.1 mJy e_Scomp rms uncertainty on Scomp 81 A1 --- l_amaj Limit flag on amaj 82- 85 F4.1 arcsec amaj Deconvolved size of major axis, or the 2σ upper limit if the source is unresolved 87- 90 F4.1 arcsec e_amaj ? rms uncertainty on amaj 92 A1 --- l_amin Limit flag on amin 93- 96 F4.1 arcsec amin ?=- Deconvolved size of minor axis, or 2σ upper limit if the source is unresolved 98-100 F3.1 arcsec e_amin ? rms uncertainty on amin 102-106 F5.1 deg PA ?=- Position angle of major axis 108-111 F4.1 deg e_PA ? rms uncertainty on PA 113 A1 --- l_SI Limit flag on SI 114-118 F5.2 --- SI ? Spectral index, with respect to NVSS flux density (1.4GHz) (1)
Note (1): Spectral index α2401400 for table3, α6101400 for table4.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Source Name (JHHMM.m+DDMM) 14- 15 I2 h RAh Right ascension (J2000) 17- 18 I2 min RAm Right ascension (J2000) 20- 24 F5.2 s RAs Right ascension (J2000) 26- 29 F4.2 arcsec e_RAs rms uncertainty on RA 31 A1 --- DE- Declination sign (J2000) 32- 33 I2 deg DEd Declination (J2000) 35- 36 I2 arcmin DEm Declination (J2000) 38- 42 F5.2 arcsec DEs Declination (J2000) 44- 47 F4.2 arcsec e_DEs rms uncertainty on DE 49- 54 F6.1 mJy S0 Best fit S0 parameter value 56- 60 F5.1 mJy E_S0 Upper limit of S0 68% confidence interval 62- 66 F5.1 mJy e_S0 Lower limit of S0 68% confidence interval 68- 72 F5.2 --- alpha Best fit spectral index α value 74- 77 F4.2 --- E_alpha Upper limit of alpha 68% confidence interval 79- 82 F4.2 --- e_alpha Lower limit of alpha 68% confidence interval 84- 89 F6.1 MHz nu1 ?=- Best fit ν1 parameter value 91- 95 F5.1 MHz E_nu1 ? Upper limit of nu1 68% confidence interval. See note (1) 97-101 F5.1 MHz e_nu1 ? Lower limit of nu1 68% confidence interval. See note (1) 102 A1 --- nenu1 [i] i for infinity 104-109 F6.1 MHz nuc ?=- Best fit νc parameter value 111-115 F5.1 MHz E_nuc ? Upper limit of nuc 68% confidence interval. See note (2) 116 A1 --- nenuc [i] i for infinity 118-122 F5.1 MHz e_nuc ? Lower limit of nuc 68% confidence interval. See note (2) 124-129 F6.2 --- log(chi2r) Least χ2reduced logarithmic value 131 A1 --- Class [0-3] Class indicator (3)
Note (1): "---" means that the upper bound of the 68% confidence interval lies below the lowest available frequency. Note (2): "---" means that the lower bound of the 68% confidence interval lies above the highest available frequency. Note (3): Class indicator as follows: 1 = to fit the flux density points the model needs the presence of self-absorption and no spectral aging 2 = to fit the flux density points the model needs the presence of spectral aging and no self-absorption 3 = to fit the flux density points the model needs the presence of self-absorption and spectral aging 0 = all other cases
Acknowledgements: Cyril Tasse, tasse(at)strw.leidenuniv.nl
(End) Patricia Vannier [CDS] 12-Jun-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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