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J/ApJ/647/13        BIMA CMB anisotropy survey               (Dawson+, 2006)

Final results from the BIMA CMB anisotropy survey and search for a signature of the Sunyaev-Zel'dovich effect. Dawson K.S., Holzapfel W.L., Carlstrom J.E., Joy M., Laroque S.J. <Astrophys. J., 647, 13-24 (2006)> =2006ApJ...647...13D
ADC_Keywords: Surveys ; Clusters, galaxy Keywords: cosmic microwave background - cosmology: observations - galaxies: clusters: general Abstract: We report the final results of our study of the cosmic microwave background (CMB) with the BIMA array. Over 1000hr of observation were dedicated to this project exploring CMB anisotropy, on scales between 1' and 2' in eighteen 6.6' FWHM fields. In the analysis of the CMB power spectrum, the visibility data are divided into two bins, corresponding to different angular scales. Description: The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 42 18 Field positions and observation times table2.dat 55 32 Point Sources and Fluxes Identified from VLA Observations (1998-2001) table3.dat 55 28 Point Sources and Fluxes Identified from VLA Observations (2002)
See also: J/ApJS/100/281 : Cosmic background anisotropies (Sugiyama 1995) J/ApJS/148/97 : The WMAP First Year Source Catalog (WMAP1) (Bennett+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Field Field designation 7- 8 I2 h RAh Right ascension (J2000) 10- 11 I2 min RAm Right ascension (J2000) 13- 16 F4.1 s RAs Right ascension (J2000) 18 A1 --- DE- Declination sign (J2000) 19- 20 I2 deg DEd Declination (J2000) 22- 23 I2 arcmin DEm Declination (J2000) 25- 26 I2 arcsec DEs Declination (J2000) 28- 31 I4 yr Date1 Year of observation 32 A1 --- --- [,] 34- 37 I4 yr Date2 ? Year of observation 39- 42 F4.1 h Time Time of observation
Byte-by-byte Description of file: table[23].dat
Bytes Format Units Label Explanations
1- 5 A5 --- Field Field designation 7- 12 F6.1 arcsec oRA Offest in right ascension from Field position (1) 14- 19 F6.1 arcsec oDE Offest in declination from Field position (1) 21- 24 I4 uJy F4.8GHz Flux at 4.8GHz 26- 30 F5.1 uJy e_F4.8GHz rms uncertainty on F4.8GHz 32- 38 F7.1 uJy F8GHz ? Flux at 8GHz (2) 40- 44 F5.1 uJy e_F8GHz ? rms uncertainty on F8GHz (2) 46- 51 F6.1 uJy F30GHz ? Flux at 30GHz (3) 53- 55 I3 uJy e_F30GHz ? rms uncertainty on 30GHz (3)
Note (1): Sources identified as [DHC2006] Field oRAoDE in Simbad, i.e. [DHC2006] BDF4 -96.8+255.7 for "BDF4 -96.8 +255.7"Note (2): Blanks for fields not observed at 8GHz. Note (2): Blanks for fields not observed at 8GHz. Note (3): For the 30GHz BIMA observations, blanks mark entries for those point sources that lie outside the primary beam and are not detected at >3σ significance.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 03-Jun-2008
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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