2005A&A...439..887P -
Astronomy and Astrophysics, volume 439, 887-900 (2005/9-1)
The VIMOS VLT deep survey. Computing the two point correlation statistics and associated uncertainties.
POLLO A., MENEUX B., GUZZO L., LE FEVRE O., BLAIZOT J., CAPPI A., IOVINO A., MARINONI C., McCRACKEN H.J., BOTTINI D., GARILLI B., LE BRUN V., MACCAGNI D., PICAT J.P., SCARAMELLA R., SCODEGGIO M., TRESSE L., VETTOLANI G., ZANICHELLI A., ADAMI C., ARNABOLDI M., ARNOUTS S., BARDELLI S., BOLZONELLA M., CHARLOT S., CILIEGI P., CONTINI T., FOUCAUD S., FRANZETTI P., GAVIGNAUD I., ILBERT O., MARANO B., MATHEZ G., MAZURE A., MERIGHI R., PALTANI S., PELLO R., POZZETTI L., RADOVICH M., ZAMORANI G., ZUCCA E., BONDI M., BONGIORNO A., BUSARELLO G., GREGORINI L., LAMAREILLE F., MELLIER Y., MERLUZZI P., RIPEPI V. and RIZZO D.
Abstract (from CDS):
We present a detailed description of the methods used to compute the three-dimensional two-point galaxy correlation function in the VIMOS-VLT deep survey (VVDS). We investigate how instrumental selection effects and observational biases affect the measurements and identify the methods to correct for them. We quantify the accuracy of our corrections using an ensemble of 50 mock galaxy surveys generated with the GalICS semi-analytic model of galaxy formation which incorporate the selection biases and tiling strategy of the real data. We demonstrate that we are able to recover the real-space two-point correlation function ξ(s) and the projected correlation function wp(rp) to an accuracy better than 10% on scales larger than 1h–1Mpc with the sampling strategy used for the first epoch VVDS data. The large number of simulated surveys allows us to provide a reliable estimate of the cosmic variance on the measurements of the correlation length r0 at z∼1, of about 15-20% for the first epoch VVDS observation while any residual systematic effect in the measurements of r0 is always below 5%. The error estimation and measurement techniques outlined in this paper are being used in several parallel studies which investigate in detail the clustering properties of galaxies in the VVDS.
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Journal keyword(s):
cosmology: large scale structure of Universe - methods: statistical - galaxies: evolution - surveys
NAME Chandra Deep Field-South
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reg
()
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
ra dec : right ascension and declination (unit and frame defined according to your Output Options)
Grey values are increasing the original precision due to the computation of frame transformations
(wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
[error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
position angle (in degrees North celestial pole to East)
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
ra dec : right ascension and declination (unit and frame defined according to your Output Options)
Grey values are increasing the original precision due to the computation of frame transformations
(wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
[error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
position angle (in degrees North celestial pole to East)
quality : flag of quality
E ≥ 10"
D : 1-10" (and some old data)
C : 0.1-1"
B : 0.01-0.1" + 2MASS, Tyc
A : VLBI, Hipparcos
bibcode : bibcode of the coordinates reference
FK4
coord.
(ep=B1950 eq=1950) :
03 30 22.4 -27 58 35
[
]
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
ra dec : right ascension and declination (unit and frame defined according to your Output Options)
Grey values are increasing the original precision due to the computation of frame transformations
(wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
[error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
position angle (in degrees North celestial pole to East)
quality : flag of quality
E ≥ 10"
D : 1-10" (and some old data)
C : 0.1-1"
B : 0.01-0.1" + 2MASS, Tyc
A : VLBI, Hipparcos
bibcode : bibcode of the coordinates reference
Gal
coord.
(ep=J2000) :
223.5732 -54.4374
[
]
Syntax of angular size is : "maj-axis min-axis angle (wtype) quality bibcode"
maj-axis : major axis size (arc minutes)
min-axis : minor axis size (arc minutes)
angle : orientation angle (in degrees)
(wtype) : wavelength class for the origin of the angular size (Rad, mm, IR, Opt, UV, Xray, Gam)
quality : flag of quality of the angular size values ( A=best quality -> E=worst quality, {� } =unknown quality)
bibcode : bibcode of the angular size reference
Angular size (arcmin):
15.84 15.84 ~ (~) D
~
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