Remi Cabanac - Academia.edu (original) (raw)
Papers by Remi Cabanac
Université de Toulouse, Dec 3, 2020
The NASA Orbital Debris Observatory (NODO) astronomical survey uses a transit 3-m liquid mirror t... more The NASA Orbital Debris Observatory (NODO) astronomical survey uses a transit 3-m liquid mirror telescope to observe a strip of sky in 20 narrow-band filters. In this article, we analyze a subset of data from the 1996 observing season. The catalog consists of 18,000 objects with 10<V<19 observed in 10 narrow-band filters ranging from 500 nm to 950 nm. We first demonstrate the reliability of the data by fitting the Bahcall-Soneira model of the Galaxy to the NODO magnitude counts and color counts at various galactic latitudes. We then perform a hierarchical clustering analysis on the sample to extract 206 objects, out of a total of 18,000, showing peculiar spectral energy distributions. It is a measure of the reliability of the instrument that we extract so few peculiar objects. Although the data and results, per se, may not seem otherwise particularly remarkable, this work constitutes a milestone in optical astronomy since this is the first article that demonstrates astromomica...
We present here additional results of a spectropolarimetric survey of a small sample of stars ran... more We present here additional results of a spectropolarimetric survey of a small sample of stars ranging from spectral type M0 to M8 aimed at investigating observationally how dynamo processes operate in stars on both sides of the full convection threshold (spectral type M4). The present paper focuses on early M stars (M0--M3), i.e. above the full convection threshold. Applying tomographic imaging techniques to time series of rotationally modulated circularly polarised profiles collected with the NARVAL spectropolarimeter, we determine the rotation period and reconstruct the large-scale magnetic topologies of 6 early M dwarfs. We find that early-M stars preferentially host large-scale fields with dominantly toroidal and non-axisymmetric poloidal configurations, along with significant differential rotation (and long-term variability); only the lowest-mass star of our subsample is found to host an almost fully poloidal, mainly axisymmetric large-scale field ressembling those found in mid...
We present in this paper the first results of a spectropolarimetric analysis of a small sample (~... more We present in this paper the first results of a spectropolarimetric analysis of a small sample (~ 20) of active stars ranging from spectral type M0 to M8, which are either fully-convective or possess a very small radiative core. This study aims at providing new constraints on dynamo processes in fully-convective stars. The present paper focuses on 5 stars of spectral type ~M4, i.e. with masses close to the full convection threshold (~ 0.35 Msun), and with short rotational periods. Tomographic imaging techniques allow us to reconstruct the surface magnetic topologies from the rotationally modulated time-series of circularly polarised profiles. We fnd that all stars host mainly axisymmetric large-scale poloidal fields. Three stars were observed at two different epochs separated by ~1 yr; we find the magnetic topologies to be globally stable on this timescale. We also provide an accurate estimation of the rotational period of all stars, thus allowing us to start studying how rotation i...
Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. ... more Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. the group or cluster within which the lens is embedded. In this article, we propose to turn this limitation to our advantage and to use precise strong lensing modelling to probe external mass distributions surrounding the lens. We consider SL2S J08544-0121, a galaxy group at z=0.35 that contains a strong lensing system. A simple elliptical isothermal potential cannot reproduce satisfactorily the strong lensing constraints. We include an external mass perturbation corresponding to the group within which the lens is embedded. The lensing properties of this perturbation are parametrised by its total mass M and a smoothing scale s that quantifies the characteristic scale over which M is distributed. For a range of these parameters, we are able to reproduce accurately the observations. This suggests that light is a good tracer of mass. Interestingly, this also shows that a localised strong le...
Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. ... more Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. the group or cluster within which the lens is embedded. In this article, we propose to turn this limitation to our advantage and to use precise strong lensing modelling to probe external mass distributions surrounding the lens. We consider SL2S J08544-0121, a galaxy group at z=0.35 that contains a strong lensing system. A simple elliptical isothermal potential cannot reproduce satisfactorily the strong lensing constraints. We include an external mass perturbation corresponding to the group within which the lens is embedded. The lensing properties of this perturbation are parametrised by its total mass M and a smoothing scale s that quantifies the characteristic scale over which M is distributed. For a range of these parameters, we are able to reproduce accurately the observations. This suggests that light is a good tracer of mass. Interestingly, this also shows that a localised strong le...
AIMS: We present data from the CFHTLS Strong Lensing Legacy Survey (SL2S). Due to the unsurpassed... more AIMS: We present data from the CFHTLS Strong Lensing Legacy Survey (SL2S). Due to the unsurpassed combined depth, area and image quality of the Canada-France-Hawaii Legacy Survey it is becoming possible to uncover a large, statistically well-defined sample of strong gravitational lenses which spans the dark halo mass spectrum predicted by the concordance model from galaxy to cluster haloes. METHODS: We describe the development of several automated procedures to find strong lenses of various mass regimes in CFHTLS images. RESULTS: The preliminary sample of about 40 strong lensing candidates discovered in the CFHTLS T0002 release, covering an effective field of view of 28 deg^2 is presented. These strong lensing systems were discovered using an automated search and consist mainly of gravitational arc systems with splitting angles between 2 and 15 arcsec. This sample shows for the first time that it is possible to uncover a large population of strong lenses from galaxy groups with typi...
We present the Strong Lensing Legacy Survey - ARCS (SARCS) sample compiled from the final T0006 d... more We present the Strong Lensing Legacy Survey - ARCS (SARCS) sample compiled from the final T0006 data release of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) covering a total non-overlapping area of 159 sq.deg. We adopt a semi-automatic method to find gravitational arcs in the survey that makes use of an arc-finding algorithm. The candidate list is pruned by visual inspection and ranking to form the SARCS sample. This list also includes some serendipitously discovered lens candidates. The SARCS sample consists of 127 lens candidates which span arc radii~2"-18" within the unmasked area of ~ 150 sq. deg. Within the sample, 54 systems are promising lenses amongst which, we find 12 giant arcs and 2 radial arc candidates. From our sample, we detect a systematic alignment of giant arcs with the ellipticity of the baryonic component of the lens in concordance with previous studies. The lens redshift distribution corresponding to both the giant arcs and all arcs, estim...
Abstract: We present preliminary results of observations made, during the spring of 1996, with th... more Abstract: We present preliminary results of observations made, during the spring of 1996, with the 3-m liquid mirror telescope of the NASA Orbital Debris Observatory. A 20-arcmin-wide strip of sky was observed at a latitude of 32 ° 56 ' N using 10 narrow-band filters. Although the detector and the optical corrector were not optimized for astronomical observations, valuable information could be extracted down to magnitude 19 in R. From these observations we are generating a catalog of positions and AB magnitudes of objects in the strip. In this present work, we show images, maps and counts representative of the dataset. NASA Orbital Debris Observatory The NASA Orbital Debris Observatory (NODO) built by NASA in Cloudcroft (New-Mexico) is equipped with a 3-m LMT. (Table I)
Spectropolarimetric observations of the selected M dwarfs were collected with NARVAL and the 2m T... more Spectropolarimetric observations of the selected M dwarfs were collected with NARVAL and the 2m Telescope Bernard Lyot (TBL), between 2007 January and 2008 February (in three different runs). (2 data files).
arXiv: Astrophysics, 2000
The UH8K wide field camera of the CFHT was used to image 0.68 deg^2 of sky. From these images, ~2... more The UH8K wide field camera of the CFHT was used to image 0.68 deg^2 of sky. From these images, ~20,000 galaxies were detected to completeness magnitudes V 0. We infer a best-fit spatial correlation length of r_00= 5.85+/-0.5 h^-1 Mpc at z=0. The peak redshift of the survey (I<22.5) is estimated to be z_peak~0.58, using the blue-evolving luminosity function from the CFRS and the flat Lambda cosmology, and r_0(z_peak)=3.5+/-0.5 h^-1 Mpc. We also detect a significant difference in clustering amplitude for the red and blue galaxies, quantitatively measured by correlation lengths of r_00=5.3+/-0.5 h^-1 Mpc and r_00=1.9+/-0.9 h^-1 Mpc respectively, at z=0.
arXiv: Astrophysics, 1997
We present preliminary results of observations made, during the spring of 1996, with the 3-m liqu... more We present preliminary results of observations made, during the spring of 1996, with the 3-m liquid mirror telescope of the NASA Orbital Debris Observatory. A 20-arcmin-wide strip of sky was observed at latitude of 32deg56 N using 10 narrow-band filters. Although the detector and the optical corrector were not optimized for astronomical observations, valuable information could be extracted down to magnitude 19 in R. From these observations we are generating a catalog of positions and AB magnitudes of objects in the strip. In this present work, we show images, maps and counts representative of the dataset.
We present high-resolution observations of Henize 2-10 in KS (2.2 μm), L ′ (3.8 μm), M ′ (4.8 μm)... more We present high-resolution observations of Henize 2-10 in KS (2.2 μm), L ′ (3.8 μm), M ′ (4.8 μm) bands. These allow for the first time to track accurately the structures at the heart of the galaxy from the optical to the radio. All radio knots previously observed can now be associated with L and KS emitting regions. This implies a revision of their physical nature. Instead of highly extinguished ultra-dense HII regions, we propose that two of the 5 radio knots are either supernova remnants or normal HII regions, while the remaining three are bona fide ultra-dense HII regions, although less obscured than was previously thought. Subject headings: galaxies: individual (Henize 2-10)
The UH8K wide field camera of the CFHT was used to image 0.68 deg of sky. From these images, ∼20,... more The UH8K wide field camera of the CFHT was used to image 0.68 deg of sky. From these images, ∼20,000 galaxies were detected to completeness magnitudes V < 23.5 and I < 22.5. The angular correlation function of these galaxies is well represented by the parameterization ω(θ) = AW θ . The slope δ ≃ −0.8 shows no significant variation over the range of magnitude. The amplitude AW decreases with increasing magnitude in a way that is most compatible with a ΛCDM model (Ω0 = 0.2, Λ = 0.8) with a hierarchical clustering evolution parameter ǫ > 0. We infer a best-fit spatial correlation length of r00 ≃ 5.85 ± 0.5 h Mpc at z = 0. The peak redshift of the survey (I ≤ 22.5) is estimated to be zpeak ∼ 0.58, using the blue-evolving luminosity function from the CFRS and the flat Λ cosmology, and r0(zpeak) ≃ 3.5 ± 0.5 h Mpc. We also detect a significant difference in clustering amplitude for the red and blue galaxies, quantitatively measured by correlation lengths of r00 = 5.3 ± 0.5 h Mpc a...
The Astrophysical Journal
This article is a theoretical consideration on the role of sensory pleasure and mental joy as opt... more This article is a theoretical consideration on the role of sensory pleasure and mental joy as optimizers of behavior. It ends with an axiomatic proposal. When they compare the human body to its environment, Philosophers recognise the cosmos as the Large Infinite, and the atomic particles as the Small Infinite. The human brain reaches such a degree of complexity that it may be considered as a third infinite in the universe, a Complex Infinite. It follows that any force capable of moving such an infinite deserves a place among the forces of the universe. Physicists have recognized four forces, the gravitational, the electromagnetic, the weak, and the strong nuclear force. Forces are defined in four dimentions (reversible or not in time) and it is postulated that these forces are valid and applicable everywhere. Pleasure and displeasure, the affective axis of consciousness, can move the infinitely complex into action and no human brain can avoid the trend to maximize its pleasure. Therefore, we suggest, axiomatically, that the affective capability of consciousness operates in a way similar to the four forces of the Physics, i.e. influences the behavior of conscious agents in a way similar to the way the four forces influence masses and particles. However, since a mental phenomenon is dimensioneless we propose to call the affective capability of consciousness the fifth influence rather than the fifth force.
Astronomy and Astrophysics
The UH8K wide field camera of the CFHT was used to image 0.68 deg2 of sky. From these images, ~ 2... more The UH8K wide field camera of the CFHT was used to image 0.68 deg2 of sky. From these images, ~ 20,000 galaxies were detected to completeness magnitudes V<23.5 and I<22.5. The angular correlation function of these galaxies is well represented by the parameterization omega (theta ) = A_W theta -delta . The slope delta =~ -0.8 shows no significant variation over the range of magnitude. The amplitude A_W decreases with increasing magnitude in a way that is most compatible with a Lambda CDM model (Omega_0 = 0.2, Lambda =0.8) with a hierarchical clustering evolution parameter epsilon >0. We infer a best-fit spatial correlation length of r00 =~ 5.85+/-0.5 h-1 Mpc at z=0. The peak redshift of the survey (I<=22.5) is estimated to be zpeak ~ 0.58, using the blue-evolving luminosity function from the CFRS and the flat Lambda cosmology, and r_0(zpeak) =~ 3.5+/-0.5 h-1 Mpc. We also detect a significant difference in clustering amplitude for the red and blue galaxies, quantitatively ...
Université de Toulouse, Dec 3, 2020
The NASA Orbital Debris Observatory (NODO) astronomical survey uses a transit 3-m liquid mirror t... more The NASA Orbital Debris Observatory (NODO) astronomical survey uses a transit 3-m liquid mirror telescope to observe a strip of sky in 20 narrow-band filters. In this article, we analyze a subset of data from the 1996 observing season. The catalog consists of 18,000 objects with 10<V<19 observed in 10 narrow-band filters ranging from 500 nm to 950 nm. We first demonstrate the reliability of the data by fitting the Bahcall-Soneira model of the Galaxy to the NODO magnitude counts and color counts at various galactic latitudes. We then perform a hierarchical clustering analysis on the sample to extract 206 objects, out of a total of 18,000, showing peculiar spectral energy distributions. It is a measure of the reliability of the instrument that we extract so few peculiar objects. Although the data and results, per se, may not seem otherwise particularly remarkable, this work constitutes a milestone in optical astronomy since this is the first article that demonstrates astromomica...
We present here additional results of a spectropolarimetric survey of a small sample of stars ran... more We present here additional results of a spectropolarimetric survey of a small sample of stars ranging from spectral type M0 to M8 aimed at investigating observationally how dynamo processes operate in stars on both sides of the full convection threshold (spectral type M4). The present paper focuses on early M stars (M0--M3), i.e. above the full convection threshold. Applying tomographic imaging techniques to time series of rotationally modulated circularly polarised profiles collected with the NARVAL spectropolarimeter, we determine the rotation period and reconstruct the large-scale magnetic topologies of 6 early M dwarfs. We find that early-M stars preferentially host large-scale fields with dominantly toroidal and non-axisymmetric poloidal configurations, along with significant differential rotation (and long-term variability); only the lowest-mass star of our subsample is found to host an almost fully poloidal, mainly axisymmetric large-scale field ressembling those found in mid...
We present in this paper the first results of a spectropolarimetric analysis of a small sample (~... more We present in this paper the first results of a spectropolarimetric analysis of a small sample (~ 20) of active stars ranging from spectral type M0 to M8, which are either fully-convective or possess a very small radiative core. This study aims at providing new constraints on dynamo processes in fully-convective stars. The present paper focuses on 5 stars of spectral type ~M4, i.e. with masses close to the full convection threshold (~ 0.35 Msun), and with short rotational periods. Tomographic imaging techniques allow us to reconstruct the surface magnetic topologies from the rotationally modulated time-series of circularly polarised profiles. We fnd that all stars host mainly axisymmetric large-scale poloidal fields. Three stars were observed at two different epochs separated by ~1 yr; we find the magnetic topologies to be globally stable on this timescale. We also provide an accurate estimation of the rotational period of all stars, thus allowing us to start studying how rotation i...
Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. ... more Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. the group or cluster within which the lens is embedded. In this article, we propose to turn this limitation to our advantage and to use precise strong lensing modelling to probe external mass distributions surrounding the lens. We consider SL2S J08544-0121, a galaxy group at z=0.35 that contains a strong lensing system. A simple elliptical isothermal potential cannot reproduce satisfactorily the strong lensing constraints. We include an external mass perturbation corresponding to the group within which the lens is embedded. The lensing properties of this perturbation are parametrised by its total mass M and a smoothing scale s that quantifies the characteristic scale over which M is distributed. For a range of these parameters, we are able to reproduce accurately the observations. This suggests that light is a good tracer of mass. Interestingly, this also shows that a localised strong le...
Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. ... more Precise modelling of strong lensing systems can be affected by external mass distributions, e.g. the group or cluster within which the lens is embedded. In this article, we propose to turn this limitation to our advantage and to use precise strong lensing modelling to probe external mass distributions surrounding the lens. We consider SL2S J08544-0121, a galaxy group at z=0.35 that contains a strong lensing system. A simple elliptical isothermal potential cannot reproduce satisfactorily the strong lensing constraints. We include an external mass perturbation corresponding to the group within which the lens is embedded. The lensing properties of this perturbation are parametrised by its total mass M and a smoothing scale s that quantifies the characteristic scale over which M is distributed. For a range of these parameters, we are able to reproduce accurately the observations. This suggests that light is a good tracer of mass. Interestingly, this also shows that a localised strong le...
AIMS: We present data from the CFHTLS Strong Lensing Legacy Survey (SL2S). Due to the unsurpassed... more AIMS: We present data from the CFHTLS Strong Lensing Legacy Survey (SL2S). Due to the unsurpassed combined depth, area and image quality of the Canada-France-Hawaii Legacy Survey it is becoming possible to uncover a large, statistically well-defined sample of strong gravitational lenses which spans the dark halo mass spectrum predicted by the concordance model from galaxy to cluster haloes. METHODS: We describe the development of several automated procedures to find strong lenses of various mass regimes in CFHTLS images. RESULTS: The preliminary sample of about 40 strong lensing candidates discovered in the CFHTLS T0002 release, covering an effective field of view of 28 deg^2 is presented. These strong lensing systems were discovered using an automated search and consist mainly of gravitational arc systems with splitting angles between 2 and 15 arcsec. This sample shows for the first time that it is possible to uncover a large population of strong lenses from galaxy groups with typi...
We present the Strong Lensing Legacy Survey - ARCS (SARCS) sample compiled from the final T0006 d... more We present the Strong Lensing Legacy Survey - ARCS (SARCS) sample compiled from the final T0006 data release of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) covering a total non-overlapping area of 159 sq.deg. We adopt a semi-automatic method to find gravitational arcs in the survey that makes use of an arc-finding algorithm. The candidate list is pruned by visual inspection and ranking to form the SARCS sample. This list also includes some serendipitously discovered lens candidates. The SARCS sample consists of 127 lens candidates which span arc radii~2"-18" within the unmasked area of ~ 150 sq. deg. Within the sample, 54 systems are promising lenses amongst which, we find 12 giant arcs and 2 radial arc candidates. From our sample, we detect a systematic alignment of giant arcs with the ellipticity of the baryonic component of the lens in concordance with previous studies. The lens redshift distribution corresponding to both the giant arcs and all arcs, estim...
Abstract: We present preliminary results of observations made, during the spring of 1996, with th... more Abstract: We present preliminary results of observations made, during the spring of 1996, with the 3-m liquid mirror telescope of the NASA Orbital Debris Observatory. A 20-arcmin-wide strip of sky was observed at a latitude of 32 ° 56 ' N using 10 narrow-band filters. Although the detector and the optical corrector were not optimized for astronomical observations, valuable information could be extracted down to magnitude 19 in R. From these observations we are generating a catalog of positions and AB magnitudes of objects in the strip. In this present work, we show images, maps and counts representative of the dataset. NASA Orbital Debris Observatory The NASA Orbital Debris Observatory (NODO) built by NASA in Cloudcroft (New-Mexico) is equipped with a 3-m LMT. (Table I)
Spectropolarimetric observations of the selected M dwarfs were collected with NARVAL and the 2m T... more Spectropolarimetric observations of the selected M dwarfs were collected with NARVAL and the 2m Telescope Bernard Lyot (TBL), between 2007 January and 2008 February (in three different runs). (2 data files).
arXiv: Astrophysics, 2000
The UH8K wide field camera of the CFHT was used to image 0.68 deg^2 of sky. From these images, ~2... more The UH8K wide field camera of the CFHT was used to image 0.68 deg^2 of sky. From these images, ~20,000 galaxies were detected to completeness magnitudes V 0. We infer a best-fit spatial correlation length of r_00= 5.85+/-0.5 h^-1 Mpc at z=0. The peak redshift of the survey (I<22.5) is estimated to be z_peak~0.58, using the blue-evolving luminosity function from the CFRS and the flat Lambda cosmology, and r_0(z_peak)=3.5+/-0.5 h^-1 Mpc. We also detect a significant difference in clustering amplitude for the red and blue galaxies, quantitatively measured by correlation lengths of r_00=5.3+/-0.5 h^-1 Mpc and r_00=1.9+/-0.9 h^-1 Mpc respectively, at z=0.
arXiv: Astrophysics, 1997
We present preliminary results of observations made, during the spring of 1996, with the 3-m liqu... more We present preliminary results of observations made, during the spring of 1996, with the 3-m liquid mirror telescope of the NASA Orbital Debris Observatory. A 20-arcmin-wide strip of sky was observed at latitude of 32deg56 N using 10 narrow-band filters. Although the detector and the optical corrector were not optimized for astronomical observations, valuable information could be extracted down to magnitude 19 in R. From these observations we are generating a catalog of positions and AB magnitudes of objects in the strip. In this present work, we show images, maps and counts representative of the dataset.
We present high-resolution observations of Henize 2-10 in KS (2.2 μm), L ′ (3.8 μm), M ′ (4.8 μm)... more We present high-resolution observations of Henize 2-10 in KS (2.2 μm), L ′ (3.8 μm), M ′ (4.8 μm) bands. These allow for the first time to track accurately the structures at the heart of the galaxy from the optical to the radio. All radio knots previously observed can now be associated with L and KS emitting regions. This implies a revision of their physical nature. Instead of highly extinguished ultra-dense HII regions, we propose that two of the 5 radio knots are either supernova remnants or normal HII regions, while the remaining three are bona fide ultra-dense HII regions, although less obscured than was previously thought. Subject headings: galaxies: individual (Henize 2-10)
The UH8K wide field camera of the CFHT was used to image 0.68 deg of sky. From these images, ∼20,... more The UH8K wide field camera of the CFHT was used to image 0.68 deg of sky. From these images, ∼20,000 galaxies were detected to completeness magnitudes V < 23.5 and I < 22.5. The angular correlation function of these galaxies is well represented by the parameterization ω(θ) = AW θ . The slope δ ≃ −0.8 shows no significant variation over the range of magnitude. The amplitude AW decreases with increasing magnitude in a way that is most compatible with a ΛCDM model (Ω0 = 0.2, Λ = 0.8) with a hierarchical clustering evolution parameter ǫ > 0. We infer a best-fit spatial correlation length of r00 ≃ 5.85 ± 0.5 h Mpc at z = 0. The peak redshift of the survey (I ≤ 22.5) is estimated to be zpeak ∼ 0.58, using the blue-evolving luminosity function from the CFRS and the flat Λ cosmology, and r0(zpeak) ≃ 3.5 ± 0.5 h Mpc. We also detect a significant difference in clustering amplitude for the red and blue galaxies, quantitatively measured by correlation lengths of r00 = 5.3 ± 0.5 h Mpc a...
The Astrophysical Journal
This article is a theoretical consideration on the role of sensory pleasure and mental joy as opt... more This article is a theoretical consideration on the role of sensory pleasure and mental joy as optimizers of behavior. It ends with an axiomatic proposal. When they compare the human body to its environment, Philosophers recognise the cosmos as the Large Infinite, and the atomic particles as the Small Infinite. The human brain reaches such a degree of complexity that it may be considered as a third infinite in the universe, a Complex Infinite. It follows that any force capable of moving such an infinite deserves a place among the forces of the universe. Physicists have recognized four forces, the gravitational, the electromagnetic, the weak, and the strong nuclear force. Forces are defined in four dimentions (reversible or not in time) and it is postulated that these forces are valid and applicable everywhere. Pleasure and displeasure, the affective axis of consciousness, can move the infinitely complex into action and no human brain can avoid the trend to maximize its pleasure. Therefore, we suggest, axiomatically, that the affective capability of consciousness operates in a way similar to the four forces of the Physics, i.e. influences the behavior of conscious agents in a way similar to the way the four forces influence masses and particles. However, since a mental phenomenon is dimensioneless we propose to call the affective capability of consciousness the fifth influence rather than the fifth force.
Astronomy and Astrophysics
The UH8K wide field camera of the CFHT was used to image 0.68 deg2 of sky. From these images, ~ 2... more The UH8K wide field camera of the CFHT was used to image 0.68 deg2 of sky. From these images, ~ 20,000 galaxies were detected to completeness magnitudes V<23.5 and I<22.5. The angular correlation function of these galaxies is well represented by the parameterization omega (theta ) = A_W theta -delta . The slope delta =~ -0.8 shows no significant variation over the range of magnitude. The amplitude A_W decreases with increasing magnitude in a way that is most compatible with a Lambda CDM model (Omega_0 = 0.2, Lambda =0.8) with a hierarchical clustering evolution parameter epsilon >0. We infer a best-fit spatial correlation length of r00 =~ 5.85+/-0.5 h-1 Mpc at z=0. The peak redshift of the survey (I<=22.5) is estimated to be zpeak ~ 0.58, using the blue-evolving luminosity function from the CFRS and the flat Lambda cosmology, and r_0(zpeak) =~ 3.5+/-0.5 h-1 Mpc. We also detect a significant difference in clustering amplitude for the red and blue galaxies, quantitatively ...