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Susanna Hagelin - One of the best experts on this subject based on the ideXlab platform.
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wind speed Vertical Distribution at mt graham
Monthly Notices of the Royal Astronomical Society, 2010Co-Authors: Susanna Hagelin, E Masciadri, Franck LascauxAbstract:The characterization of the Vertical Distribution of wind speed, V(h), is fundamental for an astronomical site for many different reasons: (i) the wind speed shear contributes to trigger optical turbulence in the whole troposphere; (ii) a few of the astroclimatic parameters, such as the wavefront coherence time (τ 0 ), depend directly on V (h); (iii) the equivalent velocity V 0 , controlling the frequency at which the adaptive optics systems have to run in order to work properly, depends on the Vertical Distribution of the wind speed and optical turbulence. Also, too strong a wind speed near the ground can introduce vibrations in the telescope structures. The wind speed at a precise pressure (200 hPa) has frequently been used to retrieve indications concerning τ 0 and the frequency limits imposed on all instrumentation based on adaptive optics systems. However, more recently, it has been proved that V 200 (the wind speed at 200 hPa) alone is not sufficient to provide exhaustive elements concerning this topic, and thus the Vertical Distribution of the wind speed is necessary. In this paper, we report on a complete characterization of the Vertical Distribution of wind speed strength, which has been carried out above Mt Graham (Arizona, USA), the site of the Large Binocular Telescope. We provide a climatological study extended over 10 yr using the operational analyses from the European Centre for Medium-Range Weather Forecasts (ECMWF). We prove that this is representative of the Vertical Distribution of the wind speed at Mt Graham, with the exception of the boundary layer. We also prove that a mesoscale model can provide reliable nightly estimates of V (h) above this astronomical site from the ground up to the top of the atmosphere (~20 km).
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wind speed Vertical Distribution at mt graham
arXiv: Instrumentation and Methods for Astrophysics, 2010Co-Authors: Susanna Hagelin, E Masciadri, Franck LascauxAbstract:The characterization of the wind speed Vertical Distribution V(h) is fundamental for an astronomical site for many different reasons: (1) the wind speed shear contributes to trigger optical turbulence in the whole troposphere, (2) a few of the astroclimatic parameters such as the wavefront coherence time (tau_0) depends directly on V(h), (3) the equivalent velocity V_0, controlling the frequency at which the adaptive optics systems have to run to work properly, depends on the Vertical Distribution of the wind speed and optical turbulence. Also, a too strong wind speed near the ground can introduce vibrations in the telescope structures. The wind speed at a precise pressure (200 hPa) has frequently been used to retrieve indications concerning the tau_0 and the frequency limits imposed to all instrumentation based on adaptive optics systems, but more recently it has been proved that V_200 (wind speed at 200 hPa) alone is not sufficient to provide exhaustive elements concerning this topic and that the Vertical Distribution of the wind speed is necessary. In this paper a complete characterization of the Vertical Distribution of wind speed strength is done above Mt.Graham (Arizona, US), site of the Large Binocular Telescope. We provide a climatological study extended over 10 years using the operational analyses from the European Centre for Medium-Range Weather Forecasts (ECMWF), we prove that this is representative of the wind speed Vertical Distribution at Mt. Graham with exception of the boundary layer and we prove that a mesoscale model can provide reliable nightly estimates of V(h) above this astronomical site from the ground up to the top of the atmosphere (~ 20 km).
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optical turbulence Vertical Distribution with standard and high resolution at mt graham
Monthly Notices of the Royal Astronomical Society, 2010Co-Authors: E Masciadri, Susanna Hagelin, J Stoesz, Franck LascauxAbstract:A characterization of the optical turbulence Vertical Distribution (C 2 N profiles) and all the main integrated astroclimatic parameters derived from the C 2 N and the wind speed profiles above the site of the Large Binocular Telescope (LBT) (Mt Graham, Arizona, USA) is presented. The statistics include measurements related to 43 nights done with a Generalized SCIDAR (GS) used in standard configuration with a Vertical resolution ΔH ~ 1 km on the whole 20 km and with the new technique (High Vertical Resolution GS) in the first kilometre. The latter achieves a resolution ΔH ~ 20-30 m in this region of the atmosphere. Measurements done in different periods of the year permit us to provide a seasonal variation analysis of the C 2 N . A discretized Distribution of C 2 N , useful for the Ground Layer Adaptive Optics (GLAO) simulations, is provided and a specific analysis for the LBT Laser Guide Star system ARGOS (running in GLAO configuration) case is done including the calculation of the 'grey zones' for J, H and K bands. Mt Graham is confirmed to be an excellent site with median values of the seeing without dome contribution e = 0.72 arcsec, the isoplanatic angle θ 0 = 2.5 arcsec and the wavefront coherence time τ 0 = 4.8 ms. We find that the OT Vertical Distribution decreases in a much sharper way than what has been believed so far in the proximity of the ground above astronomical sites. We find that 50 per cent of the whole turbulence develops in the first 80 ± 15 m from the ground. We finally prove that the error in the normalization of the scintillation that has been recently demonstrated in the principle of the GS technique affects these measurements by an absolutely negligible quantity (0.04 arcsec).
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optical turbulence Vertical Distribution with standard and high resolution at mt graham
arXiv: Instrumentation and Methods for Astrophysics, 2010Co-Authors: E Masciadri, Susanna Hagelin, J Stoesz, Franck LascauxAbstract:A characterization of the optical turbulence Vertical Distribution (Cn2 profiles) and all the main integrated astroclimatic parameters derived from the Cn2 and the wind speed profiles above the site of the Large Binocular Telescope (Mt. Graham, Arizona, US) is presented. The statistic includes measurements related to 43 nights done with a Generalized Scidar (GS) used in standard configuration with a Vertical resolution Delta(H)~1 km on the whole 20 km and with the new technique (HVR-GS) in the first kilometer. The latter achieves a resolution Delta(H)~20-30 m in this region of the atmosphere. Measurements done in different periods of the year permit us to provide a seasonal variation analysis of the Cn2. A discretized Distribution of Cn2 useful for the Ground Layer Adaptive Optics (GLAO) simulations is provided and a specific analysis for the LBT Laser Guide Star system ARGOS (running in GLAO configuration) case is done including the calculation of the 'gray zones' for J, H and K bands. Mt. Graham confirms to be an excellent site with median values of the seeing without dome contribution epsilon = 0.72", the isoplanatic angle theta0 = 2.5" and the wavefront coherence time tau0= 4.8 msec. We find that the optical turbulence Vertical Distribution decreases in a much sharper way than what has been believed so far in proximity of the ground above astronomical sites. We find that 50% of the whole turbulence develops in the first 80+/-15 m from the ground. We finally prove that the error in the normalization of the scintillation that has been recently put in evidence in the principle of the GS technique, affects these measurements with an absolutely negligible quantity (0.04").
Franck Lascaux - One of the best experts on this subject based on the ideXlab platform.
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wind speed Vertical Distribution at mt graham
Monthly Notices of the Royal Astronomical Society, 2010Co-Authors: Susanna Hagelin, E Masciadri, Franck LascauxAbstract:The characterization of the Vertical Distribution of wind speed, V(h), is fundamental for an astronomical site for many different reasons: (i) the wind speed shear contributes to trigger optical turbulence in the whole troposphere; (ii) a few of the astroclimatic parameters, such as the wavefront coherence time (τ 0 ), depend directly on V (h); (iii) the equivalent velocity V 0 , controlling the frequency at which the adaptive optics systems have to run in order to work properly, depends on the Vertical Distribution of the wind speed and optical turbulence. Also, too strong a wind speed near the ground can introduce vibrations in the telescope structures. The wind speed at a precise pressure (200 hPa) has frequently been used to retrieve indications concerning τ 0 and the frequency limits imposed on all instrumentation based on adaptive optics systems. However, more recently, it has been proved that V 200 (the wind speed at 200 hPa) alone is not sufficient to provide exhaustive elements concerning this topic, and thus the Vertical Distribution of the wind speed is necessary. In this paper, we report on a complete characterization of the Vertical Distribution of wind speed strength, which has been carried out above Mt Graham (Arizona, USA), the site of the Large Binocular Telescope. We provide a climatological study extended over 10 yr using the operational analyses from the European Centre for Medium-Range Weather Forecasts (ECMWF). We prove that this is representative of the Vertical Distribution of the wind speed at Mt Graham, with the exception of the boundary layer. We also prove that a mesoscale model can provide reliable nightly estimates of V (h) above this astronomical site from the ground up to the top of the atmosphere (~20 km).
-
wind speed Vertical Distribution at mt graham
arXiv: Instrumentation and Methods for Astrophysics, 2010Co-Authors: Susanna Hagelin, E Masciadri, Franck LascauxAbstract:The characterization of the wind speed Vertical Distribution V(h) is fundamental for an astronomical site for many different reasons: (1) the wind speed shear contributes to trigger optical turbulence in the whole troposphere, (2) a few of the astroclimatic parameters such as the wavefront coherence time (tau_0) depends directly on V(h), (3) the equivalent velocity V_0, controlling the frequency at which the adaptive optics systems have to run to work properly, depends on the Vertical Distribution of the wind speed and optical turbulence. Also, a too strong wind speed near the ground can introduce vibrations in the telescope structures. The wind speed at a precise pressure (200 hPa) has frequently been used to retrieve indications concerning the tau_0 and the frequency limits imposed to all instrumentation based on adaptive optics systems, but more recently it has been proved that V_200 (wind speed at 200 hPa) alone is not sufficient to provide exhaustive elements concerning this topic and that the Vertical Distribution of the wind speed is necessary. In this paper a complete characterization of the Vertical Distribution of wind speed strength is done above Mt.Graham (Arizona, US), site of the Large Binocular Telescope. We provide a climatological study extended over 10 years using the operational analyses from the European Centre for Medium-Range Weather Forecasts (ECMWF), we prove that this is representative of the wind speed Vertical Distribution at Mt. Graham with exception of the boundary layer and we prove that a mesoscale model can provide reliable nightly estimates of V(h) above this astronomical site from the ground up to the top of the atmosphere (~ 20 km).
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optical turbulence Vertical Distribution with standard and high resolution at mt graham
Monthly Notices of the Royal Astronomical Society, 2010Co-Authors: E Masciadri, Susanna Hagelin, J Stoesz, Franck LascauxAbstract:A characterization of the optical turbulence Vertical Distribution (C 2 N profiles) and all the main integrated astroclimatic parameters derived from the C 2 N and the wind speed profiles above the site of the Large Binocular Telescope (LBT) (Mt Graham, Arizona, USA) is presented. The statistics include measurements related to 43 nights done with a Generalized SCIDAR (GS) used in standard configuration with a Vertical resolution ΔH ~ 1 km on the whole 20 km and with the new technique (High Vertical Resolution GS) in the first kilometre. The latter achieves a resolution ΔH ~ 20-30 m in this region of the atmosphere. Measurements done in different periods of the year permit us to provide a seasonal variation analysis of the C 2 N . A discretized Distribution of C 2 N , useful for the Ground Layer Adaptive Optics (GLAO) simulations, is provided and a specific analysis for the LBT Laser Guide Star system ARGOS (running in GLAO configuration) case is done including the calculation of the 'grey zones' for J, H and K bands. Mt Graham is confirmed to be an excellent site with median values of the seeing without dome contribution e = 0.72 arcsec, the isoplanatic angle θ 0 = 2.5 arcsec and the wavefront coherence time τ 0 = 4.8 ms. We find that the OT Vertical Distribution decreases in a much sharper way than what has been believed so far in the proximity of the ground above astronomical sites. We find that 50 per cent of the whole turbulence develops in the first 80 ± 15 m from the ground. We finally prove that the error in the normalization of the scintillation that has been recently demonstrated in the principle of the GS technique affects these measurements by an absolutely negligible quantity (0.04 arcsec).
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optical turbulence Vertical Distribution with standard and high resolution at mt graham
arXiv: Instrumentation and Methods for Astrophysics, 2010Co-Authors: E Masciadri, Susanna Hagelin, J Stoesz, Franck LascauxAbstract:A characterization of the optical turbulence Vertical Distribution (Cn2 profiles) and all the main integrated astroclimatic parameters derived from the Cn2 and the wind speed profiles above the site of the Large Binocular Telescope (Mt. Graham, Arizona, US) is presented. The statistic includes measurements related to 43 nights done with a Generalized Scidar (GS) used in standard configuration with a Vertical resolution Delta(H)~1 km on the whole 20 km and with the new technique (HVR-GS) in the first kilometer. The latter achieves a resolution Delta(H)~20-30 m in this region of the atmosphere. Measurements done in different periods of the year permit us to provide a seasonal variation analysis of the Cn2. A discretized Distribution of Cn2 useful for the Ground Layer Adaptive Optics (GLAO) simulations is provided and a specific analysis for the LBT Laser Guide Star system ARGOS (running in GLAO configuration) case is done including the calculation of the 'gray zones' for J, H and K bands. Mt. Graham confirms to be an excellent site with median values of the seeing without dome contribution epsilon = 0.72", the isoplanatic angle theta0 = 2.5" and the wavefront coherence time tau0= 4.8 msec. We find that the optical turbulence Vertical Distribution decreases in a much sharper way than what has been believed so far in proximity of the ground above astronomical sites. We find that 50% of the whole turbulence develops in the first 80+/-15 m from the ground. We finally prove that the error in the normalization of the scintillation that has been recently put in evidence in the principle of the GS technique, affects these measurements with an absolutely negligible quantity (0.04").
Andres Uriarte - One of the best experts on this subject based on the ideXlab platform.
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buoyancy measurements and Vertical Distribution of eggs of sardine sardina pilchardus and anchovy engraulis encrasicolus
Marine Biology, 2004Co-Authors: D V P Conway, S H Coombs, N C Halliday, Guillermo Boyra, L D Rueda, Andres Uriarte, M B SantosAbstract:Measurements were made of the density and settling velocity of eggs of sardine (Sardina pilchardus) and anchovy (Engraulis encrasicolus), using a density-gradient column. These results were related to observed Vertical Distributions of eggs obtained from stratified Vertical Distribution sampling in the Bay of Biscay. Eggs of both species had slightly positive buoyancy in local seawater throughout most of their development until near hatching, when there was a marked increase in density and they became negatively buoyant. The settling velocity of anchovy eggs, which are shaped as prolate ellipsoids, was close to predictions for spherical particles of equivalent volume. An improved model was developed for prediction of the settling velocity of sardine eggs, which are spherical with a relatively large perivitelline volume; this incorporated permeability of the chorion and adjustment of the density of the perivitelline fluid to ambient seawater. Eggs of both species were located mostly in the top 20 m of the water column, in increasing abundance towards the surface. A sub-surface peak of egg abundance was sometimes observed at the pycnocline, particularly where this was pronounced and associated with a low-salinity surface layer. There was a progressive deepening of the depth Distributions for successive stages of egg development. Results from this study can be applied for improved plankton sampling of sardine and anchovy eggs and in modelling studies of their Vertical Distribution.
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modelling the Vertical Distribution of eggs of anchovy engraulis encrasicolus and sardine sardina pilchardus
Fisheries Oceanography, 2003Co-Authors: Guillermo Boyra, Svein Sundby, S H Coombs, L D Rueda, Bjorn Adlandsvik, M B Santos, Andres UriarteAbstract:Measurements were made of the density and settling velocity of eggs of sardine (Sardina pilchardus) and anchovy (Engraulis encrasicolus), using a density-gradient column. These results were related to observed Vertical Distributions of eggs obtained from stratified Vertical Distribution sampling in the Bay of Biscay. Eggs of both species had slightly positive buoyancy in local seawater throughout most of their development until near hatching, when there was a marked increase in density and they became negatively buoyant. The settling velocity of anchovy eggs, which are shaped as prolate ellipsoids, was close to predictions for spherical particles of equivalent volume. An improved model was developed for prediction of the settling velocity of sardine eggs, which are spherical with a relatively large perivitelline volume; this incorporated permeability of the chorion and adjustment of the density of the perivitelline fluid to ambient seawater. Eggs of both species were located mostly in the top 20 m of the water column, in increasing abundance towards the surface. A sub-surface peak of egg abundance was sometimes observed at the pycnocline, particularly where this was pronounced and associated with a low-salinity surface layer. There was a progressive deepening of the depth Distributions for successive stages of egg development. Results from this study can be applied for improved plankton sampling of sardine and anchovy eggs and in modelling studies of their Vertical Distribution.
M B Santos - One of the best experts on this subject based on the ideXlab platform.
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buoyancy measurements and Vertical Distribution of eggs of sardine sardina pilchardus and anchovy engraulis encrasicolus
Marine Biology, 2004Co-Authors: D V P Conway, S H Coombs, N C Halliday, Guillermo Boyra, L D Rueda, Andres Uriarte, M B SantosAbstract:Measurements were made of the density and settling velocity of eggs of sardine (Sardina pilchardus) and anchovy (Engraulis encrasicolus), using a density-gradient column. These results were related to observed Vertical Distributions of eggs obtained from stratified Vertical Distribution sampling in the Bay of Biscay. Eggs of both species had slightly positive buoyancy in local seawater throughout most of their development until near hatching, when there was a marked increase in density and they became negatively buoyant. The settling velocity of anchovy eggs, which are shaped as prolate ellipsoids, was close to predictions for spherical particles of equivalent volume. An improved model was developed for prediction of the settling velocity of sardine eggs, which are spherical with a relatively large perivitelline volume; this incorporated permeability of the chorion and adjustment of the density of the perivitelline fluid to ambient seawater. Eggs of both species were located mostly in the top 20 m of the water column, in increasing abundance towards the surface. A sub-surface peak of egg abundance was sometimes observed at the pycnocline, particularly where this was pronounced and associated with a low-salinity surface layer. There was a progressive deepening of the depth Distributions for successive stages of egg development. Results from this study can be applied for improved plankton sampling of sardine and anchovy eggs and in modelling studies of their Vertical Distribution.
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modelling the Vertical Distribution of eggs of anchovy engraulis encrasicolus and sardine sardina pilchardus
Fisheries Oceanography, 2003Co-Authors: Guillermo Boyra, Svein Sundby, S H Coombs, L D Rueda, Bjorn Adlandsvik, M B Santos, Andres UriarteAbstract:Measurements were made of the density and settling velocity of eggs of sardine (Sardina pilchardus) and anchovy (Engraulis encrasicolus), using a density-gradient column. These results were related to observed Vertical Distributions of eggs obtained from stratified Vertical Distribution sampling in the Bay of Biscay. Eggs of both species had slightly positive buoyancy in local seawater throughout most of their development until near hatching, when there was a marked increase in density and they became negatively buoyant. The settling velocity of anchovy eggs, which are shaped as prolate ellipsoids, was close to predictions for spherical particles of equivalent volume. An improved model was developed for prediction of the settling velocity of sardine eggs, which are spherical with a relatively large perivitelline volume; this incorporated permeability of the chorion and adjustment of the density of the perivitelline fluid to ambient seawater. Eggs of both species were located mostly in the top 20 m of the water column, in increasing abundance towards the surface. A sub-surface peak of egg abundance was sometimes observed at the pycnocline, particularly where this was pronounced and associated with a low-salinity surface layer. There was a progressive deepening of the depth Distributions for successive stages of egg development. Results from this study can be applied for improved plankton sampling of sardine and anchovy eggs and in modelling studies of their Vertical Distribution.
E Masciadri - One of the best experts on this subject based on the ideXlab platform.
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wind speed Vertical Distribution at mt graham
Monthly Notices of the Royal Astronomical Society, 2010Co-Authors: Susanna Hagelin, E Masciadri, Franck LascauxAbstract:The characterization of the Vertical Distribution of wind speed, V(h), is fundamental for an astronomical site for many different reasons: (i) the wind speed shear contributes to trigger optical turbulence in the whole troposphere; (ii) a few of the astroclimatic parameters, such as the wavefront coherence time (τ 0 ), depend directly on V (h); (iii) the equivalent velocity V 0 , controlling the frequency at which the adaptive optics systems have to run in order to work properly, depends on the Vertical Distribution of the wind speed and optical turbulence. Also, too strong a wind speed near the ground can introduce vibrations in the telescope structures. The wind speed at a precise pressure (200 hPa) has frequently been used to retrieve indications concerning τ 0 and the frequency limits imposed on all instrumentation based on adaptive optics systems. However, more recently, it has been proved that V 200 (the wind speed at 200 hPa) alone is not sufficient to provide exhaustive elements concerning this topic, and thus the Vertical Distribution of the wind speed is necessary. In this paper, we report on a complete characterization of the Vertical Distribution of wind speed strength, which has been carried out above Mt Graham (Arizona, USA), the site of the Large Binocular Telescope. We provide a climatological study extended over 10 yr using the operational analyses from the European Centre for Medium-Range Weather Forecasts (ECMWF). We prove that this is representative of the Vertical Distribution of the wind speed at Mt Graham, with the exception of the boundary layer. We also prove that a mesoscale model can provide reliable nightly estimates of V (h) above this astronomical site from the ground up to the top of the atmosphere (~20 km).
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wind speed Vertical Distribution at mt graham
arXiv: Instrumentation and Methods for Astrophysics, 2010Co-Authors: Susanna Hagelin, E Masciadri, Franck LascauxAbstract:The characterization of the wind speed Vertical Distribution V(h) is fundamental for an astronomical site for many different reasons: (1) the wind speed shear contributes to trigger optical turbulence in the whole troposphere, (2) a few of the astroclimatic parameters such as the wavefront coherence time (tau_0) depends directly on V(h), (3) the equivalent velocity V_0, controlling the frequency at which the adaptive optics systems have to run to work properly, depends on the Vertical Distribution of the wind speed and optical turbulence. Also, a too strong wind speed near the ground can introduce vibrations in the telescope structures. The wind speed at a precise pressure (200 hPa) has frequently been used to retrieve indications concerning the tau_0 and the frequency limits imposed to all instrumentation based on adaptive optics systems, but more recently it has been proved that V_200 (wind speed at 200 hPa) alone is not sufficient to provide exhaustive elements concerning this topic and that the Vertical Distribution of the wind speed is necessary. In this paper a complete characterization of the Vertical Distribution of wind speed strength is done above Mt.Graham (Arizona, US), site of the Large Binocular Telescope. We provide a climatological study extended over 10 years using the operational analyses from the European Centre for Medium-Range Weather Forecasts (ECMWF), we prove that this is representative of the wind speed Vertical Distribution at Mt. Graham with exception of the boundary layer and we prove that a mesoscale model can provide reliable nightly estimates of V(h) above this astronomical site from the ground up to the top of the atmosphere (~ 20 km).
-
optical turbulence Vertical Distribution with standard and high resolution at mt graham
Monthly Notices of the Royal Astronomical Society, 2010Co-Authors: E Masciadri, Susanna Hagelin, J Stoesz, Franck LascauxAbstract:A characterization of the optical turbulence Vertical Distribution (C 2 N profiles) and all the main integrated astroclimatic parameters derived from the C 2 N and the wind speed profiles above the site of the Large Binocular Telescope (LBT) (Mt Graham, Arizona, USA) is presented. The statistics include measurements related to 43 nights done with a Generalized SCIDAR (GS) used in standard configuration with a Vertical resolution ΔH ~ 1 km on the whole 20 km and with the new technique (High Vertical Resolution GS) in the first kilometre. The latter achieves a resolution ΔH ~ 20-30 m in this region of the atmosphere. Measurements done in different periods of the year permit us to provide a seasonal variation analysis of the C 2 N . A discretized Distribution of C 2 N , useful for the Ground Layer Adaptive Optics (GLAO) simulations, is provided and a specific analysis for the LBT Laser Guide Star system ARGOS (running in GLAO configuration) case is done including the calculation of the 'grey zones' for J, H and K bands. Mt Graham is confirmed to be an excellent site with median values of the seeing without dome contribution e = 0.72 arcsec, the isoplanatic angle θ 0 = 2.5 arcsec and the wavefront coherence time τ 0 = 4.8 ms. We find that the OT Vertical Distribution decreases in a much sharper way than what has been believed so far in the proximity of the ground above astronomical sites. We find that 50 per cent of the whole turbulence develops in the first 80 ± 15 m from the ground. We finally prove that the error in the normalization of the scintillation that has been recently demonstrated in the principle of the GS technique affects these measurements by an absolutely negligible quantity (0.04 arcsec).
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optical turbulence Vertical Distribution with standard and high resolution at mt graham
arXiv: Instrumentation and Methods for Astrophysics, 2010Co-Authors: E Masciadri, Susanna Hagelin, J Stoesz, Franck LascauxAbstract:A characterization of the optical turbulence Vertical Distribution (Cn2 profiles) and all the main integrated astroclimatic parameters derived from the Cn2 and the wind speed profiles above the site of the Large Binocular Telescope (Mt. Graham, Arizona, US) is presented. The statistic includes measurements related to 43 nights done with a Generalized Scidar (GS) used in standard configuration with a Vertical resolution Delta(H)~1 km on the whole 20 km and with the new technique (HVR-GS) in the first kilometer. The latter achieves a resolution Delta(H)~20-30 m in this region of the atmosphere. Measurements done in different periods of the year permit us to provide a seasonal variation analysis of the Cn2. A discretized Distribution of Cn2 useful for the Ground Layer Adaptive Optics (GLAO) simulations is provided and a specific analysis for the LBT Laser Guide Star system ARGOS (running in GLAO configuration) case is done including the calculation of the 'gray zones' for J, H and K bands. Mt. Graham confirms to be an excellent site with median values of the seeing without dome contribution epsilon = 0.72", the isoplanatic angle theta0 = 2.5" and the wavefront coherence time tau0= 4.8 msec. We find that the optical turbulence Vertical Distribution decreases in a much sharper way than what has been believed so far in proximity of the ground above astronomical sites. We find that 50% of the whole turbulence develops in the first 80+/-15 m from the ground. We finally prove that the error in the normalization of the scintillation that has been recently put in evidence in the principle of the GS technique, affects these measurements with an absolutely negligible quantity (0.04").
