Datasets:
ReadingTimeMachine
/
rtm-sgt-ocr-v1

Dataset card Data Studio Files Community
1
source
stringlengths
1
2.05k
⌀
target
stringlengths
1
11.7k
In this region it is impossible to select. ealaxics reliably.
In this region it is impossible to select galaxies reliably.
In optically selected surveys this is because of absorption from dust.
In optically selected surveys this is because of absorption from dust.
In infrared selected surveys due to cirrus emission.
In infrared selected surveys due to cirrus emission.
It will clearly be desirable for this excluded region to be as small as possible.
It will clearly be desirable for this excluded region to be as small as possible.
Phe last desirable property is simple density of sampling.
The last desirable property is simple density of sampling.
The more galaxies we have in à given volume. the greater. chance we will have of calculating accurate peculiar velocities: assuming our ealaxies are reliable tracers of the mass.
The more galaxies we have in a given volume, the greater chance we will have of calculating accurate peculiar velocities; assuming our galaxies are reliable tracers of the mass.
In Subsection 3.1.. we discuss how galaxy bias effects our analysis.
In Subsection \ref{subias}, we discuss how galaxy bias effects our analysis.
We then describe the PSC-z survey. our main source of galaxies.
We then describe the PSC-z survey, our main source of galaxies.
Subsection 3.2. is a general introduction to the catalogue and is. followed. by Subsections on: the niasked regions. the grouping of galaxies. the Virgo Cluster. tical effects. and redshift. distortions.
Subsection \ref{pscz} is a general introduction to the catalogue and is followed by Subsections on: the masked regions, the grouping of galaxies, the Virgo Cluster, tidal effects and redshift distortions.
In. Subsection 3.8. we discuss how we have treated. local galaxies (those with ezX500kms. 19).
In Subsection \ref{locgal}, , we discuss how we have treated local galaxies (those with $ cz \leq 500$ ).
Finally. in Subsection 3.9.. we present the distance estimations we have used to derive the observed peculiar velocities.
Finally, in Subsection \ref{dist}, we present the distance estimations we have used to derive the observed peculiar velocities.
A preliminary issue to be discussed is the elect of bias in the ealaxy distribution on our analvsis.
A preliminary issue to be discussed is the effect of bias in the galaxy distribution on our analysis.
We need a catalogue of miss tracers on which to apply the Least Action Principle. this will be a catalogue of galaxies ancl galaxy groups.
We need a catalogue of mass tracers on which to apply the Least Action Principle, this will be a catalogue of galaxies and galaxy groups.
This means that our analysis will depend on the relationship between the galaxies and the mass.
This means that our analysis will depend on the relationship between the galaxies and the mass.
In addition to our requirement that the mass is concentrated. in the galaxies (sce Section 2)). we have uncertainty [rom whether the mass associated with galaxies is dependant on their environment.
In addition to our requirement that the mass is concentrated in the galaxies (see Section \ref{nam}) ), we have uncertainty from whether the mass associated with galaxies is dependant on their environment.
This is the problem of the bias of the galaxy clistribution.
This is the problem of the bias of the galaxy distribution.
The standard approach to this problem is to use the linear bias factor b. to quantify the uncertainty in this relationship (b is given by 0,=560,,. where 9,, and a, are the over- or uncler-densities in the galaxies and the mass respectively).
The standard approach to this problem is to use the linear bias factor $b$, to quantify the uncertainty in this relationship $b$ is given by $\delta_{g}=b \delta_{m}$, where $\delta_{m}$ and $\delta_{g}$ are the over- or under-densities in the galaxies and the mass respectively).
This has the advantage that in linear theory. the ellect of b is degenerate with that ofand the results only depend on 3=Og" /b.
This has the advantage that in linear theory, the effect of $b$ is degenerate with that ofand the results only depend on $\beta=\Omega^{0.6}_{0}/b$ .
Llowever. the Least. Action Principle does
However, the Least Action Principle does
Traditionally. since standing kink waves in coronal loops were observed using TRACE. ihe measurement of damping times was of primary interest. see e.g.. Aschwancen and Armeguietal.(2007).
Traditionally, since standing kink waves in coronal loops were observed using TRACE, the measurement of damping times was of primary interest, see e.g., \citet{aschetal03} and \citet{arregui07}.
. However. for propagating kink waves it is more appropriate to study the damping leneth £j. with the expression lor wave amplitude eiven by where s is (he clistance along the waveguide and Ay is initial amplitucle.
However, for propagating kink waves it is more appropriate to study the damping length $L_{\mathrm{D}}$, with the expression for wave amplitude given by where $s$ is the distance along the waveguide and $A_0$ is initial amplitude.
From (2007).. the (transverse scale of propagating disturbances has an upper limit of about 9 Min and wavelengths are A150 Min. so assuming that the average waveguide observed with CoMP is a fluxtube of radius RS4.5 Mm. kink waves are in the long wavelength reeime where /AÀ«1.
From \citet{tomczetal07}, the transverse scale of propagating disturbances has an upper limit of about 9 Mm and wavelengths are $\lambda \gtrapprox 180$ Mm, so assuming that the average waveguide observed with CoMP is a fluxtube of radius $R \lessapprox 4.5$ Mm, kink waves are in the long wavelength regime where $R /\lambda\ll 1$.
In this limit it was shown by Terracasetal.(2010) that the TOY relation is simply given bv where f is the frequency defined by [=ey,/A and £j is an equilibrium parameter dependent on length scale of the density inhomogeneity.
In this limit it was shown by \citet{terrarretal10} that the TGV relation is simply given by where $f$ is the frequency defined by $f=v_{\mathrm{ph}}/\lambda$ and $\xi_{\mathrm{E}}$ is an equilibrium parameter dependent on length scale of the density inhomogeneity.
Equation (3)) demonstrates (hat Lp is inversely proportional to f. i.e.. the rate of damping per unit length will be ereater for higher [requencey. waves than low Irequencey. waves.
Equation \ref{TGV}) ) demonstrates that $L_{\mathrm{D}}$ is inversely proportional to $f$, i.e., the rate of damping per unit length will be greater for higher frequency waves than low frequency waves.
The parameter £j can be calculated precisely for a chosen equilibrium model. e.g.. if we choose a thin inhomogeneous boundary laver witha continuous sinusoidal profile decreasing between p; and p. then where / is the thickness of the boundary laver (seee.g..Goossensetal.1992:Ruclerman 2002)..
The parameter $\xi_{\mathrm{E}}$ can be calculated precisely for a chosen equilibrium model, e.g., if we choose a thin inhomogeneous boundary layer witha continuous sinusoidal profile decreasing between $\rho_{\mathrm{i}}$ and $\rho_{\mathrm{e}}$ then where $l$ is the thickness of the boundary layer \citep[see e.g.,][]{goossensetal92,rudrob02, goossens02}. .
IIence Equations (3)) aud (4)) demonstrate that
Hence Equations \ref{TGV}) ) and \ref{xidef}) ) demonstrate that
and Na abundances. similarly to what was found for stars on the RGB in other globular clusters.
and Na abundances, similarly to what was found for stars on the RGB in other globular clusters.
No study dedicated to light elements was carried out to our knowledge. so the hint by is our only comparison,
No study dedicated to light elements was carried out to our knowledge, so the hint by is our only comparison.
We do find a clear and bimodal CH and CN anti-correlation. which is even more striking if one considers the low number of stars observed and the relatively low S/N around 3900A.
We do find a clear and bimodal CH and CN anti-correlation, which is even more striking if one considers the low number of stars observed and the relatively low S/N around 3900.
. As for NGC 5927. the high metallicity helps in revealing CH and CN band strength variations. and the study of these metal-rich GGC would be interesting for the same reasons.
As for NGC 5927, the high metallicity helps in revealing CH and CN band strength variations, and the study of these metal-rich GGC would be interesting for the same reasons.
An HST photometric study — seeking for multiple sequences — coupled with high-resolution spectroscopy for deriving the chemical patterns of NGC 6352 could be one of the next steps in the study of chemical abundance anomalies in GGC.
An HST photometric study – seeking for multiple sequences – coupled with high-resolution spectroscopy for deriving the chemical patterns of NGC 6352 could be one of the next steps in the study of chemical abundance anomalies in GGC.
The cluster NGC 6388 Is one of 10 most massive in. the Milky Way. it is a bulge cluster. located about 3 kpe from the Galactic centre.
The cluster NGC 6388 is one of 10 most massive in the Milky Way, it is a bulge cluster, located about 3 kpc from the Galactic centre.
It is very centrally concentrated and tightly bound. and has among the highest predicted escape velocity at the cluster center 2005).
It is very centrally concentrated and tightly bound, and has among the highest predicted escape velocity at the cluster center .
Based on high-resolution FLAMES-UVES spectra. measured |Fe/H]=—-0.44+0.01(x0.03).
Based on high-resolution FLAMES-UVES spectra, measured $=-0.44 \pm 0.01 (\pm 0.03)$.
These authors also detected the presence of Na-O and Mg-Al anti-correlations. and of a Na-AI correlation among RGB stars.
These authors also detected the presence of Na-O and Mg-Al anti-correlations, and of a Na-Al correlation among RGB stars.
A clear bimodality in CH and CN was also detected on the RGB by(2009).
A clear bimodality in CH and CN was also detected on the RGB by.
. NGC 6388 is sometimes referred to as being unusual2008b):: in contrast to expectations for its high metallicity. the cluster harbours an extended blue horizontal branch1993).. and RR Lyr stars with periods much longer than expected for their metallicity.
NGC 6388 is sometimes referred to as being unusual: in contrast to expectations for its high metallicity, the cluster harbours an extended blue horizontal branch, and RR Lyr stars with periods much longer than expected for their metallicity.
In addition. the horizontal branch presents a slope. so that in the V-band its blue tail lies about 0.5 mag brighter than the red HB clump2002).
In addition, the horizontal branch presents a slope, so that in the V-band its blue tail lies about 0.5 mag brighter than the red HB clump.
. These features are not reproducible by stellar evolutionary models with an SSP of standard GGC abundance ratios. but could be explained with the presence of more than one stellar population and some self- with CNO processed material2008).
These features are not reproducible by stellar evolutionary models with an SSP of standard GGC abundance ratios, but could be explained with the presence of more than one stellar population and some self-enrichment with CNO processed material.
. The evidence for multiple stellar populations came from the most recent deep near-IR photometry of(2009). who detected two distinct sub-giant branches in this cluster.
The evidence for multiple stellar populations came from the most recent deep near-IR photometry of, who detected two distinct sub-giant branches in this cluster.
Unfortunately. the strong differential reddening and the insufficient S/N of our data prevent us from reaching any conclusion about the CH and CN correlation at the MS level.
Unfortunately, the strong differential reddening and the insufficient S/N of our data prevent us from reaching any conclusion about the CH and CN correlation at the MS level.
But given its high metallicity and total mass. this ts one of the most interesting clusters for further investigations.
But given its high metallicity and total mass, this is one of the most interesting clusters for further investigations.
In spite of the poor data for this cluster. NGC 6388 follows all the trends of other GGC with clusters parameters (Sect. 6)).
In spite of the poor data for this cluster, NGC 6388 follows all the trends of other GGC with clusters parameters (Sect. \ref{sec-trends}) ).
Besides w Centauri. M 22 is one of the first GGC that were suspected to host multiple stellar. populations and chemical anomalies1977).
Besides $\omega$ Centauri, M 22 is one of the first GGC that were suspected to host multiple stellar populations and chemical anomalies.
. Unfortunately. strong differential reddening has complicated its study1999).. therefore spectroscopic studies initially. gave conflicting results: while a spread in the CH and C abundances of RGB stars appeared unquestionable1983). some studies reported on abundance variations of 0.340.5 dex in. Ca and/or Fe. often correlated with the CH and CN variations1992)., while other studies found no significant variation i the heavy element content1991).
Unfortunately, strong differential reddening has complicated its study, therefore spectroscopic studies initially gave conflicting results: while a spread in the CH and CN abundances of RGB stars appeared unquestionable, some studies reported on abundance variations of $\pm$ 0.5 dex in Ca and/or Fe, often correlated with the CH and CN variations, while other studies found no significant variation in the heavy element content.
. This was probably because the reported variations were of the order of the quoted uncertainties2004).
This was probably because the reported variations were of the order of the quoted uncertainties.
. Recently. found that two groups of stars exist in M 22. where [Fe/H] appears correlated with the s-process elements and with [ζα/Εε]. and the usual Na. O. Al anti-correlations were found.
Recently, found that two groups of stars exist in M 22, where [Fe/H] appears correlated with the $s$ -process elements and with [Ca/Fe], and the usual Na, O, Al anti-correlations were found.
confirm that the Ca distribution shows a large spread with a possible bimodality.
confirm that the Ca distribution shows a large spread with a possible bimodality.
Our data. belonging to the unevolved stars from the sample by do not have sufficient S/N to reveal CH and CN anti-correlations or bimodalities.
Our data, belonging to the unevolved stars from the sample by do not have sufficient S/N to reveal CH and CN anti-correlations or bimodalities.
No clear bimodality was found by among RGB stars. either.
No clear bimodality was found by among RGB stars, either.
If really different metallicities co-exist in the cluster. this could further complicate the detection of anti-correlations and. of their bimodalities. if they are present.
If really different metallicities co-exist in the cluster, this could further complicate the detection of anti-correlations and of their bimodalities, if they are present.
Most probably spectral synthesis and the determination of [C/Fe] and [N/Fe] would help in clarifying the picture.
Most probably spectral synthesis and the determination of [C/Fe] and [N/Fe] would help in clarifying the picture.
The cluster NGC 6752 is one of the best studied regarding its chemical properties. given its relative proximity to us (Table 1)).
The cluster NGC 6752 is one of the best studied regarding its chemical properties, given its relative proximity to us (Table \ref{logs}) ).
It has an intermediate metallicity and a blue HB.
It has an intermediate metallicity and a blue HB.
Its orbit is remarkably similar to that of 47 Tuc2000).. and it is therefore associated with the thick dise by some authors.
Its orbit is remarkably similar to that of 47 Tuc, and it is therefore associated with the thick disc by some authors.
Many high-resolution spectroscopic studies of this cluster provide the following iron abundance measurements: [Fe/H|2—1.48+0.010.06 dex by based on FLAMES-UVES spectra of 7 giants near the RGB bump. [Fe/H]=-1.42 based on UVES spectra of MS and sub-giant stars 2001).. [Fe/H]=—1.49+0.07 for 9 SGB stars. and |Fe/H|2—1.48+0.07 for 9 turnoff stars based on FLAMES-UVES spectra2004).. |[Fe/H|2-1.61 based on 38 RGB stars observed at very high resolution2005).. and [Fe/H];=-1.56. [Fe/H],=—1.48 based on FLAMES GIRAFFE spectra of 137 RGB stars2009c).
Many high-resolution spectroscopic studies of this cluster provide the following iron abundance measurements: $=-1.48 \pm 0.01 \pm 0.06$ dex by based on FLAMES-UVES spectra of 7 giants near the RGB bump, $=-1.42$ based on UVES spectra of MS and sub-giant stars , $=-1.49 \pm 0.07$ for 9 SGB stars, and $=-1.48 \pm 0.07$ for 9 turnoff stars based on FLAMES-UVES spectra, $=-1.61$ based on 38 RGB stars observed at very high resolution, and $_I=-1.56$, $_{II}=-1.48$ based on FLAMES GIRAFFE spectra of 137 RGB stars.
. The O-Na anticorrelation is well established in NGC 6752 from observations of both MS and SGB2005).. as well as of RGB2003).
The O-Na anticorrelation is well established in NGC 6752 from observations of both MS and SGB, as well as of RGB.
. Data from and show Na-O and Al-Mg anticorrelations in stars that are both brighter and fainter than the RGB bump.
Data from and show Na-O and Al-Mg anticorrelations in stars that are both brighter and fainter than the RGB bump.
detected. very strong N abundance variations in the MS Turn-off stars.
detected very strong N abundance variations in the MS Turn-off stars.
Furhtermore.
Furhtermore,
were set using ox values obtained from the literature.
were set using $\alpha_{\rm ox}$ values obtained from the literature.
The SEDs were normalised to the £i. value. quoted. by the authors of the respective warm absorber model. if available. or otherwise from Blustinetal.(2005).
The SEDs were normalised to the $L_{\rm ion}$ value quoted by the authors of the respective warm absorber model, if available, or otherwise from \citet{blustin2005}.
. The values for Lia. Quy and Ex are listed in Table 2.. and the derived temperatures are in Table 1..
The values for $L_{\rm ion}$, $\alpha_{\rm ox}$ and $\Gamma_{\rm X}$ are listed in Table \ref{sed_properties}, and the derived temperatures are in Table \ref{wa_properties_results}.
The original calculations of the radio emission from stellar winds (Panagia&οι1975:WrightBarlow1975) assumecl that the wind was optically thick. with the blackbody emission at cach point being propagated through bremsstrahlung absorption along the line of sight.
The original calculations of the radio emission from stellar winds \citep{panagia1975,wright1975} assumed that the wind was optically thick, with the blackbody emission at each point being propagated through bremsstrahlung absorption along the line of sight.
The recent paper of Blunelell&huncic(2007).. however. calculated the flux density [rom an AGN wind by assuming that the emission emerges from the optically thin part of the
The recent paper of \citet{blundell2007}, however, calculated the flux density from an AGN wind by assuming that the emission emerges from the optically thin part of the
fashion to the real data.
fashion to the real data.
As described in. AleLure ct αἱ. (
As described in McLure et al. (
1999). the actual quasar observations consist. of. three deep GO0-sccond exposures which were complimented by three shorter snap-shot exposures of 5. 26 απ 40 seconds. designed. to ensure a unsaturated: measure of the nuclear component.
1999), the actual quasar observations consist of three deep 600-second exposures which were complimented by three shorter snap-shot exposures of 5, 26 and 40 seconds, designed to ensure a unsaturated measure of the nuclear component.
The final reduced. quasar images consist. of a stack of the three long exposures. with the central regions replaced. by a scaled. snap-shot exposure to recover the quasar’s full cdvnamic range.
The final reduced quasar images consist of a stack of the three long exposures, with the central regions replaced by a scaled snap-shot exposure to recover the quasar's full dynamic range.
The construction of the synthetic quasars proceeded. in exactly the sane fashion. with individual simulations of each of the six separate exposures.
The construction of the synthetic quasars proceeded in exactly the same fashion, with individual simulations of each of the six separate exposures.
An appropriate level of background counts were then added: to cach of the simulated exposures. before they were processed by the routine which simulated the cllects of both shot and read-out noise.
An appropriate level of background counts were then added to each of the simulated exposures before they were processed by the routine which simulated the effects of both shot and read-out noise.
The fuclicial luminosity of the simulated. host. galaxies was chosen to match the absolute magnitude of the best-lit to 2247|143 (My;= 23.8). which was typical of the 12 hosts which had been observed at the time.
The fudicial luminosity of the simulated host galaxies was chosen to match the absolute magnitude of the best-fit to 2247+14 $_{R}=-23.8$ ), which was typical of the 12 hosts which had been observed at the time.
The calculation of the absolute luminosity of the hosts at. the three redshifts was then determined. assuming a tvpica spectral index of a=1.5 for the E675W filter (fav 7). and a cosmology with Ly=50kms !Mpc. * and Qo=1.
The calculation of the absolute luminosity of the hosts at the three redshifts was then determined assuming a typical spectral index of $\alpha=1.5$ for the F675W filter $f_{\nu}\,\alpha\,\nu^{-\alpha}$ ), and a cosmology with $H_{0}=50$ $^{-1}$ $^{-1}$ and $\Omega_{0}=1$.
The cosmological dimming of the AGN point source assume a spectral index ofa=0.2 (Neugebauer et al.
The cosmological dimming of the AGN point source assumed a spectral index of $\alpha=0.2$ (Neugebauer et al.
1987).
1987).
Figure 5 shows the apparent magnitudes for all 33 host galaxies from the programme (see Dunlop et al.
Figure \ref{synthgals} shows the apparent magnitudes for all 33 host galaxies from the programme (see Dunlop et al.
2000) plottec against redshift.
2000) plotted against redshift.
Also shown are the apparent. magnitudes of the synthetic host. galaxies.
Also shown are the apparent magnitudes of the synthetic host galaxies.
There is a suggestion [rom Fie 5 that the synthetic galaxies are [ractionally too brig= compared to the data. making it arguably slightly too easy or the code to recover the galaxy parameters from the simulated images.
There is a suggestion from Fig \ref{synthgals} that the synthetic galaxies are fractionally too bright compared to the data, making it arguably slightly too easy for the code to recover the galaxy parameters from the simulated images.
This is confirmed by the results for the ull sample which show the mean absolute Luminosity of the 33 host galaxies to be Mj;=23.53. 0.27 magnitudes fainter han the svnthetic hosts used in the testing programme.
This is confirmed by the results for the full sample which show the mean absolute luminosity of the 33 host galaxies to be $_{R}=-23.53$, 0.27 magnitudes fainter than the synthetic hosts used in the testing programme.
To illustrate this point the dashed line in Fig 5. shows the apparent magnitude of the synthetic host galaxies clined wa further 0.27 magnitudes. which clearly provides a better match to the data.
To illustrate this point the dashed line in Fig \ref{synthgals} shows the apparent magnitude of the synthetic host galaxies dimmed by a further 0.27 magnitudes, which clearly provides a better match to the data.
Lowever. the overestimate of the typical iost luminosity should be more that oll-set. by the much arger range of νοτν tackled by the modelling code during testing.
However, the overestimate of the typical host luminosity should be more that off-set by the much larger range of $L_{nuc}/L_{host}$ tackled by the modelling code during testing.
While the average Liaw(δω Ofthe quasars rom the programme is only 2.6. the code has been ested with values of οςLuo in the range 0.716.
While the average $L_{nuc}/L_{host}$ of the quasars from the programme is only $2.6$, the code has been tested with values of $L_{nuc}/L_{host}$ in the range $0\rightarrow16$.
One final measure was taken to improve the realism of the synthetic quasar images.
One final measure was taken to improve the realism of the synthetic quasar images.
The empirical. PSE which was used during (he production of the svnthetie data had an artificial centroiding shift. of ~0.01" applied to it. significantly. greater than the estimated centroiding error.
The empirical PSF which was used during the production of the synthetic data had an artificial centroiding shift of $\simeq0.01\asec$ applied to it, significantly greater than the estimated centroiding error.
This precaution was taken in light of the fact that using the same PSE to convolve both the synthetic images and. the models used in the fitting process is obviously an idealised sitdation.
This precaution was taken in light of the fact that using the same PSF to convolve both the synthetic images and the models used in the fitting process is obviously an idealised situation.
The results from the moclelling of the svnthetic quasars ave listed in Tables 1.. 2. and 3..
The results from the modelling of the synthetic quasars are listed in Tables \ref{ellips}, \ref{discs} and \ref{moreres}.
Pwo features of these results are worthy of individual comment.
Two features of these results are worthy of individual comment.
Firstly. it can be seen that for both host morphologies the errors associated. with the determination of all the parameters steadily. increase with redshift. as is expected due to inevitable drop in signal-to-noise.
Firstly, it can be seen that for both host morphologies the errors associated with the determination of all the parameters steadily increase with redshift, as is expected due to inevitable drop in signal-to-noise.
Secondly. with regards to the host scalelength it can be seen to be significantly easier to accurately determine this parameter for disc hosts than for ellipticals.
Secondly, with regards to the host scalelength it can be seen to be significantly easier to accurately determine this parameter for disc hosts than for ellipticals.
This is again as is expected. considering the dilferent behaviour of the Freeman and de Vaucouleurs surface-brightness laws in the central 21".
This is again as is expected considering the different behaviour of the Freeman and de Vaucouleurs surface-brightness laws in the central $\simeq1\asec$.
"Phe cusp-like nature of the rt! [aw at small radii inevitably leads to greater dilliculty in de-coupling the relative contributions of the host and nuclear components.
The cusp-like nature of the $r^{1/4}$ law at small radii inevitably leads to greater difficulty in de-coupling the relative contributions of the host and nuclear components.
The results of the svnthetic cata testing can be summarized as follows: where successful. morphological determination refers ο ἃ AY?>25.7 between the best-litting model of the correct morphology. and the best-fitting alternative moclel. a difference equivalent to the 99.99% confidence level for a 5-xwameter fit (Press et al.
The results of the synthetic data testing can be summarized as follows: where successful morphological determination refers to a $\Delta \chi^{2}\ge 25.7$ between the best-fitting model of the correct morphology, and the best-fitting alternative model, a difference equivalent to the $99.99\%$ confidence level for a 5-parameter fit (Press et al.
1989).
1989).
Although the high degree of accuracy achieved in these simulations is impressive. it should be noted that these error estimates are only valid for he high resolution data provided bynir.
Although the high degree of accuracy achieved in these simulations is impressive, it should be noted that these error estimates are only valid for the high resolution data provided by.
As will be seen in Section 6.. the errorsassociated with ground-based cata can be significantly larger.
As will be seen in Section \ref{tip-tilt}, the errorsassociated with ground-based data can be significantly larger.
Due to the success ofthe progranune of tests outlined above. it was felt that the level of information present in the
Due to the success ofthe programme of tests outlined above, it was felt that the level of information present in the
curves we nav therefore use Eq.
curves we may therefore use Eq.
22. together with the lower branch of Eq. 19..
\ref{Fsy} together with the lower branch of Eq. \ref{Nfc}. .
For “nine (he coefficient Qu in Eq.
For $\gamma_{\rm max} \gg \gamma_{\rm min}$ , the coefficient $Q_0$ in Eq.