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In contrast. we can also take a unique value of 0, for all clusters.
In contrast, we can also take a unique value of $\delta_{g}$ for all clusters.
We tested both methods in order to find out which one was optimal.
We tested both methods in order to find out which one was optimal.
We selected the values of 6; for each cluster by comparing the cumulative distribution functions of the values of 6 for the galaxies and those from the Monte Carlo simulations of each cluster used for normalizing the DS test.
We selected the values of $\delta_{i}$ for each cluster by comparing the cumulative distribution functions of the values of $\delta$ for the galaxies and those from the Monte Carlo simulations of each cluster used for normalizing the DS test.
These simulations broke the correlation between position and velocity of the galaxies.
These simulations broke the correlation between position and velocity of the galaxies.
Therefore. they should provide the expected values of 9 of galaxies not located in substructures.
Therefore, they should provide the expected values of $\delta$ of galaxies not located in substructures.
Three different values were selected for each cluster: the maximum value of 0 obtainec from the MC simulations (οων) and the values where the cumulative distribution function of ὁ values of the simulations was equal to 0.99 (d;49) and 0.999 (9;999).
Three different values were selected for each cluster: the maximum value of $\delta$ obtained from the MC simulations $\delta_{i,max}$ ) and the values where the cumulative distribution function of $\delta$ values of the simulations was equal to 0.99 $\delta_{i,99}$ ) and 0.999 $\delta_{i,99.9}$ ).
The number of galaxies in individual samples is sometimes too small for segregation studies.
The number of galaxies in individual samples is sometimes too small for segregation studies.
Therefore. the combination of data from many clusters will make the statistical analysis more reliable.
Therefore, the combination of data from many clusters will make the statistical analysis more reliable.
Indeed. the determination of galaxies in substructure by adopting a unique value of 6, for all clusters is based on the combination of data in an ensemble cluster.
Indeed, the determination of galaxies in substructure by adopting a unique value of $\delta_{g}$ for all clusters is based on the combination of data in an ensemble cluster.
We built an ensemble cluster by normalizing the scales and velocities for each galaxy.
We built an ensemble cluster by normalizing the scales and velocities for each galaxy.
The radial distance of each galaxy to the cluster centre was therefore scaled by the rq value for the corresponding cluster. and the relative velocity of each cluster galaxy was normalized by the velocity dispersion of the cluster.
The radial distance of each galaxy to the cluster centre was therefore scaled by the $r_{200}$ value for the corresponding cluster, and the relative velocity of each cluster galaxy was normalized by the velocity dispersion of the cluster.
As pointed out by Biviano et al. (
As pointed out by Biviano et al. (
2002). the ensemble cluster is made on the implicit assumption that the distributions of galaxy types are similar in the individual clusters.
2002), the ensemble cluster is made on the implicit assumption that the distributions of galaxy types are similar in the individual clusters.
Nevertheless. those distributions can be different for several reasons. such as different observing apertures of the clusters and different galaxy incompleteness.
Nevertheless, those distributions can be different for several reasons, such as different observing apertures of the clusters and different galaxy incompleteness.
Our ensemble cluster is free from aperture bias because all our clusters are contributing at all radial distances up to 27205.
Our ensemble cluster is free from aperture bias because all our clusters are contributing at all radial distances up to $r_{200}$.
But we are not free from possible biases due to galaxy incompleteness (see Fig.
But we are not free from possible biases due to galaxy incompleteness (see Fig.
5 in ASMOT).
5 in ASM07).
This bias was avoided by building two ensemble clusters.
This bias was avoided by building two ensemble clusters.
The first was built by those galaxies brighter than M;=—20 located in clusters at z«0.1 (hereafter ECI). and the second ensemble cluster was formed with galaxies brighter than M,=—19.0 in clusters at z«0.07 (hereafter EC2).
The first was built by those galaxies brighter than $M_{r}=-20$ located in clusters at $z<0.1$ (hereafter EC1), and the second ensemble cluster was formed with galaxies brighter than $M_{r}=-19.0$ in clusters at $z<0.07$ (hereafter EC2).
In both cases only clusters with more than 30 galaxies within 2739; contribute to. the ensemble clusters.
In both cases only clusters with more than 30 galaxies within $r_{200}$ contribute to the ensemble clusters.
Taking into account all previous restrictions. EC] was built with 2593 galaxies from 44 galaxy clusters. and EC? was formed by 2400 galaxies from 34 clusters.
Taking into account all previous restrictions, EC1 was built with 2593 galaxies from 44 galaxy clusters, and EC2 was formed by 2400 galaxies from 34 clusters.
A global value for 6, was determined by analysing the cumulative distribution function of the 9 values of the Monte Carlo simulations used in the normalization of the DS test.
A global value for $\delta_{g}$ was determined by analysing the cumulative distribution function of the $\delta$ values of the Monte Carlo simulations used in the normalization of the DS test.
We selected two values of 9, for which the cumulative 0 distribution function of the MC simulations was equal to 0.95 (0,03) and 0.99 (0,55).
We selected two values of $\delta_{g}$ for which the cumulative $\delta$ distribution function of the MC simulations was equal to 0.95 $\delta_{g,95}$ ) and 0.99 $\delta_{g,99}$ ).
For our two ensemble clusters these values turned to be 0,95 21.98 and 2.03 and 6,59 22.7 and 3.0 for EC] and EC2. respectively.
For our two ensemble clusters these values turned to be $\delta_{g,95}=$ 1.98 and 2.03 and $\delta_{g,99}=$ 2.7 and 3.0 for EC1 and EC2, respectively.
Galaxies with 6 values larger than these global values were considered as galaxies i substructures.
Galaxies with $\delta$ values larger than these global values were considered as galaxies in substructures.
Note that our 0,95 value is similar to that adoptec by Biviano et al. (
Note that our $\delta_{g,95}$ value is similar to that adopted by Biviano et al. (
2002).
2002).
We have used the MC simulated clusters reported in Sec.
We have used the MC simulated clusters reported in Sec.
3.1 for determining the best value of ὃς for detecting galaxies i substructures.
3.1 for determining the best value of $\delta_{c}$ for detecting galaxies in substructures.
The substructure in the simulated clusters were
The substructure in the simulated clusters were
of explaining the dimmess of nearby galactic nuclei are required (Menou Quataert 2001: Naravan 2002). bevond the specilic scenario outlined here for the giant. flare of NGC 5905.
of explaining the dimness of nearby galactic nuclei are required (Menou Quataert 2001; Narayan 2002), beyond the specific scenario outlined here for the giant flare of NGC 5905.
Either the mass must acerete in a radiatively inefficient mode or the accretion must be suppressed or slowed down significantly.
Either the mass must accrete in a radiatively inefficient mode or the accretion must be suppressed or slowed down significantly.
The authors gratefully thank Stefanie Ixomossa for kindly. providing theROSAT data listed in Table 1 along with the conversion [actors from count rate to X-ray Iuminositv.
The authors gratefully thank Stefanie Komossa for kindly providing the data listed in Table 1 along with the conversion factors from count rate to X-ray luminosity.
The authors also thank. Jeremy. Goodman. Boldan Paczvisski and the referee for helplul commentis.
The authors also thank Jeremy Goodman, Bohdan Paczyńsski and the referee for helpful comments.
LXL and RN thank the Institute for Advanced Study ancl the Department of Astrophysical Sciences. Princeton. for hospitality while this work was being done.
LXL and RN thank the Institute for Advanced Study and the Department of Astrophysical Sciences, Princeton, for hospitality while this work was being done.
LXL’s and IMs research was supported by NASA through Chandra Postdoctoral Fellowship graat numbers PFE1-20018 (LAL) and PE9-10006 (IXM). awarded by the Chandra X-ray. Center. which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NASS-39073.
LXL's and KM's research was supported by NASA through Chandra Postdoctoral Fellowship grant numbers PF1-20018 (LXL) and PF9-10006 (KM) awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-39073.
RN's research was supported in part by NSF erant. AST-03206806.
RN's research was supported in part by NSF grant AST-9820686.
After cirenlarization. the fallback material from a tidal disruption event will form a torus al a radius r~2ryp.
After circularization, the fallback material from a tidal disruption event will form a torus at a radius $r\sim2r_T$.
The torus will then spread out. viscously anc accrete onto the black hole.
The torus will then spread out viscously and accrete onto the black hole.
The time-scale for this stage of the evolution is determined by (he viscous time-scale (Cannizzo.Lee.&Goodman1990:Ulmer1999) where Γκορ 15 Lhe IXeplerian orbital period. a is the standardviscosity parameter 1973)... and Ph is the ratio of the disk height to radius.
The time-scale for this stage of the evolution is determined by the viscous time-scale \citep{can90,ulm99} where $t_{\rm Kep}$ is the Keplerian orbital period, $\alpha$ is the standardviscosity parameter \citep{sha73}, and $h$ is the ratio of the disk height to radius.
It is easv to cheek (that [or the case of the flare in NGC 5905. where Los~LOπαςMy/10*M.)|. the accretion disk would correspond to the regime of the "middle clisk” in which electron scattering opacity dominates over (he Kramers opacity and gas pressure dominates over radiation pressure (Shakira&Sunvaev1973:NovikovThorneFrank.KingRaine 1992).
It is easy to check that for the case of the flare in NGC 5905, where $L_{\rm peak} \sim 10^{-3} L_{\rm Edd} (M_H/10^7 M_\odot)^{-1}$, the accretion disk would correspond to the regime of the “middle disk” in which electron scattering opacity dominates over the Kramers opacity and gas pressure dominates over radiation pressure \citep{sha73,nov73,fkr92}. .
. Then. P is estimaled to be
Then, $h$ is estimated to be
. . . ⊾↔↿↓⋅∪⊔⋏∙≟⋜⋯∠⇂∖⇁⋜⊔⋅↓⋜↧∣⋡↓⋖⋅⇂↓⊔⋖⋅⋜⊔⋅↓≻∪↓⋜⊔⋅↓⊳∖⋜∐↓∪⊔↓⊳∖⋜↧∠⇂⋖⊾∐⊔↓⊔⋏∙≟"AN . ⋅⊀ property of⋅ BL. Lacs. which⊀ unavoidably⊀ associates. the observed emission with beamed svnchrotron radiation [rom a relativistic jet viewed face-on.
Strong and variable linear polarisation is a defining property of BL Lacs, which unavoidably associates the observed emission with beamed synchrotron radiation from a relativistic jet viewed face-on.
Phe polarimetric properties of these sources have been thoroughly studied at. racio ancl optical wavelengths for over three decades. rich MR(c.g. Angel&Stockman1980. ...ancl AMSaikia&Salter1988)).
The polarimetric properties of these sources have been thoroughly studied at radio and optical wavelengths for over three decades, displaying rich phenomenology (e.g. \citealt{b0} and \citealt{saik}) ).
Theinner jets of active present a morphology Nnrisecl by a stationary region ofenhanced brightness.In the "core". and other luminous components ("knots") moving© at relativistic‘ speeds1 ‘and thought? to be associated with the propagation of shock perturbations.
The inner jets of active galaxies present a morphology characterised by a stationary region of enhanced brightness, the “core”, and other luminous components (“knots”) moving at relativistic speeds and thought to be associated with the propagation of shock perturbations.
‘These structures tend to be highly polarised in radio and are widely. recognised ax potential sites of particle. acceleration. and as responsible for the observed (ux variability Luehesetal.1989).
These structures tend to be highly polarised in radio and are widely recognised as potential sites of particle acceleration and as responsible for the observed flux variability \citep{hughes}.
.the jetCore brightening and the appearance of new knotsin have been linked to [aring activity extending to gamma-ray energies (Jorstadctal.
Core brightening and the appearance of new knots in the jet have been linked to flaring activity extending to gamma-ray energies \citep{jorstad01}.
200T These shocked. regions are persistent and bright | ≻↿↓⋅⇂⇂≼⇍↿⇂⇂↓⋅⋖⊾≻↕↓↥∣↓↕⋖⊾⇀∖−↓⋅⋜↧∙∖⇁⊀↓⊔↓⋜↧⋏∙≟⋖⋅⊳∖∪⇂⋅⊔↓⊀↓⊳∖−⋜↧↓⊀↓⋏∙≟⊔⋖⊾∠⇂↓≻≼∼−⊳∖≼∼⋜↧↓⋖⋅≯↕⋖⋅↥≱∖⋡ and have also been invoked to explain the quiescent level of emission observed om some blazars at these energies (e.g. Ciebelsetal.2002)).
These shocked regions are persistent and bright structures in the X-ray images of mis-aligned pc-scale jets, and have also been invoked to explain the quiescent level of emission observed from some blazars at these energies (e.g. \citealt{b5}) ).
"na In. meblazars. these knots are not resolveddue to the nt of thejet analogyto the line of sight.. but their existence is implied by with similar objects. such as M S87 (Marshalletal.
In blazars, these knots are not resolved due to the close alignment of the jet to the line of sight, but their existence is implied by analogy with similar objects, such as M 87 \citep{marshall}.
2002)... Despite the [act that in mis-alignecl objects the knots are responsible for only a fraction of the Dux. emitted. from the source. the geometrical. alignment. in. blazars provides. the recuired. amount of Doppler boos1ng. necessary CO produce the low-level of⋅ continuous. emissionMN observed. (Ciebels»etal.
Despite the fact that in mis-aligned objects the knots are responsible for only a fraction of the flux emitted from the source, the geometrical alignment in blazars provides the required amount of Doppler boosting necessary to produce the low-level of continuous emission observed \citep{b5}.
2002) lxatarzvüski:.ctal.(2008). have recently. modeled. the fulli spectral(bpne àenergyTEH distribution"u1 (SED)In of PISS BENE2155-304κ andx identified the presence of such a background. svnchrotron component. which is associated with an extended jet component (presumably the integrated contribution from all X-rav-bright knots along the jet) capable of∙ sustaining14 the low state X-ray [lux observed from the source.
\cite{kat} have recently modeled the full spectral energy distribution (SED) of PKS 2155-304 and identified the presence of such a background synchrotron component, which is associated with an extended jet component (presumably the integrated contribution from all X-ray-bright knots along the jet) capable of sustaining the low state X-ray flux observed from the source.
At verv-hieh energies (VILE). consistent detection of the BL Lac PIAS 2155-304 bv the LESS. telescopes has also established a
At very-high energies (VHE), consistent detection of the BL Lac PKS 2155-304 by the H.E.S.S. telescopes has also established a
(2010),, who suggest that macroscopic coronal jets can be scaled down to spicule-size features.
, who suggest that macroscopic coronal jets can be scaled down to spicule-size features.
We present a case study of two EEs to demonstrate the conflict with the standard bi-directional jet model and to stress the enigmatic discrepancy of lacking apparent motion.
We present a case study of two EEs to demonstrate the conflict with the standard bi-directional jet model and to stress the enigmatic discrepancy of lacking apparent motion.
As a solution of this conflict we suggest — backed up by observational evidence for helicity in spicules — that a spinning motion may be the source of EEs.
As a solution of this conflict we suggest – backed up by observational evidence for helicity in spicules – that a spinning motion may be the source of EEs.
Combining the hypothetical concept of spinning spicules with the observation of quasi-stationary Doppler-flow in EEs could be the solution of the conflict.
Combining the hypothetical concept of spinning spicules with the observation of quasi-stationary Doppler-flow in EEs could be the solution of the conflict.
In the period from Nov 12-119, 2010, SUMER ran a campaign to observe sunspots in TR emission lines.
In the period from Nov 19, 2010, SUMER ran a campaign to observe sunspots in TR emission lines.
We report two cases of EEs found outside, but in the neighbourhood of a sunspot on Nov 16 and on Nov 19, referred to as EE! and EE2.
We report two cases of EEs found outside, but in the neighbourhood of a sunspot on Nov 16 and on Nov 19, referred to as EE1 and EE2.
On Nov 16, 2010 SUMER observed the leading sunspot of active region 11124.
On Nov 16, 2010 SUMER observed the leading sunspot of active region 11124.
The slit of size 0.3"x was placed in such a way that during one hour the drift by the solar rotation would allow to image the entire spot.
The slit of size $\times$ was placed in such a way that during one hour the drift by the solar rotation would allow to image the entire spot.
A spectral window around the optically thin emission line of at 12.06 nm was read out at a cadence of 10 s. Standard data reduction procedures were applied to process the data set.
A spectral window around the optically thin emission line of at 12.06 nm was read out at a cadence of 10 s. Standard data reduction procedures were applied to process the data set.
In Fig.1 we show the drift scan as y—t plot (top), the 2—{ plot (below top) and line profiles in pixel 42 as indicated by the dashed line.
In Fig.1 we show the drift scan as $y-t$ plot (top), the $\lambda-t$ plot (below top) and line profiles in pixel 42 as indicated by the dashed line.
At this location in the plage area very close to the sunspot, a rapid brightness increase by a factor of >20 is observed at time step 9].
At this location in the plage area very close to the sunspot, a rapid brightness increase by a factor of $\ge 20$ is observed at time step 91.
The pre-event profiles have been averaged and three more profiles are shown through the event.
The pre-event profiles have been averaged and three more profiles are shown through the event.
The timing is indicated by blue arrows.
The timing is indicated by blue arrows.
Interestingly, the spectral line seems to split into two main components that are symmetrically shifted by 40 km/s towards the red and towards the blue with additional components at +100 km/s that are less strong.
Interestingly, the spectral line seems to split into two main components that are symmetrically shifted by 40 km/s towards the red and towards the blue with additional components at $\pm$ 100 km/s that are less strong.
The lightcurve is not flat, it has two maxima that are separated by ~120 s, but the overall shape with four peaks does not change over more than three minutes.
The lightcurve is not flat, it has two maxima that are separated by $\approx$ 120 s, but the overall shape with four peaks does not change over more than three minutes.
A similar observation with EE2 was completed on Nov 19, 2010, when the instrument was pointed to the leading sunspot in AR 11126.
A similar observation with EE2 was completed on Nov 19, 2010, when the instrument was pointed to the leading sunspot in AR 11126.
Again, a stationary double-component EE with velocities of +35 km/s is observed from 21:53:14 to 21:57:14 in a plage location.
Again, a stationary double-component EE with velocities of $\pm$ 35 km/s is observed from 21:53:14 to 21:57:14 in a plage location.
Similar to the case of BEI, the brightness jumps by a factor of 10 and the lightcurve is double-peaked (cf.,
Similar to the case of EE1, the brightness jumps by a factor of 10 and the lightcurve is double-peaked (cf.,
Fig.2).
Fig.2).
During both events the Sun has rotated by ~0.4” which is significantly below the spatial resolution of SUMER of 1.5".
During both events the Sun has rotated by $\approx$ 0.4" which is significantly below the spatial resolution of SUMER of 1.5".
As a by-product of this study we identified two emission lines that were also recorded in the window and not included in the SUMER spectral atlas (Curdtetal.,2001) as lines.
As a by-product of this study we identified two emission lines that were also recorded in the window and not included in the SUMER spectral atlas \citep{Curdt01} as lines.
In the atlas the window was recorded on the bare photocathode, while in this data set we could place it onto the KBr coated photocathode.
In the atlas the window was recorded on the bare photocathode, while in this data set we could place it onto the KBr coated photocathode.
All lines at 120.204 nm, 120.261 nm, 120.344 nm, 120.435 nm,j120.559 nm, 120.613 nm, 120.704 nm, 120.776 nm, 120.886 nm, 121.122 nm, and 121.018 nm are present in SUMER spectra.
All lines at 120.204 nm, 120.261 nm, 120.344 nm, 120.435 nm,120.559 nm, 120.613 nm, 120.704 nm, 120.776 nm, 120.886 nm, 121.122 nm, and 121.018 nm are present in SUMER spectra.
background: subtractions.
background subtractions.
Two cillerent PSE subtraction stags were observed for cach target. although with much longer intervals than is ideal due to time constraints.
Two different PSF subtraction stars were observed for each target, although with much longer intervals than is ideal due to time constraints.
Lt became apparent that the PSE stability was poor so that subtractions across timescales greater than 5 minutes were contaminated with many AO residuals.
It became apparent that the PSF stability was poor so that subtractions across timescales greater than 5 minutes were contaminated with many AO residuals.
Fig.
Fig.
15— shows this PSE change over time. taken from. J-band. images of 11D141569.
\ref{residuals} shows this PSF change over time, taken from -band images of HD141569.
Due to the Limited time. nothing of interest was uncovered in data taken on AIWC297.
Due to the limited time, nothing of interest was uncovered in data taken on MWC297.
However the PSE star chosen for MAVC?97 revealed a group of 4 stars in close proximity (see Fig. 16((
However the PSF star chosen for MWC297 revealed a group of 4 stars in close proximity (see Fig. \ref{psf5}( (
a)). with the closest being 1.6 areseconds from the central PSE star.
a)), with the closest being 1.6 arcseconds from the central PSF star.
No olf-mask images were taken for this object since it was originally only to be used as a PSE subtraction star. so only rough estimates of the A-magnitude were possible.
No off-mask images were taken for this object since it was originally only to be used as a PSF subtraction star, so only rough estimates of the -magnitude were possible.
Phe oecultecl profile was compared to that of an un-maskecl Hi standard star and sealed so that the wings closely matched.
The occulted profile was compared to that of an un-masked IR standard star and scaled so that the wings closely matched.
"This scale factor (corrected for integration time) was then used directly with the LR standard star magnitude and applied to the usual maenituce-Lusx relation to obtain a value of 8.9.
This scale factor (corrected for integration time) was then used directly with the IR standard star magnitude and applied to the usual magnitude-flux relation to obtain a value of 8.9.
The Α-magnitude estimate for the closest star is 122403 a value for the Hux contribution from the central star has been subtracted ancl was estimated by plotting radial averages about the star.
The }-magnitude estimate for the closest star is $12.2 \pm 0.3$ – a value for the flux contribution from the central star has been subtracted and was estimated by plotting radial averages about the star.
Phe central star ancl the outermost two stars in this image are listed in the latest Two Micron All Sky Survey (2ALASS) catalogue of point sources.
The central star and the outermost two stars in this image are listed in the latest Two Micron All Sky Survey (2MASS) catalogue of point sources.
This lists DD-04 4476 as having aA magnitude of 8.5 and the outer two stars 12.6 and. 11.3. respectively.
This lists BD-04 4476 as having a magnitude of 8.5 and the outer two stars 12.6 and 11.3 respectively.
Taking into account the estimates involved. with the focal stop and that 2ALASS cannot resolve the inner two stars. our measurements appear to be reasonable.
Taking into account the estimates involved with the focal stop and that 2MASS cannot resolve the inner two stars, our measurements appear to be reasonable.
An upgrade to OSCA was carried out in April 2003.
An upgrade to OSCA was carried out in April 2003.
Phe Gaussian occulting masks were installed along with a razor eclecd anti-scatter mask in front of the focal plane substrates (to reduce scattering from the edges of substrates on which the occulting spots are deposited).
The Gaussian occulting masks were installed along with a razor edged anti-scatter mask in front of the focal plane substrates (to reduce scattering from the edges of substrates on which the occulting spots are deposited).
Phe whole of ΟΡ Αννας also moved. and installed: at GRACE (a new. environment controlled laboratory on one of the Nasmyth. platforms on the WIPP).
The whole of OSCA was also moved and installed at GRACE (a new, environment controlled laboratory on one of the Nasmyth platforms on the WHT).
Fhis should alleviate previous problems of dust contamination and temperature problems for NAOMI.
This should alleviate previous problems of dust contamination and temperature problems for NAOMI.
OSCA is a high precision stellar. coronagraph. produced on a low budget. over a short timescale ancl mecting all the design specifications.
OSCA is a high precision stellar coronagraph, produced on a low budget, over a short timescale and meeting all the design specifications.
However. due to the limited time assigned For the commissioning and the overlap with NAOMI engineering schedules. a complete and thorough testing of OSCA has not been possible anc as a result. there have been no performance tests cone with OSCA in optimum seeing conditions«nd optimum alignment (both of OSCA and other instrumentation).
However, due to the limited time assigned for the commissioning and the overlap with NAOMI engineering schedules, a complete and thorough testing of OSCA has not been possible and as a result there have been no performance tests done with OSCA in optimum seeing conditions optimum alignment (both of OSCA and other instrumentation).
The mechanies and electronics of OSCA have operated consistently to date and succeed in maintaining the required »ositioning and alignment. including that for the Lyot stop rotation.
The mechanics and electronics of OSCA have operated consistently to date and succeed in maintaining the required positioning and alignment, including that for the Lyot stop rotation.
The deplovment mechanism for OSCA has proven ο be very successtul: it allows OSCA to be raised in to (and out of) the beam very (quickIy and with consistently accurate »oxitioning. allowing for a llexible anc varied observing oxogram over the course of a night.
The deployment mechanism for OSCA has proven to be very successful; it allows OSCA to be raised in to (and out of) the beam very quickly and with consistently accurate positioning, allowing for a flexible and varied observing program over the course of a night.
Simulations of the N[XOME and OSCA system also wave relevance for the next generation of extremely large clescopes where high contrast imagine is essential in he search for extra-solar. planets.
Simulations of the NAOMI and OSCA system also have relevance for the next generation of extremely large telescopes where high contrast imaging is essential in the search for extra-solar planets.
When designing a coronagraphie svsteni for a highly segmented aperture suitable masking in the Lyot (pupil) plane must be devised ο counteract the strong diffraction pattern that will result otherwise - reducing suppression performance and confusing he data.
When designing a coronagraphic system for a highly segmented aperture suitable masking in the Lyot (pupil) plane must be devised to counteract the strong diffraction pattern that will result otherwise - reducing suppression performance and confusing the data.