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However. the 92 cin nuage in Fi | However, the 92 cm image in Fig. |
e. 9 has a resolution of 15 arcsec or 71 kpe projected ou the aue of the sky. | \ref{Fig. 9} has a resolution of 45 arcsec or 74 kpc projected on the plane of the sky. |
Gaps in the emission of this size would not be detected. | Gaps in the emission of this size would not be detected. |
Taking a jetspeed of (Le (a tvpica spced. for conipact sviunietric objects on similar scales - Owsiauk Conway 1998: Tschager et al. 20001). | Taking a jetspeed of $0.1c$ (a typical speed for compact symmetric objects on similar scales - Owsianik Conway \cite{owsianik}; Tschager et al. \cite{tschager}) ), |
anc asstmune that we acually see the jet and not the backflow ina thivlobe. we would not detect “off periods in jet activity asting less an 2<109 vears. | and assuming that we actually see the jet and not the backflow in a thin lobe, we would not detect 'off' periods in jet activity lasting less than $2\times 10^6$ years. |
This period is louger thau the pxhalle cheth of fje preseut "ou period represeuted |wt je kpe ‘ontral component. 10!10" vers. | This period is longer than the probable length of the present `on' period represented by the kpc central component, $10^4 - 10^5$ years. |
The ον]enucc| from je structure to the NW points more towSC jisocic rather than continuous activity. | The evidence from the structure to the NW points more towards episodic rather than continuous activity. |
Iu the ceutral siloWISE, je jet ds raceable via a number of knots on 1sway roni the uucleus via component DI out to the WIluspot oei component A at a distance of ~1.2 kpc. | In the central kiloparsec, the jet is traceable via a number of knots on its way from the nucleus via component B1 out to the warmspot in component A at a distance of $\sim 1.2$ kpc. |
Iusufficieut sensitivitv παν nuit our ability to detect more of he jet on these su»ealactie scales. | Insufficient sensitivity may limit our ability to detect more of the jet on these sub-galactic scales. |
Ou larger scales. tle cussion extends ~ 1.1pe in what appears to be a more relaxed jet than its well-collimated counterpart to the SE. | On larger scales, the emission extends $\sim 1.4$ Mpc in what appears to be a more relaxed jet than its well-collimated counterpart to the SE. |
In the 21 cum mage made by Barthel et al. ( | In the 21 cm image made by Barthel et al. ( |
1985) there is a pronünent featre in the NW structure which suggests that the enerev supply may have been variable. | 1985) there is a prominent feature in the NW structure which suggests that the energy supply may have been variable. |
At 92 cii | At 92 cm (Fig. |
(Fig. 9 bottoiu) aud at 19 ci (Mack et al. | \ref{Fig. 9} bottom) and at 49 cm (Mack et al. |
1997). there Is onissjon sout rand west of the main radio axis to the NW. | 1997), there is emission south and west of the main radio axis to the NW. |
The originOo of this emission is unclear. | The origin of this emission is unclear. |
Double-double radio galaxies (Ixadser et al. 20003) | Double-double radio galaxies (Kaiser et al. \cite{kaiser}) ) |
appear o provide good evidence that activity in ACNs ca1i be recurrent. | appear to provide good evidence that activity in AGNs can be recurrent. |
Prestmably these are objects in which the ou-off evceles are couparable. | Presumably these are objects in which the `on-off' cycles are comparable. |
There may be a wide rage o duty cycles: auxmest ACNs: 30236 may be an exinuple of a sotree Which is occasionally "off. perhaps due to fre jet channel collapsing or he flow being blocked x interaction wi ha cloud or a dicyp in supply of fucl to he ceutral black tole. | There may be a wide range of duty cycles amongst AGNs; 3C236 may be an example of a source which is occasionally `off', perhaps due to the jet channel collapsing or the flow being blocked by interaction with a cloud or a drop in supply of fuel to the central black hole. |
The central structure in 3C'236 may relect t1ο normal level of activity iu the nucleiIn. | The central structure in 3C236 may reflect the normal level of activity in the nucleus. |
Mac set al. (1 995)) | Mack et al. \cite{mack2}) ) |
and Schoeninakers et al. (2000)) | and Schoenmakers et al. \cite{schoenmakers}) ) |
lave Osnuated tie age of 30236 from svuchrotron loss uodels aud spectral aging as ~105 vears. | have estimated the age of 3C236 from synchrotron loss models and spectral aging as $\sim 10^8$ years. |
The latter authors also estimate the speed of advance of the western jet iuto the interealactic media as 0.1 c. This speed is at the lower Linu of what can be measured with VLBI Or conipact jets in the nucleus (eg. | The latter authors also estimate the speed of advance of the western jet into the intergalactic medium as 0.1 c. This speed is at the lower limit of what can be measured with VLBI for compact jets in the nucleus (eg. |
Owsianils Comway L998.. Tschager et al. 2000)). | Owsianik Conway \cite{owsianik}, , Tschager et al. \cite{tschager}) ). |
region representing the objects with an additional SB component. | region representing the objects with an additional SB component. |
The plain (dashed) line anc gravecd (black) region correspond to the COSMOS (ELAS) sample. | The plain (dashed) line and grayed (black) region correspond to the COSMOS (ELAIS) sample. |
Again. the existence of such a component can be. in general. well constrained only in the presence. of data points longware A=24pm and this is valid for only and of COSMOS and LELAIS samples. respectively. | Again, the existence of such a component can be, in general, well constrained only in the presence of data points longward $\lambda=24$ and this is valid for only and of COSMOS and ELAIS samples, respectively. |
We will now attempt to put all the results from the various AGN samples together and construct a common description of their dust. properties. | We will now attempt to put all the results from the various AGN samples together and construct a common description of their dust properties. |
“Lo this end. we will first. present a summary of the results of Paper 1. that will also be used in this combined study. | To this end, we will first present a summary of the results of Paper 1, that will also be used in this combined study. |
The Iow-z simple will be exelucded from this analysis. because of the unconfirmed (stellar vs. starburst) nature of the objects. | The $z$ sample will be excluded from this analysis, because of the unconfirmed (stellar vs. starburst) nature of the objects. |
They will be taken into account. however. when discussing the star formation. as the results on this issue seem to be more robust. and only | They will be taken into account, however, when discussing the star formation, as the results on this issue seem to be more robust, and only |
The first point to make from Fig. | The first point to make from Fig. |
2 is that simulated ULX continua seem perfectly capable of generating optical line ratios observed in transition-type objects and LINERs. | \ref{fig:o3o1} is that simulated ULX continua seem perfectly capable of generating optical line ratios observed in transition-type objects and LINERs. |
The ULX ionizing continuum must include some FUV (~1- 10Ryd) in order to produce [Ο1]/Πα ratios in the correct range, but apart from this the simulated line ratios do not depend very strongly on the continuum shape. | The ULX ionizing continuum must include some FUV $\sim$ 1-10Ryd) in order to produce $[O_{I}]/H_{\alpha}$ ratios in the correct range, but apart from this the simulated line ratios do not depend very strongly on the continuum shape. |
The second point from Fig. | The second point from Fig. |
2 is that ULX black hole mass can determine whether the optical line ratio is transition-like or LINER-like. | \ref{fig:o3o1} is that ULX black hole mass can determine whether the optical line ratio is transition-like or LINER-like. |
For example, a blackbody temperature of 5x10°K, corresponds to emission from an accretion disk around a 10Mo black hole accreting near Eddington luminosity and generates a line ratio (middle point on solid curve) in the middle of the transition object region. | For example, a blackbody temperature of $5\times 10^{6}$ K, corresponds to emission from an accretion disk around a $\sim 10M_{\odot}$ black hole accreting near Eddington luminosity and generates a line ratio (middle point on solid curve) in the middle of the transition object region. |
By contrast, a blackbody temperature of 2x 10°K corresponds to an accretion disk around a 10?M5 black hole and generates a line ratio (rightmost point on solid curve) in the LINER region. | By contrast, a blackbody temperature of $2\times 10^{6}$ K corresponds to an accretion disk around a $\sim 10^{3}M_{\odot}$ black hole and generates a line ratio (rightmost point on solid curve) in the LINER region. |
From Fig. 2,, | From Fig. \ref{fig:o3o1}, |
the ’radio quiet’ L2 and T2s have [O1]/Ha< 0.2, so if they are powered by ’soft-high’ state ULXs as we suggested in McKernanetal.(2010),, the black hole masses must be «10?M and some FUV continuum is required (possibly from star formation). | the 'radio quiet' L2 and T2s have $[O_{I}]/H_{\alpha}<0.2$ , so if they are powered by 'soft-high' state ULXs as we suggested in \citet{b98}, the black hole masses must be $<10^{3}M_{\odot}$ and some FUV continuum is required (possibly from star formation). |
We will carry out more detailed simulations in the future to understand the limits on optical line ratios for different values of log U, the absorbing column and different ionizing continua, nevertheless for the purposes of this Letter, ULXs can in principle generate optical line ratios observed in LINER and transition-type nuclei. | We will carry out more detailed simulations in the future to understand the limits on optical line ratios for different values of log U, the absorbing column and different ionizing continua, nevertheless for the purposes of this Letter, ULXs can in principle generate optical line ratios observed in LINER and transition-type nuclei. |
Recently Gonzalez-Martinetal.(2009) claimed that nuclear X-ray emission in LINERs could not be due to high mass XRBs since populations of young stars in these nuclei are generally ruled out. | Recently \citet{b22} claimed that nuclear X-ray emission in LINERs could not be due to high mass XRBs since populations of young stars in these nuclei are generally ruled out. |
Of course, as discussed above, it is not necessary to have populations of young stars to account for X-ray observations of low luminosity galactic nuclei. | Of course, as discussed above, it is not necessary to have populations of young stars to account for X-ray observations of low luminosity galactic nuclei. |
Ptaketal.(2006) find that X-ray/optical flux ratios for optical counterparts to ULXs are generally consistent with LMXB in clusters. | \citet{b17} find that X-ray/optical flux ratios for optical counterparts to ULXs are generally consistent with LMXB in clusters. |
Furthermore, in M31, the distribution of variable X-ray point sources in the innermost ~ 450pc may be consistent with an ageing population of low mass XRBs (Kaaret2002). | Furthermore, in M31, the distribution of variable X-ray point sources in the innermost $\sim 450$ pc may be consistent with an ageing population of low mass XRBs \citep{b36}. |
. Therefore, integrating over the contributions from low mass XRBs is perfectly capable of powering nuclear X-ray emission for Gyrs and potentially generating a LINER- or transition object-like appearance. | Therefore, integrating over the contributions from low mass XRBs is perfectly capable of powering nuclear X-ray emission for Gyrs and potentially generating a LINER-like or transition object-like appearance. |
Although low mass likeXRBs tend to be transient, they can actually dominate the XLF with reasonable choice of duty cycles (Piro&Bildsten2002). | Although low mass XRBs tend to be transient, they can actually dominate the XLF with reasonable choice of duty cycles \citep{b38}. |
. For example, a choice of outburst rate (O.R.)~10% during ~75% of the lifetime of XRBs is a reasonable estimate for the nucleus of Cen A (Piro&Bildsten 2002). | For example, a choice of outburst rate $\sim 10\%$ during $\sim 75\%$ of the lifetime of XRBs is a reasonable estimate for the nucleus of Cen A \citep{b38}. |
. Munoetal.(2005a) suggest O.R.~1% for an estimated population of ~10—10? binaries within « 1pc of SgrA* could account for XRT observations. | \citet{b83} suggest $\sim 1\%$ for an estimated population of $\sim
10-10^{3}$ binaries within $<1$ pc of SgrA* could account for XRT observations. |
ULXs if unbeamed could have duty cycles as high as ~1096 (Kingetal. 2001).. | ULXs if unbeamed could have duty cycles as high as $\sim 10\%$ \citep{b85}. |
We should expect (at least) several low mass XRBs in ~0.5—1" X-ray observations of most galactic nuclei. | We should expect (at least) several low mass XRBs in $\sim 0.5-1''$ X-ray observations of most galactic nuclei. |
Nuclear ULXs, like that in M82 should occur with moderate levels of star formation in the nucleus, although ULXs are observed in early-type galaxies at a rate of a few per galaxy (e.g.Fabbiano&White2003). | Nuclear ULXs, like that in M82 should occur with moderate levels of star formation in the nucleus, although ULXs are observed in early-type galaxies at a rate of a few per galaxy \citep[e.g.][]{b41}. |
. Indeed the mass of the ULX in M82 suggests that it is cannibalizing its host cluster or has captured companions. | Indeed the mass of the ULX in M82 suggests that it is cannibalizing its host cluster or has captured companions. |
Another possible inconsistency between LINER X-ray emission and ULX or XRB emission is the XLF of LINER nuclei (Gonzalez-Martinetal.2009). | Another possible inconsistency between LINER X-ray emission and ULX or XRB emission is the XLF of LINER nuclei \citep{b22}. |
. However, the sample size (82) of Gonzalez-Martinetal. is limited (see (Kim&Fabbiano2004) for discussion of the dangers of this). | However, the sample size (82) of \citet{b22} is limited (see \citep{b23} for discussion of the dangers of this). |
Furthermore, their cumulative power-law indices (~—0.2, —0.8) before and after the power-law break are actually not that different from the power-law indices of XRBs at low luminosities (~—0.8) in (Kim&Fabbiano2004) or even from M31 (Kongetal. 2002), although these steepen at higher luminosities. | Furthermore, their cumulative power-law indices $\sim -0.2,-0.8$ ) before and after the power-law break are actually not that different from the power-law indices of XRBs at low luminosities $\sim -0.8$ ) in \citep{b23} or even from M31 \citep{b28}, although these steepen at higher luminosities. |
A much larger LINER sample is evidently required for a reliable understanding of the LINER XLF. | A much larger LINER sample is evidently required for a reliable understanding of the LINER XLF. |
The UV band is important in our discussion, since emission from an accretion disk around supermassive black holes should peak in the UV band. | The UV band is important in our discussion, since emission from an accretion disk around supermassive black holes should peak in the UV band. |
Maozetal(2005) found evidence for UV variability in LINER 1s and LINER 2s. | \citet{b29} found evidence for UV variability in LINER 1s and LINER 2s. |
However of the five LINER 2s in Maozetal(2005) without a compact radio core, none varied at >9596 confidence and three of the five radio-quiet LINER 2s (NGC 3486, NGC 4569 and NGC 5055 at 9,1 and 8Mpc distant respectively) were consistent with no UV variation whatsoever (Maozetal 2005).. | However of the five LINER 2s in \citet{b29} without a compact radio core, none varied at $>95\%$ confidence and three of the five radio-quiet LINER 2s (NGC 3486, NGC 4569 and NGC 5055 at 9,1 and 8Mpc distant respectively) were consistent with no UV variation whatsoever \citep{b29}. |
This suggests that hot stars rather than AGN are powering the UV emission in radio-quiet LINER 2s. | This suggests that hot stars rather than AGN are powering the UV emission in radio-quiet LINER 2s. |
X-ray imaging of LINERs reveals that extended emission or complex clumpy emission is common in LINER 2 nuclei. | X-ray imaging of LINERs reveals that extended emission or complex clumpy emission is common in LINER 2 nuclei. |
Extended emission can be explained in a nuclear ULX modelby several ULXs/XRBs in a nucleus, in a region of hot massive stars. | Extended emission can be explained in a nuclear ULX modelby several ULXs/XRBs in a nucleus, in a region of hot massive stars. |
In a small sample of L2 and T2 nuclei, around half showed clear evidence for extended emission | In a small sample of L2 and T2 nuclei, around half showed clear evidence for extended emission |
Taam. White Lost) and (Alaldsishimiaetal.1982) have not been observed to varv systematically with the persistent fux. so we cannot predict bow observing bursts at low AZ du slow sources would affect our correlations. | Taam, White 1984) and \citep{mak82}
have not been observed to vary systematically with the persistent flux, so we cannot predict how observing bursts at low $\dot M$ in slow sources would affect our correlations. |
We have found that oscillations from the 6 fast burst oscillation sources are tightly connected to plotospheric radius expansion. whereas oscillations from the 23 slow sources are about equally likely to be found iu bursts both with aud without radius expansion. | We have found that oscillations from the 6 fast burst oscillation sources are tightly connected to photospheric radius expansion, whereas oscillations from the 3 slow sources are about equally likely to be found in bursts both with and without radius expansion. |
What drives this correlation remains to be determined: is it the burst properties themselves. the oscillation frequencies. or ποιο nuscen third parameter? | What drives this correlation remains to be determined: is it the burst properties themselves, the oscillation frequencies, or some unseen third parameter? |
According to the beat frequency model of kz QPOs.the fact that zai&Amey for the "low? sources whereas MigretC2AM for the fast? ones can be accounted for if one or two autipodal hot spots ou the surface of the rotating neutron star are visible to the observer (Miller et 11998). | According to the beat frequency model of kHz QPOs,the fact that $\nu_{\rm burst}\simeq \Delta\nu_{\rm kHz}$ for the “slow” sources whereas $\nu_{\rm burst}\simeq
2\Delta\nu_{\rm kHz}$ for the “fast” ones can be accounted for if one or two antipodal hot spots on the surface of the rotating neutron star are visible to the observer (Miller et 1998). |
One possibility is that the distinction between ast aud slow oscillations is due to a difference iu the oricutation of the hot spots aud the observer with respect o the rotation axis of the star. | One possibility is that the distinction between fast and slow oscillations is due to a difference in the orientation of the hot spots and the observer with respect to the rotation axis of the star. |
This secs unlikely. | This seems unlikely. |
Radius expansion is observed with similar Likelihood from both ast aud slow sources. and therefore is uulikelv. to depend on our viewing anele. | Radius expansion is observed with similar likelihood from both fast and slow sources, and therefore is unlikely to depend on our viewing angle. |
We would not expect oscillations to © associated with radius expansion bursts oulv in the fast sources if viewing augle effects determine whether oue or wo spots are observed. | We would not expect oscillations to be associated with radius expansion bursts only in the fast sources if viewing angle effects determine whether one or two spots are observed. |
Tt also does not appear that the strengths of the bursts determine the oscillation frequencies by iguiting either one or two hot spots. | It also does not appear that the strengths of the bursts determine the oscillation frequencies by igniting either one or two hot spots. |
If this were the case. one would expect to detect slow oscillations during weal bursts without radius expausion fron the fast sources. aud fast oscillations during strong bursts from the slow sources. | If this were the case, one would expect to detect slow oscillations during weak bursts without radius expansion from the fast sources, and fast oscillations during strong bursts from the slow sources. |
Out of the 125 bursts we observed from sources ofoscillatious.. we find uno evidence for harmonic or half-Brequeucy signals with powers comparable to the signals at the frequencies in Table 1.. | Out of the 125 bursts we observed from sources of, we find no evidence for harmonic or half-frequency signals with powers comparable to the signals at the frequencies in Table \ref{sum}. |
If the distinction between slow aud fast oscillators is equivalent to a division between slow and fast rotators. Man (ov some related quantity. eg. the effective surface eravity) could determine which bursts show oscillations. | If the distinction between slow and fast oscillators is equivalent to a division between slow and fast rotators, $\nu_{\rm spin}$ (or some related quantity, e.g., the effective surface gravity) could determine which bursts show oscillations. |
Uowever. that option is not free of complications. as the transition between the burst properties for sources that exhibit fast and slow oscillatious must be very sharp. since the two populations are uot at all well separated in frequency (see Table 1)). | However, that option is not free of complications, as the transition between the burst properties for sources that exhibit fast and slow oscillations must be very sharp, since the two populations are not at all well separated in frequency (see Table \ref{sum}) ). |
When comparing the observed distribution of 1/4: to a unlforu distribution of frequencies between 250650 Iz. a IKolinogorov-Suinrnov test (e.c. Eadie et 11971) cau exclude a uniform distribution at only the 1.36 (8I'4)) confidence level. | When comparing the observed distribution of $\nu_{\rm burst}$ to a uniform distribution of frequencies between 250–650 Hz, a Kolmogorov-Smirnov test (e.g., Eadie et 1971) can exclude a uniform distribution at only the $\sigma$ ) confidence level. |
It is interesting to uote that the recent report of a oossible ~[00 Tz burst oscillation from the 101 Iz musar SAN 3658 (n t Zaud et al. | It is interesting to note that the recent report of a possible $\approx 400$ Hz burst oscillation from the 401 Hz pulsar SAX $-$ 3658 (in 't Zand et al. |
2001) would nake the Migs, distribution even more consistent with a uuiforii distribution (excluded at ouly the 0.90 or confidence level). so the putative transition would have to © Correspondingly sharper. | 2001) would make the $\nu_{\rm burst}$ distribution even more consistent with a uniform distribution (excluded at only the $\sigma$ or confidence level), so the putative transition would have to be correspondingly sharper. |
We have listed a few additional propertics of these LAINBs in Table Ἐν. | We have listed a few additional properties of these LMXBs in Table \ref{sum}. |
Neither the activity level nor the lone- average accretion rate <AP>. as determined from jicarlv 5 vears of data from the AAILSky Monitor (Levine ct al. | Neither the activity level nor the long-term average accretion rate $<\dot M>$, as determined from nearly 5 years of data from the All-Sky Monitor (Levine et al. |
1996). appears to © correlated with the frequencies of the burst oscillations. | 1996), appears to be correlated with the frequencies of the burst oscillations. |
Fast oscillations. are observed iu both ransicut and N-1)) aud persistent (c.e.. 53) sources. as well as from both low <AT> and hieh <M> sources. | Fast oscillations are observed in both transient and ) and persistent (e.g., ) sources, as well as from both low $<\dot M>$ and high $<\dot M>$ sources. |
Orbital periods are measured or ouly {| of the 9 sources. and range frou 0.81 to 19 tours. | Orbital periods are measured for only 4 of the 9 sources, and range from 0.81 to 19 hours. |
It is apparent that these burst oscillation sources are an inhomogeneous eroup. Which makes measurements of oscillations from other sources hiehllv desirable. | It is apparent that these burst oscillation sources are an inhomogeneous group, which makes measurements of oscillations from other sources highly desirable. |
We feel that the most likely explanation for the observed correlations is that the burst properties chanee differeutlv as a function of AL in fast and slow sources. | We feel that the most likely explanation for the observed correlations is that the burst properties change differently as a function of $\dot M$ in fast and slow sources. |
AN-rayv burst theory predicts that radius expansion should occur ouly at low AM (Fujimoto. Tanawa. Mivaji 1981: Avasli Joss 1982). | X-ray burst theory predicts that radius expansion should occur only at low $\dot M$ (Fujimoto, Hanawa, Miyaji 1981; Ayasli Joss 1982). |
This agrees with observations of the slow oscillator (Franco 2000: van Straaten et al. | This agrees with observations of the slow oscillator (Franco 2000; van Straaten et al. |
2000). but does not appear to hold true for the fast oscillators citepiuiunü0.. (Atwakamietal.1980)... aud (vanderKlisetal.1990). | 2000), but does not appear to hold true for the fast oscillators \\citep{mun00}, \citep{mur80}, and \citep{vdk90}. |
Tf oscillatious ouly appear at high AT (as sugeested by Franco 2001). then they would indeed be associated with radius expansion in the fast sources. but not the slow sources. | If oscillations only appear at high $\dot M$ (as suggested by Franco 2001), then they would indeed be associated with radius expansion in the fast sources, but not the slow sources. |
Furthermore. Bildsten (2000) has sueeested that some mechanism acts d these latter sources. to coufine the accreted material such that the focal AL can decrease even as the elobal AL increases. | Furthermore, Bildsten (2000) has suggested that some mechanism acts in these latter sources to confine the accreted material such that the $\dot M$ can decrease even as the global $\dot M$ increases. |
If this is true. such coufinement is somehow related to the higher frequency of the fast burst oscillations. | If this is true, such confinement is somehow related to the higher frequency of the fast burst oscillations. |
the spectral range is larger than the planet size so that the speckle pattern associated to the star can be reconstructed and eliminated using regions unaffected by the planet image. | the spectral range is larger than the planet size so that the speckle pattern associated to the star can be reconstructed and eliminated using regions unaffected by the planet image. |
Differently from the MDI described in the previous section. no assumption about the spectra of the companion objects is Spectral deconvolution should offer some advantage over the differential imaging approach. at least outside the BR. because it uses the companion spectrum as a whole. | Differently from the MDI described in the previous section, no assumption about the spectra of the companion objects is Spectral deconvolution should offer some advantage over the differential imaging approach, at least outside the BR, because it uses the companion spectrum as a whole. |
The value of the the SPHERE IFS BR ts around 0.20 aresee for the Y-J- and about 0.12 arcsec for the Y-H-mode. | The value of the the SPHERE IFS BR is around 0.20 arcsec for the Y-J-mode and about 0.12 arcsec for the Y-H-mode. |
The procedure we followed is composed of four steps: In general. we assume that observations are done with the field fixed with respect to the IFU. | The procedure we followed is composed of four steps: In general, we assume that observations are done with the field fixed with respect to the IFU. |
In this case. the pupil rotates with time on an alt-az telescope. a typical value being 30° over a | hour exposure time. | In this case, the pupil rotates with time on an alt-az telescope, a typical value being $30^{\circ}$ over a 1 hour exposure time. |
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