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The two samples do not show any significant differences in absolute magnitude (Kolmogorov-Smirnov P= 0.79). | The two samples do not show any significant differences in absolute magnitude (Kolmogorov-Smirnov $P = 0.79$ ). |
and it is these higher level products which we use in our analysis | and it is these higher level products which we use in our analysis. |
To determine the count rate of INE. Dra at each epoch we combined the X-ray events [rom each ObservationlD into a corresponding image usingxselect". | To determine the count rate of KL Dra at each epoch we combined the X-ray events from each ObservationID into a corresponding image using. |
. This image was input o the LIIZASoft tool and the routine (which akes into account effects such as vignetting. exposure and he point spread function) to determine the count rate and error at the position of INL. Dra. | This image was input to the HEASoft tool and the routine (which takes into account effects such as vignetting, exposure and the point spread function) to determine the count rate and error at the position of KL Dra. |
We show the count rates or the individual observations in the lower panel of Figure 3.. | We show the count rates for the individual observations in the lower panel of Figure \ref{swift-light}. |
Since the count rates are low. we created images using more than one observation and. determined the count rate rom these. | Since the count rates are low, we created images using more than one observation and determined the count rate from these. |
We also show these results in the lower panel of Figure 3. as thicker symbols. | We also show these results in the lower panel of Figure \ref{swift-light} as thicker symbols. |
In the lower panel of Figure we show the X-ray data olded on a 61.5 day. period. | In the lower panel of Figure \ref{fold-long} we show the X-ray data folded on a 61.5 day period. |
We created4. an image from. all rw X-ray. data taken in the low optical state and also the ligh optical state. | We created an image from all the X-ray data taken in the low optical state and also the high optical state. |
Phe mean count rates (O.00258+0.00029 s for the low optical state ancl 0.00190270.00036 ct/s for he high optical state) are over-plottecl as thicker lines in Figure 4.. | The mean count rates $\pm$ 0.00029 ct/s for the low optical state and $\pm$ 0.00036 ct/s for the high optical state) are over-plotted as thicker lines in Figure \ref{fold-long}. |
Although the mean X-ray lux during the low Xical state is higher than that of the high optical state he dillerence is not significant: we find no evidence that the X-ray [lux changed significantly. between the high and low optical states. | Although the mean X-ray flux during the low optical state is higher than that of the high optical state the difference is not significant: we find no evidence that the X-ray flux changed significantly between the high and low optical states. |
We also tested whether there was a change in the soft/hard (0.1.1keV/1.IOkeV) ratio between the low and high optical states — there was none. | We also tested whether there was a change in the soft/hard (0.1–1keV/1–10keV) ratio between the low and high optical states – there was none. |
UsingXSELECT we initially extracted an X-ray spectrum of WL Dra over a time interval when it was in a low optical state. | Using we initially extracted an X-ray spectrum of KL Dra over a time interval when it was in a low optical state. |
In addition. we extracted. a background: spectrum [rom a source free region. | In addition, we extracted a background spectrum from a source free region. |
We used the appropriate response matrix from the calibration Liles and. created. an auxiliary file using the ΗΛΡο toolxrtmkarf. | We used the appropriate response matrix from the calibration files and created an auxiliary file using the HEASoft tool. |
We fitted the N-ray. spectrum of KL Dra in a low optical state using the thermal plasma model and the neutral absorption mocel. | We fitted the X-ray spectrum of KL Dra in a low optical state using the thermal plasma model and the neutral absorption model. |
Keeping the metallicity fixed at solar (but with the hydrogen abundance fixed. at zero) we found a good [it to the data (4200.84. 6 degrees of [reedom). | Keeping the metallicity fixed at solar (but with the hydrogen abundance fixed at zero) we found a good fit to the data 0.84, 6 degrees of freedom). |
The hydrogen column density determined from. our mocel fits is consistent with the total hydrogen column density to the edge ofthe Galaxy in the direction of KL Dra (~7401077. | The hydrogen column density determined from our model fits is consistent with the total hydrogen column density to the edge of the Galaxy in the direction of KL Dra $\sim7.4\times10^{20}$. |
Dickey Lockman 1990). | Dickey Lockman 1990). |
Since. we found no evidence that the X-ray Fux varied between the low and high optical states we created a second spectrum using all the X-ray data. | Since, we found no evidence that the X-ray flux varied between the low and high optical states we created a second spectrum using all the X-ray data. |
Using a model in which the metallicity was fixed at solar we obtained a fit with VZ—11.12. 8 dof. | Using a model in which the metallicity was fixed at solar we obtained a fit with 1.12, 8 dof. |
We give the fits with associated errors in Table 1.. | We give the fits with associated errors in Table \ref{xray-fits}. |
Ramsay et al. ( | Ramsay et al. ( |
2006) determined the N-rav and UV luminosities for S XM. €Vn. systems: of those. 5. had distances determined. using parallax measurements. | 2006) determined the X-ray and UV luminosities for 8 AM CVn systems: of those, 5 had distances determined using parallax measurements. |
The X-rav luminosity of those 5 systems decreases as the orbital period. increases. | The X-ray luminosity of those 5 systems decreases as the orbital period increases. |
Dased on this trend. we predict that a system with an orbital period of 25 mins should have an X- luminosity of Lx~5.107+2. | Based on this trend, we predict that a system with an orbital period of 25 mins should have an X-ray luminosity of $L_{\rm X}\sim5\times10^{30}$. |
Phis is very similar to CR Boo 107JL. Ramsay et. al. | This is very similar to CR Boo $\times10^{30}$, Ramsay et al. |
2006) with has an orbital period. very. close to WL Dra. | 2006) with has an orbital period very close to KL Dra. |
Our findings imply that KWL Dra [ies at a distance of 550S50pe (using the standard error on the unabsorbed bolometric X-ray Lux. ‘Table 1)). | Our findings imply that KL Dra lies at a distance of 550–850pc (using the standard error on the unabsorbed bolometric X-ray flux, Table \ref{xray-fits}) ). |
Phe UV Luminosity is more uncertain since it is cillicult to constrain the temperature of the UV. component (which derives from the primary white cwarl plus the accretion disc). | The UV luminosity is more uncertain since it is difficult to constrain the temperature of the UV component (which derives from the primary white dwarf plus the accretion disc). |
However. taking the lead from Ramsay et al. ( | However, taking the lead from Ramsay et al. ( |
2006). we fix a single blackbods with a range of temperature (10000.400001). and fix the normalisation of the blackbody so that it matches the measured UV Εν (we used the uvred absorption component inXSPEC. Arnaud. 1996). | 2006), we fix a single blackbody with a range of temperature (10000–40000K), and fix the normalisation of the blackbody so that it matches the measured UV flux (we used the absorption component in, Arnaud 1996). |
Setting theUV flux near the UV maximum (6«10.17 Figure 3)) we find à UV luminosity of 10%? Hor | Setting theUV flux near the UV maximum $6\times10^{-15}$, Figure \ref{swift-light}) ) we find a UV luminosity of $\times10^{33}$ for |
1n hierarchical models for galaxy formation. structures grow due to the accretion of smaller svstems which formed. at earlier times. | In hierarchical models for galaxy formation, structures grow due to the accretion of smaller systems which formed at earlier times. |
According to this scheme. these svstems should not only be in the cluster itself but also in its vicinity. harbouring an important number of groups or small clusters of galaxies. | According to this scheme, these systems should not only be in the cluster itself, but also in its vicinity, harbouring an important number of groups or small clusters of galaxies. |
In this sense. clusters of galaxies represent high density enhancements in the clistribution of galaxies. | In this sense, clusters of galaxies represent high density enhancements in the distribution of galaxies. |
On the basis of this scenario. it is natural to ask whether physical properties of structures depend on its proximity to high density regions. which. as previously mentioned. may be well represented. by rich clusters of galaxies: or. if on the contrary. they evolve independently on the presence of denser regions. | On the basis of this scenario, it is natural to ask whether physical properties of structures depend on its proximity to high density regions, which, as previously mentioned, may be well represented by rich clusters of galaxies; or, if on the contrary, they evolve independently on the presence of denser regions. |
Several works have focussed on the evolution o£ substructures inside massive svstems in simulations or rich ealaxy clusters Clormen et al. | Several works have focussed on the evolution of substructures inside massive systems in simulations or rich galaxy clusters (Tormen et al. |
1998. Ghigna et al. | 1998, Ghigna et al. |
2000. ‘Vavlor Babul 2003. De Lucia ct al. | 2000, Taylor Babul 2003, De Lucia et al. |
2003): nevertheless. not much attention has been paid to structures in the outer regions of these systems. | 2003); nevertheless, not much attention has been paid to structures in the outer regions of these systems. |
Hence. it is not well known if some of the behaviours of substructures inside the clusters. could also be applicable to groups in their periphery. | Hence, it is not well known if some of the behaviours of substructures inside the clusters, could also be applicable to groups in their periphery. |
Einasto et al. ( | Einasto et al. ( |
2003) have investigated the properties of loose groups in the Las Campanas Redshift) Survey (LOLGs). in the vicinity of rich clusters of galaxies. including clusters from the Abell ancl APAL catalogues. X-ray clusters and also a sample of the richest. groups from. the LOLC catalogue itself. | 2003) have investigated the properties of loose groups in the Las Campanas Redshift Survey (LCLGs), in the vicinity of rich clusters of galaxies, including clusters from the Abell and APM catalogues, X-ray clusters and also a sample of the richest groups from the LCLG catalogue itself. |
By using an additional sample. consisting of all those LOLGs which do not neighbour a rich cluster. they have been able to compare the properties obtained for dense-environment LOLGs with those of ἱνρίσα LOLGs. | By using an additional sample, consisting of all those LCLGs which do not neighbour a rich cluster, they have been able to compare the properties obtained for dense-environment LCLGs with those of typical LCLGs. |
They found that in most cases. the observed richness of groups near rich clusters is larger than the corresponding value for groups in the comparison sample. | They found that in most cases, the observed richness of groups near rich clusters is larger than the corresponding value for groups in the comparison sample. |
The same ellect is shown when using Abell counts as a measure of groups richness. | The same effect is shown when using Abell counts as a measure of groups richness. |
The harmonic radius and the velocity dispersion are also somewhat larger in the neighbourhood of rich clusters than in typical loose groups. | The harmonic radius and the velocity dispersion are also somewhat larger in the neighbourhood of rich clusters than in typical loose groups. |
Thev also found a strong. mass scerceation: indicating that loose groups in the vicinity of clusters have masses that are [arger than mean masses of eroups drawn from the comparison sample. | They also found a strong mass segregation; indicating that loose groups in the vicinity of clusters have masses that are larger than mean masses of groups drawn from the comparison sample. |
The same trend | The same trend |
NGC 10907 |SD(s)b: deVaucouleursetal. 1991]|| is a nearby (D = 1L5 Ape: 1" = 70 pe. Tully 1988)) barred spiral galaxy. | NGC 1097 [SB(s)b; \citealt{dev91}] ] is a nearby (D = 14.5 Mpc; $\arcsec$ = 70 pc, \citealt{tully}) ) barred spiral galaxy. |
A pair of dust lanes are located at the leading edges of the major bar. | A pair of dust lanes are located at the leading edges of the major bar. |
A radio coutinuuu nuage at 1.165 CGIIz shows faint ridges coinciding with the dust lanes (Ibunuucletal.1987). | A radio continuum image at 1.465 GHz shows faint ridges coinciding with the dust lanes \citep{hum87}. |
. The nucleus is thought to be a transition object fromLINER to Sevfert l (Storchi-Beremannuctal.2003). | The nucleus is thought to be a transition object fromLINER to Seyfert 1 \citep{stor03}. |
. Detailed studies ou the nucleus show morphological aud kinematic evidences of the unclear spirals on the order of 30 pc. aud was interpreted as part of the fucling chain to the very center (Fathictal.2006:Davieset2009:vandeVen 20103. | Detailed studies on the nucleus show morphological and kinematic evidences of the nuclear spirals on the order of 30 pc, and was interpreted as part of the fueling chain to the very center \citep{fathi06,davies09,van10}. |
. NGC 1097 is also an IRAS bright ealaxy (Sandersetal. 2003). | NGC 1097 is also an IRAS bright galaxy \citep{sanders03}. |
. The coutzibution of large amount of IR fiux arise froun its 1 kpce-ciremnnuclear starburst ring (c.g.al. 2000). | The contribution of large amount of IR flux arise from its 1 kpc-circumnuclear starburst ring \citep[e.g.,][]{hum87,tele81,kot00}. |
. The starburst ring hosts hot-spots" composed! with super star clusters identified in HIST images (Barthetal. 1995).. aud was suggested to have an instantaneous burst of star formation which occured ~ 67 λατ ago (Isotilainenetal.2000). | The starburst ring hosts ”hot-spots“ composed with super star clusters identified in HST images \citep{barth95}, and was suggested to have an instantaneous burst of star formation which occurred $\sim$ 6–7 Myr ago \citep{kot00}. |
. The molecular gas of NGC 1097 in the nuclear region has been previously mapped iu the dense gas tracer of UCN(J = 0). low excitation lines of 12C0(J = 10) aud -CO(J = 21) (Kohnoctal2003:sichetal.2008.hereafterPaper D.. | The molecular gas of NGC 1097 in the nuclear region has been previously mapped in the dense gas tracer of HCN(J = 1–0), low excitation lines of $^{12}$ CO(J = 1–0) and $^{12}$ CO(J = 2–1) \citep[][hereafter Paper I]{koh03,hsieh08}. |
These maps show a central concentration comedent with the peak of the 6-c1ài radio continuum core (Ibununueletal.LOST). as well as a molecular ring coincident with the starburst ring. | These maps show a central concentration coincident with the peak of the 6-cm radio continuum core \citep{hum87}, as well as a molecular ring coincident with the starburst ring. |
A paix of molecular ridges coincident with the dust lanes are also detected. auc show non-circular motions. possibly caused by the bar-poteutial dyaiuuies (ee.Athanassoula1992:.b). | A pair of molecular ridges coincident with the dust lanes are also detected, and show non-circular motions, possibly caused by the bar-potential dynamics \citep[e.g.,][]{atha,athb}. |
. The molecular rine has a typical wari. temperature (fk~100 E) and denser gas (ny,~105 P) consisteut with the starburst euvironments (Wildetal.1992:Aalto1995). | The molecular ring has a typical warm temperature $T_{\rm K} \sim 100$ K) and denser gas $n_{\rm H_{2}} \sim 10^{3}$ $^{-3}$ ) consistent with the starburst environments \citep{wild92,aalto95}. |
. The molecular ring exhibits a twin-peak structure iu the resolution interferometric CO aud ICN maps. where a pair of molecular concentrations are located in the intersection of the molecular dust lanes and the star orniue rine. | The molecular ring exhibits a twin-peak structure in the resolution interferometric CO and HCN maps, where a pair of molecular concentrations are located in the intersection of the molecular dust lanes and the star forming ring. |
Its oricutation is nearlv perpendicular to he stellar bar. | Its orientation is nearly perpendicular to the stellar bar. |
The twin-peak has higher IT, colwuiu density than the surrounding ring. aud similar features jiwe been seen in other barred galaxies. aud cau be explained bv the crowding of gas streamlines (e.g...I&eu- 1999).. | The twin-peak has higher $_{2}$ column density than the surrounding ring, and similar features have been seen in other barred galaxies, and can be explained by the crowding of gas streamlines \citep[e.g.,][]{ken92, rey97,koh99}. . |
The eas flow eradually changes direction aud wierates toward the ceuter of the ealaxy to acciunulate | The gas flow gradually changes direction and migrates toward the center of the galaxy to accumulate |
satellites. | satellites. |
Thanks to wide field) charge-coupled-devices (CCDs). the past lew vears have witnessed (he discovery of a large number of these objects [see for a comprehensive review]. | Thanks to wide field charge-coupled-devices (CCDs), the past few years have witnessed the discovery of a large number of these objects [see \citet{Jewitt07} for a comprehensive review]. |
At the time of writing of this article. 108 irregular satellites have been discovered. of which 55 belong to. Jupiter. making the Jovian satellite svstem the largest aunong all planets. | At the time of writing of this article, 108 irregular satellites have been discovered, of which 55 belong to Jupiter, making the Jovian satellite system the largest among all planets. |
Due to ils proximity. the irregular satellites of Jupiter have been the subject of extensive observational and theoretical research. | Due to its proximity, the irregular satellites of Jupiter have been the subject of extensive observational and theoretical research. |
Many of the dynamical characteristics of (hese objects. such as their orbital stability. dvnamical grouping ancl their collision probability have long been studied (SahaandTremaine1993:Carrubaetal.2002;Nesvorn*2003:Nesvorny2007:Douskos.IxalantonisandMarkellos. 2007). | Many of the dynamical characteristics of these objects, such as their orbital stability, dynamical grouping and their collision probability have long been studied \citep{Saha93,Carruba02,Nesvorny03,Nesvorny04,Beauge06,
Beauge07,Douskos07}. |
. There is. however. one interesting feature in the distribution of Jovian imegulars that has not vet been fully understood. | There is, however, one interesting feature in the distribution of Jovian irregulars that has not yet been fully understood. |
As shown by SheppardandJewitt(2003).. (he region extending from the orbit of Callisto. the outermost Galilean satellite al 26 Jupiter-racdii (11). to the periastron of Thenmisto (o7610). Jupiter's innermost irregular satellite. is void of irregulars. | As shown by \citet{Sheppard03}, the region extending from the orbit of Callisto, the outermost Galilean satellite at 26 Jupiter-radii $({R_J})$ , to the periastron of Themisto $(\sim 76{R_J})$, Jupiter's innermost irregular satellite, is void of irregulars. |
Observations suggest the presence of similar void regions around all four giant. planets. | Observations suggest the presence of similar void regions around all four giant planets. |
Table 1 and figure I show this in more detail. | Table 1 and figure 1 show this in more detail. |
As seen from figure I. satellite void regions also exist. (he currently known iregular satellites of the eiant planets. | As seen from figure 1, satellite void regions also exist the currently known irregular satellites of the giant planets. |
Theoretical studies have indicated that there may be (wo possible scenarios for (lie existence of such void regions: ejection from the svstem due (o mutual interactions with other irregular satellites and. in the case of satellites that are the remnants of collisions. clustering around their parent bodies (INuiper1956:Pollack.Burns.audTauber1979;KesslerandNesvorny 2007). | Theoretical studies have indicated that there may be two possible scenarios for the existence of such void regions; ejection from the system due to mutual interactions with other irregular satellites and, in the case of satellites that are the remnants of collisions, clustering around their parent bodies \citep{Kuiper56,Pollack79,Kessler81,Thomas91,Krivov02,
Nesvorny03,Nesvorny04,Beauge07}. |
. The focus of this paper is. however. on the lack of irregular satellites in theboundary between regulars and irregulars. | The focus of this paper is, however, on the lack of irregular satellites in the between regulars and irregulars. |
We are interested in understanding of why no irregular satellite exists between (he outermost Galilean satellite and Jupiters innernmost irregular one. | We are interested in understanding of why no irregular satellite exists between the outermost Galilean satellite and Jupiter's innermost irregular one. |
The lack of irregular satellites in the boundary. between regulars and irregulars may be attributed to the distribution of the orbits of the latter bodies. | The lack of irregular satellites in the boundary between regulars and irregulars may be attributed to the distribution of the orbits of the latter bodies. |
Since irregular satellites appear to have been captured from heliocentric orbits. it max be natural to expect them to prelerably have laree semimajor axes. ancl therefore not to exist in close orbits. | Since irregular satellites appear to have been captured from heliocentric orbits, it may be natural to expect them to preferably have large semimajor axes, and therefore not to exist in close orbits. |
Proving this to be so would be an important contribution to the subject. but. unfortunately. none of the models of capture is sufficiently specific to be used in (his way. | Proving this to be so would be an important contribution to the subject, but, unfortunately, none of the models of capture is sufficiently specific to be used in this way. |
The N-body capture model ol Nesvorny.Vokrouhlické.andMorbidelli(2007) does roughly match the distribution of irregular satellites of some planets. bul not of Jupiter. | The N-body capture model of \citet{Nesvorny07}
does roughly match the distribution of irregular satellites of some planets, but not of Jupiter. |
In this paper. we examine (he possibility of a dynamical originfor the existence of (his satellite-void boundary region. | In this paper, we examine the possibility of a dynamical originfor the existence of this satellite-void boundary region. |
Tu the preseut (third) paper we cotinue investigating the optical properties of a suuple of 51 nid-IBR Wari Sevferts selected from the sample of IR-warm IRAS sources of De (111) (DeCj)etal.19857. ancl DeCrijpetal. 1992). | In the present (third) paper we continue investigating the optical properties of a sample of 54 mid-IR Warm Seyferts selected from the sample of IR-warm IRAS sources of De Grijp \cite{grijp87} and \cite{grijp92}) ). |
Our control sample contains 16 iid-IR Cold IRAS ealaxics. selected ο span simular redshift aud uuilosity ranges as fje Wari sample. | Our control sample contains 16 mid-IR Cold IRAS galaxies, selected to span similar redshift and luminosity ranges as the Warm sample. |
Iu Chatzic]Juistou20002. (jereafter Paor 1) we prescuted our optic:d nuaeiug data. | In \cite{paper1} (hereafter Paper I) we presented our optical imaging data. |
In Chatzichristou20TP, (hereafter Paper II) we discussed aux iuterconipared the optical properies of t10se παΗ])es. resulting YOU our aperture phoolnetry aud searclie Or correlations with thei IR properties. | In \cite{paper2} (hereafter Paper II) we discussed and intercompared the optical properties of these samples, resulting from our aperture photometry and searched for correlations with their IR properties. |
Iu. the preseut third paper we will prescut. :uialvse aud discuss tjo results oD onr surface plotomerv. performed on mios O our sauple objects. | In the present third paper we will present, analyse and discuss the results of our surface photometry, performed on most of our sample objects. |
This pzyper is organized as follows: in Section 2 we ασe our nethod of azinmuthal clIpse fitting. two-component decomposition of the projected 1-D helt profiles auxL their parametrization. | This paper is organized as follows: in Section 2 we summarize our method of azimuthal ellipse fitting, two-component decomposition of the projected 1-D light profiles and their parametrization. |
Tn Sections Sand [owe disciss the various structura parineters characterizing the light distributions aud interconipare our Warm and Cold (ub)suuples. | In Sections 3 and 4 we discuss the various structural parameters characterizing the light distributions and intercompare our Warm and Cold (sub)samples. |
Our conclusions aro sunuarized in Section 5. | Our conclusions are summarized in Section 5. |
Most of the available isophotal fitting procedures approximate the galaxian isoohotes with ellipses at increasing radii aud gubsequeuIv perform. surface aud aperture photometry within ¢ch ellipse. | Most of the available isophotal fitting procedures approximate the galaxian isophotes with ellipses at increasing radii and subsequently perform surface and aperture photometry within each ellipse. |
The basic idea is to sample the image at predefined radi (or rather seuiinajor axis lenetis) along an elliptical path. so fiat the inteusity is fje παλιο at all sampling poiuts within the noise. | The basic idea is to sample the image at predefined radii (or rather semi-major axis lengths) along an elliptical path, so that the intensity is the same at all sampling points within the noise. |
The intensity distribution along the ellipse is fitted. by weighted least-squares to an haruonic expression of he type being the position angle: the harmonic amplitudes Ay.By.As.Bo paraietrize errors in the fitting procedure. | The intensity distribution along the ellipse is fitted by weighted least-squares to an harmonic expression of the type being the position angle; the harmonic amplitudes $A_{1},B_{1},A_{2},B_{2}$ parametrize errors in the fitting procedure. |
Ouce the best fit ellipse has been obtained. the residuals along this ellipse are parametrized as These higdier harmonic amplitudes οιD, characterize the deviations of a eive1 ellipse from perfect isophotometry. | Once the best fit ellipse has been obtained, the residuals along this ellipse are parametrized as These higher harmonic amplitudes $A_{n},B_{n}$ characterize the deviations of a given ellipse from perfect isophotometry. |
The metl100 is described by Jedrzejesslà.1987.. | The method is described by \cite{jedrzejewski87}. |
AmongC» available ellipse fittingC» algorithmsC» we lave utilized the WEGAL sib-packaee of the IRAF/STSDAS applicatims. Which is based upon a combination of tasks that are proved and/or extended versions of the original routines wihin the ISOPIIOTE subpackage. | Among available ellipse fitting algorithms we have utilized the WFGAL sub-package of the IRAF/STSDAS applications, which is based upon a combination of tasks that are improved and/or extended versions of the original routines within the ISOPHOTE subpackage. |
Οιr moettod is described in Chatzichristou1999 andl Was appied to all of our objects for which cither photomeric information was available or which possessed wellresoved morphologies. | Our method is described in \cite{thesis} and was applied to all of our objects for which either photometric information was available or which possessed well-resolved morphologies. |
Azthally averaged profiles have two iuportaut advantages over radial (usually along major aud minor axes) profiles: first. they allow snoothius ofi ibhoimoegeneities that could be due to non-unuiforily distrilited cust. reeious of enliauced star forlation. or to he presence of non-axisvuuuetric featureSs and second. they provide iuproved S/N ratio. | Azimuthally averaged profiles have two important advantages over radial (usually along major and minor axes) profiles: first, they allow smoothing of inhomogeneities that could be due to non-uniformly distributed dust, regions of enhanced star formation, or to the presence of non-axisymmetric features and second, they provide improved S/N ratio. |
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