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This is the technique employed to obtain the spectra ol sandar stars. and it mases djore ellicient use of telescope time. | This is the technique employed to obtain the spectra of standard stars, and it makes more efficient use of telescope time. |
When extended sources are concerned. a separate set of exposures aken from a nearby dark region of he sky is needed. a process conmmouly relerred to as 10clciig. | When extended sources are concerned, a separate set of exposures taken from a nearby dark region of the sky is needed, a process commonly referred to as nodding. |
€) The task was developed to reduce spec‘a from exteucded sources. therefore it asstJes hat a set of scy exposures was taken alone witli le science exposures. in order to reilove he elluric emissioi lines. | The task was developed to reduce spectra from extended sources, therefore it assumes that a set of sky exposures was taken along with the science exposures, in order to remove the telluric emission lines. |
There are two ways by which users can inform the software about tle lalire oL each image. iuuelv: interactively identifying thet1 viaDSO. or providing ai ASCII ile with the type of exposure with respect to its itLnerical order. | There are two ways by which users can inform the software about the nature of each image, namely: interactively identifying them via, or providing an ASCII file with the type of exposure with respect to its numerical order. |
For further details refer to the Mantal. | For further details refer to the Manual. |
No attempt was made to provice a software solution for identifying «illerent vpes of exposwes. as specilic criteria regardiug tle spectrum of the astronomical targe WOic lave to be precelined. adding. in our judgement. uiuecessary complexity to the code. | No attempt was made to provide a software solution for identifying different types of exposures, as specific criteria regarding the spectrum of the astronomical target would have to be predefined, adding, in our judgement, unnecessary complexity to the code. |
Nodding patterus that make best use of telescope tite use each sky exposure in more tlall one | Nodding patterns that make best use of telescope time use each sky exposure in more than one |
(AL,p<—19.66) aud one [aiu sample (—19.66<Myp18.5). | $M_b\leq-19.66$ ) and one faint sample $-19.66<M_b\leq 18.5$ ). |
They also have predictions of reduced projected 3PCEFs of tte Inbaler for tle concordance cosmological model. which are ineasured in an N-body sinulation. | They also have predictions of reduced projected 3PCFs of the matter for the concordance cosmological model, which are measured in an $N$ -body simulation. |
In their Vigures 17 and 18. they compare the observed Qj, aud the predicted Qp.m for different triangle slapes. wlich provide the information we need to do the two-paratrjeter fit. | In their Figures 17 and 18, they compare the observed $Q_{p,g}$ and the predicted $Q_{p,m}$ for different triangle shapes, which provide the information we need to do the two-parameter fit. |
A dile‘ent parameterizatn) Lis adopted by Jing&Borner(2001) to characterize a triangle. οe paralneter (rp. the length ofud the sho‘test side) for the size and two parameters (2t and. 0) lor Ie shape. wit ithe leugtl “the hree sides being rj. wry. and (uv+c)rg. | A different parameterization is adopted by \citet{Jing04} to characterize a triangle, one parameter $r_p$, the length of the shortest side) for the size and two parameters $u$ and $v$ ) for the shape, with the lengths of the three sides being $r_p$, $u r_p$, and $(u+v)r_p$ . |
In their figures. the κ)+)PCFs are plotted as a function ol e (five eqial linear bins in the rauge 0SUp<1) for several combina10115 of rp aud η. | In their figures, the 3PCFs are plotted as a function of $v$ (five equal linear bins in the range $0\leq v \leq 1$ ) for several combinations of $r_p$ and $u$. |
For the two-yaratjeter [ii. we choose the case with the largest value of ry they have. i.e.. 3.254IN pe. aud --2.09 | For the two-parameter fit, we choose the case with the largest value of $r_p$ they have, i.e., $3.25h^{-1}{\rm Mpc}$ , and $u=2.09$. |
if the ve depeudenuce is trauslatec intoan angular dependence. the ive data pcjnts oulv cover ᾧ f‘om SO" to 156. with the withis [9]‘the five angular bins bei[n]0 12°. 13°. 15°. 19°. aud LI. | If the $v$ dependence is translated into an angular dependence, the five data points only cover $\Phi$ from $\sim 80^\circ$ to $\sim 180^\circ$, with the widths of the five angular bins being $12^\circ$, $13^\circ$, $15^\circ$, $19^\circ$, and $44^\circ$. |
We see that the last bin suears the augular depeucdence a lot. | We see that the last bin smears the angular dependence a lot. |
So when ueasuriung the 3PCFs from galaxy. clustering data. adoptiug tle (ry3hpos-P) parameterization auc dividing 9 iuo narrow bius are probably more stitable to probe Iie angular dependence than he (rg.tet') parameterization. | So when measuring the 3PCFs from galaxy clustering data, adopting the $(r_{p13},r_{p23},\Phi)$ parameterization and dividing $\Phi$ into narrow bins are probably more suitable to probe the angular dependence than the $(r_p,u,v)$ parameterization. |
Since tlie errorbars ou the measveljeus are large ancl the scales are not truv in the weakly uouinear regime. we can100 obtain robst constraints on galaxy bias )araiuelters. | Since the errorbars on the measurements are large and the scales are not truly in the weakly nonlinear regime, we cannot obtain robust constraints on galaxy bias parameters. |
Nevertheless. application of the foriualii1 gives bias factors for galaxies in the bright (faint) saigle that are cousisteit with b =ldanudbo=O0(b=1.1la dbo —0). somewhat higher 6 han expeced but not absurdly so. | Nevertheless, application of the formalism gives bias factors for galaxies in the bright (faint) sample that are consistent with $b=1.8$ and $b_2=0$ $b=1.1$ and $b_2=0$ ), somewhat higher $b$ than expected but not absurdly so. |
If the »ojection is uot infitite. the kitd of relation shown in eqation (16)) also holds as loug as we use tle finite projected correlatiou finetious in the clefinition «LO, (equation [18]]). | If the projection is not infinite, the kind of relation shown in equation \ref{eqn:Qbias}) ) also holds as long as we use the finite projected correlation functions in the definition of $Q_p$ (equation \ref{eqn:Qpdef}] ]). |
Strictly speaking. 1 this case. the integration of the product of 2PCFs in te right side of equation (17)) canuot be written as the prodicl ol we,’2 except for €Crya)E(προ). | Strictly speaking, in this case, the integration of the product of 2PCFs in the right side of equation \ref{eqn:PCFgm}) ) cannot be written as the product of $w_p$ 's except for $\xi(r_{p13})\xi(r_{p23})$. |
However. the product of iy s should remain as a good approxination to tje results. | However, the product of $w_p$ 's should remain as a good approximation to the results. |
If one is uot saislied with the approximation. although it is good. oue can always compue exact values of these ittegratious Lor (y, aud form (Qepg from the observation in tlO Wav. | If one is not satisfied with the approximation, although it is good, one can always compute exact values of these integrations for $Q_{p,m}$ and form $Q_{p,g}$ from the observation in the way. |
Based on equation (17) . we still have the relation iu equation (1 9)). | Based on equation \ref{eqn:PCFgm}) ), we still have the relation in equation \ref{eqn:Qbiasp}) ). |
The result cai also be geieralized to a projected fiekl. where »rojected. correlations include he effect of the selection functiou (see Fry&Thomas 1999)). | The result can also be generalized to a projected field, where projected correlations include the effect of the selection function (see \citealt{Fry99}) ). |
Base| on equation (17)). it is easy o show that equation (19)) Iolds lor Qj delined in terms of selectior-[unction-weighted projected 9PCFEs aud 3PCEs. | Based on equation \ref{eqn:PCFgm}) ), it is easy to show that equation \ref{eqn:Qbiasp}) ) holds for $Q_p$ defined in terms of selection-function-weighted projected 2PCFs and 3PCFs. |
Fry&ΤΙOLias(1999) perforiu a systematic study of projection ellects on the 'educed 3PCEFs. | \citet{Fry99}
perform a systematic study of projection effects on the reduced 3PCFs. |
TIey show tlat projectlous that are not deep enoueh would change the shape of he reduced 3PCF :uid thus bias the estiration of galaxy Dias [factors. | They show that projections that are not deep enough would change the shape of the reduced 3PCF and thus bias the estimation of galaxy bias factors. |
However. this is based ou the comparison with tte three-dinensional reduced 3PCF of tle matter. | However, this is based on the comparison with the reduced 3PCF of the matter. |
Our poiut here is that once he reduced 3PCF of the maler is calcilated by taking account. of the selection fiuction. galaxy jas factors can be correctly inferred by conmipariug it with he observed reduced projected 3PCFEs of galaxies. | Our point here is that once the reduced 3PCF of the matter is calculated by taking account of the selection function, galaxy bias factors can be correctly inferred by comparing it with the observed reduced projected 3PCFs of galaxies. |
That is. weshouk always form Q,, aud Opin iu thesame way. | That is, weshould always form $Q_{p,g}$ and $Q_{p,m}$ in thesame way. |
The depth of the survey should be much larger than tje extent of structures caused N galaxy peculiar velocities so that wecan caleulate 3PCFs of the 1iatter in real space. | The depth of the survey should be much larger than the extent of structures caused by galaxy peculiar velocities so that wecan calculate 3PCFs of the matter in real space. |
BuchalteVWamionkowski.&Jalle(2000) also | \citet{Buchalter00} also |
which is obscurecl by the aceretion How during the eclipse absorption cip. | which is obscured by the accretion flow during the pre-eclipse absorption dip. |
Eclipsing polars have long been the target of dedicated X-rav observations. | Eclipsing polars have long been the target of dedicated X-ray observations. |
Many. of these polars show a distinct sight and faint phase as the accretion region rotates into view and out of view and many show a characteristic pre-eclipse absorption dip. | Many of these polars show a distinct bright and faint phase as the accretion region rotates into view and out of view and many show a characteristic pre-eclipse absorption dip. |
In these svstems there is no evidence or à second accretion pole. | In these systems there is no evidence for a second accretion pole. |
One of the few eclipsing polars o show emission throughout the binary phase is V2301 Oph (Ramsay Cropper 2007). | One of the few eclipsing polars to show emission throughout the binary phase is V2301 Oph (Ramsay Cropper 2007). |
We find that in the case of5731. X-ray emission is also seen throughout he orbital phase. | We find that in the case of, X-ray emission is also seen throughout the orbital phase. |
| We attempted to invert the X-ray light curves and map the X-ray regions on the white ciwarf using an approach similar to that of Cropper Llorne (1994). | We attempted to invert the X-ray light curves and map the X-ray regions on the white dwarf using an approach similar to that of Cropper Horne (1994). |
However. because of the relatively low signal to noise of the data we could not identify a unique solution. | However, because of the relatively low signal to noise of the data we could not identify a unique solution. |
In 83 we noted the presence of a broad dip in soft X-rays at oO ~0.4 which could be attributed to either an accretion stream (since there is no similar feature at higher energies) or the rotation of the accretion region(s) as they come into and out of view. | In 3 we noted the presence of a broad dip in soft X-rays at $\phi\sim$ 0.4 which could be attributed to either an accretion stream (since there is no similar feature at higher energies) or the rotation of the accretion region(s) as they come into and out of view. |
In the former case. the dip could. be due to à second accretion stream obscuring our line of sight to the accretion region located. in the lower hemisphere of the white dwarf. | In the former case, the dip could be due to a second accretion stream obscuring our line of sight to the accretion region located in the lower hemisphere of the white dwarf. |
To our knowledge this would make unique amongst polars in showing two absorption dips. | To our knowledge this would make unique amongst polars in showing two absorption dips. |
In the latter case. the change in the soft X-ray lieht curve could be due to either the rotation of two accretion regions. located in opposite hemispheres. or the rotation of one relatively large. polar region. ( | In the latter case, the change in the soft X-ray light curve could be due to either the rotation of two accretion regions, located in opposite hemispheres, or the rotation of one relatively large polar region. ( |
Our inversion maps showed that both scenarios could. re-produce the soft X-ray light curves). | Our inversion maps showed that both scenarios could re-produce the soft X-ray light curves). |
The fact that soft N-rays emitted at the base of the aceretion region are optically thick ancl hence viewing angle dependant could account for the change in the soft. X-ray Dux. | The fact that soft X-rays emitted at the base of the accretion region are optically thick and hence viewing angle dependant could account for the change in the soft X-ray flux. |
In contrast. the harder X-rays are optically. thin and therefore not viewing angle dependant. | In contrast, the harder X-rays are optically thin and therefore not viewing angle dependant. |
Optical polarimetry data would. be able to confirm the presence of two accretion poles. | Optical polarimetry data would be able to confirm the presence of two accretion poles. |
However. since is rather faint. this may. prove challenging. | However, since is rather faint, this may prove challenging. |
Ramsay Cropper (2004) presented the results of a snap-shot survey of polars observed in a high accretion. state usingNAIAL-Newtou. | Ramsay Cropper (2004) presented the results of a snap-shot survey of polars observed in a high accretion state using. |
They found that 7 out of 21 systems did not show a clistinet soft. X-ray component. | They found that 7 out of 21 systems did not show a distinct soft X-ray component. |
Vogel ct al (2008) also report that 2NMMp. 1312234|173651) which was discovered. serendipitously usingNewton. does not show a soft. X-ray component. | Vogel et al (2008) also report that 2XMMp J131223.4+173659, which was discovered serendipitously using, does not show a soft X-ray component. |
We have searched. the iterature for further observations of polars observed: using in a high state: we find an additional 6 xus. ( | We have searched the literature for further observations of polars observed using in a high state: we find an additional 6 polars. ( |
We are aware of a number of observations of »»blars in the high state which have been carried out bu mwve not as of vet been published). | We are aware of a number of observations of polars in the high state which have been carried out but have not as of yet been published). |
V1300 Ori (Schwarz et al 2005). V1432. Aql (Rana et al 2005) and SDSS J075240.45|362823.2 (Llomer οἱ al 2005) all show cistinc soft. X-ray components. while SDSS J072910.68|365838.3 and SDSS J170053.30|400357.6 (Llomer οἱ al 2005) clo not. | V1309 Ori (Schwarz et al 2005), V1432 Aql (Rana et al 2005) and SDSS J075240.45+362823.2 (Homer et al 2005) all show distinct soft X-ray components while SDSS J072910.68+365838.3 and SDSS J170053.30+400357.6 (Homer et al 2005) do not. |
In the case of SDSS J015543.4|002807.2. (Schmidt. et a 2005) the existence of a soft component is not required. at a high significance and hence we define it as not having a soft. X-ray component. | In the case of SDSS J015543.4+002807.2 (Schmidt et al 2005) the existence of a soft component is not required at a high significance and hence we define it as not having a soft X-ray component. |
We therefore find that LO out of 27 systems observed in a high state do not show a distinct soft X-ray componoent. | We therefore find that 10 out of 27 systems observed in a high state do not show a distinct soft X-ray component. |
ltamsav Cropper (2007) suggested that if. the temperature of the re-processed. N-ravs. was low enough. it would not be observable using the X-rav detectors. | Ramsay Cropper (2007) suggested that if the temperature of the re-processed X-rays was low enough, it would not be observable using the X-ray detectors. |
Εις view is also supported by the analysis carried out by Vogel et al (2008) on observations of 2NMMp J131223.41173659. | This view is also supported by the analysis carried out by Vogel et al (2008) on observations of 2XMMp J131223.4+173659. |
Phe reason for this could be that. the accretion How covers a larger fraction of the photosphere of the white cwarl or that the mass accretion. rate is. lower than in systems which showed a soft. component (since Alinx(Alrhy where A is the mass accretion rate anc f is the fractional area over which accretion is occurring). | The reason for this could be that the accretion flow covers a larger fraction of the photosphere of the white dwarf or that the mass accretion rate is lower than in systems which showed a soft component (since $kT_{bb}\propto({\dot{M}/f}^{1/4})$, where $\dot{M}$ is the mass accretion rate and $f$ is the fractional area over which accretion is occurring). |
There is no obvious reason as to why some polars woutle have accretion occurring over a larger area than others: they share no common characteristi¢s such as magnetic fiel streneth or orbital period. | There is no obvious reason as to why some polars would have accretion occurring over a larger area than others: they share no common characteristics such as magnetic field strength or orbital period. |
Indeed. as noted by Ramsay Cropper (2004) two systems (BY Cam and RAN 21155s) have one pole which shows a soft component and one pole which does not. | Indeed, as noted by Ramsay Cropper (2004) two systems (BY Cam and RX J2115--58) have one pole which shows a soft component and one pole which does not. |
Further. three svstems which have at least one pole which does not show a soft component are asvnchronous systems. | Further, three systems which have at least one pole which does not show a soft component are asynchronous systems. |
However. V1432 Aql which does show a soft component is also an asvachronous polar. | However, V1432 Aql which does show a soft component is also an asynchronous polar. |
We have serencdipttously discovered. a faint polar.5731. with an orbital period of 2.9 h. in the 2XMMi catalogue. | We have serendipitously discovered a faint polar, with an orbital period of 2.9 h, in the 2XMMi catalogue. |
We have identified the optical counterpart as a ro2] object and it shows a deep eclipse in the optical and X-ray bands lasting ~12 mins. | We have identified the optical counterpart as a $r\sim21$ object and it shows a deep eclipse in the optical and X-ray bands lasting $\sim$ 12 mins. |
At soft X-ray energies there is a distinctive drop in counts starting ~0.3 eveles before the eclipse. | At soft X-ray energies there is a distinctive drop in counts starting $\sim$ 0.3 cycles before the eclipse. |
This is due to the accretion stream obscuring the accretion region in the upper hemisphere of the white cdwarf. | This is due to the accretion stream obscuring the accretion region in the upper hemisphere of the white dwarf. |
A second dip is seen in soft N-ravs at ὁ —0.4 which could. either be due to obscuration of the accretion region bv a second stream or clue to the rotation of the accretion region(s) rotating into and out of view. | A second dip is seen in soft X-rays at $\phi\sim$ 0.4 which could either be due to obscuration of the accretion region by a second stream or due to the rotation of the accretion region(s) rotating into and out of view. |
Amonest eclipsing polars. is unusual in that X-ray emission | Amongst eclipsing polars, is unusual in that X-ray emission |
Let us examine the density and pressure distribution for the shell solution derived in § ??.. | Let us examine the density and pressure distribution for the shell solution derived in $\S$ \ref{sss2}. |
We define the density and pressure enhancements as These functions are normalized to be unity in region Ll. where the poloidal magnetic field lines are radial for the shell solution. | We define the density and pressure enhancements as These functions are normalized to be unity in region I, where the poloidal magnetic field lines are radial for the shell solution. |
In Fig. 14. | In Fig. \ref{fig:sol2enhanceA}, |
the pressure and density. enhancements. 2X4 and 24, are plotted for b=a2.3«24.Oa10 when a=SN and &zíd(«—b)]. | the pressure and density enhancements, $\Delta P_A$ and $\Delta D_A$ are plotted for $b=a/2,~ 3a/4,~ 9a/10$ when $a=0.8$ and $k=\pi/[4(a-b)]$. |
In all hree cases. the pressure ane density. pulses appear at the top of t1ο magnetic Looos. | In all three cases, the pressure and density pulses appear at the top of the magnetic loops. |
Their amplitudes are larger for a thinner shell. | Their amplitudes are larger for a thinner shell. |
The pea kot1e pressure enhancement appears behind that ο “the censity enhancement. | The peak of the pressure enhancement appears behind that of the density enhancement. |
This structure comes from the requirement for t1e force balance with the eravitv. | This structure comes from the requirement for the force balance with the gravity. |
As mentioned in 1 29 this relativistic self-similar solution is similar to the static solution in which the force balance is attained. | As mentioned in $\S$ \ref{energetics}, this relativistic self-similar solution is similar to the static solution in which the force balance is attained. |
As plasma is swept up into the shell. the density increases inside the shell. | As plasma is swept up into the shell, the density increases inside the shell. |
Fo support the gravity by this excess density. the pressure eradient appears behind the density enhancement. | To support the gravity by this excess density, the pressure gradient appears behind the density enhancement. |
Ehe density decrease behind the pressure enhancement also comes from the requirement for the force balance. | The density decrease behind the pressure enhancement also comes from the requirement for the force balance. |
Since the decrease of the density enables the buovaney force to push the plasma in the radial direction. this buovaney force maintains the pressure pulse. | Since the decrease of the density enables the buoyancy force to push the plasma in the radial direction, this buoyancy force maintains the pressure pulse. |
Thesestructures are identical to those in non-relativistic solution (Low 1982). | Thesestructures are identical to those in non-relativistic solution \citep{1982ApJ...261..351L}. . |
Fig. | Fig. |
15. plots Ao and AD for b=a2.Bea+.θα19 wlen v=OS and &=sπ4abj]. | \ref{fig:sol2enhanceQ} plots $\Delta P_Q$ and $\Delta D_Q$ for $b=a/2,~3a/4,~9a/10$ when $a=0.8$ and $k=\pi/[4(a-b)]$. |
As menioned in t ?. the Lorentz force exerted by the toroidal magnetic Lecls always reduces the pressure. | As mentioned in $\S$ \ref{sss}, the Lorentz force exerted by the toroidal magnetic fields always reduces the pressure. |
A local minimur nol the density enhancement AD locates behind a local maximum of dALo/dy. | A local minimum of the density enhancement $\Delta D_Q$ locates behind a local maximum of $d\Delta P_Q/d\eta$. |
his structure also comes from the force baance. | This structure also comes from the force balance. |
Pressure gradient force balances with the buovancy force in the rarefied region. | Pressure gradient force balances with the buoyancy force in the rarefied region. |
Next we examine the structure of the Dux rope solution derived in ο ??.. | Next we examine the structure of the flux rope solution derived in $\S$ \ref{sss3}. |
We define the normalized toroidal magnetic field strength as Solid curve in Fig. | We define the normalized toroidal magnetic field strength as Solid curve in Fig. |
16 shows AZ, as a function of 5g for b=r0.95e. while the dash ancl dot-dashed ones show that [or b—0.8e and b=0.65e. respectively. | \ref{fig:sol3Qenhance} shows $\Delta B_\phi$ as a function of $\eta$ for $b=0.95a$, while the dash and dot-dashed ones show that for $b=0.8a$ and $b=0.65a$, respectively. |
Other parameters are fixed at e=0.8 and &=παby]. | Other parameters are fixed at $a=0.8$ and $k=\pi/[4(a-b)]$. |
Ehe toroidal magnetic field has à peak inside the Dux rope. | The toroidal magnetic field has a peak inside the flux rope. |
Is amplitude is larger for a larger e and a thinner shell. | Its amplitude is larger for a larger $a$ and a thinner shell. |
Phe shell structure also appears behind the loop top (see Fig. | The shell structure also appears behind the loop top (see Fig. |
10. and 11)). | \ref{fig:sol3A}
and \ref{fig:sol3Q}) ). |
Solid curve in Fig. | Solid curve in Fig. |
17. shows AB? whichcorresponds to the magnetic pressure by | \ref{fig:sol3QPDenhance} shows $\Delta B_\phi^2$ , whichcorresponds to the magnetic pressure by |
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