source
stringlengths 1
2.05k
⌀ | target
stringlengths 1
11.7k
|
|---|---|
The and lines are hardly present, and therefore,all the plasmaN emitting the observed N lines resides outside of the binary orbit while some of the flux in the hotter line also originates from within the orbit. | The and lines are hardly present, and therefore, the plasma emitting the observed N lines resides outside of the binary orbit while some of the flux in the hotter line also originates from within the orbit. |
In order to explain the changes from day 22.9 to 34.9, the line emission that was first seen to come from the inner regions Hef and intercombination has to be moved to further outside toescape eclipses by line)the companion on day 34.9. | In order to explain the changes from day 22.9 to 34.9, the line emission that was first seen to come from the inner regions $\beta$ and intercombination line) has to be moved to further outside toescape eclipses by the companion on day 34.9. |
While for the He-like intercombination line one could argue | While for the He-like intercombination line one could argue |
in the derived o lies at a smaller p than observed. and objects with nearly circular projections are over-produced. | in the derived $\phi$ lies at a smaller $p$ than observed, and objects with nearly circular projections are over-produced. |
The best-fitting oblate distribution consists of cores that are intrinsically more flattened than in the prolate case. which also may be considered a priori less likely (Myers et al.. | The best-fitting oblate distribution consists of cores that are intrinsically more flattened than in the prolate case, which also may be considered a priori less likely (Myers et al., |
1991). | 1991). |
While the poor agreement may simply be a result of restricting c to be gaussian. a less generic form of c used in the oblate. but not i the prolate. case has little justification. | While the poor agreement may simply be a result of restricting $\psi$ to be gaussian, a less generic form of $\psi$ used in the oblate, but not in the prolate, case has little justification. |
We also applied the 4 analysis to the axis ratio distributior of hjina et ((1999). | We also applied the $\chi^2$ analysis to the axis ratio distribution of Jijina et (1999). |
The same qualitative result was found. but with less of a difference between the oblate (4=0.97) and prolate (47= 0.88) These results make clear that. despite recent claims to the contrary. the observed o(p) is reasonably well-fit by a gaussiar distribution 4) of randomly-oriented prolate spheroids. | The same qualitative result was found, but with less of a difference between the oblate $\chi^2 = 0.97$ ) and prolate $\chi^2 = 0.88$ ) These results make clear that, despite recent claims to the contrary, the observed $\phi (p)$ is reasonably well-fit by a gaussian distribution $\psi (q)$ of randomly-oriented prolate spheroids. |
This consequently weakens the motivation for triaxial models which. in any case. have no theoretical basis in. the context of gaseous. equilibrium clouds. | This consequently weakens the motivation for triaxial models which, in any case, have no theoretical basis in the context of gaseous, equilibrium clouds. |
We shall use these best-fit intrinsic distributions to generate peak intensities for simulated datasets in 335.. | We shall use these best-fit intrinsic distributions to generate peak intensities for simulated datasets in \ref{sec-intrins}. |
Consider a cloud core in which the mass distribution ts constant on similar ellipsoids. either oblate or prolate. | Consider a cloud core in which the mass distribution is constant on similar ellipsoids, either oblate or prolate. |
In an optically thin tracer. the particular line of sight corresponding to the peak intensity { (or peak flux density: units Jy/beam) represents the complete column through the It should therefore depend upon the apparent axis ratio p. | In an optically thin tracer, the particular line of sight corresponding to the peak intensity $I$ (or peak flux density; units Jy/beam) represents the complete column through the It should therefore depend upon the apparent axis ratio $p$. |
Thus we have (Richstone 1979; Merritt 1982): no op, toblateY3) I(0)) — gle = pl, (prolate). where 0 is the angle between the observer's line of sight and the equatorial plane. 7,=/(0) is the intensity as seen toward the same plane. and 7,=7(x/2) is the intensity as seen down the polar axis. | Thus we have (Richstone 1979; Merritt 1982): ) = I_e = I_p ) ) = I_e = p I_p ), where $\theta$ is the angle between the observer's line of sight and the equatorial plane, $I_e = I (0)$ is the intensity as seen toward the same plane, and $I_p = I(\pi/2)$ is the intensity as seen down the polar axis. |
The intrinsic and apparent axis ratios. g and p. are related to @ via Γρ”ια(oblate)cos”:= |-d21»(prolate). | The intrinsic and apparent axis ratios, $q$ and $p$, are related to $\theta$ via ^2 &=& ) ^2 &=& ). |
sin3= In both cases. the value p=] refers to the case in which the object is viewed along the polar axis. and therefore has a circular projection. | In both cases, the value $p = 1$ refers to the case in which the object is viewed along the polar axis, and therefore has a circular projection. |
Let us assume. in the first approximation. that: (1) the cores are randomly oriented. and (ii) 7, does not vary from one core to the next in à population of either all-oblate or all-prolate spheroids. | Let us assume, in the first approximation, that: (i) the cores are randomly oriented, and (ii) $I_p$ does not vary from one core to the next in a population of either all-oblate or all-prolate spheroids. |
Then the observed intensity 7 will increase towards p—bam the prolate case. and decrease towards p=1 in the oblate case. | Then the observed intensity $I$ will increase towards $p=1$ in the prolate case, and decrease towards $p=1$ in the oblate case. |
Specifically. the expected slopes in a (log 7. log p) plot are +1 and —1. respectively (throughout this paper. log denotes log;o). [ | Specifically, the expected slopes in a (log $I$, log $p$ ) plot are $+1$ and $-1$, respectively (throughout this paper, log denotes $_{10}$ ). [ |
For applications in the context of elliptical galaxies. see Marchant Olson (1979). Richstone (1979). and Olson de Vaucouleurs (1981).] | For applications in the context of elliptical galaxies, see Marchant Olson (1979), Richstone (1979), and Olson de Vaucouleurs (1981).] |
In Figures 2 and 3 we plot the relation between log / and log p for each subsample of the combined continuum dataset. | In Figures 2 and 3 we plot the relation between log $I$ and log $p$ for each subsample of the combined continuum dataset. |
The sample of Chint et ((1997) is shown in Figure 2a. | The sample of Chini et (1997) is shown in Figure $a$. |
This sample contains only 21 data points. and while there ts some suggestion of an increasing trend of J with p. it is not statistically significant. | This sample contains only 21 data points, and while there is some suggestion of an increasing trend of $I$ with $p$, it is not statistically significant. |
The same is true of the Motte et ((1998) data from Ophiuchus. shown in Figure 25. | The same is true of the Motte et (1998) data from Ophiuchus, shown in Figure $b$. |
While the above two samples show no significant trend. the Orion B dataset of MOI (N=64 resolved objects). shown in Figure 3a. is more definitive. | While the above two samples show no significant trend, the Orion B dataset of M01 $N = 64$ resolved objects), shown in Figure $a$, is more definitive. |
Although there 1s considerable scatter. a correlation does exist between log { and log p. | Although there is considerable scatter, a correlation does exist between log $I$ and log $p$. |
The linear (parametric) correlation coefficient (C.C.) is 0.35. with a significance of greater than 99 percent. | The linear (parametric) correlation coefficient (C.C.) is 0.35, with a significance of greater than 99 percent. |
Under the more general assumption that the underlying distributions of / and p are not binormal. we can perform the nonparametric Spearman and Kendall (rank correlation) tests. | Under the more general assumption that the underlying distributions of $I$ and $p$ are not binormal, we can perform the nonparametric Spearman and Kendall (rank correlation) tests. |
These give a coefficient of 0.29 and a significance of 98 percent. | These give a coefficient of 0.29 and a significance of 98 percent. |
The point at dog p. log 7) 7(-0.05. is clearly an outlier. | The point at (log $p$, log $I$ ) $\simeq (-0.05, 4)$ is clearly an outlier. |
It corresponds to NGC IRS. a known4) outflow source. | It corresponds to NGC 2071--IRS, a known outflow source. |
Since we wish to focus on starless cores in this study. we exclude it from further This lowers the rank C.C. to 0.27 with a significance of 96.3 percent. | Since we wish to focus on starless cores in this study, we exclude it from further This lowers the rank C.C. to 0.27 with a significance of 96.3 percent. |
The best-fit straight line to the data is given by log T=AlogpB. with A=0.50+£0.18 and B=2.563:0.06. | The best-fit straight line to the data is given by log $I = A~{\rm log}~p + B$, with $A = 0.50 \pm 0.18$ and $B = 2.56 \pm 0.06$. |
The above fit was performed neglecting the stated observational errors in log 7 and log p (32). | The above fit was performed neglecting the stated observational errors in log $I$ and log $p$ \ref{sec-data}) ). |
While this might be considered reprehensible. we found that including the errors gave a goodness-of-fit parameter that was too low to be acceptable by the usual standard (>107: Press et 11992). | While this might be considered reprehensible, we found that including the errors gave a goodness-of-fit parameter that was too low to be acceptable by the usual standard $\gae 10^{-3}$; Press et 1992). |
This result does not cast aspersions on the validity of the correlation stated above (which does not depend on the errors). nor need it necessarily lower our confidence in the fitted values of A and B. | This result does not cast aspersions on the validity of the correlation stated above (which does not depend on the errors), nor need it necessarily lower our confidence in the fitted values of $A$ and $B$. |
Rather. it is a familiar feature of data that have a scatter larger than the formal errors. | Rather, it is a familiar feature of data that have a scatter larger than the formal errors. |
In particular. it indicates that the uncertainties ascribed to 7 are We present ample support for this statement. along with a consistency check of the above fitted parameters. in $5.5.. | In particular, it indicates that the uncertainties ascribed to $I$ are We present ample support for this statement, along with a consistency check of the above fitted parameters, in \ref{sec-simul}. |
There amore robust analysis is used to determine the model goodness-of-fit for the data (specifically. the Monte Carlo simulation of synthetic data sets). | There a more robust analysis is used to determine the model goodness-of-fit for the data (specifically, the Monte Carlo simulation of synthetic data sets). |
Many of the cores (18/82. or 22 percent) in the sample are unresolved. and therefore are not included in the above fit. | Many of the cores (18/82, or 22 percent) in the sample are unresolved, and therefore are not included in the above fit. |
Interestingly. despite the fact that all are So detections. none has a peak intensity exceeding 0.25 Jy/beam. | Interestingly, despite the fact that all are $\sigma$ detections, none has a peak intensity exceeding 0.25 Jy/beam. |
If the apparent ellipticities of the unresolved cores are distributed in the same way as the rest of the sample. this then suggests that there are more elongated than round sources amongst this | If the apparent ellipticities of the unresolved cores are distributed in the same way as the rest of the sample, this then suggests that there are more elongated than round sources amongst this sub-population. |
Finally. we note that while the observed slope of the above | Finally, we note that while the observed slope of the above |
damp eccentricity. and paraicterize the efficiency of the damping via a bulk viscosity a, written iu tenus of a Shakura-Sunvacy (1973) a parameter. | damp eccentricity, and parameterize the efficiency of the damping via a bulk viscosity $\alpha_e$ written in terms of a Shakura-Sunyaev (1973) $\alpha$ parameter. |
Linearizatiou of the two-dimensional fluid equations (in the inviscid lait. except for the aforementioned bulk viscosity) vields an evolution equation for the ecceutricity (CoodechildOeilvie 2006). The first two terms on the right hand side describe precession driven by anv uou-WNeplerian part of the disk potential and by pressure eradicuts within the disk. | Linearization of the two-dimensional fluid equations (in the inviscid limit, except for the aforementioned bulk viscosity) yields an evolution equation for the eccentricity \citep{goodchild06}, The first two terms on the right hand side describe precession driven by any non-Keplerian part of the disk potential and by pressure gradients within the disk. |
These terms do not change the maeguitude of the eccentricity. | These terms do not change the magnitude of the eccentricity. |
The third term has the form of a Schréoddingcer equation it describes waves of eccentricity that propagate racially through the disk aud are damped by the action of viscosity. | The third term has the form of a Schröddinger equation – it describes waves of eccentricity that propagate radially through the disk and are damped by the action of viscosity. |
Theoretically. it is expected that accretion clisks in Active Calactic Nuclei (ACN) ought.| to be selt-eravitating at the relatively laree radi where masmg occurs, aud this peruüts some simplification of the evolution equation. | Theoretically, it is expected that accretion disks in Active Galactic Nuclei (AGN) ought to be self-gravitating at the relatively large radii where masing occurs, and this permits some simplification of the evolution equation. |
We write the surface deusity as a power-law in radius. and compute the disk poteutial Pain from the enclosed disk nass assumndue a spherically svuuuctric mass distribution. | We write the surface density as a power-law in radius, and compute the disk potential $\Phi_{\rm disk}$ from the enclosed disk mass assuming a spherically symmetric mass distribution. |
We asstune that over the relatively narrow radial rauge for which masing occurs the souud speed e; can be taken (approximately) to be constaut. aud note that p2//2h and that fh=c,/0. | We assume that over the relatively narrow radial range for which masing occurs the sound speed $c_s$ can be taken (approximately) to be constant, and note that $\rho \simeq \Sigma / 2h$ and that $h = c_s / \Omega$. |
The rate of precession due to pressure eradicuts is thon X(2 (a coustant at the radii where lasing occurs). while the rate of precession due to the uon-Iepleriau poteutial is XX. which rises with the diskinass?. | The rate of precession due to pressure gradients is then $\propto
c_s^2$ (a constant at the radii where masing occurs), while the rate of precession due to the non-Keplerian potential is $\propto \Sigma_0$, which rises with the disk. |
. Their ratio. therefore depeuds upon the disk mass — iu low mass disks precession will be dominated by the pressure term while in higher mass disks eravity will dominate. | Their ratio, therefore depends upon the disk mass – in low mass disks precession will be dominated by the pressure term while in higher mass disks gravity will dominate. |
The latter hiat is probably appropriate for lasing disks. | The latter limit is probably appropriate for masing disks. |
At the radii of the order of a tenth of a pe where the masing ds observed it ds likely that disks around supermassive black holes are selferavitating (Iolvchalov&Sunvacy1980:Clarke19885:Shlosiman.Beecluan&Frank1990:Coodman 2003). | At the radii – of the order of a tenth of a pc – where the masing is observed it is likely that disks around supermassive black holes are self-gravitating \citep{kolychalov80,clarke88,
shlosman90,goodman03}. |
. Selferavitatius disks develop spiral structure. whose existence in the NCC 1258 disk is linted at bv observations of clustering and asviuuetry iu the mascr enisson regious (Maoz1995:Maoz&Melxee1998). | Self-gravitating disks develop spiral structure, whose existence in the NCG 4258 disk is hinted at by observations of clustering and asymmetry in the maser emission regions \citep{maoz95,maoz98}. |
. For a selferavitating disk ΑΠλέων~Gr)Ἡ, Efe)1eran~Pfr. aud pressure effects are negligible. | For a self-gravitating disk $M_{\rm BH} / M_{\rm disk} \approx (h/r)^{-1}$, $\vert \dot{E}_{\rm p} \vert / \vert \dot{E}_{\rm grav} \vert \sim
h/r$, and pressure effects are negligible. |
ees Writingriting p=Ξpe;pel the evolution. equation (3)) then sinplifies to. We study the eccentricity evolution nuplied by this equation in 8223. | Writing $p = \rho c_s^2$ the evolution equation \ref{eq_evolve}) ) then simplifies to, We study the eccentricity evolution implied by this equation in 3. |
Equation (3)) is an extremely simple represcutation of the evolution of an eccentric fluid disk. | Equation \ref{eq_evolve}) ) is an extremely simple representation of the evolution of an eccentric fluid disk. |
The most obvious limitation is the use of a linear equation rather than the nonlinear formalisu, developed by Ovilwic(2001). | The most obvious limitation is the use of a linear equation rather than the nonlinear formalism developed by \cite{ogilvie01}. |
. The linear equation ought to provide an approximate description of the dynamics at late times. when the eccentricity is πια. but will evidently fail if the iitial eccentricity and / or its variation with radius is large. | The linear equation ought to provide an approximate description of the dynamics at late times, when the eccentricity is small, but will evidently fail if the initial eccentricity and / or its variation with radius is large. |
A second and even iore important lanitation concerus the uncertain nature of the eccentricity damping. | A second and even more important limitation concerns the uncertain nature of the eccentricity damping. |
We have parameterized the damping via a bulk viscosity rather than the usual shear viscosity used in the Shakura-Suuvaev theory of accretion disks because disks dominated by a Navier-Stokes shear viscosity are uustable to of ecceutric modes (Nato1983:Ovilvic 2001). | We have parameterized the damping via a bulk viscosity – rather than the usual shear viscosity used in the Shakura-Sunyaev theory of accretion disks – because disks dominated by a Navier-Stokes shear viscosity are unstable to of eccentric modes \citep{kato83,ogilvie01}. |
. This is probably not a physical problem. rather it reflects the fact that angular momentui transport mediated by the maguetorotational instability (Balbus&Hawley 1998).. sclf-eravity. or other physical wechanisis cannot be well described via ai Navier-Stokes shear viscosity. | This is probably not a physical problem, rather it reflects the fact that angular momentum transport mediated by the magnetorotational instability \citep{balbus98}, self-gravity, or other physical mechanisms cannot be well described via a Navier-Stokes shear viscosity. |
For our purposes we simply assune that the stress dn the disk acts such as to damp eccentricity. paralucterize that damping cfiicicncy (arbitrarily) via a bulk viscosity. aud treat a, as a free parameter. | For our purposes we simply assume that the stress in the disk acts such as to damp eccentricity, parameterize that damping efficiency (arbitrarily) via a bulk viscosity, and treat $\alpha_e$ as a free parameter. |
The terms dn equations (3)) and (7)) describing precession do not alter the magnitude of the disk eccentricity. | The terms in equations \ref{eq_evolve}) ) and \ref{eq_simplified}) ) describing precession do not alter the magnitude of the disk eccentricity. |
The wave-like term proportional to ~ change the local eccentricity, but preserves ai global invariant (Ctoodchild&Oegilvie2006).. Damping: of o2£ occurs due to the viscous. teri at a rate The presence of eccentricity waves cans that the radial profile of £ ueeds to be cousidered aloug with the temporal evolution. | The wave-like term proportional to $\gamma$ change the local eccentricity, but preserves a global invariant \citep{goodchild06}, Damping of ${\cal{E}}^2$ occurs due to the viscous term at a rate The presence of eccentricity waves means that the radial profile of $E$ needs to be considered along with the temporal evolution. |
This requires a uuucerical solution of equation (7)). which we defer to 8233.2. | This requires a numerical solution of equation \ref{eq_simplified}) ), which we defer to 3.2. |
For au estimate. however. we can define a local damping timescale. | For an estimate, however, we can define a local damping timescale, |
A periodogram constructed from the radial velocities. selected an unambiguous period. and a sinusoidal fit of the form e(f)=>|Wsinj2a(tTo)/P] gave with an RMS residual of oulv 8 kin 1... | A periodogram constructed from the radial velocities, selected an unambiguous period, and a sinusoidal fit of the form $v(t) = \gamma + K \sin [2 \pi (t - T_0) / P]$ gave with an RMS residual of only $8$ km $^{-1}$. |
The initial epoch Ty corresponds to the inferior conjunction of the primary. | The initial epoch $T_0$ corresponds to the inferior conjunction of the primary. |
Figue 2. shows the spectroscopic trail obtained at MDAL Observatory: Πα and 2AAG3LF. 6371 clearly trace the primary orbit bolstering the plotospleric identification of the silicon lines. | Figure \ref{fig2} shows the spectroscopic trail obtained at MDM Observatory: $\alpha$ and $\lambda\lambda$ 6347, 6371 clearly trace the primary orbit bolstering the photospheric identification of the silicon lines. |
Wo found uo spectroscopic signatures of the faint secondary star. | We found no spectroscopic signatures of the faint secondary star. |
The folded radial velocity curve follows a circular orbit (Fig. 2)). | The folded radial velocity curve follows a circular orbit (Fig. \ref{fig2}) ). |
The period aud A-velocity imply a mass function for the secondary Or. asstuune QeAf;=0.185+0.010iusun.. Mo2O86nisun.. so the companion must be a compact object. | The period and $K$ -velocity imply a mass function for the secondary or, assuming $M_1=0.185\pm0.010$, $M_2\ga 0.86$, so the companion must be a compact object. |
If the unseen companion is below the Chandrasekhar uut Ah=135iisun.. then the inclination /2607. | If the unseen companion is below the Chandrasekhar limit $M_2\la 1.35$, then the inclination $i\ga60^\circ$. |
No radio sources are found in the vicinitv of the ELM. white dwarf iu the NRAO-VLA Skv Survey (NVSS) with a seusitivitv of ~(0. 5nuuJv at 11400 MIIZ (Coudouetal.1998).. contrasting with the detection of the milli-secoud pulsar PSR J1012;52307 iu the NWSS (hKaplanetal.1998) and other radio observations (Nicastroetal.1995). | No radio sources are found in the vicinity of the ELM white dwarf in the NRAO-VLA Sky Survey (NVSS) with a sensitivity of $\sim0.5$ mJy at 1400 MHz \citep{con1998}, contrasting with the detection of the milli-second pulsar PSR J1012+5307 in the NVSS \citep{kap1998} and other radio observations \citep{nic1995}. |
. Pulsar companious to ELM. white chwarfs are relatively rare (Aeiicrosetal.20090) and we couclude that the companion to the ELM white dwarfGALEN J1717|6757 Is a luassive white dwarf. | Pulsar companions to ELM white dwarfs are relatively rare \citep{agu2009} and we conclude that the companion to the ELM white dwarfGALEX J1717+6757 is a massive white dwarf. |
We folded the Dialkóww photometric time series on our ephemeris. | We folded the kóww photometric time series on our ephemeris. |
Iucludiug all V. data. the time series folde« ou half the period has a weak amplitude of 1.50. nae and a maxiuun at phase 0.30+0.02 (statistica error only}. i.e. close to phase 0.25 expected for ellipticity fect. | Including all $V$ data, the time series folded on half the period has a weak amplitude of $1.5\pm0.4$ mmag and a maximum at phase $0.30\pm0.02$ (statistical error only), i.e. close to phase 0.25 expected for ellipticity effect. |
Using (Popper&Etzel1981) we verified that the amplitude calculated from the mode for the svsteni parameters agrees with the observe uplitude. | Using \citep{pop1981} we verified that the amplitude calculated from the model for the system parameters agrees with the observed amplitude. |
The V. time series folded ou the period has a stronger amplitude of 2.240. {πας with a maxi at phase 0.81 250.03. Ίνοι, also zz20 from phase 0.75 expectec for relativistic bezug. | The $V$ time series folded on the period has a stronger amplitude of $2.2\pm0.4$ mmag with a maximum at phase $0.81\pm0.03$ , i.e., also $\approx 2\sigma$ from phase 0.75 expected for relativistic beaming. |
Figure 3 shows the folded V | Figure \ref{fig3} shows the folded $V$ |
drawn. | drawn. |
We calculated aox for the reference sample in an identical fashion to our absorbed QSO sample except that we assume no intrinsic X-ray absorption and ay=0.98 for the RINOS AGN. | We calculated $\alpha_{OX}$ for the reference sample in an identical fashion to our absorbed QSO sample except that we assume no intrinsic X-ray absorption and $\alpha_{X}=0.98$ for the RIXOS AGN. |
The reference sample has a mean OON)—149 and a standard deviation ex=0.16: the distribution of eox for the reference saniple is shown in lig. 5.. | The reference sample has a mean $\langle \alpha_{OX}\rangle =
1.49$ and a standard deviation $\sigma_{OX} = 0.16$ ; the distribution of $\alpha_{OX}$ for the reference sample is shown in Fig. \ref{fig:rixosalphaox}. |
For comparison. the SDSS sample presented. in Stratevactal.(2005). has a very similar clistribution of ων. With faoxy?=1:15 and σων=0.15. | For comparison, the SDSS sample presented in \citet{strateva05} has a very similar distribution of $\alpha_{OX}$, with $\langle \alpha_{OX}\rangle = 1.48$ and $\sigma_{OX} = 0.18$. |
In "Table 3 we see that with the exception. of RAJIP4913.. the absorbed QSOs have aox values within two standard. deviations. of faox) for the reference distribution. | In Table \ref{tab:modelfits} we see that with the exception of , the absorbed QSOs have $\alpha_{OX}$ values within two standard deviations of $\langle \alpha_{OX}\rangle$ for the reference distribution. |
ForNJ124913.. the level of cliserepancy depends strongly on the N-ray spectral model. | For, the level of discrepancy depends strongly on the X-ray spectral model. |
Ehe ionized absorber fit gives the most consistent oox value. at 2.3 standard deviations from the mean of the reference sample. while the Gt with a cold. absorber and. fitted ax οἶνος the most discrepant value of aoy=1.96. -2.9) standard ceviations from the mean of the reference sample. | The ionized absorber fit gives the most consistent $\alpha_{OX}$ value, at 2.3 standard deviations from the mean of the reference sample, while the fit with a cold absorber and fitted $\alpha_{X}$ gives the most discrepant value of $\alpha_{OX} =
1.96$, $> 2.9$ standard deviations from the mean of the reference sample. |
Indeed. this value of aox is larger than anv eox in the RINOS reference sample or the SDSS sample of Stratevaetal.(2005).. suggesting that the model with a cold absorber and the continuum slope fitted asa free varameter would also require a highly: unusual spectra energy. distribution for124913. | Indeed, this value of $\alpha_{OX}$ is larger than any $\alpha_{OX}$ in the RIXOS reference sample or the SDSS sample of \citet{strateva05}, suggesting that the model with a cold absorber and the continuum slope fitted asa free parameter would also require a highly unusual spectral energy distribution for. |
While thas rather twpical values of aox in Table 3... we note hat if we correct for the intrinsic extinction. equivalen o E(B V)=0.2. suggested by the UV. continuum shape (Section 3.1)). the ax would increase by 0.40. Ieacing to an abnormal αων for the cold absorber. fitted ἂν mode or this source as well as for11NJ124913. | While has rather typical values of $\alpha_{OX}$ in Table \ref{tab:modelfits}, we note that if we correct for the intrinsic extinction equivalent to $-$ V)=0.2, suggested by the UV continuum shape (Section \ref{sec:uvlines}) ), the $\alpha_{OX}$ would increase by 0.40, leading to an abnormal $\alpha_{OX}$ for the cold absorber, fitted $\alpha_{X}$ model for this source as well as for. |
. Overall. the ionized. absorber model is. consisten with the five QSOs having unremarkable underlving X-rav continua ancl optical to N-rav. spectral energy distributions. | Overall, the ionized absorber model is consistent with the five QSOs having unremarkable underlying X-ray continua and optical to X-ray spectral energy distributions. |
In contrast. if the X-ray absorbers are modeled as cold. gas. the QSOs require a combination of cold absorption. unusual X-ray continua. ancl unusual optical to N-rav spectral energy distributions. | In contrast, if the X-ray absorbers are modeled as cold gas, the QSOs require a combination of cold absorption, unusual X-ray continua, and unusual optical to X-ray spectral energy distributions. |
\We therefore: consider. that the ionized absorber model provides a simpler. less contrived solution than the mocel in which the X-ray absorber is cold. | We therefore consider that the ionized absorber model provides a simpler, less contrived solution than the model in which the X-ray absorber is cold. |
We also note that the presence of UY absorption lines with EW25 in the restframe UV spectra of all five QSOs (and SLIIV. in aancl 15NJ163308)). provides. independent: confirmation that these objects are viewed through columns of ionized eas. | We also note that the presence of IV absorption lines with $>5$ in the restframe UV spectra of all five QSOs (and IV in and ) provides independent confirmation that these objects are viewed through columns of ionized gas. |
Therefore. in what follows we adopt. the. ionized absorber fits as the best description of the N-ray spectra. | Therefore in what follows we adopt the ionized absorber fits as the best description of the X-ray spectra. |
Our study has revealed absorption from ionizecl gas in both the rest-frame UV. spectra. ancl in the X-ray spectra of our sample of X-ray absorbed QSOs. | Our study has revealed absorption from ionized gas in both the rest-frame UV spectra and in the X-ray spectra of our sample of X-ray absorbed QSOs. |
Inthe nearby Universe. ionized absorbersare common in Seyfert ealaxies (e.g.—Revnolcls.1997:Georgeοἱal.. ο... and have been studied in some detail (Blustinοἱal. 2005).. | Inthe nearby Universe, ionized absorbersare common in Seyfert galaxies \citep[e.g. ][]{reynolds97,george98}, , and have been studied in some detail \citep{blustin07,steenbrugge05}. . |
Therefore in trving to | Therefore in trying to |
there is a detection of a flare. | there is a detection of a flare. |
Subsets and Splits
No saved queries yet
Save your SQL queries to embed, download, and access them later. Queries will appear here once saved.