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As found by Oliveretal.(2010) and. Clementsetal. (2010)... most published models significantly over-predict the number of bright sources at these wavelengths and have shallower slopes.
As found by \citet{Oliver:2010b} and \citet{Clements:2010}, most published models significantly over-predict the number of bright sources at these wavelengths and have shallower slopes.
We tind somewhat better agreement at fainter fluxes. at or below the break. but the agreement is still not perfect.
We find somewhat better agreement at fainter fluxes, at or below the break, but the agreement is still not perfect.
Our main systematic uncertanties arise from οι understanding of the SPIRE —beams.
Our main systematic uncertanties arise from our understanding of the SPIRE beams.
We find that a high-pass filter is etfective in removing the signature of clustering from our counts. but in the future it may be preferable to attempt to directly marginalize over clustering using simple models.
We find that a high-pass filter is effective in removing the signature of clustering from our counts, but in the future it may be preferable to attempt to directly marginalize over clustering using simple models.
These observations represent only ~60 hours of the 900 hours of observations that HerMES will ultimately obtain (although not all of these are with SPIRE).
These observations represent only $\sim 60$ hours of the 900 hours of observations that HerMES will ultimately obtain (although not all of these are with SPIRE).
The final dataset will cover a wide range of depths and areas.
The final dataset will cover a wide range of depths and areas.
This will significantly increase our ability to constrain dN/dS.
This will significantly increase our ability to constrain $dN/dS$.
Having a number of well-seperated deep fields will also allow a direct measurement of sample variance.
Having a number of well-seperated deep fields will also allow a direct measurement of sample variance.
The authors would like to thank Guillaume Patanchon and Phil Maloney for many useful discussions.
The authors would like to thank Guillaume Patanchon and Phil Maloney for many useful discussions.
J. Glenn and A. Conley acknowledge support from NASA Herschel GTO grant 1394366. sponsored by the Jet Propulsion Laboratory.
J. Glenn and A. Conley acknowledge support from NASA Herschel GTO grant 1394366, sponsored by the Jet Propulsion Laboratory.
SPIRE has been developed by a consortium of institutes led by Carditf (UK) and including LLethbridge (Canada): NAOC (China: CEA. LAM (France): IPSI. PPadua (italy): IAC (Spain): Stockholm Observatory (Sweden): Imperial College London. RAL. UCL-MSSL. UKATC. SSussex (UK): Caltech. JPL. NHSC. CColorado (USA).
SPIRE has been developed by a consortium of institutes led by Cardiff (UK) and including Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Padua (italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Sussex (UK); Caltech, JPL, NHSC, Colorado (USA).
This developement has been supported by national funding agencies: CSA (Canada NAOC (China): CEA. CNES. CNRS (France): AST (Italy: MCINN (Spain): SNSB (Sweden): STFC (UK): and NASA (USA).
This developement has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).
The data presented in this paper will be released through theHerschel Database in Marseille. HeDaM thttpz//hedam.oamp-fr/HerMES».
The data presented in this paper will be released through the Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES).
given velocity dispersion. the mean surface density within an elfective radius is too low.
given velocity dispersion– the mean surface density within an effective radius is too low.
In order to match these observed: properties of elliptical galaxies with MOND. it is necessary to exploit other degrees of freedom: models must deviate from being strictly isothermal with a fixed degree of orbital anisotropy.
In order to match these observed properties of elliptical galaxies with MOND, it is necessary to exploit other degrees of freedom: models must deviate from being strictly isothermal with a fixed degree of orbital anisotropy.
In order to explore these possible degrees of freedom. Sanders (2000) has considered. polvtropic spheres with an anisotropy. parameter. 3=1o,2σι. which.. varies. systematically with radius as in the Osipkov-Moerritt models. jmoatf(r|ora) (ns ds the anisotropy radius. Binney ‘Tremaine LOST).
In order to explore these possible degrees of freedom, Sanders (2000) has considered polytropic spheres with an anisotropy parameter, $\beta = 1-{\sigma_t}^2/{\sigma_r}^2$, which varies systematically with radius as in the Osipkov-Merritt models, $\beta = r^2/(r^2+{r_a}^2)$, $r_a$ is the anisotropy radius, Binney Tremaine 1987).
For a polytropic sphere of index η the racial velocity dispersion-density relationship is given by where ;l is a constant {0» Corresponds to the isothermal sphere).
For a polytropic sphere of index $n$ the radial velocity dispersion-density relationship is given by where $A$ is a constant $n\rightarrow \infty$ corresponds to the isothermal sphere).
Lt was found that a range 12«nκ16 was sullicient to match the the mean value and. wide dispersion of elfective radius for a given velocity dispersion. provided that the anisotropy radius also varies over the range 2«έν<25.
It was found that a range $12<n<16$ was sufficient to match the the mean value and wide dispersion of effective radius for a given velocity dispersion, provided that the anisotropy radius also varies over the range $2<r_a/r_{eff}<25$.
πο luminosity or mass density distribution within these objects is similar to that. of a Jalle model (Jalle 1982): within roughly rep the density falls as r7 and. beyond. steepens. tor
The luminosity or mass density distribution within these objects is similar to that of a Jaffe model (Jaffe 1982): within roughly $r_{eff}$ the density falls as $r^{-2}$ and beyond steepens to $r^{-4}$.
Sphericallv symmetric N-body caleulations with MONDian moclifice eravitv (Bekenstein Alilerom 1984). demonstrate that objects resembling such Large à polvtropic spheres may actualy condense and. recollapse out of the Hubble. flow (Sanders 2008).
Spherically symmetric N-body calculations with MONDian modified gravity (Bekenstein Milgrom 1984) demonstrate that objects resembling such large $n$ polytropic spheres may actually condense and recollapse out of the Hubble flow (Sanders 2008).
Each model. characterised by a particular value of n and ρε. exhibits its own exact ALox6! relationship but for all models combined there is a large dispersion in this relation.
Each model, characterised by a particular value of $n$ and $r_a/r_{eff}$, exhibits its own exact $M\propto \sigma^4$ relationship but for all models combined there is a large dispersion in this relation.
None-the-less. in spite of the dispersion. in homology. the moclels lie on a narrow fundamental plane where 6,2 and ο are the velocity dispersion. and the average surface density respectively within r.55/2 (the coellicients here diller slightly from those given hy Sanders because of scaling to rr rp/2).
None-the-less, in spite of the dispersion in homology, the models lie on a narrow fundamental plane where $\sigma_{e2}$ and $\Sigma_{e2}$ are the velocity dispersion and the average surface density respectively within $r_{eff}/2$ (the coefficients here differ slightly from those given by Sanders because of scaling to $r_{eff}/2$ ).
This is seen to be quite close to the Newtonian virial expectation and within the errors of the more Fundamental plane defined bv the gravitational lenses.
This is seen to be quite close to the Newtonian virial expectation and within the errors of the more fundamental plane defined by the gravitational lenses.
In fact. both the MOND and lensing fundamental planes are well-approximated by the virial relation for Newtonian Jalle nmoclels.
In fact, both the MOND and lensing fundamental planes are well-approximated by the virial relation for Newtonian Jaffe models.
As above. the MOND fundamental plane relation may be expressed. in terms of a MOND FP mass (projected within r.rr/2) as a function of the dimensional mass unit στηςδές.
As above, the MOND fundamental plane relation may be expressed in terms of a MOND FP mass (projected within $r_{eff}/2$ ) as a function of the dimensional mass unit $\sigma^2 r_{eff}/2G$.
This is shown by the thick line in 11.
This is shown by the thick line in 1.
This is the original ensemble of 360 anisotropic. polvtropic models covering the range described above.
This is the original ensemble of 360 anisotropic, polytropic models covering the range described above.
We see that it is almost coincident with the observations of Bolton et al.
We see that it is almost coincident with the observations of Bolton et al.
We may also apply the MOND fundamental plane relation in order to calculate the mass of a lens galaxy. projected within rey¢/2. from. the observed. velocity dispersion and ellective radius.
We may also apply the MOND fundamental plane relation in order to calculate the mass of a lens galaxy, projected within $r_{eff}/2$, from the observed velocity dispersion and effective radius.
Εις caleulated MOND FP mass is plotted against the observed lensing mass in 22.
This calculated MOND FP mass is plotted against the observed lensing mass in 2.
Lt is evident that the MOND EP mass is closely proportional to the lens mass. but about less on average.
It is evident that the MOND FP mass is closely proportional to the lens mass, but about less on average.
This is understancable because the MOND FP mass is the total projected barvonie mass: the lensing mass. however. includes a phantom dark matter contribution because. MOND. or its relativistic extension. TeVes (Bekenstein 2004). provides extra dellection along the line-of-sight. (Alortloek& 2006).
This is understandable because the MOND FP mass is the total projected baryonic mass; the lensing mass, however, includes a phantom dark matter contribution because MOND, or its relativistic extension, TeVeS (Bekenstein 2004), provides extra deflection along the line-of-sight \cite{mt01,zeal06}.
. lt is of interest to compare the MOND M/L. values with population svnthesis models.
It is of interest to compare the MOND M/L values with population synthesis models.
In 33 (lower panel) he indicated ML values within +,55/2 are plotted against rὁ colour ancl compared. to the theoretical models. of Bell οἱ al. (
In 3 (lower panel) the indicated M/L values within $r_{eff}/2$ are plotted against $r-i$ colour and compared to the theoretical models of Bell et al. (
2003).
2003).
The luminosities have been determined rom the observed Sloan magnitudes applying both Ix- and evolutionary corrections (Pogeianti 1907) and reduced by a actor of about three to correspond to that within rr5/2.
The luminosities have been determined from the observed Sloan magnitudes applying both K- and evolutionary corrections (Poggianti 1997) and reduced by a factor of about three to correspond to that within $r_{eff}/2$.
We see that MOND ML values closely track the theoretical values.
We see that MOND M/L values closely track the theoretical values.
The upper panel is the same except that the ML is hat determined from the projected lensing mass.
The upper panel is the same except that the M/L is that determined from the projected lensing mass.
Again the same trend is present although the ollset discussed above is evident.
Again the same trend is present although the offset discussed above is evident.
The current. multi-Gcld relativistic extensions of MOND. such as TeVes. are characterisecl by a physical metric which is distinct [rom the Einstein. or gravitational. metric.
The current multi-field relativistic extensions of MOND, such as TeVeS, are characterised by a physical metric which is distinct from the Einstein, or gravitational, metric.
The transformation between the two metrics is “cisformal” and chosen such that the relationship between the total weak Ποιά. gravitational force. ancl the cellection of. photons. is identical to that of General Relativity: specifically. the dellection angle is given by where the integral is along the line of sight and
The transformation between the two metrics is “disformal” and chosen such that the relationship between the total weak field gravitational force and the deflection of photons is identical to that of General Relativity; specifically, the deflection angle is given by where the integral is along the line of sight and
used here.
used here.
Such a sampler might be expected to. reduce the run-time of the method. which (compared to a clirec inversion or a downhill simplex \> minimisation) is ils major disadvantage: to produce cach posterior clistribution shown in the figures of this paper à computation time of several hours with a 1 Gllz processor was required.
Such a sampler might be expected to reduce the run-time of the method, which (compared to a direct inversion or a downhill simplex $\chi^2$ minimisation) is its major disadvantage: to produce each posterior distribution shown in the figures of this paper a computation time of several hours with a 1 GHz processor was required.
The evidence calculation takes rather longer. since the numerica precision comes from repeated posterior explorations.
The evidence calculation takes rather longer, since the numerical precision comes from repeated posterior explorations.
The computation time scales approximately as NanaNyrauueters (?).. prompting careful design of the sampler anc likelihood calculation.
The computation time scales approximately as $N_{\rm data} \times N_{\rm parameters}$ \citep{MCMC}, prompting careful design of the sampler and likelihood calculation.
However. the alternatives for coping with noisy cata can be just as time consuming: for instance resampling of the data to generate confidence limits (e.g.2) cllectively performs the same caleulations as the ALCALIC process. but with more limited. output.
However, the alternatives for coping with noisy data can be just as time consuming; for instance resampling of the data to generate confidence limits \citep[\eg][]{COS/All++03} effectively performs the same calculations as the MCMC process, but with more limited output.
Nevertheless. it is the computational cost of the method that is perhaps the most urgent aspect to be addressed in further work.
Nevertheless, it is the computational cost of the method that is perhaps the most urgent aspect to be addressed in further work.
We have developed an algorithm based. on the Markov-Chain Monte-Carlo. technique for. investigating simple but. manv-parameter models. of. elusters.
We have developed an algorithm based on the Markov-Chain Monte-Carlo technique for investigating simple but many-parameter models of clusters.
Lhe method allows straightforward inclusion of many datasets. correctly weighting cach catapoint according to its assumed likelihood: by exploring the posterior probability distribution rather than the likelihood we can incorporate information on the cluster from. other sources. via. the parameter prior densities.
The method allows straightforward inclusion of many datasets, correctly weighting each datapoint according to its assumed likelihood; by exploring the posterior probability distribution rather than the likelihood we can incorporate information on the cluster from other sources via the parameter prior densities.
Calculation of the Bayesian evidence by thermodynamic integration during the burn-in period can be done to sullicient accuracy to allow different astrophysical models to be compared: this statistic automatically includes the common-sense of Occam's razor. allowing movement away from the simplest assumed mocdels only when the data require it.
Calculation of the Bayesian evidence by thermodynamic integration during the burn-in period can be done to sufficient accuracy to allow different astrophysical models to be compared; this statistic automatically includes the common-sense of Occam's razor, allowing movement away from the simplest assumed models only when the data require it.
Applying the method to simulated weak gravitational lensing ancl interferometric Sunvaev-Zel'dovich. οσοι data we draw the following conclusions: This last. point is one worth returning to: under the assumption of a Universal cluster gas fraction the mocel-independent inference for cach independent: member of a sample of IN. clusters can be combined. by straightforward multiplication. of their posterior. probability: distributions. reducing the uncertainty on this parameter by a factor of approximately ON’.
Applying the method to simulated weak gravitational lensing and interferometric Sunyaev-Zel'dovich effect data we draw the following conclusions: This last point is one worth returning to; under the assumption of a Universal cluster gas fraction the model-independent inference for each independent member of a sample of $N$ clusters can be combined by straightforward multiplication of their posterior probability distributions, reducing the uncertainty on this parameter by a factor of approximately $\sqrt N$
models have been proposed to explain quasar variability (e.g.Lyubarskii
models have been proposed to explain quasar variability \citep[e.g.][]{lyubarskii1997}.
In this Letter, we demonstrate that for the observed 1997)..variability characteristics, such an inhomogeneous disk can simultaneously explain multiple discrepancies between AGN observations and accretion disk theory.
In this Letter, we demonstrate that for the observed variability characteristics, such an inhomogeneous disk can simultaneously explain multiple discrepancies between AGN observations and accretion disk theory.
Inhomogeneous disks can be large enough to explain the microlensing observations, while their temperature fluctuations on small spatial scales naturally explain the observed simultaneous variability across optical wavelengths.
Inhomogeneous disks can be large enough to explain the microlensing observations, while their temperature fluctuations on small spatial scales naturally explain the observed simultaneous variability across optical wavelengths.
Temperatures exceeding the local thin disk value lead to broader spectra extending into the UV, consistent with quasar spectra without invoking a Compton scattering medium.
Temperatures exceeding the local thin disk value lead to broader spectra extending into the UV, consistent with quasar spectra without invoking a Compton scattering medium.
We assume that i) the optical/UV emission observed from AGN originates in an optically thick accretion disk.
We assume that i) the optical/UV emission observed from AGN originates in an optically thick accretion disk.
ii) Variations in the disk occur locally, and are uncorrelated on large spatial scales.
ii) Variations in the disk occur locally, and are uncorrelated on large spatial scales.
iii) Fluid in the disk is on circular Keplerian orbits.
iii) Fluid in the disk is on circular Keplerian orbits.
Assumption i) allows us to model the disk emission using temperature alone, while ii) requires that the disk be inhomogeneous.
Assumption i) allows us to model the disk emission using temperature alone, while ii) requires that the disk be inhomogeneous.
Assumption iii) is only used for computing microlensing light curves, where the disk surface brightness map enters into the magnification light curve produced.
Assumption iii) is only used for computing microlensing light curves, where the disk surface brightness map enters into the magnification light curve produced.
Kellyetal. found that quasar light curves are well described (2009)as a CAR(1) process, a random walk that tends to return to a mean value on a typical timescale.
\citet{kellyetal2009} found that quasar light curves are well described as a CAR(1) process, a random walk that tends to return to a mean value on a typical timescale.
The timescale they found was roughly 200 days, consistent with the thermal timescale in the predicted optical emission region of many AGN.
The timescale they found was roughly 200 days, consistent with the thermal timescale in the predicted optical emission region of many AGN.
This behavior was confirmed for SDSS Stripe 82 quasars by MacLeodetal.
This behavior was confirmed for SDSS Stripe 82 quasars by \citet{macleod2010}.
The amplitude of variations in typical sources is (2010)..10—20%.
The amplitude of variations in typical sources is $10-20\%$.
To produce this variability amplitude with multiple, independent regions in the disk requires larger local variations (total variance «N-! for N independent zones).
To produce this variability amplitude with multiple, independent regions in the disk requires larger local variations (total variance $\propto N^{-1}$ for $N$ independent zones).
The local accretion disk flux and effective temperature will then no longer be a monotonic function of radius r, but will fluctuate with azimuth and time.
The local accretion disk flux and effective temperature will then no longer be a monotonic function of radius $r$, but will fluctuate with azimuth and time.
This will cause the disk spectrum within an annulus to have stronger emission at shorter wavelengths than if the same flux were emitted at constant temperature.
This will cause the disk spectrum within an annulus to have stronger emission at shorter wavelengths than if the same flux were emitted at constant temperature.
Consequently, the outer portions of the disk will contribute more flux than for a uniform disk, causing the disk to appear larger at a particular wavelength.
Consequently, the outer portions of the disk will contribute more flux than for a uniform disk, causing the disk to appear larger at a particular wavelength.
The thin disk is broadly consistent with many observed properties of black hole accretion flows, and follows from the conservation of angular momentum and energy in the gravitational potential of the black hole.
The thin disk is broadly consistent with many observed properties of black hole accretion flows, and follows from the conservation of angular momentum and energy in the gravitational potential of the black hole.
Its global time-averaged properties are likely correct.
Its global time-averaged properties are likely correct.
Assuming a geometrically thin, optically thick disk the local flux can be written F,(r,¢,t)= 7B,(T), where E, is the flux at the frequency v, B, is the Planck function and T=(Ε/σι)1/3, and σι is the Stefan-Boltzmann constant.
Assuming a geometrically thin, optically thick disk the local flux can be written $F_\nu (r,\phi,t)=\pi B_\nu (T)$ , where $F_\nu$ is the flux at the frequency $\nu$, $B_\nu$ is the Planck function and $T=(F/\sigma_b)^{1/4}$, and $\sigma_b$ is the Stefan-Boltzmann constant.
In the thin disk case, Tοςr-?/ well outside the innerdisk edge and is independent of ¢ and t everywhere.
In the thin disk case, $T \propto r^{-3/4}$ well outside the innerdisk edge and is independent of $\phi$ and $t$ everywhere.
We fitted the spectra of from both XMM1 and XMM? using various spectral models.
We fitted the spectra of from both XMM1 and XMM2 using various spectral models.
We jointly fitted the spectra from all three cameras, i.e., pn, MOS1, and MOS2, and their relative normalizations were left free.
We jointly fitted the spectra from all three cameras, i.e., pn, MOS1, and MOS2, and their relative normalizations were left free.
We only report the normalization results corresponding to the pn camera.
We only report the normalization results corresponding to the pn camera.
MOS1 and MOS2 differ by about 10% (the largest one ~20%)), less than the error bars.
MOS1 and MOS2 differ by about $\%$ (the largest one $\sim$ ), less than the error bars.
We fitted the spectra in the 0.2-10 keV energy band.
We fitted the spectra in the 0.2–10 keV energy band.
We were unsure the X-ray emission mechanism of our source.
We were unsure the X-ray emission mechanism of our source.
Thus we first tested the common single-component models to see whether any of them can describe our X-ray spectra well: a single temperature blackbody (BB), a multi-color disk (MCD), a PL, a broken PL, a cut-off PL, an APEC thermal plasma model, and a thermal bremsstrahlung spectrum.
Thus we first tested the common single-component models to see whether any of them can describe our X-ray spectra well: a single temperature blackbody (BB), a multi-color disk (MCD), a PL, a broken PL, a cut-off PL, an APEC thermal plasma model, and a thermal bremsstrahlung spectrum.
They are models bbodyrad, diskbb, powerlaw, bknpower, cutoffpl, APEC, and bremss in XSPEC, respectively.
They are models bbodyrad, diskbb, powerlaw, bknpower, cutoffpl, APEC, and bremss in XSPEC, respectively.
All models include the absorption described by the WABS model in XSPEC; our results change little with alternative absorption models such as PHABS or TBABS in XSPEC.
All models include the absorption described by the WABS model in XSPEC; our results change little with alternative absorption models such as PHABS or TBABS in XSPEC.
All these simple models fail to describe one or both of the sspectra, with residuals above 1 keV typically seen.
All these simple models fail to describe one or both of the spectra, with residuals above 1 keV typically seen.
For indication, we report the PL index Τρι, of the fits using the PL model.
For indication, we report the PL index $\Gamma_{\rm PL}$ of the fits using the PL model.
We obtained Τρι,= 5.86+0.27 for XMM1 (x2(v)21.13(117)) and 6.88+0.09 for XMM2
We obtained $\Gamma_{\rm PL}=5.86$$\pm$ 0.27 for XMM1 $\chi^2_\nu$ $\nu$ )=1.13(117)) and $\pm$$0.09$ for XMM2 $\chi^2_\nu$ $\nu$ )=2.25(286)).
The lower x? value for XMMI to some degree is due ((x2(v)=2.25(286)).to poorer data.
The lower $\chi^2$ value for XMM1 to some degree is due to poorer data.
We next attempted to fit the spectra with the double-component models MCD+PL and BB+PL, finding that they describe both the XMM1 and XMM2 spectra much better than the above common single-component models, with the xy? values decreased by more than 140 for the total degrees of freedom of about 400 of both the XMM1 and XMM2 spectra.
We next attempted to fit the spectra with the double-component models MCD+PL and BB+PL, finding that they describe both the XMM1 and XMM2 spectra much better than the above common single-component models, with the $\chi^2$ values decreased by more than 140 for the total degrees of freedom of about 400 of both the XMM1 and XMM2 spectra.
As a way to model the hard component self-consistently, we also fitted the spectra with SIMPL(MCD) and SIMPL(BB).
As a way to model the hard component self-consistently, we also fitted the spectra with SIMPL(MCD) and SIMPL(BB).
SIMPL (inXSPECI2;Steineretal.2009) is an empirical convolution model of Comptonization in which a fraction (fsc) of the input seed photons are converted into a power law parametrized by an index (lgnupr).
SIMPL \citep[in XSPEC12;][]{stnamc2009} is an empirical convolution model of Comptonization in which a fraction $f_{\rm SC}$ ) of the input seed photons are converted into a power law parametrized by an index $\Gamma_{\rm SIMPL}$ ).
We assume that all the scattered photons are up-scattered in energy in this model.
We assume that all the scattered photons are up-scattered in energy in this model.
The best-fitting values of the column density are consistent between XMM1 and XMM2, with Νη--(Τ.6 and (8.6+0.6)x107° cm-?, respectively, using the 10:50).model MCD+PL.
The best-fitting values of the column density are consistent between XMM1 and XMM2, with $N_{\rm H}$ $(7.6^{+1.5}_{-2.6})$ and $(8.6$$\pm$$0.6)$$\times$$10^{20}$ $^{-2}$, respectively, using the model MCD+PL.
Thus, we chose to fit both spectra with a common value of Ng.
Thus, we chose to fit both spectra with a common value of $N_{\rm H}$.
The final results are given in Table 3..
The final results are given in Table \ref{tbl:mcd+pl}.
The best-fitting values of Ny are slightly higher than the Galactic value of 6.1x102° em~? from the Leiden/Argentine/Bonn Survey of Galactic HI (Kalberlaetal.2005),, probably indicating a small intrinsic absorption.
The best-fitting values of $N_{\rm H}$ are slightly higher than the Galactic value of $\times$$10^{20}$ ${\rm cm}^{-2}$ from the Leiden/Argentine/Bonn Survey of Galactic HI \citep{kabuha2005}, probably indicating a small intrinsic absorption.
For the model MCD+PL, we show the unfolded spectra and residuals in Figure 3..
For the model MCD+PL, we show the unfolded spectra and residuals in Figure \ref{tbl:mcd+pl}.
In this model, the spectra are dominated by the MCD component at energies below 1 keV. The fraction of the MCD component is about and for XMM1 and XMM2, respectively (the 0.2-10 keV unabsorbed flux; Table 3)).
In this model, the spectra are dominated by the MCD component at energies below 1 keV. The fraction of the MCD component is about and for XMM1 and XMM2, respectively (the 0.2–10 keV unabsorbed flux; Table \ref{tbl:mcd+pl}) ).
The 0.2-10 keV flux increases from XMM1 to XMM2 by factor of 8.8 or 5.8
The 0.2–10 keV flux increases from XMM1 to XMM2 by a factor of 8.8 (absorbed) or 5.8 (unabsorbed).
We also aestimate the luminosity, (absorbed)using the bolometric (unabsorbed).flux of each spectral component.
We also estimate the luminosity, using the bolometric flux of each spectral component.
The disk inclination is uncertain, and we assume it to be 60°.
The disk inclination is uncertain, and we assume it to be $\degr$.
The PL component diverges at low energies, and we integrate its flux above 0.2 keV. We obtain luminosities of 1.70 and 6.38x10* erg s! for XMM1 and XMM32, respectively (Table 3)).
The PL component diverges at low energies, and we integrate its flux above 0.2 keV. We obtain luminosities of 1.70 and $\times$ $^{43}$ erg $^{-1}$ for XMM1 and XMM2, respectively (Table \ref{tbl:mcd+pl}) ).
For comparison, the corresponding 0.2-10 keV luminosities are 0.47 and 2.70x10*? erg s1, respectively.
For comparison, the corresponding 0.2–10 keV luminosities are 0.47 and $\times$ $^{43}$ erg $^{-1}$, respectively.