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Finally. a number of authors (??) have suggested that clust associated: with strong ssvstems results in a reduction in the observed | Finally, a number of authors \citep{2006ApJ...648L..93P, 2007ApJ...659..218P} have suggested that dust associated with strong systems results in a reduction in the observed |
This is the main reason for the rather low metallicity nieasured in the simulated clusters (seo Table 1). | This is the main reason for the rather low metallicity measured in the simulated clusters (see Table 1). |
Au nuproved treatment of the chemical curichment of the eas in simulations requires accounting for the contribution ποια SNTa. hereby includiug detailed stellar vields aud stellar evolution models (e.8.. Tornatore et al. | An improved treatment of the chemical enrichment of the gas in simulations requires accounting for the contribution from SN–Ia, hereby including detailed stellar yields and stellar evolution models (e.g., Tornatore et al. |
2001. and references therein). | 2004, and references therein). |
As we have shown. the soft CXCOSRS is associated to clumped gas a a temperature of a few tenths of keV. At such cluperatures. a significant fraction of the emissivitv is associated o ietal lines. | As we have shown, the soft excess is associated to clumped gas at a temperature of a few tenths of keV. At such temperatures, a significant fraction of the emissivity is associated to metal lines. |
Therefore. an underestinate of the plasma metallicity would lead to an underestimate of the svuthetic soft flux. from the una chuups. while leaving nearlv unaffected the soft flux from the hot cluster atmosphere. | Therefore, an underestimate of the plasma metallicity would lead to an underestimate of the synthetic soft flux from the warm clumps, while leaving nearly unaffected the soft flux from the hot cluster atmosphere. |
Iu this respect. the values of the soft excess presented here may be somewhat uucderestinated. | In this respect, the values of the soft excess presented here may be somewhat underestimated. |
We have studied a sample of 20 simulated. clusters. extracted. from a. laree SPILT cosimological sunulatiou of a concordalce ACDAL imodoel with the alu of exploring the presence aud the origin of the soft Xrav excess In ealaxy clusters. | We have studied a sample of 20 simulated clusters, extracted from a large SPH cosmological simulation of a concordance $\Lambda$ CDM model, with the aim of exploring the presence and the origin of the soft X--ray excess in galaxy clusters. |
Besides the eas cynics. our siauulation mceludes the treatieut of star formation and enerev feedback frou galactic winds powered bv superuovae. | Besides the gas dynamics, our simulation includes the treatment of star formation and energy feedback from galactic winds powered by supernovae. |
As such it provides a quite realistic description of the evolution of the diffuse gas in a cosmological euvironinoeut. | As such it provides a quite realistic description of the evolution of the diffuse gas in a cosmological environment. |
Each cluscr is observed inm projection. by iucludiug the line-ofsigit contribution from the surrounding larec-scale gas distribution. | Each cluster is observed in projection, by including the line-of-sight contribution from the surrounding large-scale gas distribution. |
This allows us to verify whether siuulated chisters predict any soft excess of therma origin aud whether such au excess is generated within or outside the cluster virial region. | This allows us to verify whether simulated clusters predict any soft excess of thermal origin and whether such an excess is generated within or outside the cluster virial region. |
Our analvsis is aimed at mimicking the observational procedure followec o» Bonamente et al. ( | Our analysis is aimed at mimicking the observational procedure followed by Bonamente et al. ( |
2002. 2003). i their analysis of ROSATPSPC data. | 2002, 2003), in their analysis of ROSAT–PSPC data. |
For each cluster we compute he correspondingC» enüssonweighted[m] temperature aux uctallicity iu a relatively hard energy baud. | For each cluster we compute the corresponding emission–weighted temperature and metallicity in a relatively hard energy band. |
These values are then used το calculate the spectrin of a one-cluperature auc oue-metallicity plasina model. | These values are then used to calculate the spectrum of a one-temperature and one-metallicity plasma model. |
The fux medicted by this spectra in a softer band is then colmpared to that from the svuthetic spectruu. computed Nw osununndunue over the coutributiou of all the eas particles vine within the "observational exliuder of cach simulated cluster. | The flux predicted by this spectrum in a softer band is then compared to that from the synthetic spectrum, computed by summing over the contribution of all the gas particles lying within the “observational cylinder” of each simulated cluster. |
Our main results cau be sunaaarized as follows, | Our main results can be summarized as follows. |
A eeneral conclusion of our analysis is that a soft Nvay excess of thermal origin is naturally predicted bv hydrodyuanical smiulatious of ealaxy clusters in a cosinological euvironnient. | A general conclusion of our analysis is that a soft X–ray excess of thermal origin is naturally predicted by hydrodynamical simulations of galaxy clusters in a cosmological environment. |
While this is an interesting resultse. we believe that the comparison between data | While this is an interesting result, we believe that the comparison between data |
wherex is the population vector, whose components x;, (j = 1,..,Nx) represent the fractional contribution of each SSP in the base to the total synthetic flux at Ap. | where is the population vector, whose components $x_j$, (j = $\star$ ) represent the fractional contribution of each SSP in the base to the total synthetic flux at $\lambda_0$. |
bj, is the spectrum of the jth SSP of the base of elements normalized at Ap, the reddening term is represented by r,=10944119, Mi, is the synthetic flux at the normalisation wavelength, ® denotes the convolution operator and G(v,,0,) is the Gaussian distribution used to model the line-of-sight stellar motions, which is centred at velocity νι. with dispersion σι. | $b_{j,\lambda}$ is the spectrum of the $j$ th SSP of the base of elements normalized at $\lambda_0$, the reddening term is represented by $r_{\lambda}=10^{-0.4(A_{\lambda}-A_{\lambda 0})}$, $M_{\lambda 0}$ is the synthetic flux at the normalisation wavelength, $\otimes$ denotes the convolution operator and $G(v_{\star},\sigma_{\star})$ is the Gaussian distribution used to model the line-of-sight stellar motions, which is centred at velocity $v_{\star}$ with dispersion $\sigma_{\star}$. |
However, note that due to the low spectral resolution of EPS models in the NIR, the a, values cannot be derived in a reliable way from the synthesis, thus, we do not use them. | However, note that due to the low spectral resolution of EPS models in the NIR, the $\sigma_{\star}$ values cannot be derived in a reliable way from the synthesis, thus, we do not use them. |
For details on c, see Sec. ??.. | For details on $\sigma_{\star}$ see Sec. \ref{results}. |
The final fit is carried out minimizing the equation: where emission lines and spurious features are excluded from the fit by fixing w,=0. | The final fit is carried out minimizing the equation: where emission lines and spurious features are excluded from the fit by fixing $w_{\lambda}$ =0. |
In Eq. 3,, | In Eq. \ref{streq}, |
the most important ingredient in stellar population synthesis is the base set, b;,. | the most important ingredient in stellar population synthesis is the base set, $b_{j,\lambda}$. |
As default base uuses the SSPs of Bruzual&Charlot(2003). | As default base uses the SSPs of \citet{bc03}. |
. However, these SSPs do not include the effect of the contribution of thermally pulsating asymptotic giant branch (TP-AGB) stars, whose contribution is enhanced in the NIR and crucial to model the stellar populations in this spectral region (seeRiffeletal.2007,2008b,2009d,2010b;Martinsetal. 2010). | However, these SSPs do not include the effect of the contribution of thermally pulsating asymptotic giant branch (TP-AGB) stars, whose contribution is enhanced in the NIR and crucial to model the stellar populations in this spectral region \citep[see][]{rogerio07,rogerio08,rogerio09,rogemar10b,martins10}. |
. Thus, we update the base using the Maraston(2005) Evolutionary Population Synthesis (EPS) models as described in Riffeletal.(2009d). | Thus, we update the base using the \citet{maraston05} Evolutionary Population Synthesis (EPS) models as described in \citet{rogerio09}. |
. The base comprises SSPs synthetic spectra covering 12 ages (t =0.01,0.03, 0.05, 0.1, 0.3, 0.5, 0.7, 1, 2, 5, 9 and 13 Gyr) and four metallicities (Z =0.02, 0.5, 1, 2 Zo). | The base comprises SSPs synthetic spectra covering 12 ages $t=$ 0.01,0.03, 0.05, 0.1, 0.3, 0.5, 0.7, 1, 2, 5, 9 and 13 Gyr) and four metallicities $Z=$ 0.02, 0.5, 1, 2 $_\odot$ ). |
We also include black-body functions for temperatures in the range KK in steps of KK (Riffeletal. and a power-law (F,ος v-!?) in order to account for possible contributions from dust emission (BB) and from a featureless continuum (FC), respectively, at the nucleus (e.g.CidFernan-desetal. 2004). | We also include black-body functions for temperatures in the range K in steps of K \citep{rogerio09} and a power-law $F_\nu\propto\nu^{-1.5}$ ) in order to account for possible contributions from dust emission $BB$ ) and from a featureless continuum $FC$ ), respectively, at the nucleus \citep[e.g.][]{cid04}. |
. The same spectral base was used to map the age distribution of the stellar population in the inner 300 pc of 11066 (Riffeletal.2010b). | The same spectral base was used to map the age distribution of the stellar population in the inner 300 pc of 1066 \citep{rogemar10b}. |
. In Fig. | In Fig. |
3 (top-left) we show an optical image of 11157 taken with the Wide Field and Planetary Camera 2 (WFPC2) at the Hubble SpaceTelescope (HST) through the filter F606W (Malkan,Gorjian&Tam 1998). | \ref{large} (top-left) we show an optical image of 1157 taken with the Wide Field and Planetary Camera 2 (WFPC2) at the Hubble SpaceTelescope (HST) through the filter F606W \citep{malkan98}. |
. The um NIFS datacube continuum image is also shown in Fig. | The $\mu$ m NIFS datacube continuum image is also shown in Fig. |
3 (top-right). | \ref{large} (top-right). |
In order to illustrate the accuracy of our fits, we show in Fig. | In order to illustrate the accuracy of our fits, we show in Fig. |
3 (bottom) sample spectra, obtained within 0711x0"11 apertures for four distinct positions: the nucleus (position N marked at top-left panel of Fig. 3)) | \ref{large} (bottom) sample spectra, obtained within $\times$ 1 apertures for four distinct positions: the nucleus (position N marked at top-left panel of Fig. \ref{large}) ) |
and 0’44 west (position A), 0"55 south-east (position B) and 0788 north-east (position C) of the nucleus. | and 4 west (position A), 5 south-east (position B) and 8 north-east (position C) of the nucleus. |
The synthetic spectra were overploted on the data as dotted lines. | The synthetic spectra were overploted on the data as dotted lines. |
As can be observed in this figure, the modelling of the stellar population reproduces very well the continuum/absorption spectra at all positions of 11157. | As can be observed in this figure, the modelling of the stellar population reproduces very well the continuum/absorption spectra at all positions of 1157. |
Following Riffeletal.(2010b) the observed and synthetic spectra were normalized at um, a region free of emission/absorption lines (Riffeletal. 2008b).. | Following \citet{rogemar10b} the observed and synthetic spectra were normalized at $\mu$ m, a region free of emission/absorption lines \citep{rogerio08}. . |
No contribution of the FC and/or BB components was necessary in order to reproduce the the nuclear continuum in 11157. | No contribution of the $FC$ and/or $BB$ components was necessary in order to reproduce the the nuclear continuum in 1157. |
Similar result was obtained by Riffeletal.(2009d) | Similar result was obtained by \citet{rogerio09} |
the A-band surface brightness in that region of the Galaxy, as is also the case in external galaxies such as NGC 3379 (which is part of the D06 sample). | the $K$ -band surface brightness in that region of the Galaxy, as is also the case in external galaxies such as NGC 3379 (which is part of the D06 sample). |
used a 1 Ms eexposure to show that, indeed, most of the Galactic Ridge emission originates from individual faint point sources, specifically accreting white dwarfs and cataclysmic variable stars. | used a 1 Ms exposure to show that, indeed, most of the Galactic Ridge emission originates from individual faint point sources, specifically accreting white dwarfs and cataclysmic variable stars. |
At present it is not possible to remove directly the contribution of faint thermal point sources to the X-ray luminosity in the samples of D06 and MJ10. | At present it is not possible to remove directly the contribution of faint thermal point sources to the X-ray luminosity in the samples of D06 and MJ10. |
However, we can use the tight correspondence, reported by?,, between the X-ray luminosity of these faint sources and the K-band luminosity, to estimate their importance. | However, we can use the tight correspondence, reported by, between the X-ray luminosity of these faint sources and the $K$ -band luminosity, to estimate their importance. |
We do this below, in refsec:LxLk.. | We do this below, in \\ref{sec:LxLk}. |
We conclude from this comparison that the contribution from faint thermal point sources is potentially significant for 5 or 6 faint ellipticals from D06, and for 3 ellipticals from MJ10. | We conclude from this comparison that the contribution from faint thermal point sources is potentially significant for 5 or 6 faint ellipticals from D06, and for 3 ellipticals from MJ10. |
Unfortunately, there are no large, homogeneously analysed samples of normal disc galaxies observed with oorXMM-Newton,, analogous to those of D06 and MJ10 for ellipticals. | Unfortunately, there are no large, homogeneously analysed samples of normal disc galaxies observed with or, analogous to those of D06 and MJ10 for ellipticals. |
This may, in part, be due to the commonly held belief (arising from ROSAT'ss low detection rate of coronal gas) that disc galaxies do not possess X-ray-luminous coronae, suggesting that there is little point in obtaining X-ray observations of such systems for the purpose of studying hot gas. | This may, in part, be due to the commonly held belief (arising from s low detection rate of coronal gas) that disc galaxies do not possess X-ray-luminous coronae, suggesting that there is little point in obtaining X-ray observations of such systems for the purpose of studying hot gas. |
In spite of this, there is a growing body of work on small samples of disc galaxies that shows that these galaxies do indeed have detectable diffuse, coronal emission. | In spite of this, there is a growing body of work on small samples of disc galaxies that shows that these galaxies do indeed have detectable diffuse, coronal emission. |
As we will show below, the properties of the hot coronae of disc galaxies are remarkably similar to those of ellipticals of the same mass. | As we will show below, the properties of the hot coronae of disc galaxies are remarkably similar to those of ellipticals of the same mass. |
Our heterogeneous sample of disc galaxies is taken from a number of studies, including Str04,, WO5,, T06,,LO7,, OWOO9,, Sun07,,JO8,, and ROO. | Our heterogeneous sample of disc galaxies is taken from a number of studies, including , , , , and . |
. Str04, W05, T06, L07, and ROO all studied disc galaxies. | Str04, W05, T06, L07, and R09 all studied disc galaxies. |
Str04 used tto observe a sample of 10 star-forming galaxies, 7 of which are classified as starbursts. | Str04 used to observe a sample of 10 star-forming galaxies, 7 of which are classified as starbursts. |
W05 report on oobservations of 7 ‘normal’ star-forming galaxies. | W05 report on observations of 7 `normal' star-forming galaxies. |
T06 observed with aa sample of 9 normal star-forming disc galaxies. | T06 observed with a sample of 9 normal star-forming disc galaxies. |
LO7 observed the nearly edge-on Sombrero galaxy (M104) withChandra. | L07 observed the nearly edge-on Sombrero galaxy (M104) with. |
. R09 Observed two quiescent edge-on disc galaxies withChandra,, but found no significant diffuse emission away from the disc. | R09 observed two quiescent edge-on disc galaxies with, but found no significant diffuse emission away from the disc. |
For all these studies we use only the reported X-ray luminosity (or upper limits) of the hot gas (see Table 9 of Str04, Table 1 of W05, and Table 9 of Τ06). | For all these studies we use only the reported X-ray luminosity (or upper limits) of the hot gas (see Table 9 of Str04, Table 1 of W05, and Table 9 of T06). |
Since we exclude the luminosity from the region that is spatially coincident with the disc, there is no significant contribution from faint thermal point sources to the X-ray luminosities of disc galaxies that we analyse here. | Since we exclude the luminosity from the region that is spatially coincident with the disc, there is no significant contribution from faint thermal point sources to the X-ray luminosities of disc galaxies that we analyse here. |
OW09, however, observed a sample of 6 nearby disc galaxies withNewton. | OW09, however, observed a sample of 6 nearby disc galaxies with. |
For these systems emission from faint thermal point sources could be a contaminant but, as we show below, the expected contribution from these sources is much smaller than the total measured X-ray luminosities. | For these systems emission from faint thermal point sources could be a contaminant but, as we show below, the expected contribution from these sources is much smaller than the total measured X-ray luminosities. |
Finally, S07 and 108 reported X-ray detections (and upper limits) of optically luminous early and late type galaxies in several nearby galaxy groups and clusters. | Finally, S07 and J08 reported X-ray detections (and upper limits) of optically luminous early and late type galaxies in several nearby galaxy groups and clusters. |
We have elected to use their late type galaxies to complement our relatively small sample, in spite of the fact that the luminosity of these systems could be influenced by the group/cluster environment (e.g., if ram pressure strips some of the hot gas). | We have elected to use their late type galaxies to complement our relatively small sample, in spite of the fact that the luminosity of these systems could be influenced by the group/cluster environment (e.g., if ram pressure strips some of the hot gas). |
In a forthcoming study (McCarthy et prep), however we show (using cosmological hydrodynamical simulations) that, for those galaxies that are not completely stripped of their gas, the X-ray luminosity is largely unchanged by ram pressure stripping. | In a forthcoming study (McCarthy et ), however, we show (using cosmological hydrodynamical simulations) that, for those galaxies that are not completely stripped of their gas, the X-ray luminosity is largely unchanged by ram pressure stripping. |
This is because the X-ray luminosity is very centrally concentrated so the brightest gas is the very last to be stripped. | This is because the X-ray luminosity is very centrally concentrated so the brightest gas is the very last to be stripped. |
In this section, we examine correlations between the X-ray luminosity of the hot gas and the near-infrared (K-band) luminosity of the galaxy, as well as the temperature of the hot gas, inferred from X-ray spectroscopy. | In this section, we examine correlations between the X-ray luminosity of the hot gas and the near-infrared $K$ -band) luminosity of the galaxy, as well as the temperature of the hot gas, inferred from X-ray spectroscopy. |
We begin by examining, as a function of stellar morphology, the scaling of the diffuse soft X-ray luminosity with the K-band luminosity,Lx,, which is a good proxy for stellar mass. | We begin by examining, as a function of stellar morphology, the scaling of the diffuse soft X-ray luminosity with the $K$ -band luminosity, which is a good proxy for stellar mass. |
We have converted X-ray luminosities quoted in other passbands into the bband using the | We have converted X-ray luminosities quoted in other passbands into the band using the |
however we show in the figure the predicted: contribution of normal galaxies. which is significant at these faint Ηχος (see also Busswell Shanks. 2001). | however we show in the figure the predicted contribution of normal galaxies, which is significant at these faint fluxes (see also Busswell Shanks, 2001). |
The predicted. density of bright. sub-mm galaxies (SMCs: Sus)74 mw) is 783 27. in very good agreement with the error-weighted mean of T68£89 7 for the observational data shown in relf-850ents.. | The predicted density of bright sub-mm galaxies (SMGs; $S_{850}>4$ mJy) is 783 $^{-2}$, in very good agreement with the error-weighted mean of $768\pm89$ $^{-2}$ for the observational data shown in \\ref{f-850cnts}. |
? The 1.5E0.1 Jv deg= sub-mm background. contribution made by the ECDES X-ray sources. provides a crucial observational constraint on our obscured GN model. as we can use the model to generate a predicted: sub-mam backeround contribution from only those AGN with 2.0 keV. N-rav fluxes greater than the L1.10I {limit of the ECDES survey. | The $1.5 \pm 0.1$ Jy $^{-2}$ sub-mm background contribution made by the ECDFS X-ray sources provides a crucial observational constraint on our obscured AGN model, as we can use the model to generate a predicted sub-mm background contribution from only those AGN with 0.5--2.0 keV X-ray fluxes greater than the $1.1\times 10^{-16}$ limit of the ECDFS survey. |
We find that usingthe model shown in reff-550ents.. this predicted: background. is 2.3 Jv 7 =50% greater than the measured. value. | We find that usingthe model shown in \\ref{f-850cnts}, this predicted background is 2.3 Jy $^{-2}$, $\approx50$ greater than the measured value. |
This. initially appears to indicate that our mocel is over-preclicting the contribution which AGN make in the sub-mm. | This initially appears to indicate that our model is over-predicting the contribution which AGN make in the sub-mm. |
However. the wright sub-mm source counts in the ECDES are known to » lower than in other fields. by as much as a factor of 2 eet al.. | However, the bright sub-mm source counts in the ECDFS are known to be lower than in other fields, by as much as a factor of 2 et al., |
. 2009). | 2009). |
This deficiency of bright sub-mam sources in he ECDES may explain why the total stacked sub-mim (ux of ECDES AGN is lower than the model prediction. | This deficiency of bright sub-mm sources in the ECDFS may explain why the total stacked sub-mm flux of ECDFS AGN is lower than the model prediction. |
Nevertheless. we can revise the model to bring the oedieted sub-mam: background. [rom X-rav-detected αν into line with the observations. | Nevertheless, we can revise the model to bring the predicted sub-mm background from X-ray-detected AGN into line with the observations. |
We make this revision »v altering the cust covering factor. which is the only remaining free parameter in the mocoel after fixing the dust empoerature at 30K and the emissivity index at 3=1.5. | We make this revision by altering the dust covering factor, which is the only remaining free parameter in the model after fixing the dust temperature at 30K and the emissivity index at $\beta=1.5$. |
Gunn Shanks assume a covering factor fice=1.0. which represents an isotropic distribution of dust. | Gunn Shanks assume a covering factor $f_{cov}=1.0$, which represents an isotropic distribution of dust. |
LE we instead ake fice=0.65. the predicted: sub-mun background. [rom X-rav-detected AGN falls to 1.5 Jy 7. consistent. with he observationalvalue. | If we instead take $f_{cov}=0.65$, the predicted sub-mm background from X-ray-detected AGN falls to 1.5 Jy $^{-2}$, consistent with the observationalvalue. |
In this revised. model. however. the total AGN contribution to the sub-mm sources counts is lower dashed line in reff-550cent s)). | In this revised model, however, the total AGN contribution to the sub-mm sources counts is lower (long-dashed line in \\ref{f-850cnts}) ). |
Phe model now accounts for only around hall of bright sources: the predicted number of SMCs falls from. the 783 quoted above to 367. 27. | The model now accounts for only around half of bright sources: the predicted number of SMGs falls from the 783 $^{-2}$ quoted above to 367 $^{-2}$. |
However. while. this value is lower than most of the observational data. it agrees very well with the observed SAIC: sky. density of 335+34 7? for the ECDES. | However, while this value is lower than most of the observational data, it agrees very well with the observed SMG sky density of $335\pm34$ $^{-2}$ for the ECDFS. |
This is significant. because it means that our non-unified ACN model. simultaneously matches the tota ECDES noumber counts and the measured sub-mam background Lux from the ECDES X-ray. sources. | This is significant, because it means that our non-unified AGN model simultaneously matches the total ECDFS number counts and the measured sub-mm background flux from the ECDFS X-ray sources. |
Pherefore. our. origina moclel. which matches the total sub-mim source counts wel and precicts a background contribution of 2.3 Jv deg.7 from Sus2021.110| ssources. may represent a more valid description of the ACN contribution to the sub-mm population in other more typical [iclds. | Therefore, our original model, which matches the total sub-mm source counts well and predicts a background contribution of 2.3 Jy $^{-2}$ from $S_{0.5-2.0}\ge1.1\times 10^{-16}$ sources, may represent a more valid description of the AGN contribution to the sub-mm population in other more typical fields. |
‘Taking the model which matches the measured 1540.1 Jv 7 sub-mm flux from Sus2.02Ld101° AA-ray sources. we can make further tests by. predicting the expected sub-mim. background: contribution from X-ray sources in other X-ray. [lux ranges. | Taking the model which matches the measured $1.5 \pm 0.1$ Jy $^{-2}$ sub-mm flux from $S_{0.5-2.0}\ge1.1\times 10^{-16}$ X-ray sources, we can make further tests by predicting the expected sub-mm background contribution from X-ray sources in other X-ray flux ranges. |
This is shown in reft-eblilux.. | This is shown in \\ref{f-eblflux}. |
We measure the actual sub-nim background associated with ECDLES sources to several X-ray [lux limits and compare to the predictions. | We measure the actual sub-mm background associated with ECDFS sources to several X-ray flux limits and compare to the predictions. |
The figure indicates that the model is predicting the trend with flux generally very well. | The figure indicates that the model is predicting the trend with flux generally very well. |
Since the data in reft-eblilux. include those in reff-smstacks empha.. this also shows that our AGN mocol fits the data in that figure. | Since the data in \\ref{f-eblflux} include those in \\ref{f-smstacks} , this also shows that our AGN model fits the data in that figure. |
We can also test the models preclictions against the result in πιΠΕ where we found that Ly>LOM ssources are brighter in the sub-mm. | We can also test the model's predictions against the result in \\ref{f-smflxlum}, where we found that $L_X>10^{44}$ sources are brighter in the sub-mm. |
Lhe AGN model naturally predicts such a luminosity dependence. since the amount of light that can be absorbed in the X-ray/optical (ancl subsequentIy reraciated in the sub-mm) is proportional to the intrinsic N-rav/optical Iuminosity. | The AGN model naturally predicts such a luminosity dependence, since the amount of light that can be absorbed in the X-ray/optical (and subsequently reradiated in the sub-mm) is proportional to the intrinsic X-ray/optical luminosity. |
A simple test we can do with the model is to calculate the expected sub-mam background. from AGN which are brighter or fainter than the characteristic luminosity L. | A simple test we can do with the model is to calculate the expected sub-mm background from AGN which are brighter or fainter than the characteristic luminosity $L^{*}$. |
This prediction should be consistent with the result from reff-smllxlum. since Le107 aat the z2 redshift expected for sub-muim sources (Aired et al.. | This prediction should be consistent with the result from \\ref{f-smflxlum} since $L^*\approx10^{44}$ at the $z\approx2$ redshift expected for sub-mm sources (Aird et al., |
2010). | 2010). |
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