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We summarize the derived parameters for the three LBNe in Table 3. | We summarize the derived parameters for the three LBNe in Table 3. |
We note that our modeled Bj are rather similar to those found for regions with a similar low electron density. e.g. S264 and G124.9-0.1 (Paper D. | We note that our modeled $B_{\parallel}$ are rather similar to those found for regions with a similar low electron density, e.g. S264 and G124.9+0.1 (Paper I). |
Besides the three LBN objects there are more 26 cm Faraday Screen structures in the field of Fig. | Besides the three LBN objects there are more $\lambda$ 6 cm Faraday Screen structures in the field of Fig. |
9. Some were listed below. which we. however. will not analyze in detail in this paper. | Some were listed below, which we, however, will not analyze in detail in this paper. |
A large area with very uniform PAs. which deviate about 22° from the Galactic plane direction.can be identified in southwestern direction of the "drumstick". | A large area with very uniform $PA$ s, which deviate about $\degr$ from the Galactic plane direction,can be identified in southwestern direction of the “drumstick”. |
This Faraday | This Faraday |
(mnlv cosmic shear. | only cosmic shear. |
This analysis did not xecdict an 1provement in the results. which would require lüeher Sienal-to-noise ratio at large scales. | This analysis did not predict an improvement in the results, which would require higher signal-to-noise ratio at large scales. |
The introduction of CFEIITLS-TOO03— «ata là a 1VATAPS|BAOSNe analvsis provides aun interesting Conmbiuation. breaking the on degeneracy present iu lat analvsis (Fie. 1. | The introduction of CFHTLS-T0003 data in a WMAP5+BAO+SNe analysis provides an interesting combination, breaking the $\omega_\cdm-\omega_\nu$ degeneracy present in that analysis (Fig. \ref{fig:joint} , |
left paucl). | left panel). |
The jint analysis violIs 0.03 eV <Soan,sz0.51 eV at the confidence level. mareially excludi πωο inos (Fie.L.. when | The joint analysis yields 0.03 eV $< \sum m_\nu<0.54$ eV at the confidence level, marginally excluding massless neutrinos (Fig. \ref{fig:joint}, |
right panel). | right panel). |
The prefercuc Or nnssve Os is lost the data is corrected ‘or a possible uderestination of the shear signal. which siumatious xdicae mav be aroundά | The preference for massive neutrinos is lost when the data is corrected for a possible underestimation of the shear signal, which simulations indicate may be around. |
ν, Tn this case. the result ufts ο Snycz0.53 eV. The CFITTLS data also shows Some disaereenment with the result of WNLADP5. | In this case, the result shifts to $\sum m_\nu<0.53$ eV. The CFHTLS data also shows some disagreement with the result of WMAP5. |
Tudeed. if a cosmde-hear fiducial WALAPS uinodel was usec. tje expected combined WMADP5|BAOSNeCFIITLS (oustraiut would be tighter: 3i,<0.LE eV. Finalv. we «rowed that CFITTLS-TOX03 data do not improve the XVALTAPS|BAOSNe coustraints ou the neutrine 1jas if trey contain a bias larecr han | Indeed, if a cosmic-shear fiducial WMAP5 model was used, the expected combined WMAP5+BAO+SNe+CFHTLS constraint would be tighter: $\sum m_\nu<0.44$ eV. Finally, we showed that CFHTLS-T0003 data do not improve the WMAP5+BAO+SNe constraints on the neutrino mass if they contain a bias larger than. |
After subinission of the mauuscript. a simular study was subiuitted by Τοήκα (2008). also using; CEFITTLS-TU003. cosnüc shear data to constrain the aux"utro mass. | After submission of the manuscript, a similar study was submitted by Ichiki (2008), also using CFHTLS-T0003 cosmic shear data to constrain the neutrino mass. |
Both analyses take a similar approach. the main dierences: beiug: they use the cosmic shear correlation "uuction. which is more affected NsvstenmatiCSS απ op»osed to the aperturec-nniass dispersion: the l1011-4mussian shear covariance matrix is also computed i- dierent wares. ax is the likelihood analysis. | Both analyses take a similar approach, the main differences being: they use the cosmic shear correlation function, which is more affected bysystematics, as opposed to the aperture-mass dispersion; the non-Gaussian shear covariance matrix is also computed in different ways, as is the likelihood analysis. |
Their netrie mass coustraiuts from cosmic shear ouNo are weaker, which is consistent with the fact hey impose weaker priors. and εhe results for a WALAPSDAO|SNe|CFIITLS joint analysis are very simular. | Their neutrino mass constraints from cosmic shear only are weaker, which is consistent with the fact they impose weaker priors, and the results for a WMAP5+BAO+SNe+CFHTLS joint analysis are very similar. |
Besides the neutrino mass. we also considerκ. the (fective iuuber of relativisic degrees of freedoms. Nog. | Besides the neutrino mass, we also considered the effective number of relativistic degrees of freedom, $\Neff$. |
οAID anisotropies are by far more sensitive than ¢“OSL *shear anc CFITLS-To0003 ata prodced an alos flat likelihoo: with respect to his paramet¢y. | CMB anisotropies are by far more sensitive than cosmic shear and CFHTLS-T0003 data produced an almost flat likelihood with respect to this parameter. |
This prevened us from using the osNo degeneracy. caused by a lüeher Nag delaving f1ο dnatter-raciation equivalence aiixl the ¢‘corresponding chreezine of matter perturbations. which have less time to grow. | This prevented us from using the $\sigma_8-\Neff$ degeneracy, caused by a higher $\Neff$ delaying the matter-radiation equivalence and the corresponding defreezing of matter perturbations, which have less time to grow. |
Tn μιWary. the CFUTLS coziic-shear has already Sufficien statistical precision for the accuracv ¢4 the results o he affected by systelatics. | In summary, the CFHTLS cosmic-shear has already sufficient statistical precision for the accuracy of the results to be affected by systematics. |
The CFIITLS leusiug svsteniaics collaboration is currently ΠΟΙΟtakine avery detailed anc lerethy anavais of those systematics. | The CFHTLS lensing systematics collaboration is currently undertaking a very detailed and lengthy analysis of those systematics. |
The staistical precision is however still insufficicut to allow us to miprove current constraints on the neutrine lass. | The statistical precision is however still insufficient to allow us to improve current constraints on the neutrino mass. |
Fiture eround-based aud space-borue obser"ations (suchasKIDS.Paun-STARRS.DES.LSST.SNAP-LJDEM.EUCLIDzsurvevs:seePeacocketal.2006 "m with better statistics. larger scales. ancl also the lise of tomographic techniques. will allow to perform luore elaborate analyses. for iustiuce enabling to relax the asstuuption of degeneracy between mass eigeustates, | Future ground-based and space-borne observations \cite[such as KIDS,
Pan-STARRS, DES, LSST, SNAP-L, JDEM, or EUCLID surveys; see][]{ESAESOreport}, with better statistics, larger scales, and also the use of tomographic techniques, will allow to perform more elaborate analyses, for instance enabling to relax the assumption of degeneracy between mass eigenstates. |
From the theoretical poiut-of-vlew. a more suitable coluputation of the matter power spectra in the non-linear regime will be mandatory. Oo take more careful account of the effects of massive neurinos without relviug Ol apples based on ACDAL ΑΛ οxdv simulations. | From the theoretical point-of-view, a more suitable computation of the matter power spectrum in the non-linear regime will be mandatory, to take more careful account of the effects of massive neutrinos without relying on mappings based on $\Lambda$ CDM $N$ -body simulations. |
This nuelt be achievable using either sandard perturbation theory (e.g...Saitoetal.2008). or a resununation schienie (see0.8...Crocce&Scoccinimro2OG:Pietroui2008). | This might be achievable using either standard perturbation theory \cite[e.g.,][]{nupt} or a resummation scheme \citep[see e.g.,][]{ptr1, ptr2}. |
. It wil be interesting. eventually. to investigate the degeneracy with the low-redshitt pivsies (OXO20). such as relonization and dark energy. relevaut if jn,ς0.01 eV. Qn this mass scale. the normal/iuverted hierarchy of niass states can also be distinguished. | It will be interesting, eventually, to investigate the degeneracy with the low-redshift physics $z\lesssim 20$ ), such as reionization and dark energy, relevant if $m_\nu\lesssim0.01$ eV. On this mass scale, the normal/inverted hierarchy of mass states can also be distinguished. |
Nore elaborate models allowiug for an 1iteractioun betweeἩ olnassive neutrinos and a quintesscice field (Brookfieldetal.2006).. or i which mass-varving neutrinos lxshave as dd negative pressure fluid. which could then be the origin of the cosmic acceleratiou (Fardouetal.2001). may then also be considered. | More elaborate models allowing for an interaction between massive neutrinos and a quintessence field \cite{mQ2}, or in which mass-varying neutrinos behave as a negative pressure fluid, which could then be the origin of the cosmic acceleration \cite{mQ1}, , may then also be considered. |
Dereddening the magnitudes with the absorption on the line of sight does. however. not lead to any known stellar spectral type for a Galactic source. | Dereddening the magnitudes with the absorption on the line of sight does, however, not lead to any known stellar spectral type for a Galactic source. |
This. the detection in the UV-band. and the intrinsic absorption of the source would tend to favour a Sey 2 AGN. | This, the detection in the UV-band, and the intrinsic absorption of the source would tend to favour a Sey 2 AGN. |
IGR J11187—5438 was first reported by Birdetal.(2007). | IGR $-$ 5438 was first reported by \citet{bird07}. |
. The source was detected at a 18-60 keV significance of 6.307 during 1016 ks of observations. | The source was detected at a 18–60 keV significance of $\sigma$ during 1016 ks of observations. |
There is a single source in the 2MASS point source catalogue within ffrom the XRT position. | There is a single source in the 2MASS point source catalogue within from the XRT position. |
2MASS J11182121-5437286 is at aaway from the centre of the eerror box. | 2MASS J11182121-5437286 is at away from the centre of the error box. |
The source is also visible in the DSS IL IR and R-Band images. although it 15 quite weak in the latter. | The source is also visible in the DSS II IR and R-Band images, although it is quite weak in the latter. |
The UVOT was not operating during either of the We combined the two observations to perform a spectral analysis. | The UVOT was not operating during either of the We combined the two observations to perform a spectral analysis. |
The average spectrum has 1328 ets for a total of 21888 s exposure. | The average spectrum has 1328 cts for a total of 21888 s exposure. |
An absorbed power law fits the data well (y;=0.91 for 55 DOF). | An absorbed power law fits the data well $\chi_\nu^2=0.91$ for 55 DOF). |
The value of the absorption is compatible with the Galactic absorption along the line of sight. which may mean that the source is not intrinsically absorbed. | The value of the absorption is compatible with the Galactic absorption along the line of sight, which may mean that the source is not intrinsically absorbed. |
IGR 13149-4422 was first reported in. Sazonovetal. (2007)ÀÀ and Krivonosetal.(2007). | IGR J13149+4422 was first reported in \citet{sazonov07}Â Â and \citet{Krivonos07}. |
The latter give an IBIS position of 13h I4m 58s wwith a Γ-σ uncertainty as high as2. | The latter give an IBIS position of 13h 14m 58s with a $\sigma$ uncertainty as high as. |
1.. It was then tentatively identified with Mrk 248 a Sey 2 AGN at z=0.037 al.. 2007). | It was then tentatively identified with Mrk 248 a Sey 2 AGN at z=0.037 \citep{sazonov07}. |
. The best Swift//XRT position is ffrom the IBIS position. therefore within the 90% confidence error box. | The best /XRT position is from the IBIS position, therefore within the $\%$ confidence error box. |
It is compatible with the best reported position of UGC 8327 NEDO2 (at RApoo=ll3 hl5m 17.270s. ponn=++44°24/25"660 according to the latest measurements available in NED. thus at ffrom the centre of the eerror box). | It is compatible with the best reported position of UGC 8327 NED02 (at 13 h15m 17.270s, 60 according to the latest measurements available in NED, thus at from the centre of the error box). |
Note that this is also at 16788 from the position reported in Bodagheeetal.(2007).. and in SIMBAD for Mrk 248. | Note that this is also at 8 from the position reported in \citet{bodaghee07}, and in SIMBAD for Mrk 248. |
We remark that SIMBAD reports an earlier measurement than NED. and also mentions Mrk 248 as being UGC 8327. a pair of interacting galaxies (UGC 8327). | We remark that SIMBAD reports an earlier measurement than NED, and also mentions Mrk 248 as being UGC 8327, a pair of interacting galaxies (UGC 8327). |
NED. on the other hand. associates Mrk 248 with one of the components of the pair of interacting galaxies (UGC 8327 NEDO2). | NED, on the other hand, associates Mrk 248 with one of the components of the pair of interacting galaxies (UGC 8327 NED02). |
Mrk 248 is also reported in the 2MASS extended source catalogue as 2MASX J13151725+4424259 whose best position is at only aaway from the best X-ray position. | Mrk 248 is also reported in the 2MASS extended source catalogue as 2MASX J13151725+4424259 whose best position is at only away from the best X-ray position. |
The 2MASS source is also classified as an emission line. galaxy in SIMBAD. | The 2MASS source is also classified as an emission line galaxy in SIMBAD. |
An extended or blended source ts also clearly visible in the UVOT UVM2 and UVWI images within the XRT error box. | An extended or blended source is also clearly visible in the UVOT UVM2 and UVW1 images within the XRT error box. |
The spatial comeidence between all sources likely indicates that IGR J13149+4422 is a Sey 2 AGN. | The spatial coincidence between all sources likely indicates that IGR J13149+4422 is a Sey 2 AGN. |
We extracted a spectrum from three. pointings. | We extracted a spectrum from three pointings. |
The spectrum has 964 cts for a total of 15116 s. It is well fitted by an absorbed power law (y72 1.11 for 32 DOF). | The spectrum has 964 cts for a total of 15116 s. It is well fitted by an absorbed power law $\chi^2$ =1.11 for 32 DOF). |
We note the presence of positive residuals at low energy. | We note the presence of positive residuals at low energy. |
The value of iis about 430 times higher than the average absorption along the line of sight. which indicates that the source is an intrinsically absorbed AGN as would be expected in the case of a Sey 2 AGN. | The value of is about 430 times higher than the average absorption along the line of sight, which indicates that the source is an intrinsically absorbed AGN as would be expected in the case of a Sey 2 AGN. |
IGR J14579-4308 was first reported by Kalemeietal.(2005) from an IBIS/ISGRI observation of SN 1006. | IGR $-$ 4308 was first reported by \citet{kalemci05} from an IBIS/ISGRI observation of SN 1006. |
It was promptly suggested to be an AGN due to its positional coincidence with VV 780 a Sey 2 AGN. | It was promptly suggested to be an AGN due to its positional coincidence with VV 780 a Sey 2 AGN. |
Revnivtsevetal.(2006) later reported the presence of the source from a survey of the Galactic Crux arm tangent. | \citet{revnivtsev05} later reported the presence of the source from a survey of the Galactic Crux arm tangent. |
The XRT images show that the field 1s crowded with about five bright sources in the field of view (Fig. 2)). | The XRT images show that the field is crowded with about five bright sources in the field of view (Fig. \ref{fig:14579}) ). |
Only the brightest source is. however. found within the maximum of eerror box of ISGRIA (Revnivtsevetal..2006). | Only the brightest source is, however, found within the maximum of error box of ISGRIÂ \citep{revnivtsev05}. |
. It is labeled | in Fig. 2.. | It is labeled 1 in Fig. \ref{fig:14579}. |
The best XRT position is aaway from the reported position of IC 4518/ VV 780 which rules out an association between the X-ray source and the AGN. | The best XRT position is away from the reported position of IC 4518/ VV 780 which rules out an association between the X-ray source and the AGN. |
Birdetal.(2007) suggested a possible association of the INTEGRAL source with IC 4518A. a Sey 2 galaxy as inferred from optical spectroscopy (Masettietal..2007).. also the western component of a pair of interacting galaxies named MCG-07-31-001. | \citet{bird07} suggested a possible association of the INTEGRAL source with IC 4518A, a Sey 2 galaxy as inferred from optical spectroscopy \citep{masetti07c}, also the western component of a pair of interacting galaxies named MCG-07-31-001. |
The best pposition is. indeed. just away from the position of IC 4518A (also named VV 780 NEDO1) as reported in NED. | The best position is, indeed, just away from the position of IC 4518A (also named VV 780 NED01) as reported in NED. |
Our aanalysis. therefore. strengthens the association of both objects. and we confirm that IGR J14579-4308 is a Sey 2 galaxy. | Our analysis, therefore, strengthens the association of both objects, and we confirm that IGR $-$ 4308 is a Sey 2 galaxy. |
For many vears the forest has been considered a differeut class of objects with respect to ealaxics. | For many years the forest has been considered a different class of objects with respect to galaxies. |
The available sensitivity was too low to detect ay sig of nonprimordial coumposition iu the intergalactic eas clouds at Ligh redshift. | The available sensitivity was too low to detect any sign of non–primordial composition in the intergalactic gas clouds at high redshift. |
Thanks to the advent of high resolutiou aud signaltonoise spectroscopy. the old idea ou the majority of quasar absorption lines has been revisited aud opened im the last few vears a still pending debate ou the connection between he forest and the galaxy formation of the carly Universe. | Thanks to the advent of high resolution and signal–to–noise spectroscopy, the old idea on the majority of quasar absorption lines has been revisited and opened in the last few years a still pending debate on the connection between the forest and the galaxy formation of the early Universe. |
The detection of ious differcut from CTV in optically thin clouds is made complicated by jurder observational conditions. whereas the still too poor knowledge of the ionisatiou imechaisus which determine the jou abundances in those clouds its often discouraged attempts of metal coutent estimations as a functiou of redshift aud of TT colum: density. | The detection of ions different from CIV in optically thin clouds is made complicated by harder observational conditions, whereas the still too poor knowledge of the ionisation mechanisms which determine the ion abundances in those clouds has often discouraged attempts of metal content estimations as a function of redshift and of HI column density. |
However abundance investigation of he clouds has fundamental implications iu the understanding of the enrichment processes in the ICAL by Pop IIT stars in the +75 Universe. | However abundance investigation of the clouds has fundamental implications in the understanding of the enrichment processes in the IGM by Pop III stars in the $z>5$ Universe. |
The sample of optically thin absorption lines with 11.5«logNyy<16.5 has been obtained by hieh resolution spectroscopy. mainly HIRÁAS/IKeck (Sougaila 1997h) but also by EMMI/NTT for the 223.7 svstems (Savaglio ct al. | The sample of optically thin absorption lines with $14.5 < \log N_{\rm HI} < 16.5$ has been obtained by high resolution spectroscopy, mainly HIRAS/Keck (Songaila 1997b) but also by EMMI/NTT for the $z\gsim 3.7$ systems (Savaglio et al. |
1991). | 1997). |
For all the systems CTV aud/or SUV aud CTL detections or upper luits are | For all the systems CIV and/or SiIV and CII detections or upper limits are |
of cool (0.5 keV) gas. | of cool (0.5 keV) gas. |
We focus the discussion on these two findings. | We focus the discussion on these two findings. |
Asymmetries in the temperature. entropy and abundance maps like we see to the South-West of the core of are fairly common in clusters of galaxies. | Asymmetries in the temperature, entropy and abundance maps like we see to the South-West of the core of are fairly common in clusters of galaxies. |
Usually. these low-temperature regions. or cold fronts. are confined by a sharp surface brightness discontinuity (see?.forareview).. | Usually, these low-temperature regions, or cold fronts, are confined by a sharp surface brightness discontinuity \citep[see][for a review]{markevitch2007}. |
For Abell 2052. ? already describe the elliptical shape of inner the core in the North-South direction. | For Abell 2052, \citet{blanton2009} already describe the elliptical shape of inner the core in the North-South direction. |
But just outside the region with the X-ray cavities. the core shows ellipticity in the NE-SW direction with an enhanced surface brightness area in the South-West. | But just outside the region with the X-ray cavities, the core shows ellipticity in the NE-SW direction with an enhanced surface brightness area in the South-West. |
This NE-SW ellipticity is seen in both XMM-Newton and Chandra images. | This NE-SW ellipticity is seen in both XMM-Newton and Chandra images. |
A sharp discontinuity. however. is not seen directly in the current Images. | A sharp discontinuity, however, is not seen directly in the current images. |
By extracting a radial profile for a pie shaped region in the South. we do see a discontinuity in the mean count rate at an angular distance of 3.2’ from the central cD galaxy. | By extracting a radial profile for a pie shaped region in the South, we do see a discontinuity in the mean count rate at an angular distance of $^{\prime}$ from the central cD galaxy. |
The ellipticity of the low-temperature region. the relatively weak discontinuity at the edge. and no evidence for structure in the pressure map or pressure profile suggest that the asymmetry is not due to a recent large merger event. | The ellipticity of the low-temperature region, the relatively weak discontinuity at the edge, and no evidence for structure in the pressure map or pressure profile suggest that the asymmetry is not due to a recent large merger event. |
Also the cooling core is not disrupted. which means that the cause of the disruption was either weak ora long time ago. | Also the cooling core is not disrupted, which means that the cause of the disruption was either weak or a long time ago. |
The fact that we see only a significant jump in surface brightness and Fe abundance across the discontinuity most likely indicates gas sloshing (?).. | The fact that we see only a significant jump in surface brightness and Fe abundance across the discontinuity most likely indicates gas sloshing \citep{markevitch2001}. |
In this case. a small merger event or a larger merger in the distant past caused the dark matter and the associated cool gas to oscillate in the gravitational potential of the cluster. | In this case, a small merger event or a larger merger in the distant past caused the dark matter and the associated cool gas to oscillate in the gravitational potential of the cluster. |
We only observe a gradual temperature. density. entropy. or pressure gradient across the cold front. and the entropy on the inside of the 20iscontinuity is lower than on the outside. | We only observe a gradual temperature, density, entropy, or pressure gradient across the cold front, and the entropy on the inside of the discontinuity is lower than on the outside. |
This means that the 'elocity of the front must be subsonic. and the discontinuity 18 sot a shock. | This means that the velocity of the front must be subsonic, and the discontinuity is not a shock. |
Contrary to. the lack of significant thermodynamic Ooiscontinuities found in the profiles. the iron abundance jumps own roughly 0.2 solar units across the front. | Contrary to the lack of significant thermodynamic discontinuities found in the profiles, the iron abundance jumps down roughly 0.2 solar units across the front. |
Numerical »imulations show that sloshing motions can indeed cause discontinuities in abundance profiles (?).. | Numerical simulations show that sloshing motions can indeed cause discontinuities in abundance profiles \citep{ascasibar2006}. |
This jump in tron abundance suggests that the sloshing motions are a mechanism to transport low-entropy metal-rich gas to the outer parts of the cluster. | This jump in iron abundance suggests that the sloshing motions are a mechanism to transport low-entropy metal-rich gas to the outer parts of the cluster. |
Recently. the same effect has also been observed in (?).. | Recently, the same effect has also been observed in \citep{simionescu2010}. |
The fact that metal transport is observed in these deep observations of clusters of galaxies suggests that gas sloshing is generally a very important and a dominating effect in the transport of metals to the outer parts of clusters. | The fact that metal transport is observed in these deep observations of clusters of galaxies suggests that gas sloshing is generally a very important and a dominating effect in the transport of metals to the outer parts of clusters. |
It is interesting that the discontinuity in the tron abundance is very sharp. while the temperature profile changes more gradually. | It is interesting that the discontinuity in the iron abundance is very sharp, while the temperature profile changes more gradually. |
This has not only been observed in Abel] 2052. but. for example. also in (?).. | This has not only been observed in Abell 2052, but, for example, also in \citep{simionescu2010}. |
The general shape of the surface brightness. temperature. and iron abundance profiles in Abell 2052 look remarkably similar to those observed in M87. | The general shape of the surface brightness, temperature, and iron abundance profiles in Abell 2052 look remarkably similar to those observed in M87. |
The shape suggests that conduction may play a larger role than previously thought. | The shape suggests that conduction may play a larger role than previously thought. |
Earlier observations have shown that conduction should be suppressed across cold fronts (22). likely due to the presence of magnetic fields parallel to the front. | Earlier observations have shown that conduction should be suppressed across cold fronts \citep{ettori2000,markevitch2007} likely due to the presence of magnetic fields parallel to the front. |
However. when a cold front ages. thermal conduction between the cool and hot gas may gradually smooth the temperature jump without affecting the jump m metalicity. | However, when a cold front ages, thermal conduction between the cool and hot gas may gradually smooth the temperature jump without affecting the jump in metalicity. |
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