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There are some ring-like structures in the temperature map.
There are some ring-like structures in the temperature map.
The entropy state of the cluster ICM appears to correspond to the late stage of a core disruption with filaments of the low-entropy gas spread over a large volume.
The entropy state of the cluster ICM appears to correspond to the late stage of a core disruption with filaments of the low-entropy gas spread over a large volume.
The position of the entropy minimum ts offset from the peak in the pressure.
The position of the entropy minimum is offset from the peak in the pressure.
The cluster has a clover leaf structure in the entropy map like the 0532.9-3701.
The cluster has a clover leaf structure in the entropy map like the 0532.9–3701.
Two pressure maxima could indicate the core rebounce.
Two pressure maxima could indicate the core rebounce.
The symmetry in the pressure map ts regained at 1.5 areminute radius.
The symmetry in the pressure map is regained at 1.5 arcminute radius.
The spectroscopic analysis is reported in Table 12. and Fig.12..
The spectroscopic analysis is reported in Table \ref{t:cl13:t} and \ref{f:cl13}.
The scenario of the disrupted core (region 4) is supported by the spectral analysis (see also Fig.14)).
The scenario of the disrupted core (region 4) is supported by the spectral analysis (see also \ref{f:maps}) ).
The pressure enhancement (region 5) is marginal.
The pressure enhancement (region 5) is marginal.
Famous for its Chandra image (Markevitch et al.
Famous for its Chandra image (Markevitch et al.
2002). the bullet cluster has some distinct features. which also allow us to understand the observation of other clusters.
2002), the bullet cluster has some distinct features, which also allow us to understand the observation of other clusters.
With à Mach number of 3. deduced from the shape of the bullet itself (angle of the Mach cone). the subcluster makes an entropy enhancement in front of it.
With a Mach number of 3, deduced from the shape of the bullet itself (angle of the Mach cone), the subcluster makes an entropy enhancement in front of it.
There are two other large entropy peaks behind and to the south from the bullet.
There are two other large entropy peaks behind and to the south from the bullet.
Apart from the small-scale structure in the center. there appears to be a lack of features on the pressure map. which we attribute to the propagation of the shock out to large radii. thus strongly reducing the contrast.
Apart from the small-scale structure in the center, there appears to be a lack of features on the pressure map, which we attribute to the propagation of the shock out to large radii, thus strongly reducing the contrast.
Therefore. the bullet indicates a situation of a strong merger that is just completed in the center and now moves to outskirts.
Therefore, the bullet indicates a situation of a strong merger that is just completed in the center and now moves to outskirts.
The entropy structure of the core of the main cluster appears disrupted. yet the minimum ts retained. while becoming shallow.
The entropy structure of the core of the main cluster appears disrupted, yet the minimum is retained, while becoming shallow.
In the temperature map we see clear signatures of turbulence. as indicated by the stochastic fluctuations. which in other clusters correspond to a late stage of merging.
In the temperature map we see clear signatures of turbulence, as indicated by the stochastic fluctuations, which in other clusters correspond to a late stage of merging.
This once again demonstrates that the time scales for the relaxation are very different for the cluster center and
This once again demonstrates that the time scales for the relaxation are very different for the cluster center and
greater in these regions.
greater in these regions.
Finally. galaxies with redshifts below 0.01 were excluded. because at these low redshifts the galaxies are very extended and their optical positions are consequently uncertain.
Finally, galaxies with redshifts below 0.01 were excluded, because at these low redshifts the galaxies are very extended and their optical positions are consequently uncertain.
2.
2.
The remaining sample was cross—correlated with the NVSS catalogue.
The remaining sample was cross–correlated with the NVSS catalogue.
À list of candidate galaxies that might be associated with multi-NVSS-component radio sources was derived.
A list of candidate galaxies that might be associated with multi-NVSS-component radio sources was derived.
3.
3.
yoThese multi-NVSS-component candidates were investigated: by necessity. a small proportion of this analysis had to be done visually rather than through automated procedures.
These multi–NVSS–component candidates were investigated; by necessity, a small proportion of this analysis had to be done visually rather than through automated procedures.
Tf a galaxy was confirmed to be associated with a multi-NVSS-component source. the integrated flux densities of the NVSS components were summed to provide the radio source flux density.
If a galaxy was confirmed to be associated with a multi–NVSS–component source, the integrated flux densities of the NVSS components were summed to provide the radio source flux density.
4,
4.
All galaxies matched with a single NVSS source were then cross—correlated with the FIRST catalogue.
All galaxies matched with a single NVSS source were then cross–correlated with the FIRST catalogue.
Note. however. that the presence of a FIRST counterpart was not for a source to be accepted.
Note, however, that the presence of a FIRST counterpart was not for a source to be accepted.
If there was no FIRST counterpart. then the source was accepted or rejected solely upon its NVSS properties.
If there was no FIRST counterpart, then the source was accepted or rejected solely upon its NVSS properties.
5.
5.
If a single FIRST counterpart was associated with the NVSS source. then the source was accepted or rejected on the basis of the properties of the FIRST counterpart.
If a single FIRST counterpart was associated with the NVSS source, then the source was accepted or rejected on the basis of the properties of the FIRST counterpart.
For accepted. matches. however. the adopted radio flux density was taken from the NVSS data.
For accepted matches, however, the adopted radio flux density was taken from the NVSS data.
6.
6.
If multiple FIRST components were associated with the NVSS source. then the source was accepted if it satisfied. criteria for a single-component source (with unrelated additional FIRST sources) or for a radio source with multiple FIRST components.
If multiple FIRST components were associated with the NVSS source, then the source was accepted if it satisfied criteria for a single-component source (with unrelated additional FIRST sources) or for a radio source with multiple FIRST components.
Again. the NVSS catalogue was used to provide the most accurate measure of the radio flux density.
Again, the NVSS catalogue was used to provide the most accurate measure of the radio flux density.
The exact criteria for accepting and rejecting matches in the procedures outlined above were tested and retined using Monte—Carlo simulations.
The exact criteria for accepting and rejecting matches in the procedures outlined above were tested and refined using Monte--Carlo simulations.
Ten catalogues of random sky locations were constructed. over the same sky area as the SDSS survey.
Ten catalogues of random sky locations were constructed, over the same sky area as the SDSS survey.
Each catalogue contained the same number as positions as the list of SDSS galaxies. and these random catalogues were taken through exactly the same steps of cross-comparison with the radio data as the SDSS galaxy catalogue.
Each catalogue contained the same number as positions as the list of SDSS galaxies, and these random catalogues were taken through exactly the same steps of cross–comparison with the radio data as the SDSS galaxy catalogue.
In the subsections that follow. the resulting optimal selection criteria are described. together with the completeness and reliability estimates provided by the Carlo simulations.
In the subsections that follow, the resulting optimal selection criteria are described, together with the completeness and reliability estimates provided by the Monte--Carlo simulations.
Note that the flux densities adopted for the NVSS sources are true integrated flux densities. rather than the peak flux densities quoted in the NVSS catalogues.
Note that the flux densities adopted for the NVSS sources are true integrated flux densities, rather than the peak flux densities quoted in the NVSS catalogues.
The formulae for conversion of peak flux densities to integrated flux densities are provided by Condon shorteitecon98..
The formulae for conversion of peak flux densities to integrated flux densities are provided by Condon \\shortcite{con98}.
Only those radio sources with total flux densities (after summing NVSS components if necessary) above mmJy are retained.
Only those radio sources with total flux densities (after summing NVSS components if necessary) above mJy are retained.
This flux density limit corresponds to approximately 10 times the noise level of the NVSS maps. and is adopted because: (1) at this significance level. all sources should be real and have well—determined positions: (ii) at this flux density limit. the sample is as sensitive to extended single-component NVSS sources (which will have a lower peak flux density) as it is to point sources. and the sensitivity to multi-component NVSS sources will not be significantly worse (for example. a mmJy source composed of two individual components of mmJy would be found).
This flux density limit corresponds to approximately 10 times the noise level of the NVSS maps, and is adopted because: (i) at this significance level, all sources should be real and have well--determined positions; (ii) at this flux density limit, the sample is as sensitive to extended single–component NVSS sources (which will have a lower peak flux density) as it is to point sources, and the sensitivity to multi–component NVSS sources will not be significantly worse (for example, a mJy source composed of two individual components of mJy would be found).
The 5mmly limit corresponds to about 107 + at redshift0.1. which is approximately where the radio luminosity function switches from being dominated by star forming galaxies (low luminosities) to being dominated by AGN thigh luminosities).
The mJy limit corresponds to about $10^{23}$ $^{-1}$ at redshift, which is approximately where the radio luminosity function switches from being dominated by star forming galaxies (low luminosities) to being dominated by AGN (high luminosities).
In order to search for possible multi-component NVSS sources. a search was made for multiple sources within a radius of 3 aremins from each optical galaxy.
In order to search for possible multi-component NVSS sources, a search was made for multiple sources within a radius of 3 arcmins from each optical galaxy.
This distance was selected to be large enough that any genuine multi-component radio source should have at least two matches. but still much smaller than the typical separation of NVSS sources (8-10 aremins).
This distance was selected to be large enough that any genuine multi-component radio source should have at least two matches, but still much smaller than the typical separation of NVSS sources (8-10 arcmins).
For galaxies with two NVSS matches within 3 aremins. the top panels of Fig |. compare the offsets of the two NVSS matches from the optical position for SDSS galaxies (eft) and for an equivalent number of random positions (right).
For galaxies with two NVSS matches within 3 arcmins, the top panels of Fig \ref{nvssdbls} compare the offsets of the two NVSS matches from the optical position for SDSS galaxies (left) and for an equivalent number of random positions (right).
There are a large number of SDSS galaxies for which the nearer NVSS component lies within 15 aresec of the optical galaxy: these are predominantly galaxies containing a single-component NVSS source and the other NVSS source is physically unrelated.
There are a large number of SDSS galaxies for which the nearer NVSS component lies within 15 arcsec of the optical galaxy; these are predominantly galaxies containing a single–component NVSS source and the other NVSS source is physically unrelated.
Such sources were classified as single-component matches (see below).
Such sources were classified as single–component matches (see below).
In addition to these. there is a clear excess of SDSS galaxies (compared to random) that have the two NVSS components each offset by 20-50 aresec from the optical position.
In addition to these, there is a clear excess of SDSS galaxies (compared to random) that have the two NVSS components each offset by 20-50 arcsec from the optical position.
For these systems. the flux-weighted mean position of the two NVSS sources is often within 15 aresee of the optical galaxy (indicated. by the diamonds in the upper panel of Fig L1).
For these systems, the flux-weighted mean position of the two NVSS sources is often within 15 arcsec of the optical galaxy (indicated by the diamonds in the upper panel of Fig \ref{nvssdbls}) ).
Candidate NVSS doubles are therefore selected to be sources with both NVSS components closer than 90 arcsec. a flux-weighted mean position closer than 15 üresec. and the nearer component offset by more than whichever is smaller out of 15 arcsec and the offset of the second source minus 20 arcsec.
Candidate NVSS doubles are therefore selected to be sources with both NVSS components closer than 90 arcsec, a flux-weighted mean position closer than 15 arcsec, and the nearer component offset by more than whichever is smaller out of 15 arcsec and the offset of the second source minus 20 arcsec.
These selection criteria are indicated by the lines on Fig l|..
These selection criteria are indicated by the lines on Fig \ref{nvssdbls}.
The 90 aresee limit is chosen since larger offsets are relatively unlikely and the contamination by random galaxies gets increasingly large beyond this.
The 90 arcsec limit is chosen since larger offsets are relatively unlikely and the contamination by random galaxies gets increasingly large beyond this.
Even with this limit. there is still significant contamination. but the next step of comparison with FIRST helps to alleviate much of this.
Even with this limit, there is still significant contamination, but the next step of comparison with FIRST helps to alleviate much of this.
All of these candidate doubles were cross-correlated with the FIRST catalogue.
All of these candidate doubles were cross-correlated with the FIRST catalogue.
If these are true extended doubles then they may have a central FIRST component associated with a radio source core. and in addition they are likely to be missing flux in the FIRST data due to their extended nature: indeed they may well be undetected by FIRST.
If these are true extended doubles then they may have a central FIRST component associated with a radio source core, and in addition they are likely to be missing flux in the FIRST data due to their extended nature; indeed they may well be undetected by FIRST.
If they are not true doubles. but two individual NVSS sources. then it is likely that a single or double FIRST counterpart is present at each NVSS location. with little missing flux.
If they are not true doubles, but two individual NVSS sources, then it is likely that a single or double FIRST counterpart is present at each NVSS location, with little missing flux.
The candidate doubles were thus classified into three categories: (a) accepted doubles: sources were accepted as NVSS doubles if jey either have a FIRST source within 3 arcsee of the optical yosition. or they satisfy the following three conditions (i) no detected FIRST component (ie.
The candidate doubles were thus classified into three categories: (a) accepted doubles: sources were accepted as NVSS doubles if they either have a FIRST source within 3 arcsec of the optical position, or they satisfy the following three conditions (i) no detected FIRST component (ie.
all of the flux is resolved out by FIRST): ai) both NVSS components lie within 60 aresee of ye SDSS position (larger sources may have additional NVSS Components outside of the 3 aremin limit. and so need to be checked visually: and (it) the angle NVSSI-SDSS-NVSS?2 greater jan. 135 degrees (Ge.
all of the flux is resolved out by FIRST); (ii) both NVSS components lie within 60 arcsec of the SDSS position (larger sources may have additional NVSS components outside of the 3 arcmin limit, and so need to be checked visually); and (iii) the angle NVSS1-SDSS-NVSS2 greater than 135 degrees (ie.
consistent with a double radio source with a bend of «45 degrees).
consistent with a double radio source with a bend of $<45$ degrees).
Edge-on local starburst ealaxies show unambiguous evidence for ~10 kiloparsec-scale. weaklIy-collimated. ijpolar outflows (Ileckiiun.Lehuert&Armus1993).
Edge-on local starburst galaxies show unambiguous evidence for $\sim 10$ kiloparsec-scale, weakly-collimated, bipolar outflows \citep{heck93}.
Cirrent theory holds that these galactic superwinds are owvered by the collective mechanical power of large nuubers of Type II superuovae (SNe) aud stellay siuds. hat result from the laree population of massive stars ornmed in the starburst Chevalier&Cleese(L985). renceforth CC).
Current theory holds that these galactic superwinds are powered by the collective mechanical power of large numbers of Type II supernovae (SNe) and stellar winds, that result from the large population of massive stars formed in the starburst \citet{cc}, henceforth CC).
Tf this mechanical euergv is cfiicicutly hermalized m the starburst region converted back into the thermal οποίον of a hot eas Bbv shocks. as SNe and stellar winds collideV then a pressure-driven outflow roni the galaxy results.
If this mechanical energy is efficiently thermalized in the starburst region converted back into the thermal energy of a hot gas by shocks, as SNe and stellar winds collide), then a pressure-driven outflow from the galaxy results.
The hot gas blows out of the host ealaxv ISM along the minor axis. forming the outflows seen in snon-thenual. radio cussion. optical enission lines. ax μαoft thermal XN-rav enüssonu in the halos of local starbursts.
The hot gas blows out of the host galaxy's ISM along the minor axis, forming the outflows seen in non-thermal radio emission, optical emission lines, and soft thermal X-ray emission in the halos of local starbursts.
Superwiuds are of cosmological interest απ they transport large amounts of eas. in particular ucwly svuthesized heavy elemieuts aud energy. mto the media (OAD.
Superwinds are of cosmological interest as they transport large amounts of gas, in particular newly synthesized heavy elements, and energy, into the medium (IGM).
Quautifving this mass. metal aud energv transport in local starburst galaxies is essential for understanding the significance of outflows from star-fornuue ealaxics integrated. over the history of the Universe.
Quantifying this mass, metal and energy transport in local starburst galaxies is essential for understanding the significance of outflows from star-forming galaxies integrated over the history of the Universe.
Uowever. even the basic physical propertics of local superwiuds such as mass outflow rates. energv content. abundances ancl kinematics are uncertain.
However, even the basic physical properties of local superwinds such as mass outflow rates, energy content, abundances and kinematics are uncertain.
Measuring the pliysical properties of the hot eas driving hese outflows is of crucial ο or several simple reasons,
Measuring the physical properties of the hot gas driving these outflows is of crucial importance for several simple reasons.
Firstly. the hot eas efiicicutly transports the uajoritv of the euergv of the outtlow Strickland&Stevens (2000))).
Firstly, the hot gas efficiently transports the majority of the energy of the outflow \citet{ss2000}) ).
Secondly. the SN-heated eas is thought o contain the majority of the newly svuthesized metals.
Secondly, the SN-heated gas is thought to contain the majority of the newly synthesized metals.
Finally. this energetic gas ultimately controls the ejection of mass from the galaxy. (although the majority of the uass of the outflow may be in ambient ISAL swept-up by he wind. this eas is accelerated to high velocity by the vot. fast. wind fluid. CC).
Finally, this energetic gas ultimately controls the ejection of mass from the galaxy (although the majority of the mass of the outflow may be in ambient ISM swept-up by the wind, this gas is accelerated to high velocity by the hot, fast, wind fluid, CC).
Iu principle. X-ray observations of the thermal emission roni hot gas in superwinds can be used to measure he properties of the hot eas.
In principle, X-ray observations of the thermal emission from hot gas in superwinds can be used to measure the properties of the hot gas.
Large amounts ofROSAT and N-rav data on starbursts already: exists (see
Large amounts of and X-ray data on starbursts already exists (see
time ἀσίαν effects (Rubilar&Eckut2001:Wein-bereetal.
time delay effects \citep{rubilar,weinberg}.
2005).. For example. a torus of matter of mass m orbiting the black hole at a distance Rowill induce fractional changes in the appareut angular momentum and quadrupole moment of order 6.7/7~GnΑΠΑΟ1v)
For example, a torus of matter of mass $m$ orbiting the black hole at a distance $R$ will induce fractional changes in the apparent angular momentum and quadrupole moment of order $\delta J/J \sim (m/M)(R/M)^{1/2}(1/\chi)$
We will construct models for the mass distributions of the bulge. disc. bar and dark matter halo using paranieters [from previous studies. anc map light ravs [rom the measured image positions to the source plane.
We will construct models for the mass distributions of the bulge, disc, bar and dark matter halo using parameters from previous studies, and map light rays from the measured image positions to the source plane.
Varving the contribution of cach component will vary the convergence and shear within the images and. shift their. back-mapped positions in the source plane.
Varying the contribution of each component will vary the convergence and shear within the images and shift their back-mapped positions in the source plane.
A potential solution is obtained when a particular addition of the four components produces a common source position.
A potential solution is obtained when a particular addition of the four components produces a common source position.
Clearly. the four images originate from the same point in the source plane.
Clearly, the four images originate from the same point in the source plane.
The actual position of the source quasar cannot be constrained.
The actual position of the source quasar cannot be constrained.
The centre of the galaxy will be considered. fixed. given the relatively few degrees of freedom.
The centre of the galaxy will be considered fixed given the relatively few degrees of freedom.
Rotation curves for potential solutions will be produced and compared with neutral hydrogen rotation measurements and the measured mass lving within the images.
Rotation curves for potential solutions will be produced and compared with neutral hydrogen rotation measurements and the measured mass lying within the images.
The combination of both lensing and dynamical constraints increases the number of constrained parameters. and consequently reduces the number of unknowns.
The combination of both lensing and dynamical constraints increases the number of constrained parameters and consequently reduces the number of unknowns.
The mocels used for the mass clistributions of the four principal galactic components are standard profiles from the literature. tailored to suit this galaxy.
The models used for the mass distributions of the four principal galactic components are standard profiles from the literature, tailored to suit this galaxy.
The bulece is modelled as both à. modified ce Vaucouleurs surface mass cistribution (cde Vaucouleurs 1948. 1959). where it is assumed the mass follows the light (constant mass-to-light ratio) and an exponential surface mass profile. as in the models of Schmidt (1996).
The bulge is modelled as both a modified de Vaucouleurs surface mass distribution (de Vaucouleurs 1948, 1959), where it is assumed the mass follows the light (constant mass-to-light ratio) and an exponential surface mass profile, as in the models of Schmidt (1996).
The modification to both allows the introduction of an ellipticity.- c. such that for the de Vaucouleurs profile. where M is the value of the surface mass density at that position. ry is the characteristic scale length of the bulge. and e is defined. by. where e and b are the semi-major and minor axes respectivelv.
The modification to both allows the introduction of an ellipticity, $e$, such that for the de Vaucouleurs profile, where $\Sigma$ is the value of the surface mass density at that position, $r_b$ is the characteristic scale length of the bulge, and $e$ is defined by, where $a$ and $b$ are the semi-major and minor axes respectively.
Phe central. surface. density (Xo 1057). is denoted “he.
The central surface density $\Sigma_0\times$ $^{3.33}$ ) is denoted `bg'.
The exponential profile is mocellec simply by introducing the ellipticitv (assumed to be a projection elfect). and again "bg is the central surface mass clonsity.
The exponential profile is modelled simply by introducing the ellipticity (assumed to be a projection effect), and again `bg' is the central surface mass density.
The dise is mocelled as an exponential surface density.
The disc is modelled as an exponential surface density.
Unlike the bulge which is treated: with the ellipticity as measured. the disc is rotated to its measured inclination of i607.
Unlike the bulge which is treated with the ellipticity as measured, the disc is rotated to its measured inclination of $i$ $^{\circ}$.
This involves projecting the volume to a surface mass density by rotating the z-axis and redefining co-ordinates.
This involves projecting the volume to a surface mass density by rotating the $z$ -axis and redefining co-ordinates.
lU we assume the disc is uniformly clistributecd in. the direction. then we can simply. write. where the proportionality. includes a factor reflecting the thickness of the cise. assumed to be constant. ancl ry is the characteristic disc scale length.
If we assume the disc is uniformly distributed in the $z$ direction, then we can simply write, where the proportionality includes a factor reflecting the thickness of the disc, assumed to be constant, and $r_d$ is the characteristic disc scale length.
Upon rotation about the a-axis (such that it becomes the major axis of the ellipse) by the inclination angle. 760. the surface mass density is the integral through the rotated axis. 2’ where the limits of integration bound. the origina constant disc thickness at the inclination angle. (taken as Az=h00pe). the primec co-ordinates represent the new. observed. Cartesian system and ‘de’ denotes the centra surface mass clonsity.
Upon rotation about the $x$ -axis (such that it becomes the major axis of the ellipse) by the inclination angle, $i$ $^{\circ}$, the surface mass density is the integral through the rotated axis, $z^\prime$, where the limits of integration bound the original constant disc thickness at the inclination angle (taken as $\Delta{z}$ =500pc), the primed co-ordinates represent the new, observed Cartesian system and `dc' denotes the central surface mass density.
The bar has been extensively modelled: by Schmid (1996) and we will use his surface mass clistribution au position angle.
The bar has been extensively modelled by Schmidt (1996) and we will use his surface mass distribution and position angle.
Schmidt uses a Ferrers model with an ellipticity. €. where ‘br’ is the central surface density. A is the Ferrers exponent. and the Gr.y) co-ordinates lic in the rotated (rame of the bar.
Schmidt uses a Ferrers model with an ellipticity, $e$, where `br' is the central surface density, $\lambda$ is the Ferrers exponent, and the $(x,y)$ co-ordinates lie in the rotated frame of the bar.
Sehimidt. finds different exponents.. ellipticities ancl scale lengths depending on the profiles used to fit to the light distribution.
Schmidt finds different exponents, ellipticities and scale lengths depending on the profiles used to fit to the light distribution.
For an exponential bulge and disc. he finds A=2 e=0.64 and b—1.02:0.3 arcsec fit the observations best.
For an exponential bulge and disc, he finds $\lambda$ =2, $e$ =0.64 and $\pm$ 0.3 arcsec fit the observations best.
For a de Vaucouleurs bulge ancl exponential disc. he finds A=O0.5. e—0.89 and b=3.10.9 arcsec.
For a de Vaucouleurs bulge and exponential disc, he finds $\lambda$ =0.5, $e$ =0.89 and $\pm$ 0.9 arcsec.