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Fig.	Fig.
10 shows the expected. projected temperature profile divided by the pre-shock temperature profile as a function of radius.	\ref{fig:shock_kT} shows the expected projected temperature profile divided by the pre-shock temperature profile as a function of radius.
The ~5 per cent rise in the temperature and the ~40 aresec thick shock in the observed. projected temperature profile are fully consistent with the shock model given an average Mach number AZ=1.25 (see Fig. 16)).	The $\sim$ 5 per cent rise in the temperature and the $\sim$ 40 arcsec thick shock in the observed, projected temperature profile are fully consistent with the shock model given an average Mach number $M=1.25$ (see Fig. \ref{fig:shock_kT}) ).
We. therefore. conclude that the high pressure ring is consistent with a shock with Al=1.25.	We, therefore, conclude that the high pressure ring is consistent with a shock with $M=1.25$.
"Thick shocks have also been observed. in the Perseus Cluster (see Fabian 2006). which does not show a clear temperature jump at the Leading edge of the front.	Thick shocks have also been observed in the Perseus Cluster (see Fabian 2006), which does not show a clear temperature jump at the leading edge of the front.
The small increase in temperature within the thick over-pressurized. ring in MSS? suggests that. shock heating is present in these systems but that the thickness and the small amount of heating associated with these weak shocks makes temperature increases dillieult to detect.	The small increase in temperature within the thick over-pressurized ring in 87 suggests that shock heating is present in these systems but that the thickness and the small amount of heating associated with these weak shocks makes temperature increases difficult to detect.
AX second shock is seen closer to the core (~40. arcsec: Section 3. Fig. 7))	A second shock is seen closer to the core $\sim40$ arcsec; Section 3.2; Fig. \ref{fig:zoom}) )
Phe properties of this shock are cillicult to constrain due to its proximity to the core.	The properties of this shock are difficult to constrain due to its proximity to the core.
Many other surface brightness features the cavities filled. with racio plasma seen in Fig. 7))	Many other surface brightness features the cavities filled with radio plasma seen in Fig. \ref{fig:zoom}) )
are observed. at similar raclii. preventing an accurate determination of the pre-shock gas properties and the Mach. number.	are observed at similar radii, preventing an accurate determination of the pre-shock gas properties and the Mach number.
However. the projected temperature jump seen to the south of the AGN at rp~40 aresce (3 kpe: Fig. 7)).	However, the projected temperature jump seen to the south of the AGN at $r\sim40$ arcsec (3 kpc; Fig. \ref{fig:zoom}) ),
suggests a Mach number of at least MZ1.	suggests a Mach number of at least $M\approxgt1.2$.
The presence of the two shocks suggests that AGN outbursts are fairly common.	The presence of the two shocks suggests that AGN outbursts are fairly common.
The estimated Mach numbers from these shocks and their relative distances can be used to determine the frequency of these outbursts.	The estimated Mach numbers from these shocks and their relative distances can be used to determine the frequency of these outbursts.
These shocks suggest that AGN outbursts occur approximately every ~10 Alves.	These shocks suggest that AGN outbursts occur approximately every $\sim10$ Myrs.
Shock heating is likely only relevant in the central regions of the cluster because shocks significantly weaken as they expand.	Shock heating is likely only relevant in the central regions of the cluster because shocks significantly weaken as they expand.
HE repeated shocks occur every LO Alves. as is suggested. here. then AGN driven. weak shocks could produce enough energy to olfset the radiative cooling of the ICM (Nulsen 2007).	If repeated shocks occur every $\sim10$ Myrs, as is suggested here, then AGN driven, weak shocks could produce enough energy to offset the radiative cooling of the ICM (Nulsen 2007).
36hhringer (1995: see also Churazoy 2001) propose that rising bubbles filled with radio emitting plasma may be responsible for dragging cool. metal-rich gas up out of the central regions of clusters.	Böhhringer (1995; see also Churazov 2001) propose that rising bubbles filled with radio emitting plasma may be responsible for dragging cool, metal-rich gas up out of the central regions of clusters.
Buovant bubbles will rise to a height that depends on their entropy. stopping when they reach their appropriate adiabat.	Buoyant bubbles will rise to a height that depends on their entropy, stopping when they reach their appropriate adiabat.
This process may. explain the observed. radio edges at ro~300400 aresee (2331 kpe) and also at r~4005200 aresce (3139 κρο.	This process may explain the observed radio edges at $r\sim300-400$ arcsec (23–31 kpc) and also at $r\sim400-500$ arcsec (31–39 kpc).
When the bubbles reach their maximum height. they flatten.	When the bubbles reach their maximum height, they flatten.
A consequence of this interpretation is that metal-rich gas rising with the radio bubbles should be deposited at a radius similar to that at which the bubbles Hlatten.	A consequence of this interpretation is that metal-rich gas rising with the radio bubbles should be deposited at a radius similar to that at which the bubbles flatten.
Our abundance profiles show evidence for enhancements in Fe abundance at 320«r400 aresee (see Figs.	Our abundance profiles show evidence for enhancements in Fe abundance at $320<r<400$ arcsec (see Figs.
9bb. I0bb).	\ref{fig:kTFe}b b, \ref{fig:kTFeNS}b b).
This is a similar radius to the outer edges of the X-ray. armis.	This is a similar radius to the outer edges of the X-ray arms.
Indeed. bumps are observed in the abundance profiles of all elements except Oxygen (Paper IH).	Indeed, bumps are observed in the abundance profiles of all elements except Oxygen (Paper III).
The amount of Fe that is uplifted can be determined from the excess metallicity measured at that racdus and the eas mass.	The amount of Fe that is uplifted can be determined from the excess metallicity measured at that radius and the gas mass.
In detail. where Alp. and AZp. are the mass ancl excess abundance of Le. M, is the gas mass. and fie=npemna.(Ny.MEREMED is the mass fraction of Fe (Locleers 2003).	In detail, where $M_{{\rm Fe}}$ and ${\Delta Z_{{\rm Fe}}}$ are the mass and excess abundance of Fe, $M_{{\rm g}}$ is the gas mass, and $f_{{\rm Fe}}=\left<m_{{\rm Fe}}\right>/\left<m_{{\rm i\odot}}\right> \times \left( N_{{\rm Fe}}/\Sigma_{{\rm i}} N_{{\rm i}}\right)_{{\rm lodd}}$ is the mass fraction of Fe (Lodders 2003).
We measurect the gas. mass ancl excess ke abundance in the northern sector from a deprojection analysis (using data from position angles of -10555 degrees).	We measure the gas mass and excess Fe abundance in the northern sector from a deprojection analysis (using data from position angles of -108–55 degrees).
This implies a total mass of uplifted Fe of 10 M...	This implies a total mass of uplifted Fe of $\sim1.0\times 10^6$ $_{\odot}$.
We compare this to the Ee mass currently present in the arms (Simionescu 2008).	We compare this to the Fe mass currently present in the arms (Simionescu 2008).
For a gas mass of 5«107 Al. and an Fe abundance of 2.2. those authors measure an Le mass of 1.5«10° M. in the X-ray bright. cool armis.	For a gas mass of $5\times10^8$ $_{\odot}$ and an Fe abundance of 2.2, those authors measure an Fe mass of $1.5\times10^6$ $_{\odot}$ in the X-ray bright, cool arms.
Thus. a single generation of uplifted. metals from buovant »ibbles is. in principle. enough. to explain the observed excess be mass at large radius.	Thus, a single generation of uplifted metals from buoyant bubbles is, in principle, enough to explain the observed excess Fe mass at large radius.
Ht is unknown how much of the uplifted metals will remain at large radius after the xibbles Hatten.	It is unknown how much of the uplifted metals will remain at large radius after the bubbles flatten.
Lower significance bumps at higher radius hat coincide with previous generations of radio bubbles may argue that this process occurs over multiple generations.	Lower significance bumps at higher radius that coincide with previous generations of radio bubbles may argue that this process occurs over multiple generations.
I is ikely that the magnetic field configuration and its evolution will also have an impact Bosedanovié 2009).	It is likely that the magnetic field configuration and its evolution will also have an impact Bogdanović 2009).
In the Perseus. Cluster. metallicity enhancements also correspond well to the edges of several radio lobes. which suggests a similar origin to that discussed here (see Sanders 2005).	In the Perseus Cluster, metallicity enhancements also correspond well to the edges of several radio lobes, which suggests a similar origin to that discussed here (see Sanders 2005).
This process may also partly explain the metallicity ridges observed around the central regions of some cool core galaxy clusters (Sanders 2005: Sanders 2009: Million 2010).	This process may also partly explain the metallicity ridges observed around the central regions of some cool core galaxy clusters (Sanders 2005; Sanders 2009; Million 2010).
We note that bumps in the Fe abundance profiles are not clearly observed to the south.	We note that bumps in the Fe abundance profiles are not clearly observed to the south.
However. the mean Le abundance is larger in the south than in the north and a cold [ront is located at a similar raclius (Simionescu 2007. 2010). making the identification of such a bump more cillieult.	However, the mean Fe abundance is larger in the south than in the north and a cold front is located at a similar radius (Simionescu 2007, 2010), making the identification of such a bump more difficult.