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![Temperature map obtained by using 4 X-ray colours ([0.3-1], [1-2], [2-4.5], [4.5-8] keV) and estimating the expected count rate with XSPEC for a thermal MEKAL model, with fixed Galactic absorption N H = 4.85 × 10 20 cm −2 and metallicity Z = 0.3Z ⊙. Superposed are the X-ray contours. The features outside the last contours are not significant, as they are mainly due to noise fluctuations.](profile/Myriam-Gitti/publication/1801935/figure/fig4/AS:668980905791492@1536508885096/Temperature-map-obtained-by-using-4-X-ray-colours-03-1-1-2-2-45-45-8-keV.png)
Temperature map obtained by using 4 X-ray colours ([0.3-1], [1-2], [2-4.5], [4.5-8] keV) and estimating the expected count rate with XSPEC for a thermal MEKAL model, with fixed Galactic absorption N H = 4.85 × 10 20 cm −2 and metallicity Z = 0.3Z ⊙. Superposed are the X-ray contours. The features outside the last contours are not significant, as they are mainly due to noise fluctuations.
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![Fig. 4. Temperature map obtained by using 4 X-ray colours ([0.3-1],...](profile/Myriam-Gitti/publication/1801935/figure/fig4/AS:668980905791492@1536508885096/Temperature-map-obtained-by-using-4-X-ray-colours-03-1-1-2-2-45-45-8-keV_Q320.jpg)
We report on an XMM-Newton observation of RX J1347.5-1145 (z=0.451), the most luminous X-ray cluster of galaxies currently known, with a luminosity L_X = 6.0 \pm 0.1 \times 10^45 erg/s in the [2-10] keV energy band. We present the first temperature map of this cluster, which shows a complex structure. It identifies the cool core and a hot region at...
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... temperature image of the central cluster region shown in Fig. 4 is build from X-ray colours. Specifically, we produce the mosaics of MOS images in four different energy bands ([0.3- 1] keV, [1][2] keV, [2-4.5] keV and [4.5-8] keV), subtract the background and divide the resulting images by the exposure maps. A temperature is obtained by fitting the values in each pixel with a thermal plasma. In ...
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... It may be noted that a similar hot patch has been reported for the ICM of the cool-core cluster RX J1347.5-1145 (Gitti & Schindler 2004). Here, we may recall an alternative mechanism, according to which radio mini-haloes represent aggregate radio output from type-Ia supernovae occurring in the stellar population distributed across the cluster core (Omar 2019). ...
Clusters of galaxies are excellent laboratories for studying recurring nuclear activity in galactic nuclei since their hot gaseous medium can vastly prolong the detectability of their radio lobes via better confinement. We report here a multi-band study of the sparsely studied galaxy cluster Abell 980, based on our analysis of {\it{Chandra}} X-ray and the GMRT (150 and 325 MHz) and EVLA (1.5 GHz) radio archival data, revealing an unusually rich phenomenology. It is shown to be a quasi-relaxed cluster with a cool core ($T\sim4.2$ keV) surrounded by a hot and extensive intracluster medium (ICM) at $T\sim6.8$ keV. The radio emission shows a rich diversity, having (i) two large diffuse sources of ultra-steep spectrum (USS), extending to opposite extremities of the ICM, each associated with an X-ray brightness discontinuity (cold front), (ii) a bright radio-double of size $\sim55$ kpc coinciding with the central BCG, and (iii) a diffuse radio source, likely a mini-halo of size $\sim110$~kpc around the BCG which possesses a huge ellipsoidal stellar halo of extent $\sim 80$~kpc. The association of cold fronts with two highly aged (~ 260 Myr) USS sources in a cool-core cluster, makes it a very rare system. These USS sources are probably radio lobes from a previous episode of jet activity in the BCG, driven buoyantly towards the outskirts of the X-ray halo, thereby creating the cold fronts. A deeper radio image of this cluster may provide a rare opportunity to verify the recently proposed alternative model which explains radio mini-haloes as the aggregate radio emission from Type I supernovae occurring in the giant stellar halo extended across the cluster core.
... RX J1347.5-1145 is a famous system that has been the subject of numerous SZ effect studies over the past two decades (Pointecouteau et al. 1999;Komatsu et al. 2001;Pointecouteau et al. 2001;Kitayama et al. 2004;Zemcov et al. 2012;Sayers et al. 2016a;Kitayama et al. 2016). It is one of the most massive galaxy clusters observed, with a well-defined cool core and a highly relaxed morphology over most of its projected surface (Allen et al. 2002;Gitti & Schindler 2004;Mantz et al. 2015). However, there is clear evidence for a shock to the SE of the core, with a corresponding enhancement to the thermal SZ effect signal in that region (Mason et al. 2010;Plagge et al. 2013;Ueda et al. 2018;Di Mascolo et al. 2019). ...
We present a measurement of the relativistic corrections to the thermal Sunyaev–Zel’dovich (SZ) effect spectrum, the rSZ effect, toward the massive galaxy cluster RX J1347.5-1145 by combining submillimeter images from Herschel-SPIRE with millimeter wavelength Bolocam maps. Our analysis simultaneously models the SZ effect signal, the population of cosmic infrared background galaxies, and the galactic cirrus dust emission in a manner that fully accounts for their spatial and frequency-dependent correlations. Gravitational lensing of background galaxies by RX J1347.5-1145 is included in our methodology based on a mass model derived from the Hubble Space Telescope observations. Utilizing a set of realistic mock observations, we employ a forward modeling approach that accounts for the non-Gaussian covariances between the observed astrophysical components to determine the posterior distribution of SZ effect brightness values consistent with the observed data. We determine a maximum a posteriori (MAP) value of the average Comptonization parameter of the intracluster medium (ICM) within R 2500 to be 〈 y 〉 2500 = 1.56 × 10 ⁻⁴ , with corresponding 68% credible interval [1.42, 1.63] × 10 ⁻⁴ , and a MAP ICM electron temperature of 〈 T sz 〉 2500 = 22.4 keV with 68% credible interval spanning [10.4, 33.0] keV. This is in good agreement with the pressure-weighted temperature obtained from Chandra X-ray observations, 〈 T x,pw 〉 2500 = 17.4 ± 2.3 keV. We aim to apply this methodology to comparable existing data for a sample of 39 galaxy clusters, with an estimated uncertainty on the ensemble mean 〈 T sz 〉 2500 at the ≃ 1 keV level, sufficiently precise to probe ICM physics and to inform X-ray temperature calibration.
... RX J1347.5-1145 is a famous system that has been the subject of numerous SZ effect studies over the past two decades (Pointecouteau et al. 1999;Komatsu et al. 2001;Pointecouteau et al. 2001;Kitayama et al. 2004;Zemcov et al. 2012b;Sayers et al. 2016a;Kitayama et al. 2016). It is one of the most massive galaxy clusters observed, with a well-defined cool core and a highly relaxed morphology over most of its projected surface (Allen et al. 2002;Gitti & Schindler 2004;Mantz et al. 2015). However, there is clear evidence for a shock to the SE of the core, with a corresponding enhancement to the thermal SZ effect signal in that region (Mason et al. 2010;Plagge et al. 2013;Ueda et al. 2018;Di Mascolo et al. 2019). ...
We present a measurement of the relativistic corrections to the thermal Sunyaev-Zel'dovich (SZ) effect spectrum, the rSZ effect, toward the massive galaxy cluster RX J1347.5-1145 by combining sub-mm images from Herschel-SPIRE with mm-wave Bolocam maps. Our analysis simultaneously models the SZ effect signal, the population of cosmic infrared background (CIB) galaxies, and galactic cirrus dust emission in a manner that fully accounts for their spatial and frequency-dependent correlations. Gravitational lensing of background galaxies by RX J1347.5-1145 is included in our methodology based on a mass model derived from HST observations. Utilizing a set of realistic mock observations, we employ a forward modelling approach that accounts for the non-Gaussian covariances between observed astrophysical components to determine the posterior distribution of SZ effect brightness values consistent with the observed data. We determine a maximum a posteriori (MAP) value of the average Comptonization parameter of the intra-cluster medium (ICM) within R$_{2500}$ to be $\langle y \rangle_{2500} = 1.56 \times 10^{-4}$, with corresponding 68~per cent credible interval $[1.42,1.63] \times 10^{-4}$, and a MAP ICM electron temperature of $\langle \textrm{T}_{\textrm{sz}} \rangle_{2500} = 22.4$~keV with 68~per cent credible interval spanning $[10.4,33.0]$~keV. This is in good agreement with the pressure-weighted temperature obtained from {\it Chandra} X-ray observations, $\langle \textrm{T}_{\textrm{x,pw}}\rangle_{2500} = 17.4 \pm 2.3$~keV. We aim to apply this methodology to comparable existing data for a sample of 39 galaxy clusters, with an estimated uncertainty on the ensemble mean $\langle \textrm{T}_{\textrm{sz}} \rangle_{2500}$ at the $\simeq 1$~keV level, sufficiently precise to probe ICM physics and to inform X-ray temperature calibration.
... RXCJ1347.5-1144 [74]). For all clusters which are classified as 'low metallicity', we fix z/z ⊙ = 0.3 to obtain a lower upper limit of the cooling rates. ...
In this thesis, I present the results of my PhD research on the cooling flow problem in galaxy clusters. The centre of relaxed galaxy clusters has a short radiative cooling time suggesting the presence of a massive cooling flow. However, early studies using high resolution X-ray spectroscopy indicated much lower levels of cooling rate. AGN feedback is thought to be the most likely energy source to balance radiative cooling, though the energy transport and dissipation mechanisms are still under debate. In this work, I study whether AGN feedback can actually balance radiative cooling in a large number of galaxy clusters using high resolution X-ray spectroscopy. The first chapter contains the necessary background of the cooling flow problem and AGN feedback. This is followed by a chapter describing data reduction of XMM-Newton observations. In the third chapter, I present a study of 45 nearby cool core galaxy clusters and groups, where I measure the radiative cooling rate in the softest X-ray band. Then I select a small sub sample of bright clusters to understand the mass temperature profile of the gas in Chapter 4. In Chapter 5, I present a deep study of recent XMM-Newton observations of two luminous clusters at intermediate redshift. Finally, I extend my research on 40 more clusters within a much larger range of distances corresponding to redshift up to 0.6.
... This value is twice as large as that for the outer lobes and the obtained kinetic temperature is four times higher. Meanwhile, the overall temperature of the very luminous cluster of galaxies RX J1347.5-1145 is kT ∼10 keV (Allen, Schmidt & Fabian 2002;Gitti et al. 2004). The high value of kT of the inner lobes of J0028+0035 is, however, comparable to the one Birzan et al. (2017) found for some high-redshift AGNs. ...
We report discovery of a double–double radio source (DDRS) J0028+0035. We observed it with LOFAR, GMRT, and the VLA. By combining our observational data with those from the literature, we gathered an appreciable set of radio flux density measurements covering the range from 74 MHz to 14 GHz. This enabled us to carry out an extensive review of physical properties of the source and its dynamical evolution analysis. In particular, we found that, while the age of the large-scale outer lobes is about 245 Myr, the renewal of the jet activity, which is directly responsible for the double–double structure, took place only about 3.6 Myr ago after about 11 Myr long period of quiescence. Another important property typical for DDRSs and also present here is that the injection spectral indices for the inner and the outer pair of lobes are similar. The jet powers in J0028+0035 are similar too. Both these circumstances support our inference that it is in fact a DDRS which was not recognized as such so far because of the presence of a coincident compact object close to the inner double so that the centre of J0028+0035 is apparently a triple.
... Using this method and the two different z=4 stellarto-halo mass estimates outlined above, we derive a z=0 mass of »= M 2 8 10 z 0 15 ( -) M e . This halo mass is extremely large, rivaling that of fully evolved galaxy clusters seen locally today (e.g., Gitti & Schindler 2004;Gavazzi et al. 2009). Both halo mass evolution functions require a variety of assumptions that we cannot constrain; e.g., the method used in Lemaux et al. (2014) was derived for a single halo, and the growth curves derived in Chiang et al. (2013) are highly dependent on the presumed volume of the observed galaxy overdensity. ...
Recent simulations and observations of massive galaxy cluster evolution predict that the majority of stellar mass buildup happens within cluster members by z = 2, before cluster virialization. Protoclusters rich with dusty, star-forming galaxies (DSFGs) at z > 3 are the favored candidate progenitors for these massive galaxy clusters at z ∼ 0. We present here the first study analyzing stellar emission along with cold dust and gas continuum emission in a spectroscopically confirmed z = 4.002 protocluster core rich with DSFGs, the Distant Red Core (DRC). We combine new Hubble Space Telescope and Spitzer data with existing Gemini, Herschel, and Atacama Large Millimeter/submillimeter Array observations to derive individual galaxy-level properties and compare them to coeval field and other protocluster galaxies. All of the protocluster members are massive (>10 ¹⁰ M ⊙ ), but not significantly more so than their coeval field counterparts. Within uncertainty, all are nearly indistinguishable from galaxies on the star-forming versus stellar mass main-sequence relationship and the star formation efficiency plane. Assuming no future major influx of fresh gas, we estimate that these gaseous DSFGs will deplete their gas reservoirs in ∼300 Myr, becoming the massive quiescent ellipticals dominating cluster cores by z ∼ 3. Using various methodologies, we derive a total z = 4 halo mass of ∼10 ¹⁴ M ⊙ and estimate that the DRC will evolve to become an ultramassive cluster core of mass ≳10 ¹⁵ M ⊙ by z = 0.
... This halo mass is extremely large, rivaling that of fully evolved galaxy clusters seen locally today (e.g. Gitti & Schindler 2004;Gavazzi et al. 2009). Both halo mass evolution functions require a variety of assumptions of which we cannot constrain; e.g. the method used in Lemaux et al. (2014) was derived for a single halo, and the growth curves derived in Chiang et al. (2013) are highly dependent on the presumed volume of the observed galaxy overdensity. ...
Recent simulations and observations of massive galaxy cluster evolution predict that the majority of stellar mass build up happens within cluster members by $z=2$, before cluster virialization. Protoclusters rich with dusty, star-forming galaxies (DSFGs) at $z>3$ are the favored candidate progenitors for these massive galaxy clusters at $z\sim0$. We present here the first study analyzing stellar emission along with cold dust and gas continuum emission in a spectroscopically confirmed $z=4.002$ protocluster core rich with DSFGs, the Distant Red Core (DRC). We combine new \textit{HST} and \textit{Spitzer} data with existing Gemini, \textit{Herschel}, and ALMA observations to derive individual galaxy-level properties, and compare them to coeval field and other protocluster galaxies. All of the protocluster members are massive ($>10^{10}$ M$_\odot$), but not significantly more so than their coeval field counterparts. Within uncertainty, all are nearly indistinguishable from galaxies on the star-forming vs. stellar mass main-sequence relationship. However, when placed on the star formation efficiency plane, DRC components exhibit starburst-like characteristics with SFRs 10-100$\times$ greater than the expected field value at a given molecular gas mass. Assuming no future major influx of fresh gas, we estimate that these gas poor (f$_\mathrm{gas}<25\%$) yet bursty DSFGs will deplete their gas reservoirs in $<30$ Myr. Using various methodologies, we derive a total $z=4$ halo mass of $\sim10^{14}$ M$_\odot$, and estimate that the DRC will evolve to become an ultra-massive cluster core of mass $\gtrsim10^{15}$ M$_\odot$ by $z=0$.
... performed by the Nobeyama Bolometer Array (NOBA; Komatsu et al. 2001) provided early indications of a significant enhancement of the SZ signal to the south-east of the X-ray emission peak (i.e. the 'south-eastern SZ excess'). Subsequent X-ray observations of the cluster by Chandra (Allen, Schmidt & Fabian 2002), XMM-Newton (Gitti & Schindler 2004), and Suzaku (Ota et al. 2008) confirmed the existence of a south-eastern extension in the proximity of the core region, manifesting temperatures higher than the average value of the surrounding ICM. The evidence of a disturbed SZ morphology was Shown are the HST-ACS optical image (top), the Chandra 0.5-3.5 keV Xray surface brightness (SB) map (middle), and the Compton y image of the SZ effect created by feathering the ACA, ALMA, and Bolocam data (bottom; see Section 3 for a description of the SZ data). ...
... We first address the highest temperature gas, which should be associated with the compressed or shock-heated regions. Our temperature map in Fig. 7 suggests that T 20 keV in some regions (for various independent analyses of the X-ray data, see Gitti & Schindler 2004, Ota et al. 2008, Kreisch et al. 2016, which immediately implies that uncertainties on the temperature based on Chandra or XMM-Newton data are very large, especially on the upper side of the confidence interval. Better constraints are provided by the Suzaku satellite, which uses a combination of X-ray CCDs with an additional HXD instrument, sensitive to temperatures above 10 keV. ...
We report the joint analysis of single-dish and interferometric observations of the Sunyaev–Zeldovich (SZ) effect from the galaxy cluster RX J1347.5−1145. We have developed a parametric fitting procedure that uses native imaging and visibility data, and tested it using the rich data sets from ALMA, Bolocam, and Planck available for this object. RX J1347.5−1145 is a very hot and luminous cluster showing signatures of a merger. Previous X-ray-motivated SZ studies have highlighted the presence of an excess SZ signal south-east of the X-ray peak, which was generally interpreted as a strong shock-induced pressure perturbation. Our model, when centred at the X-ray peak, confirms this. However, the presence of two almost equally bright giant elliptical galaxies separated by ∼100 kpc makes the choice of the cluster centre ambiguous, and allows for considerable freedom in modelling the structure of the galaxy cluster. For instance, we have shown that the SZ signal can be well described by a single smooth ellipsoidal generalized Navarro–Frenk–White profile, where the best-fitting centroid is located between the two brightest cluster galaxies. This leads to a considerably weaker excess SZ signal from the south-eastern substructure. Further, the most prominent features seen in the X-ray can be explained as predominantly isobaric structures, alleviating the need for highly supersonic velocities, although overpressurized regions associated with the moving subhaloes are still present in our model.
... A higher angular resolution observation of the SZE was performed by Komatsu et al. (2001) using the Nobeyama Bolometer Array and they found a prominent substructure which has no counterpart in the soft X-ray image from ROSAT. The presence of the substructure has been confirmed by Chandraand XMMNewton(e.g., Allen et al. 2002;Gitti & Schindler 2004) as well as by more recent SZE measurements ( Mason et al. 2010;Korngut et al. 2011;Plagge et al. 2013;Adam et al. 2014;Kitayama et al. 2016). Allen et al. (2002) measured the mean temperature of the ICM to be over 10 keV, which is relatively high compared to other typical clusters. ...
RX J1347.5-1145 (z = 0.451) is one of the most luminous X-ray galaxy clusters; it hosts a prominent cool core and exhibits a signature of a major merger. We present the first direct observational evidence for the subsonic nature of the sloshing motion of the cool core. We find that a residual X-ray image from the Chandra X-ray Observatory after removing the global emission shows a clear dipolar pattern characteristic of gas sloshing, whereas we find no significant residual in the Sunyaev-Zel'dovich effect (SZE) image from the Atacama Large Millimeter/submillimeter Array (ALMA). We estimate the equation of state of perturbations in the gas from the X-ray and SZE residual images. The inferred velocity is km s⁻¹, which is much lower than the adiabatic sound speed of the intracluster medium in the core. We thus conclude that the perturbation is nearly isobaric, and the gas sloshing motion is consistent with being in pressure equilibrium. Next, we report evidence for gas stripping of an infalling subcluster, which likely shock-heats the gas to a temperature well in excess of 20 keV. Using the mass distribution inferred from strong lensing images of the Hubble Space Telescope (HST), we find that the mass peak is located away from the peak position of the stripped gas with a statistical significance of >5σ. Unlike for the gas sloshing, the velocity inferred from the equation of state of the excess hot gas is comparable to the adiabatic sound speed expected for the 20 keV intracluster medium. All of the results support that the southeast substructure is created by a merger. On the other hand, the positional offset between the mass and the gas limits the self-interaction cross section of dark matter to be less than 3.7 h ⁻¹ cm² g⁻¹ (95% CL). © 2018. The American Astronomical Society. All rights reserved..
... Association of the strong radio source with the cooling flow cluster Abell 2390 suggest that this cluster falls in the class of the radio mini-halo and is similar in size to that of the Perseus cluster (Burns et al. 1992). Non-spherical and more irregular morphology of diffuse radio emission from Abell 2390 is similar to that seen in the mini-halo of A2626 (Gitti and Schindler 2004). We also plot the radio emission contours at 4.8 GHz (blue) and 8.4 GHz (cyan) from the VLA data in the same figure. ...
We present results based on the systematic analysis of high resolution 95\,ks
\textit{Chandra} observations of the strong cool core cluster Abell 2390 at the
redshift of z = 0.228, which hosts an energetic radio AGN. This analysis has
enabled us to investigate five X-ray deficient cavities in the hot atmosphere
of Abell 2390 within central 30\arcsec, three of which are newly detected.
Presence of these cavities have been confirmed through a various image
processing techniques like, the surface brightness profiles, unsharp masked
image, as well as 2D elliptical model subtracted residual map. Temperature
profile as well as 2D temperature map revealed structures in the distribution
of ICM, in the sense that ICM in NW direction is relatively cooler than that on
the SE direction. Two temperature jumps, one from 6\,keV to 9.25\,keV at 72 kpc
on the north direction, and the other from 6\,keV to 10.27\,keV at 108 kpc in
the east direction have been observed. These temperature jumps are associated
with the shocks with Mach numbers 1.54$\pm$0.08 and 1.69$\pm$ 0.09,
respectively. Unsharp masked image for A2390 reveals an X-ray edge at
$\sim$74\arcsec (268\,kpc), which is found to coincide with the complex radio
edge due to weak radio sources. The entropy profile at the core reveals a floor
at 12.20$\pm$2.54 keV cm$^2$ and hence confirms intermittent heating by AGN.
The diffuse radio emission mapped using the 1.4\,GHz VLA L-band data fills in
all the X-ray cavities, and exhibit highly irregular morphology with an
elongation along the cool ICM region. The mechanical power injected by the AGN
in the form of X-ray cavities is found to be 3.3$\times$10$^{46}$ erg\,s$^{-1}$
and is roughly two orders of magnitude higher than that lost by the ICM in the
form of X-ray emission, confirming that AGN feedback is capable enough to
quench cooling flow in this cluster.
