XMM-Newton X-ray and HST weak gravitational lensing study of the extremely X-ray luminous galaxy cluster \RXJ(z=0.902)

XMM-Newton X-ray and HST weak gravitational lensing study of the extremely X-ray luminous galaxy cluster ClJ120958.9+495352 ($z=0.902$)

Key Words.:
galaxies: clusters: general - galaxies: clusters: individual: Cl 120958.9+495352 - X-rays: galaxies: clusters - gravitational lensing:weak
13456789

Abstract

Context:Observations of relaxed, massive and distant clusters can provide important tests of standard cosmological models, for example by using the gas mass fraction. To perform this test, the dynamical state of the cluster and its gas properties have to be investigated. X-ray analyses provide one of the best opportunities to access this information and to determine important properties such as temperature profiles, gas mass, and the total X-ray hydrostatic mass. For the last of these, weak gravitational lensing analyses are complementary independent probes that are essential in order to test whether X-ray masses could be biased.

Aims:We study the very luminous, high redshift () galaxy cluster Cl 120958.9+495352 using XMM-Newton data. We measure global cluster properties and study the temperature profile and the cooling time to investigate the dynamical status with respect to the presence of a cool core. We use Hubble Space Telescope (HST) weak lensing data to estimate its total mass and determine the gas mass fraction.

Methods:We perform a spectral analysis using an XMM-Newton observation of 15 ks cleaned exposure time. As the treatment of the background is crucial, we use two different approaches to account for the background emission to verify our results. We account for point spread function effects and deproject our results to estimate the gas mass fraction of the cluster. We measure weak lensing galaxy shapes from mosaic HST imaging and select background galaxies photometrically in combination with imaging data from the William Herschel Telescope.

Results:The X-ray luminosity of Cl 120958.9+495352 in the  keV band estimated from our XMM-Newton data is  erg/s and thus it is one of the most X-ray luminous clusters known at similarly high redshift. We find clear indications for the presence of a cool core from the temperature profile and the central cooling time, which is very rare at such high redshifts. Based on the weak lensing analysis, we estimate a cluster mass of and a gas mass fraction of in good agreement with previous findings for high redshift and local clusters.

Conclusions:

1 Introduction

In the paradigm of hierarchical structure formation very massive and distant clusters should be extremely rare. These clusters provide the opportunity for many interesting astrophysical and cosmological studies. The gas mass fraction () of dynamically relaxed clusters is an important probe of cosmological models (Allen et al. 2008, Mantz et al. 2014) as the matter content of these objects should approximately match the matter content of the universe (e.g., White et al. 1993, Allen et al. 2011, and references therein). In particular high-redshift clusters are of interest where the leverage on the cosmology is largest.

The cooling time for these clusters is very short and the presence of a cool core is believed to be strongly related to the dynamical status of the cluster (e.g., Hudson et al. 2010). McDonald et al. (2017) studied the evolution of the ICM and cool core clusters over the past 10 Gyr. Their results imply that from redshift to cool cores basically do not evolve in size, density, and mass. Additionally, the level of agreement of the properties of these rare clusters with existing scaling relations (e.g., Reichert et al. 2011, Pratt et al. 2009) has great significance for cosmology as the properties can provide tests of these scaling laws and assess whether they are in line with standard cosmological predictions.

So far, only a few of these rare, relaxed, massive, and high redshift objects have been found; two examples are Cl0046.3+8530 (Maughan et al. 2004b) and Cl1226.9+3332 (Maughan et al. 2004a). In the Massive Cluster Survey (MACS) (Ebeling et al. 2007, Ebeling et al. 2010), many interesting objects have been identified, for example extreme cooling in cluster cores such as MACS1931.8-2634 (Ehlert et al. 2011), and a number of dynamically relaxed clusters that can be used for cosmological tests. However, almost all of those relaxed clusters are at smaller redshifts than the object studied here. Two of the most distant clusters at , Cl1415.1+3612 () and 3C 186 (), were studied in detail by Babyk (2014) and Siemiginowska et al. (2010) using deep Chandra observations. The observations revealed a cool core for both objects with a short cooling time for Cl1415.1+3612 within the core region of  Gyr and a gas-mass fraction consistent with local clusters for 3C 186. With respect to the luminosity, another extreme example is the El Gordo galaxy cluster at with  erg/s (Menanteau et al. 2012) which is one of the most massive and luminous clusters found so far.

Figure 1: Combined, cleaned, exposure corrected, and smoothed MOS image of Cl 120958.9+495352. White circles show the excluded point sources.

For cosmological tests, the total cluster mass is an important quantity for which weak gravitational lensing provides an independent probe in addition to the X-ray hydrostatic mass. The gravitational potential imprints coherent distortions onto the observed shapes of background galaxies (e.g., Bartelmann & Schneider 2001; Schneider 2006). Measurements of these weak lensing distortions directly constrain the projected mass distributions and cluster masses (Hoekstra et al. 2013). These measurements are sensitive to the total matter distribution, including both dark matter and baryons. Especially at high redshifts, the Hubble Space Telescope (HST) is an essential tool for the analysis of such objects as ground-based telescopes are not able to resolve the shapes of the very distant background galaxies.

Recently, Buddendiek et al. (2015) performed a combined search of distant massive clusters using ROSAT All Sky Survey and Sloan Digital Sky Survey (SDSS) data covering an area of 10,000 deg. They found 83 high-grade candidates for X-ray luminous clusters between and obtained William Herschel Telescope (WHT) or Large Binocular Telescope (LBT) imaging to confirm the candidates. One of the clusters they found is special in many respects: Cl 120958.9+495352 is the most X-ray luminous cluster in their sample. Also, it has the second highest spectroscopically confirmed redshift in their sample, and their richness and Sunyaev-Zel’dovich (SZ) measurements independently indicate a high cluster mass. According to the Planck catalog of SZ sources (Planck Collaboration et al. 2015) Cl 120958.9+495352 is on par with the five most X-ray luminous clusters found at . It is thus a valuable candidate for a distant cooling-core cluster and provides a great opportunity to study one of these rare systems in detail.

In this work we perform a spectroscopic XMM-Newton and HST weak lensing study of this extraordinary object found by Buddendiek et al. (2015). We investigate the temperature profile with respect to the presence of a cool core and determine the cooling time within  kpc. In Sec. 2 we describe the properties of Cl 120958.9+495352, the data reduction procedure, and the analysis strategy for HST and XMM-Newton and for the XMM-Newton background. Sec. 3 gives the results, which are then discussed in Sec. 4.

Throughout the analysis we use a flat CDM cosmology with  km/s/Mpc, and . All uncertainties are given at the 68% confidence level and overdensities refer to the critical density. All magnitudes are in the AB system.

2 Observations and data analysis

2.1 XMM-Newton analysis

Data reduction

Cl 120958.9+495352 is the most luminous cluster in the sample of Buddendiek et al. (2015). From the ROSAT data, this cluster already appears to be one of the most luminous known at high redshifts with an observer-frame luminosity of  erg/s (Buddendiek et al. 2015). They measure the spectroscopic redshift to be and their SZ data yields a mass of .

We analyze XMM-Newton observations of the cluster with  ks cleaned exposure time (XMM-Newton observation IDs 0722530101 and 0722530201, PI of the joint XMM-Newton and HST program: T. Schrabback). The observations were performed in October and November 2013 (see Tab. 1) and were executed over the course of two revolutions, which we analyze simultaneously.

Following the standard data reduction procedure10 using SAS version 14.0.0, we use the ODF data and apply cifbuild to catch up with the latest calibration and odfingest to update the ODF summary file with the necessary instrumental housekeeping information. Then we proceed by applying emchain and epchain (for MOS and PN detector, respectively) to create calibrated event files.

On these calibrated files we apply the following filters for the event pattern of the triggered CCD pixels (the numbering is based to the ASCA GRADE selection) and the quality flag of the pixels: PATTERN for the MOS detectors, for PN PATTERN ; FLAG for both detectors. Because of anomalous features on CCD4 of MOS1, we additionally filter out events falling onto this chip. The CCD3 and CCD6 of MOS1 were damaged by micro meteorite events and the data of these detectors cannot be used.

In a next step we create light curves for both revolutions and all detectors in the energy range  keV. The observation in the second revolution shows strong flaring for a large fraction of the exposure time. We apply a clipping to all the light curves to filter the flared time intervals and inspected the light curves afterwards which then show no further hint of flaring. This removes approximately half of the exposure time for the second observation (revolution 2546).

To detect point sources in the field of view (FOV), we create images from the event files for all detectors in five energy bands between  keV. These images are provided in the task edetect_chain.

Rev. date R.A. Dec. Cleaned exp. time Filter
2545 Oct. 2013 182.512 49.926 9.6 ks thick
2546 Nov. 2013 182.510 49.924 5.1 ks thick
Table 1: Details of the XMM-Newton observation of Cl 120958.9+495352.

Spectral fitting

An X-ray image of the cluster is shown in Fig. 1. We select three annular regions around the center and choose the region sizes such that we can achieve a S/Bkg ratio (i.e., counts/counts) of in the outermost annulus and higher for the inner regions to avoid systematic biases. The final regions are and . We fit the spectra of all annuli and for all detectors and the two observations simultaneously using the Cash-Statistic (cstat option) in XSPEC. For the cluster emission we use an absorbed APEC model with a column density from Willingale et al. (2013), which also includes molecular hydrogen and the solar metal abundance table from Asplund et al. (2009). We assume the same abundance in all annuli and thus link the corresponding model parameters. The XMM-Newton point spread function (PSF) is HEW. We correct for the effect of photon mixing between different annuli due of the PSF as described in Sec. 2.1.5.

From our HST data (Sec. 3.1) we estimate and therefore, for the estimation of the global cluster properties, we extract spectra in this region. For the analysis of such a high redshift cluster, the background treatment is crucial. The different background components are described in Sec. 2.1.3 and 2.1.4 and we follow two approaches for the treatment of the background:

  1. Background modeling One approach is to model all the different background components individually in the fitting procedure. These components are described in the following sections. We determine models for the quiescent particle background and the X-ray background and use them in the fitting of the cluster emission. We additionally introduce a power-law model to account for the residual soft proton emission, which is left over emission after the flare filtering. The index is linked for the two MOS detectors while the normalizations for each detector are independent. We use an energy range between  keV. The results of this approach can be found in Sec. 3.2.

  2. Background subtraction The cluster has a small extent on the sky, thus we do not expect significant cluster emission beyond estimated from our HST data. For this reason we are able to subtract the full background from the spectra. To do so, we extract background spectra in an annulus between . This region lies completely on the MOS CCD1 chips which is important because the particle background shows strong variations between the different chips. Also for PN this region is close enough to the source extraction region to properly model the Ni and Cu lines. As for the first method, the energy range is  keV and the results of this procedure are described in Sec. 3.2.

Quiescent particle background

The quiescent particle background (QPB) is caused by highly energetic particles interacting with the detector and the surrounding material. It is composed of a continuum emission and fluorescent lines from various elements contained in the assembly of the satellite. XMM-Newton is equipped with a filter wheel system which can be used to measure the level of the QPB. When the filter is closed, only the high energy particles can penetrate the filter and a spectrum of the QPB can be obtained. We use merged event files of the filter-wheel-closed observations which are close to the time of the observation (revolution for the MOS detectors and for PN). The continuum part of the spectrum can be described by two power laws, while the fluorescent lines are modeled by Gaussians. The QPB varies for all detectors and with the position on the detector. Therefore, we fit the model in two regions – from (the source region, which lies completely on CCD1 for the MOS destectors) and from (the region where we determine the X-ray background, see Sec. 2.1.4) – for all detectors independently. For the QPB, diagonal responses are used in the fit and no ancillary response file (ARF) is applied as these particles do not suffer from instrumental effects such as vignetting. The spectra with the best fit models are shown in Fig. 2. When fitting the cluster emission, the QPB normalizations of the power-law components and the Gaussian lines are allowed to vary separately by , due to possible spatial and temporal variations of the QPB.

Figure 2: Spectra and best fit models of the QPB obtained from the filter-wheel-closed observations and extracted on the central chip in the region for MOS1 (black), MOS2 (red) and PN (green) and normalized to the extraction area.

X-ray background

The X-ray background (XRBG) emission is caused by different sources: 1.) a local component and solar wind charge exchange, 2.) a component from the Milky Way halo plasma, and 3.) the superposition of the X-ray emission from distant AGNs causing a diffuse background (CXB). To model these background components we extract a spectrum in a region , where no cluster emission is expected. Additionally, ROSAT All-Sky-Survey data11 are used to support the estimation of the background parameters at energies between  keV. The first XRBG component can be modeled using an APEC model with temperature and normalization as free fitting parameters. The redshift and the abundance are set to 0 and 1, respectively. The second component can be described by an absorbed APEC model. The superposition of AGN emission was analyzed by De Luca & Molendi (2004) and can be modeled by an absorbed power law with a photon index of 1.41. We accounted for the particle background in this annulus by using the previously determined model in Sec. 2.1.3 in the region with two floating multiplicative constants () for the continuum part and the fluorescent lines. We additionally introduce a power-law model to account for the residual soft proton emission. Also for this model we use diagonal response matrices.

The XRBG spectra and the best fit models for the different components are shown in Fig. 3 for the off-axis region between and .

Figure 3: Spectra and best fit models for the XRBG + QPB for MOS1 (black), MOS2 (red), and PN (green) in the region . The different components of the XRBG are shown as dotted, dash-dotted and dashed lines for the local, halo and CXB component, respectively. The power law component for the residual soft proton emission is shown as short-dashed line. For the spectra and models of the QPB see Fig. 2.

PSF correction

The extent of the cluster on the sky is small; therefore, we have to choose annular region sizes which suffer from the PSF size of XMM-Newton. This causes “mixing” of photons, i.e., photons originating from a certain region on the sky are detected in another region on the detector. This has an impact on the spectra and influences the measurements, especially the determination of the temperature profile. To avoid this we introduce a PSF correction. The XMM-Newton task arfgen allows us to calculate cross-region ARFs. Via these cross-region ARFs the effective area for the emission coming from one particular region, but detected in another, is estimated. These ARFs can then be used in the fitting process to account for the PSF effects. Therefore, we introduced additional absorbed APEC models for each combination of photon mixing (e.g., photons from region 1 on the sky but detected in region 2 on the detector, etc.). These models use the cross-region ARFs and the model parameters are linked to the parameters of the annulus the emission truly originates from, as described in the corresponding SAS-thread12. We neglect the PSF effects for the emission coming from the outermost annulus to the two inner annuli as the effective area for this mixing is close to zero.

2.2 HST analysis

Here we perform a weak gravitational lensing analysis based on new Hubble Space Telescope observations of Cl 120958.9+495352, obtained within the joint XMM-Newton+HST program (HST program ID 13493). Weak lensing measurements require accurate measurements of the shapes of background galaxies well behind the cluster. Given the high redshift of Cl 120958.9+495352, typical weak lensing background galaxies are at redshifts . As most of them are unresolved in ground-based seeing-limited data, HST observations are key for this study. Specifically, we analyze observations obtained with the Advanced Camera for Surveys (ACS) in the F606W filter in a mosaic covering a area (corresponding to  Mpc), with integration times of 1.9 ks per pointing, each split into four exposures.

The data reduction and analysis is conducted with the same pipeline that was used for the weak lensing analysis of high-redshift galaxy clusters from the South Pole Telescope Sunyaev-Zel’dovich Survey (Bleem et al. 2015) presented in Schrabback et al. (2016, hereafter S16). Therefore, we only summarize the main analysis steps here and refer the reader to S16 for further details.

For the ACS data reduction we employ basic calibrations from CALACS, the correction for charge-transfer inefficiency from Massey et al. (2014), MultiDrizzle (Koekemoer et al. 2003) for the cosmic ray removal and stacking, and scripts for the image registration and improvement of masks from Schrabback et al. (2010). We detect objects using Source Extractor (Bertin & Arnouts 1996) and measure shapes using the KSB+ formalism (Kaiser et al. 1995; Luppino & Kaiser 1997; Hoekstra et al. 1998) as implemented by Erben et al. (2001) with adaptions for HST measurements described in Schrabback et al. (2007, 2010). In particular, we apply a model for the temporally and spatially varying HST PSF constructed from a principal component analysis of ACS stellar field observations. In order to estimate cluster masses from weak lensing, accurate knowledge of the source redshift distribution is required. Here we follow the approach from S16, who first apply a color selection to remove cluster galaxies from the source sample, and then estimate the redshift distribution based on CANDELS photometric redshift catalogs (Skelton et al. 2014), to which they apply consistent selection criteria, as used in the cluster fields, and statistical corrections for photometric redshift outliers.

For the color selection we make use of additional -band observations of Cl 120958.9+495352 obtained with the Prime Focus Camera PFIP (Prime Focus Imaging Platform) on the 4.2 m William Herschel Telescope (ID: W14AN004, PI: Hoekstra) on March 26, 2014. These observations were taken with the new red-optimized RED+4 detector, which has an imaging area of pixels, with a pixel scale of 027 and an field of view. We reduce these data using theli (Erben et al. 2005; Schirmer 2013), co-adding exposures of a total integration time of  ks and reaching a limit of in circular apertures of , with an image quality of , where corresponds to the FLUX_RADIUS parameter from Source Extractor. We use SDSS (SDSS Collaboration et al. 2016) for the photometric calibration and convolve the ACS F606W imaging to the ground-based resolution to measure colors. For galaxies at the cluster redshift the 4000Å/Balmer break is located within this filter pair. Therefore, by selecting very blue galaxies in this color, we can cleanly remove the cluster galaxies, while selecting the majority of the background sources carrying the lensing signal (see S16). To account for the increased scatter at faint magnitudes we apply a magnitude-dependent selection () for galaxies with magnitudes () measured in 07 diameter apertures from the non-convolved ACS images. These cuts correspond to a color selection in the CANDELS catalogs of (). In order to select consistent galaxy populations between the cluster field and the CANDELS catalogs we additionally apply consistent lensing shape cuts and add photometric scatter to the deeper CANDELS catalogs as empirically estimated in S16. The depth of our final weak lensing catalog for Cl 120958.9+495352   is mostly limited by the mediocre seeing conditions during the WHT observations, which require us to substantially degrade the F606W images in the PSF matching for the color measurements. As a result, we have to apply a rather stringent selection based on the Source Extractor auto magnitude, which results in a final galaxy number density of 9.6/arcmin, while the shape catalog extends to . We therefore recommend that future programs following a similar observing strategy should ensure that complementary ground-based observations are conducted under good seeing conditions in order to fully exploit the statistical power of the HST weak lensing shape catalogs.

Taking the magnitude distribution and shape weights of our color-selected source catalog into account, we estimate an effective mean geometric lensing efficiency of based on the CANDELS analysis (see S16 for details).

3 Results

3.1 HST results

In Fig. 4 we show contours of the weak lensing mass reconstruction of Cl 120958.9+495352, overlaid onto a color image from the ACS/WFC F606W imaging and WFC3/IR imaging obtained in F105W (1.2 ks) and F140W (0.8 ks). The reconstruction employs a Wiener filter (McInnes et al. 2009; Simon et al. 2009), as further detailed in S16. Divided by the r.m.s. image of the reconstructions of 500 noise fields, the contours indicate the signal-to-noise ratio of the weak lensing mass reconstruction, starting at in steps of . The reconstruction peaks at 12:10:00.26, +49:53:48.2, with a positional uncertainty of 23 in each direction (estimated by bootstrapping the source catalog), which makes it consistent with the locations of the X-ray peak and the BCG at the level.

Fig. 5 displays the measured tangential reduced shear profile of Cl 120958.9+495352   as a function of the projected separation from the X-ray peak, combining measurements from all selected galaxies with , as done in S16. Fitting these measurements within the radial range assuming a model for a spherical NFW density profile according to Wright & Brainerd (2000) and the mass-concentration relation from Diemer & Kravtsov (2015), we constrain the cluster mass to and .

Here we have corrected for a small expected bias of % (%) for () caused by the simplistic mass model, as estimated by S16 and further detailed in Applegate et al. (in prep.) using the analysis of simulated cluster weak lensing data. Differing from S16 we assume negligible miscentering for the bias correction, justified by the regular morphology of the cluster and precise estimate of the X-ray cluster center. The quoted statistical uncertainty includes shape noise, uncorrelated large-scale structure projections, and line-of-sight variations in the source redshift distribution, while the systematic error estimate takes shear calibration, redshift errors, and mass modeling uncertainties into account (see S16 for details). Here we have doubled the systematic mass modeling uncertainties used in S16 as we include somewhat smaller scales in the fit13. When restricting the radial range in the fit to the more conservative range from S16, the resulting constraints are and with smaller expected and corrected biases of 3% (5%) for () and smaller systematic uncertainties, but increased statistical errors.

For the comparison to the X-ray measurements we additionally require weak lensing mass estimates for an overdensity . When assuming the Diemer & Kravtsov (2015) mass-concentration relation and extrapolating the bias corrections14, the weak lensing mass constraints correspond to when including measurements from scales , and when restricting the analysis to scales .

We expect that our mass estimation procedure is unbiased within the quoted systematic uncertainties for a random population of massive clusters. For an individual cluster like the one studied here, deviations in the density profile from the assumed NFW profile with a concentration from the Diemer & Kravtsov (2015) mass-concentration relation lead to additional scatter in the mass estimates. To estimate the order of magnitude of this effect we repeat the mass fits for scales using different concentrations. Based on simulations, Duffy et al. (2008) find that the scatter around the median concentration is approximately lognormal with for relaxed clusters. Approximately matching the expected limits, fixed concentrations () change the best fit mass constraints for by () compared to the default analysis using the Diemer & Kravtsov (2015) mass-concentration relation which yields a concentration of at the best fitting mass. These variations are negligible compared to the statistical uncertainties of the study presented here. It should be noted that this analysis assumes spherical cluster models, which can lead to extra scatter due to triaxiality when comparing to X-ray results.

Figure 4: HST color image of Cl 120958.9+495352 based on the ACS/WFC F606W (blue) and WFC3/IR F105W (green), and F140W (red) imaging. The white contours indicate the signal-to-noise ratio of the weak lensing mass reconstruction, starting at in steps of , with the cross marking the peak position, which is consistent with the X-ray peak (red square) and BCG position (magenta star) within the uncertainty of 23 in each direction.
Figure 5: Tangential reduced shear profile (black solid circles) of Cl 120958.9+495352, measured around the X-ray peak. Here we combine the profiles of four magnitude bins between , as done in S16. The curve shows the corresponding best fitting NFW model prediction constrained by fitting the data within the range , assuming the mass-concentration relation from Diemer & Kravtsov (2015). The gray open circles indicate the reduced cross-shear component, which has been rotated by 45 degrees and constitutes a test for systematics. These points have been shifted by  Mpc for clarity.

In Fig. 4, the signal-to-noise ratio contours of the mass reconstruction appear to be slightly elliptical, extending towards the south-southwest, which is tentatively in agreement with the location of some apparent early-type cluster galaxies. To investigate whether this elliptical shape is actually significant, we estimate the shape of the mass peak using Source Extractor both for the actual mass reconstruction and the reconstructions originating from the bootstrap-resampled catalogs. Using the Source Extractor estimates of the semi-major and semi-minor axes and , as well as the position angle measured towards the north from west, we compute complex ellipticities with , as employed in weak lensing notation (e.g., Bartelmann & Schneider 2001). Using the dispersion of the estimates from the boostrapped samples as errors, our resulting estimate is consistent with a round mass distribution (). Hence, the apparent elliptical shape is not significant.

3.2 XMM-Newton results

Global cluster properties

The global properties for both methods of the treatment of the background are summarized in Tab. 2. The overall properties agree well between the two methods.

The rest-frame luminosity of the cluster in the  keV band is  erg/s and  erg/s, for background-modeling and background-subtraction method, respectively, estimated from the spectral fit. It is thus comparable to the most X-ray luminous MACS clusters, but at even higher redshift. These values are also in very good agreement with the findings by Buddendiek et al. (2015) after applying a K-correction.

background-modeling background-subtraction
[keV]
[]
norm

with being the angular diameter distance to the source.

Table 2: Global cluster properties between

Temperature and density

Figure 6: Deprojected and PSF-corrected temperature profile of Cl 120958.9+495352. Red (dark gray) solid diamonds show the deprojected (projected) result using the background-subtraction method. Blue (light gray) dashed diamonds corresponds to the background-modeling method.

We compare the results for the two approaches of the background treatment for temperature and density profile. Fig. 6 shows the temperature profile of Cl 120958.9+495352 for both approaches, and Tab. 3 gives the results.

background-modeling
[keV]
[]       
norm
background-subtraction
[keV]
[]       
norm

with being the angular diameter distance to the source.

Table 3: Fit results for the three radial bins for both methods of background treatment. The abundance is linked between all annuli.

Overall we see a very good agreement between the two different background methods. The temperature of the central bin is well constrained in both cases and both profiles show a good indication of a cool core. This makes Cl 120958.9+495352 one of only a few such objects known at high redshifts. The upper uncertainties in the outer two bins are large which is mainly related to the correlation between the parameters due to the PSF correction and the limited statistics. Even if no PSF correction is applied, the cool core remains and the uncertainty of the second temperature decreases by a factor of and of the outermost temperature by a factor of .

We determine the gas density profile using the PSF-corrected normalizations of the APEC model, which is defined as

(1)

where corresponds to the th annulus from the center and is the angular diameter distance to the source. The volume along the line of sight is the corresponding cylindrical cut through a sphere with inner and outer radii of the th annulus. We adopt . Due to the small extent of the cluster, there is only limited radial resolution. Therefore, we perform a simple deprojection method following Ettori et al. (2002).

The emission integral () and temperature () in ring are given by

(2)
(3)

with being the volume of the cylindrical cut corresponding to ring through spherical shell , and the electron and proton density, and the emissivity. By subtracting the contribution of the overlying shells in each annulus, we determine the deprojected electron density profiles for both background treatment methods shown in Fig. 7. As for the temperature, the two density profiles agree very well showing that our background treatment works well in both cases.

As an additional test for the background-subtraction method we choose an even larger inner radius of the background region () and repeat the analysis. We find only marginal differences and thus conclude that no significant cluster emission is present in the background-region.

Figure 7: Deprojected and PSF-corrected electron density profile of Cl 120958.9+495352. Red solid diamonds show the result using the background-subtraction method. Blue dashed diamonds correspond to the background-modeling method. The width of the diamonds corresponds to the radial bin size.

As can be seen in Fig. 1, we detect a point source close to the center of the cluster. To investigate the impact of the point source, we increase the exclusion radius around this source by 50% and repeat the fit. Due to the lowered statistics, the uncertainties clearly increase but we find no significant impact compared to the nominal values.

Gas mass fraction

From the gas mass profile and the total mass inside a given radius , the gas mass fraction can be obtained:

(4)

We note that, given the limited XMM-Newton spatial resolution, a very robust determination of the total mass from the hydrostatic equation is difficult as this would require high spatial resolution measurements of the density and temperature profile. Therefore, we use the total mass based on our weak lensing HST estimates and the corresponding (see Sec. 3.1). As a cross-check, we also determine the gas-mass fraction using the relation obtained by Hoekstra (2007) for the total mass.

The HST results yield . For the estimation of , we include an additional 30% triaxiality/projection uncertainty and a 10% uncertainty from the mass-concentration relation on . From 10000 Monte Carlo (MC) realizations of , we estimate and for each realization the gas mass within the corresponding , assuming a constant density in each shell. This yields  M and  M for the background-subtraction and background-modeling method, respectively, which are in very good agreement. Combining these results, we estimate for both methods. We note that through this procedure the given uncertainties on , , and are, on the one hand, correlated and, on the other hand, the assumption of constant density in each shell is only a rough approximation, which is why the uncertainty on is lower than naively expected. A more general estimate is obtained by using a beta-model for the density profile and following the same procedure as described above. We fix the core radius to a typical value of and assume a slope of (as also used in, e.g., Pacaud et al. 2016), but including 15% scatter on the latter. is estimated from our HST results. This yields for both background methods. Yet another approach is to estimate and its uncertainties at a fixed radius (i.e., assuming that the true is known), in which case the uncertainties on and are uncorrelated and directly propagate onto , which then yields . Here, we take the result using the beta-model as default.

Hoekstra (2007) estimated the relation for a galaxy cluster sample of 20 X-ray luminous objects at intermediate redshifts up to . They find a slope consistent with the one from Pratt et al. (2009), which is also used in the redshift evolution study of Reichert et al. (2011) and also consistent with the (inverted) slope of Maughan (2007) who assumed self-similar evolution. Using the relation from Hoekstra (2007) and assuming 30% intrinsic scatter, we find M for the background-subtraction method and M for the background-modeling method and (using the corresponding )  M and  M, respectively. This yields for both background methods, and is in very good agreement with our previous findings using the weak lensing mass.

3.3 Cooling time

To estimate the cooling time, we further reduced the size of the central region to corresponding to  kpc and performed the same PSF correction and deprojection method as described above. The cooling time is given by (Hudson et al. 2010)

(5)

where is the ion density and the cooling function. Within  kpc we find  cm and  keV. This yields a short cooling time for Cl 120958.9+495352 within  kpc of  Gyr for the background subtraction method and  Gyr for the background modeling method. Hudson et al. (2010) studied the cool cores for a local sample of 64 clusters within with Chandra. According to their findings, Cl 120958.9+495352 belongs to the weak cool core clusters; however, it should be taken into account that the radius, in which they determine the cooling time, is much smaller than what is possible for Cl 120958.9+495352 and, presumably, within this radius the cooling time would be even lower, possibly resulting in a strong cool core classification.

4 Discussion and conclusions

Our results show that Cl 120958.9+495352, according to Planck Collaboration et al. (2015), belongs to the most luminous galaxy clusters known at . Compared to the total mass estimate from Buddendiek et al. (2015) of , we find a slightly lower value from our weak lensing analysis of , which is, however, compatible within the uncertainties.

As discussed in, e.g., Sanderson et al. (2009) and Semler et al. (2012) there is a tight correlation between the dynamical state of the cluster and the presence and strength of a cool core. We find strong indications for the presence of a cool core, and the two different approaches for the background handling yield similar results which gives us confidence in our treatment of the background. The temperature profile shows a clear drop towards the center and the cooling time within  kpc is short with  Gyr and  Gyr for the background-subtraction and background-modeling method, respectively. Another indicator for the morphological state is the offset between the BCG and the X-ray emission peak (see, e.g., Rossetti et al. 2016, Mahdavi et al. 2013, Hudson et al. 2010). Rossetti et al. (2016) define a relaxed cluster by an offset smaller than . For Cl 120958.9+495352 the offset is about ( kpc) corresponding to (using the BCG position given in Buddendiek et al. 2015, see also Fig. 4), which is another indication for the relaxed nature of the system. Our HST weak lensing study also shows that the mass reconstruction peak is compatible with the BCG position and the X-ray peak within . As investigated in Sec. 3.1, the apparent elliptical shape of the lensing mass reconstruction is not significant. Hence, the results are consistent with a round mass distribution.

In a bottom-up scenario for structure formation, massive cool core systems should be extremely rare at high redshifts. Their gas mass fractions should not depend on the cosmological model. However, the apparent evolution varies for different assumed cosmologies. Previous measurements from Allen et al. (2008) and Mantz et al. (2014) show that their data are in good agreement with the standard cosmological model, showing a flat behavior of with redshift. However, these data only contain a few objects at very high redshifts. Therefore, clusters like Cl 120958.9+495352 are valuable objects for cosmology.

We obtain a gas mass fraction of , which is consistent with the result from Allen et al. (2008) for their full cluster sample and also consistent with the assumed CDM cosmology (, ). We performed several tests, i.e., we used an scaling relation for the total mass and tested the assumption of constant density in each shell, to verify this result and find very good agreement. Mantz et al. (2014) measured the gas mass fraction in an annulus from excluding the core of the clusters to minimize gas depletion uncertainties and intrinsic scatter in the inner part. They find typical values between and are thus consistent with our findings and Allen et al. (2008).

Reichert et al. (2011) studied the evolution of cluster scaling relations up to redshift . They use the relations from Pratt et al. (2009) for the local clusters and obtain a bias-corrected evolution factor. Testing this scaling relation with our estimated global gas temperature yields a luminosity that is about 40% smaller than our measured value. This result is, at least partially, expected due to the presence of a cool core. However, the uncertainties solely due to the uncertainties of the slope and normalization of the scaling relation (assuming they are uncorrelated) are already large (%).

The cluster Cl 120958.9+495352 is interesting not only with respect to cosmology, but also to its astrophysics. At redshift the time span for this massive object to form a cool core is very short. As XMM-Newton is not able to fully resolve the core structure, we aim for higher spatial resolution data in a future project to robustly determine the X-ray hydrostatic mass and to perform a detailed study of the core properties.

Acknowledgements.
This work is based on joint observations made with the NASA/ESA Hubble Space Telescope, using imaging data from program 13493 (PI: Schrabback) and XMM-Newton data (IDs 0722530101 and 0722530201), as well as WHT data (ID W14AN004, PI: Hoekstra). ST and TS acknowledge support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under projects 50 OR 1210, 50 OR 1308, 50 OR 1407, and 50 OR 1610. ST and THR acknowledge support by the German Research Association (DFG) through grant RE 1462/6 and the Transregio 33 “The Dark Universe” sub-project B18. ST also acknowledges support from the Bonn-Cologne Graduate School of Physics and Astronomy. LL acknowledges support from the Chandra X-ray Observatory grant GO3-14130B and from the Chandra X-ray Center through NASA contract NAS8-03060. Support for Program number GO-13493 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.

Footnotes

  1. institutetext: Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
    email: thoelken@astro.uni-bonn.de
  2. email: thoelken@astro.uni-bonn.de
  3. institutetext: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
  4. institutetext: Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305-4085, USA
  5. institutetext: Department of Physics, Stanford University, 452 Lomita Mall, Stanford, CA 94305-4085, USA
  6. institutetext: SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA
  7. institutetext: Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, the Netherlands
  8. institutetext: Kavli Institute for Cosmological Physics, University of Chicago, 5640 S Ellis Ave, Chicago, IL 60637
  9. institutetext: Cadmus, Energy Services Division, ​16 N. Carroll Street, Suite 900, Madison, WI 53703
  10. see heasarc.gsfc.nasa.gov/docs/xmm/abc/
  11. obtained with the HEASARC X-ray background tool heasarc.gsfc.nasa.gov/cgi-bin/Tools/xraybg/xraybg.pl
  12. cosmos.esa.int/web/xmm-newton/sas-thread-esasspec
  13. In the analysis of simulated data we find that the mass biases increase by factors of when changing from the default lower limit kpc from S16 to kpc as employed here. Following S16, we estimate the residual uncertainty of the bias correction as a relative factor of the bias value. Accordingly, the uncertainty increases by approximately a factor of two.
  14. This is necessary given that the analysis from S16 as a function of provides bias estimates for and only, as masses are not available for the simulations used to derive the bias values. We do propagate the statistical uncertainty of this extrapolation, but note that it is negligible compared to the statistical uncertainty of the mass constraints for Cl 120958.9+495352.

References

  1. Allen, S. W., Evrard, A. E., & Mantz, A. B. 2011, ARA&A, 49, 409
  2. Allen, S. W., Rapetti, D. A., Schmidt, R. W., et al. 2008, MNRAS, 383, 879
  3. Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481
  4. Babyk, I. 2014, Baltic Astronomy, 23, 93
  5. Bartelmann, M. & Schneider, P. 2001, Phys. Rep, 340, 291
  6. Bertin, E. & Arnouts, S. 1996, A&AS, 117, 393
  7. Bleem, L. E., Stalder, B., de Haan, T., et al. 2015, ApJS, 216, 27
  8. Buddendiek, A., Schrabback, T., Greer, C. H., et al. 2015, MNRAS, 450, 4248
  9. De Luca, A. & Molendi, S. 2004, A&A, 419, 837
  10. Diemer, B. & Kravtsov, A. V. 2015, ApJ, 799, 108
  11. Duffy, A. R., Schaye, J., Kay, S. T., & Dalla Vecchia, C. 2008, MNRAS, 390, L64
  12. Ebeling, H., Barrett, E., Donovan, D., et al. 2007, ApJ, 661, L33
  13. Ebeling, H., Edge, A. C., Mantz, A., et al. 2010, MNRAS, 407, 83
  14. Ehlert, S., Allen, S. W., von der Linden, A., et al. 2011, MNRAS, 411, 1641
  15. Erben, T., Schirmer, M., Dietrich, J. P., et al. 2005, Astronomische Nachrichten, 326, 432
  16. Erben, T., Van Waerbeke, L., Bertin, E., Mellier, Y., & Schneider, P. 2001, A&A, 366, 717
  17. Ettori, S., Fabian, A. C., Allen, S. W., & Johnstone, R. M. 2002, MNRAS, 331, 635
  18. Hoekstra, H. 2007, MNRAS, 379, 317
  19. Hoekstra, H., Bartelmann, M., Dahle, H., et al. 2013, Space Sci. Rev., 177, 75
  20. Hoekstra, H., Franx, M., Kuijken, K., & Squires, G. 1998, ApJ, 504, 636
  21. Hudson, D. S., Mittal, R., Reiprich, T. H., et al. 2010, A&A, 513, A37
  22. Kaiser, N., Squires, G., & Broadhurst, T. 1995, ApJ, 449, 460
  23. Koekemoer, A. M., Fruchter, A. S., Hook, R. N., & Hack, W. 2003, in HST Calibration Workshop : Hubble after the Installation of the ACS and the NICMOS Cooling System, ed. S. Arribas, A. Koekemoer, & B. Whitmore, 337
  24. Luppino, G. A. & Kaiser, N. 1997, ApJ, 475, 20
  25. Mahdavi, A., Hoekstra, H., Babul, A., et al. 2013, ApJ, 767, 116
  26. Mantz, A. B., Allen, S. W., Morris, R. G., et al. 2014, MNRAS, 440, 2077
  27. Massey, R., Schrabback, T., Cordes, O., et al. 2014, MNRAS, 439, 887
  28. Maughan, B. J. 2007, ApJ, 668, 772
  29. Maughan, B. J., Jones, L. R., Ebeling, H., & Scharf, C. 2004a, MNRAS, 351, 1193
  30. Maughan, B. J., Jones, L. R., Lumb, D., Ebeling, H., & Gondoin, P. 2004b, MNRAS, 354, 1
  31. McDonald, M., Allen, S. W., Bayliss, M., et al. 2017, ArXiv e-prints
  32. McInnes, R. N., Menanteau, F., Heavens, A. F., et al. 2009, MNRAS, 399, L84
  33. Menanteau, F., Hughes, J. P., Sifón, C., et al. 2012, ApJ, 748, 7
  34. Pacaud, F., Clerc, N., Giles, P. A., et al. 2016, A&A, 592, A2
  35. Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2015, A&A, 581, A14
  36. Pratt, G. W., Croston, J. H., Arnaud, M., & Böhringer, H. 2009, A&A, 498, 361
  37. Reichert, A., Böhringer, H., Fassbender, R., & Mühlegger, M. 2011, A&A, 535, A4
  38. Rossetti, M., Gastaldello, F., Ferioli, G., et al. 2016, MNRAS, 457, 4515
  39. Sanderson, A. J. R., Edge, A. C., & Smith, G. P. 2009, MNRAS, 398, 1698
  40. Schirmer, M. 2013, ApJS, 209, 21
  41. Schneider, P. 2006, in: Gravitational Lensing: Strong, Weak & Micro, Saas-Fee Advanced Course 33, Swiss Society for Astrophysics and Astronomy, G. Meylan, P. Jetzer & P. North (Eds.), Springer-Verlag: Berlin, p. 269
  42. Schrabback, T., Applegate, D., Dietrich, J. P., et al. 2016, MNRAS  submitted
  43. Schrabback, T., Erben, T., Simon, P., et al. 2007, A&A, 468, 823
  44. Schrabback, T., Hartlap, J., Joachimi, B., et al. 2010, A&A, 516, A63
  45. Schrabback, T., Hilbert, S., Hoekstra, H., et al. 2015, MNRAS, 454, 1432
  46. SDSS Collaboration, Albareti, F. D., Allende Prieto, C., et al. 2016, ApJS submitted (also arXiv:1608.02013)
  47. Semler, D. R., Šuhada, R., Aird, K. A., et al. 2012, ApJ, 761, 183
  48. Siemiginowska, A., Burke, D. J., Aldcroft, T. L., et al. 2010, ApJ, 722, 102
  49. Simon, P., Taylor, A. N., & Hartlap, J. 2009, MNRAS, 399, 48
  50. Skelton, R. E., Whitaker, K. E., Momcheva, I. G., et al. 2014, ApJS, 214, 24
  51. White, S. D. M., Navarro, J. F., Evrard, A. E., & Frenk, C. S. 1993, Nature, 366, 429
  52. Willingale, R., Starling, R. L. C., Beardmore, A. P., Tanvir, N. R., & O’Brien, P. T. 2013, MNRAS, 431, 394
  53. Wright, C. O. & Brainerd, T. G. 2000, ApJ, 534, 34
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minumum 40 characters
   
Add comment
Cancel
Loading ...
104396
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description