1 Introduction

Combined high-resolution X-ray and radio observational studies of gas-rich cool-core clusters have provided us with ample evidence regarding the impact of energy released by the central active galactic nucleus (AGN) on the surrounding intracluster medium (ICM) (see reviews, Fabian 2012; Gitti et al. 2012; McNamara & Nulsen 2012). These evidences have been witnessed in the form of giant cavities, shocks in the X-ray surface brightness, and their coincidence with the radio plasma lobes (Rafferty et al. 2006; Bîrzan et al. 2008; Dunn et al. 2010; Chon et al. 2012; Canning et al. 2013). The close association of the X-ray cavities with the radio lobes in several cool core clusters implies that radio bubbles inflated by the jets from central AGN displaces hot gas in its vicinity and carve cavities or depressions in the X-ray surface brightness (Fabian et al. 2006; Wilson et al. 2006; David et al. 2009; Vagshette et al. 2016, 2017; Pandge et al. 2019).

The superb angular resolution capabilities of Chandra X-ray telescope have also enabled us to perform a detailed study of previously unseen edges in the hot gas environment, commonly known as shocks and cold fronts. These edges exhibit sharp discontinuities in the surface brightness (SB) and temperature profiles (Markevitch et al. 2002; Markevitch & Vikhlinin 2007). Although shocks mark pressure discontinuities, the pressure profile remains almost continuous across the edge due to a cold front and have been observed in several other cluster environments (e.g., Owers et al. 2009; Ghizzardi et al. 2010; de Plaa et al. 2010; Ettori et al. 2013; Gastaldello et al. 2013; Andrade-Santos et al. 2016) of both, relaxed and merging. The origin of the cold fronts in relaxed clusters is likely related to gas sloshing induced by off-axis minor mergers (Ascasibar & Markevitch 2006; Roediger et al. 2011), while that in the merging clusters is due to the merger of a gas-rich system easily discernible in the plane of the sky (Markevitch et al. 2001; Mathis et al. 2005; Markevitch & Vikhlinin 2007; Owers et al. 2011; Ogrean et al. 2013; Pandge et al. 2017; Botteon et al. 2018). Therefore, cold front study provides us with a crucial probe for the ICM dynamics (Zuhone & Roediger 2016).

This paper presents a combined study of 30 ks Chandra X-ray data and 46.8 ks, 1.4 GHz GMRT radio data on the cool-core cluster RXCJ0352.9\(+\)1941 aimed at investigating evidence and energetics of the AGN outbursts operative in the core of this cluster. RXCJ0352.9\(+\)1941 is reported to host a centrally concentrated H\(\alpha \) emitting gas pointing towards its quiescent undisturbed state (Hamer et al. 2016) with the H\(\alpha \) based star formation rate equal to 12.6 \(M_{\odot }\) yr\(^{-1}\) (Pulido et al. 2018). A radio source of relatively flat spectrum was reported to coincide with the core of this cluster, with its C and X band unresolved radio emission exhibiting a small Giga-Hertz Peaked Source (GPS) like structure and a one-sided tail (Hogan et al. 2015). A recent X-ray study of this cluster has reported the detection of a pair of cavities (Shin et al. 2016). However, their role in the AGN feedback and association with radio emission remained unexplored. This paper is structured as Section 2 describes a detailed analysis of the Chandra and GMRT data on this cluster. The results derived from the morphological and spectral analysis of the X-ray emission are presented in Section 3, while Section 4 discusses the results and effectiveness of the AGN feedback. Finally, we summarize our important findings in Section 5.

Throughout the paper, we adopt cosmological parameters \(H_0 = 70\) km s\(^{-1}\) Mpc\(^{-1}\), \(\Omega _m = 0.27\) and \(\Omega _{\Lambda } = 0.73\); translating to a scale of 1.98 kpc arcsec\(^{-1}\) at the redshift \(z = 0.109\) of RXCJ0352.9\(+\)1941. All quoted errors for spectral analysis stand for the 90% confidence level unless otherwise stated. Metallicities were measured relative to the solar metallicity table of Grevesse & Sauval (1998).

Fig. 1
figure 1

Left panel: Exposure corrected blank sky background subtracted 0.5–3.0 keV \(2.0 \times 2.0\) arcmin\(^2\) Chandra image of RXCJ0352.9\(+\)1941. The image was convolved with a 2D Gaussian kernel of 1 pixel \(=\) 0.492 arcsec for better visibility. Green arrows on the north and south represent substructures. The white central spot represents the hard X-ray point source (AGN). A magnified view of the central region is shown in the inset. The cyan ellipse presents the extended X-ray emission from the cluster. Right panel: GGM filtered image of RXCJ0352.9\(+\)1941 on a scale of 3\(\sigma \). The edge in the surface brightness is indicated by the white arrows. Yellow arrows in this figure delineate the north substructure in the X-ray emission.

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2 Observations and data reduction

2.1 Chandra X-ray data

RXCJ0352.9\(+\)1941 was observed on 18 December 2008 by Chandra X-ray observatory (OBSID 10466) for an effective exposure of 30 ks (Table 1) in VFAINT mode with the object focused on the back-illuminated CCD ACIS-S3. Level-1 event file on this target was retrieved from the Chandra Data Archive (CDA). It was reprocessed using chandra_repro routine of Chandra Interactive Analysis of Observations (CIAO; Fruscione et al. 2006) version 4.12 and calibration files CALDB (version 4.9.5). High background flares from the light curve were identified and removed from the event file using the 3\(\sigma \) clipping method in the lc_sigma_clip task, which yielded a net exposure time of 27.20 ks. System-supplied background files corresponding to the observations were identified from the blank-sky frames using acis_bkgrnd_lookup task, which were re-projected to match the observation pointing, roll angle, and were normalized to match the 10–12 keV count rates in the science frame (Hickox & Markevitch 2006). The CIAO tool wavdetect was used to identify point sources within the cluster environment, then confirmed by visual inspection; except for central, all other point sources were removed from the further analysis. The holes due to the removal of the sources were filled in with the background emission employing the dmfilth tool. For details on X-ray data analysis, readers are referred to Sonkamble et al. (2015).

Table 1 Chandra observation log.
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2.2 GMRT radio data

To examine the spatial correspondence between the X-ray deficiencies and the radio emission from the source associated with the cluster, we observed RXCJ0352.9\(+\)1941 at 1420 MHz using GMRT (Swarup et al. 1991). The observations were carried out with 32-MHz bandwidth divided into 512 channels during two observing runs on 22 and 23 October 2016 for a total of 13 h (46.8 ks, Project Code 31_048). The data were recorded in the LL and RR polarization with an integration time per visibility during both observing runs equal to 16 s. Standard sources 3C 147 and 0431\(+\)206 were also observed during these flux and phase calibration runs, respectively. The GMRT data were analyzed using the NRAO Astronomical Image Processing Software (AIPS) semi-automated pipeline-based radio-reduction package for flagging and calibration purposes. After applying the band-pass calibration, the data were averaged using the SPLAT task with care that no bandwidth smearing was happening. The data on the target were then split out using the task SPLIT and were imaged with the task IMAGR and weight parameter robust \(=\) 0. Then, amplitude and phase self-calibration were performed after three rounds of phase-only self-calibration. The image faceting was used to correct the data for the ‘w’ term errors, which were then stitched together using the AIPS task FLATN. Finally, the image was corrected for the primary beam response using the AIPS task PBCOR to achieve the rms noise level of 0.05 mJy beam\(^{-1}\).

3 Results

3.1 X-ray imaging

Figure 1 (left panel) displays an adaptively smoothed, background-subtracted, and exposure-corrected 0.5–3.0 keV Chandra image of RXCJ0352.9\(+\)1941. The image was convolved with a 2D Gaussian kernel of 1 pixel \(=\) 0.492 arcsec for better representation. At the center of the cluster, we find a bright X-ray point source (\(\alpha = 03^\textrm{h}52^\textrm{m}59''05\), \(\delta =+19^{\circ }40'59''68\)), which is surrounded by an extended X-ray emission of diameter \(\sim \)40 arcsec (\(\sim \)80 kpc) shown by the cyan ellipse. In the magnified view of the central region shown in the inset, we see hints of X-ray deficit regions along the SE and NW directions of the X-ray peak. In addition to this, we also find spiral-like emission substructures on the north and the south marked by green arrows. These spiral-like emission substructures suggest that the gas in this system is in a state of sloshing like that evident in several other clusters, such as MACS J0416.1−2403 (Ogrean et al. 2015), MACS J1149.6\(+\)2223 (Ogrean et al. 2016), MACS J0717.5\(+\)3745 (van Weeren et al. 2016) and MACS J0553.4−3342 (Pandge et al. 2017).

Fig. 2
figure 2

Left panel: 0.5–3.0 keV unsharp masked image constructed by subtracting a 10-pixel Gaussian smoothed image from that smoothed with 2 pixels. Green ellipses highlight X-ray deficit cavities. Notice the excess emission substructures evident in this image. Right panel: 0.5–3.0 keV 2D double \(\beta \)-model subtracted residual map of RXCJ0352.9\(+\)1941. Green ellipses show cavities on the SE and NW of the X-ray center. Black arrows indicate regions of substructures in the form of excess X-ray emission.

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With a spiral structure, there is a great possibility of finding edges within the cluster. To reveal this, we constructed a Gaussian Gradient Magnitude (GGM) filtered image of RXCJ0352.9\(+\)1941 following Sanders et al. (2016). GGM determines the magnitude of surface brightness gradients using Gaussian derivatives. To produce the GGM-filtered image, we used the background-subtracted, exposure-corrected 0.5–3.0 keV Chandra image yielding the \(\sigma = 3\) arcsec Gaussian width smoothed image of the magnitude of surface brightness gradient (Sanders et al. 2016). The resultant GGM image is shown in Figure 1 (right panel), which delineates the signatures of disturbed ICM. This image reveals a substructure in the north (yellow arrows) and is consistent with those evident in Figure 1 (left panel). The white arrows highlight the presence of the edge in the bright surface.

To better visualize the substructures in the surface brightness distribution of this cluster, we have constructed a 0.5–3.0 keV unsharp masked image as discussed in Pandge et al. (2013). This was achieved by subtracting a wider 10-pixel Gaussian smoothed image from that smoothed with a 2-pixel Gaussian. The resultant unsharp mask image is shown in the left panel of Figure 2, which delineates two X-ray deficit cavities (NW and SE) and excess emission in the north and south directions.

Fig. 3
figure 3

Left panel: A 2D double \(\beta \)-model subtracted residual image overlaid with 20 different segments used to study the variation of counts at the cavity locations. Right panel: X-ray count variations are plotted. Notice the dip in counts compared to the mean value shown by a horizontal line.

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We also obtain a 2D smooth model subtracted residual map (Figure 2, right panel) of the cluster emission. In the present case, as the background subtracted, exposure corrected image (Figure 1, left panel) and unsharp mask images revealed asymmetries in the X-ray surface brightness, which means a single 2D \(\beta \)-model would not be suitable, therefore, to obtain its smooth model we fitted the X-ray emission with a double 2D \(\beta \)-model like used by Ichinohe et al. (2015). This was achieved by combining beta2d \(+\) beta2d models within Sherpa (Freeman et al. 2001) with Cash statistics. The resultant residual map (Figure 2, right panel) showed several interesting features in the central region of RXCJ0352.9\(+\)1941, including a pair of X-ray cavities (NW and SE, green ellipses). The size of the cavity is typically determined by visual inspection of X-ray images, such as unsharp mask, beta model subtracted residual image, and surface brightness profile (Doria et al. 2012). This method relies on the quality of the X-ray data and is susceptible to systematic errors. Discrepancies in cavity size and shape reported by different authors can vary significantly based on the approach adopted, leading to differences in the measurements (e.g., Gitti et al. 2010; O’Sullivan et al. 2011; Doria et al. 2012). Here, we measured cavity sizes from the residual image (\(8.54 \times 6.56\) kpc for NW cavity and \(8.22 \times 5.68\) kpc for SE cavity) and are comparable to what was reported by Shin et al. (2016), with an error margin of about 20%. We also found two additional substructures exhibiting excess emission (highlighted by green arrows) on the north and south of the X-ray center, as evident in Figure 1 (left panel). The substructure on the south appears to be more extended than that on the north.

We also conducted an X-ray count rate variation study to verify the significance of the X-ray surface brightness depressions. We extracted counts from 20 identical segments within annular regions ranging from 2 to 12 arcsec from a background subtracted image in the 0.5–3.0 keV range. It should be noted that the \(\beta \)-model subtracted image in Figure 3 (left panel) is only for better visualization of depressions. The count rate plot in the right panel reveals a decrease in segments 1–7 and 9–13 due to the NW and SE depressions, respectively. These depressions are usually referred to as X-ray cavities. While the residual image shows some additional depression at the position of segments 13 and 14, the count variation does not show signs of an X-ray depression in those sectors. Therefore, this is most likely not a real feature but an artifact caused by the over-subtraction of the model. Similarly, the complex central region of the cluster and its heavier smoothing may also contribute to generating such artifacts in the image. Such artifacts have been reported in O’Sullivan et al. (2012).

3.2 X-ray surface brightness profiles

To examine the overall morphology of the ICM in this cluster environment, we calculated the azimuthally averaged surface brightness profile of the X-ray emission. This was done by extracting counts from concentric circular annuli centered on the X-ray peak of the background and subtracting \(0.5-3.0\) keV Chandra image of this cluster. The extracted surface brightness was then fitted with the standard \(\beta \)-model (Cavaliere & Fusco-Femiano 1976) using Sherpa beta1d task (Freeman et al. 2001), which resulted in \(r_c \sim 10.12\pm 0.22\) arcsec and \(\beta \sim 0.54\pm 0.002\). The best fit azimuthally averaged (0–360\(^{\circ }\)) surface brightness profile is shown in Figure 4 (left panel, dark continuous line), while the data points are shown in dark filled circles. As the central emission could be dramatically different in different systems, the best-fit parameters may not be consistent with those in other groups and clusters. To further examine any discontinuities in the surface brightness, we also derive such profiles for the emission extracted from three different wedge-shaped sectorial regions, which are shown in the same figure. Here, the profile for sector I (covering 170–220\(^{\circ }\)) is shown by a green continuous line with data points in green open triangles, sector II (275–350\(^{\circ }\)) magenta line and stars, and sector III (350–100\(^{\circ }\)) shown with the blue line and data with blue down-triangles. All angles are measured in the counter-clockwise direction. We add arbitrary offsets in the abscissa to visualize better for these profiles. The profiles along sectors I and III show small deficits at about 10.5 arcsec (20.80 kpc) and 5.20 arcsec (10.30 kpc), respectively, with significance ranging from 3\(\sigma \) to 5\(\sigma \) as seen from the bottom of Figure 4 (left panel). Profiles along sector II and sector III exhibit excess emission between a radius of 20\(''\) to 40\(''\), probably due to the brighter extended emission and spiral substructure on the north and south. That was observed in Figures 1 and 2 with a significance between 4\(\sigma \) to 5\(\sigma \). Sector II profile also exhibits an edge (discontinuity) in the surface brightness at about 31 arcsec.

Fig. 4
figure 4

Left panel: 0.5–3.0 keV azimuthally averaged X-ray surface brightness along with the best-fit 1D \(\beta \)-model (black filled circles and black solid line). In the same figure, we also plot the surface brightness profiles extracted from the wedge-shaped sectors I, II, and III, respectively, covering 170–220\(^{\circ }\), 275–350\(^{\circ }\), and 350–100\(^{\circ }\). We add arbitrary offsets in the abscissa to better visualize these profiles. The continuous lines in these profiles show best fit \(\beta \)-models. Deviations among the data points relative to the best-fit \(\beta \) model are shown in the bottom panel. Right panel: The surface brightness along sector II fitted with a broken power-law density model (solid blue line). The corresponding 3D gas density model is shown in the inset, while the lower panel shows residuals of the fit.

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The discontinuity in the surface brightness distribution along sector II was further explored and its geometry was modeled. The center and shape of the discontinuity were considered as evident in the GGM image shown by white arrows (Figure 1, right panel). We then extracted the surface brightness profile of the X-ray photons along sector II, which were divided into appropriate bins. These extractions were then fitted with the deprojected broken power-law density model within PROFFIT V 1.4.Footnote 1 This was found to be an effective tool for investigating discontinuity in the surface brightness (Eckert et al. 2011, 2012) and has been used in literature for several systems (Storm et al. 2018; Parekh et al. 2020; Bruno et al. 2021). This broken power-law model is defined as:

$$\begin{aligned} n(r) =\left\{ \begin{array}{ll} Cn_{\textrm{0}} \left( \frac{r}{r_{\textrm{jump}}}\right) ^{-\alpha 1}, &{} \text {if } r \le r_{\textrm{jump}}, \\ n_{\textrm{0}} \left( \frac{r}{r_{\textrm{jump}}}\right) ^{-\alpha 2}, &{} \text {if } r > r_{\textrm{jump}},\\ \end{array}\right. \end{aligned}$$
(1)

where n(r) represents the electron density at the projected distance r, \(n_0\) the density normalization, \(C = n_{\textrm{e}_2}/n_{\textrm{e}_1}\) represents the compression factor at the discontinuity, \(\alpha \)1 and \(\alpha \)2 the power-law indices on either side of the discontinuity, and \(r_\textrm{jump}\) the radius corresponding to the putative discontinuity or jump.

The surface brightness extraction and the best-fit broken power law are shown in Figure 4 (right panel). This analysis reveals a break at around 31 arcsec (62 kpc). To ensure this discontinuity is not an artifact we tried several extraction ranges by varying the angular widths as well as the radial bin sizes as suggested by Canning et al. (2017). Additionally, the task PROFFIT itself ensures proper detection of discontinuity in the selected area. The resultant best-fit analysis, within statistical limits, yielded the power-law indices across the discontinuity as \(\alpha 1 = 0.95\pm 0.02\) and \(\alpha 2 = 1.66\pm 0.04\), while the density jump factor as \(1.37\pm 0.05\) (Table 2). The discontinuity radius obtained from the fit is \(r_\textrm{jump} = 0.51\pm 0.009\) arcmin. We also tried to check discontinuities in other directions of the cluster emission; however, lower statistics in the present Chandra image failed to find those.

Table 2 Cold front and broken power-law properties.
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3.3 Spectral analysis of the ICM emission

3.3.1 Radial profiles of thermodynamical parameters

To investigate the radial dependence of the ICM properties, we computed azimuthally averaged projected profiles of thermodynamic parameters, such as ICM temperature, metallicity, and pressure. For this, we extracted 0.5–8.0 keV spectra from 9 different concentric annuli centered on the X-ray peak of RXCJ0352.9\(+\)1941, using task specextract within CIAO. The weighted redistribution matrix file (RMF) and weighted auxiliary response file (ARF) were derived for each extractions. The widths of the annuli were set so that each region had a minimum of \(\sim \)2000 background-subtracted counts, binned with a minimum of 25 counts per bin. Spectra from each of the annulus were then fitted individually using XSPEC version 12.12.0 (Arnaud 1996) with an absorbed single temperature thermal model (tbabs \(\times \) apec) (Smith et al. 2001; Foster et al. 2012). The Galactic hydrogen column density was fixed at \(N_\textrm{H} = 1.37\times 10^{21}\) cm\(^{-2}\) (Dickey & Lockman 1990), while the redshift was fixed at \(z=0.109\). The resultant best-fit parameters, such as temperature and metallicity, were estimated from constrained spectra.

We then compute the electron density \(n_\textrm{e}\) (cm\(^{-3}\)) using apec normalization and the expression provided in Alvarez et al. (2022):

$$\begin{aligned} n_{\textrm{e}} =&\, \biggl [1.2 N \times 4.07\times 10^{-10}(1+z)^2 \nonumber \\&\times \biggl (\frac{D_A}{\textrm{Mpc}}\biggl )^2\biggl (\frac{V}{\mathrm{Mpc^3}}\biggl )^{-1}\biggl ]^{1/2}, \end{aligned}$$
(2)

where \(D_A\) the angular diameter distance, V the volume of the spherical shell used for extraction, N the apec normalization in XSPEC, and z the redshift of the object. We assume the ratio of electron to hydrogen density (\(n_\textrm{e}/n_\textrm{H}\)) equal to 1.2 (Boehringer & Hensler 1989) and compute the pressure and entropy of the gas within each annulus using \(p = nkT\) and \(S = kT n_\textrm{e}^{-2/3}\), where \(n = 1.92 n_\textrm{e}\) for an ideal gas.

Fig. 5
figure 5

Azimuthally averaged projected profiles (green open diamonds) of temperature (upper), metallicity (middle), and pressure (lower) plotted as a function of radial distance. We also plot the projected (red-filled circles) and the deprojected profiles (blue crosses) for the extraction along sector II. The vertical blue dashed line indicates the position of the discontinuity.

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The resultant azimuthally averaged projected profiles of temperature (upper), metallicity (middle), and pressure (lower) as a function of radial distance are shown by green diamonds in Figure 5. Like several other cool-core clusters, the temperature profile (upper panel) of RXCJ0352.9\(+\)1941 takes a minimum value in the core, which then increases in the radially outer part (David et al. 2009; Sun et al. 2009; Pandge et al. 2012, 2013; Sonkamble et al. 2015). This profile also exhibits a discontinuity in temperature at \(\sim \)31 arcsec (vertical dashed line). It was noticed that there was a slight inconsistency in the pressure profile, as illustrated in the lower panel.

To understand the nature of plasma parameters along the wedge-shaped sector II, we also extract spectra from 9 different sectorial regions, which are shown by red-filled circles in the same figure. Temperature and pressure profiles of azimuthally averaged and sectorial plots show similar features across the edge. This sectorial plot also shows a jump from \(2.27\pm 0.1\) keV to \(3.24\pm 0.2\) keV in the temperature and a marginal jump in the metallicity at \(\sim \)31 arcsec. A marginal discontinuity in the pressure profile (lower panel) is also evident at this location. However, such changes in the pressure profiles at the location of discontinuity have also been reported in some other systems, e.g., PKS0745−191 (Sanders et al. 2014), A2052 (Blanton et al. 2011), Virgo (Forman et al. 2007), and Perseus (Fabian et al. 2003) and may represent a weak shock associated with the AGN feedback. To confirm that the jump in pressure is not due to the projection effect of the brightness distribution, we applied the following deprojection technique. This was done by deriving the three-dimensional structure of the ICM using deprojectFootnote 2 tool and following the ‘onion peeling’ method presented by Blanton et al. (2003). This method removes the contamination from the external layers of ICM. Here, we obtained the deprojected temperature profile by extracting X-ray photons from 6 different annuli along the wedge-shaped sector II. The widths of the annuli were adjusted to achieve the best S/N. Here, we first fit the X-ray spectrum extracted from the outermost shell with an absorbed apec model to obtain the temperature, abundance and normalization parameters. We then removed the contribution from the outer layer from the successive shells to obtain parameters of the inner shell by adding another apec component. This resulted in very few counts, forcing us to increase the bin size to reach the required statistics. We repeated this procedure until we reached the center of the cluster. The resultant profile of the deprojected values of ICM temperature is shown in Figure 5 by a blue cross. Even in the deprojection, the temperature and metallicity profiles follow the same projected trend. Here, a sharp temperature jump of \(1.44\pm 0.53\) keV from \(2.01\pm 0.19\) to \(3.45\pm 0.50\) keV is evident at about 31 arcsec. The pressure profile in the deprojection analysis, unlike in the projected case, remains continuous across the edge. Thus, a jump in the temperature with constant pressure across the edge confirms its association with a cold front and is discussed separately in Section 4.4.

Fig. 6
figure 6

2D temperature (left panel) and metallicity (right panel) maps of the ICM obtained from contour binning technique. The GMRT 1.4 GHz radio contours are overlaid on both images with levels of \(2,8,32,128\times \sigma \). The rms noise is \(\sigma =0.05\) mJy beam\(^{-1}\), and the resolution is \(2.6\times 2.0\) arcsec.

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3.3.2 2D temperature and metallicity maps

To better understand the 2D spatial variations of temperature and metallicity distribution of ICM in RXCJ0352.9\(+\)1941 environment, we have computed its 2D maps. We used the contour binning technique (CONTBIN) of Sanders (2006). This technique identifies the brightest pixels in the point sources removed X-ray image and generates a spatial bin of all such pixels that have the same brightness, which then grows pixel by pixel until it reaches the expected S/N (\(\approx \)40 with 1600 net counts). We used the geometric constrain factor of \(C = 2\) to avoid the formation of elongated bins. The 0.5–3.0 keV Chandra image was analyzed, and 21 bins were successfully identified. The spectra extracted from each bin were fitted independently, adopting \(\chi ^2\) minimization. The derived values of temperature and metallicity were then used to plot their 2D maps and are shown in Figure 6. The typical errors on the temperature map vary from 5% in the central region to 13% in the outskirts, while those in the metallicity map vary from 20% to 35%, respectively.

The temperature map reveals two arc-shaped regions in the north-east at 50 arcsec (100 kpc) and 114 arcsec (226 kpc) exhibiting the highest value of ICM temperature relative to the ambient gas and are measured to be \(4.25\pm 0.33\) keV and \(4.87\pm 0.61\) keV, respectively. It is believed that such arc-shaped patterns in the ICM distribution are the manifestations of the angular momentum of the ICM (Tittley & Henriksen 2005; Ascasibar & Markevitch 2006; ZuHone et al. 2011; Vazza et al. 2012). The temperature map clearly reveals that the coolest gas is segregated in the central region of the cluster, implying that the system has a cool core. It is also evident that the cooler, lower entropy gas has elliptical morphology orientated along the northeast to southwest, as noticed in Section 3.1. To check the association of the X-ray emitting gas with radio emission, we overlay 1.4 GHz GMRT radio contours on the temperature map, which confirms its spatial association with the X-ray gas envelope. The low entropy structures in the central region are likely due to the expanding X-ray cavities in the core region. These might have uplifted the low entropy gas or have triggered its condensation (see, McNamara et al. 2016; Gendron-Marsolais et al. 2017; Tremblay et al. 2018). The metallicity map (Figure 6, right panel) also reveals arc-shaped morphology of high metallicity gas of \(0.68\pm 0.26\) \(Z_{\odot }\) at 50 arcsec along the eastern direction. This map also reveals asymmetry in the metallicity of gas distributed along the north-east and the south-west directions. These asymmetries, in turn, suggest that the metallicity mixing due to sloshing is slow and implies that the disturbances caused by the passage of sub-cluster and/or cold fronts are not enough to reach the uniform metallicity mixing. This agrees with the findings of Ghizzardi et al. (2014) for the Abell 496 cluster.

3.3.3 Nuclear point source emission

Chandra image of RXCJ0352.9\(+\)1941 exhibits a prominent central X-ray source (\(\alpha _\mathrm{J2000.0}=03^\textrm{h} 52^\textrm{m} 59''005 \), \(\delta _\mathrm{J2000.0}=+19^{\circ } 40' 59''68\)) coinciding with the radio core of the AGN. To understand the emission characteristics of the central source we first find out its spectral hardness \((\textrm{HR}) = (\textrm{H} - \textrm{S})/(\textrm{H} + \textrm{S})\), where S and H, respectively, represent the X-ray counts in Soft (0.5–2 keV) and Hard (2–8 keV) bands extracted from the central 2 arcsec region centered on the X-ray peak (Wang et al. 2004). We also estimate the hardness of the surroundings by extracting counts from a circular annulus of width 2 arcsec surrounding the central source. This analysis yielded hardness values of \(-\) \(0.24 \pm 0.04\) and \({-}0.40 \pm 0.02\), respectively, for the central source and the environment. This clearly indicates that the central source is significantly dense than its surroundings, providing strong evidence for the association of AGN with RXCJ 0352.9\(+\)1941.

For a better understanding of the spectral nature of the central source of this cluster, we also perform spectral fitting of the 0.5–8.0 keV X-ray photons from the same central 2 arcsec region. This could produce a total of 560 background-subtracted counts, which were then imported to the XSPEC and fitted with a combined thermal apec and a power-law component. The power law was included to account for the emission from the central hard source, as evidenced above. This analysis yielded the best fit temperature value of 1.30\(^{+0.30}_{-0.27}\) keV for the ICM metallicity fixed at \(Z = 0.35\) \(Z_{\odot }\), while the power-law yielded best-fit photon index of \(\Gamma = 0.72\) (Table 3). This, in turn, confirms that the central source associated with the cluster is hard enough to deliver (2–10 keV) X-ray luminosity of \(L_{X} = 9.66\times 10^{42}\) erg s\(^{-1}\) mainly originating from the non-thermal means.

Table 3 Spectral properties of the nuclear emission.
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3.4 Radio emission features

As reported in Green et al. (2016), RXCJ0352.9\(+\)1941 cluster hosts a brightest cluster galaxy (BCG). The LoFAR telescope detected a radio-loud AGN associated with the central BCG at 144 MHz (Bîrzan et al. 2020). Additionally, we detect extended radio jet-like diffuse emissions at GMRT 1.4 GHz. To visualize the emission, we overlayed 1.4 GHz GMRT radio contours on the Pan-STARRS1 ‘r’ band image of this cluster (Figure 7). This GMRT image is produced with CASA robust parameter \(=\) 0. The final image has an rms of about 50 \(\mu \)Jy beam\(^{-1}\) with a beam of \(2.6''\times 2.0''\) and a position angle of 71.8\(^\circ \). The 1.4 GHz contours reveal a strong core with a flux density of 13.7 mJy that co-insides with the central BCG. The radio map also shows the AGN outflow of non-thermal particles in the form of diffuse radio jet-like emission. The longest radio jet (marked as secondary jet or ‘sj’ in Figure 7) appears to be extended up to 20 arcsec  (40 kpc) towards the northeast direction, along the major axis of the BCG. Although an inner pair of jet-like emissions (marked as primary jet or ‘pj’ and ‘pj\('\)’ in Figure 7) along the minor axis of the BCG is also apparent, there is no clear evidence of the counter jet for ‘sj’ along the south-west. Even though a couple of isolated radio sources, possibly due to the counter lobe, are found towards ‘sj\('\)’, it cannot be confirmed due to the low fidelity of these sources, as they may also be artifacts. Nevertheless, we compute and report here the total radio emission flux density of the AGN and jets within \(3\sigma \) contour as \(S_{1.4}=20.8\pm 2.1\) mJy at 1.4 GHz.

Fig. 7
figure 7

GMRT 1.4 GHz radio contours at 2.5, 10, 40, 160 \(\times \sigma \) overlaid on the Pan-STARRS1 ‘r’ band image.

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4 Discussion

4.1 X-ray cavities as calorimeters

The 2D \(\beta \)-model subtracted residual map and unsharp mask image revealed a pair of X-ray cavities in the central region of RXCJ0352.9\(+\)1941, one on the NW and the SE of its X-ray center (Figure 2). Detection of a pair of X-ray cavities in the environment of this cluster was also reported by Shin et al. (2016). Assuming that such cavities manifest AGN outbursts, Rafferty et al. (2006) have used such cavities as calorimeters and quantified the mechanical energy injected by the radio jets into the ICM. Like Shin et al. (2016), we assume the ellipsoidal shape of the X-ray cavities carved by the radio jets originating from the central AGN. The radio lobes of the AGN displace hot gas carving bubbles or cavities by doing pV work during their outbursts. These cavities then rise buoyantly in the wake of the ICM until they reach pressure equilibrium. At the equilibrium, the buoyant velocity of the cavities exceeds the expansion velocity, and they get detached from the jets, hence delivering their enthalpy to the ICM. Assuming that the cavities are filled with relativistic plasma, we compute the total enthalpy content of each of the cavities as \(E_\textrm{cav} = 4pV\) (Bîrzan et al. 2004). Here, p is the pressure of the surrounding ICM and V is the volume of each cavity. Then, the cavity power was estimated as follows:

$$\begin{aligned} P_\textrm{cav} = \frac{E_\textrm{cav}}{t_\textrm{cav}} = \frac{4pV}{t_\textrm{cav}}, \end{aligned}$$
(3)
Table 4 Cavity energetics.
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where \(t_\textrm{cav}\) represented the age of the cavity and was estimated using the buoyant rise time \(t_\textrm{buoy} \sim R\sqrt{SC_D/2gV}\) (Rafferty et al. 2006). Here, R is the projected distance of the cavity from the cluster center, g the gravitational acceleration (\(g = 2\sigma ^2 / R\)) with stellar velocity dispersion \(\sigma = 239\) km s\(^{-1}\) (Pulido et al. 2018), \(S(=\pi R_w^2)\) cross-section area of the cavity, \(R_w\) radius of the cavity measured perpendicular to the jet axis and \(C_D=0.75\), the drag coefficient (Churazov et al. 2001). The plasma pressures p surrounding the X-ray cavities estimated from the projected analysis (Table 4) were used to estimate cavity enthalpy. The volume of the cavities was determined using \(V = 4 \pi R_l R_{w}^2 /3\) with \(R_l\) as the semi-major axis along the radio jet. For the ellipsoidal cavities of sizes given in Table 4, we quantify the power content of the NW and SE cavities as \(6.01\times 10^{44}\) and \(1.89\times 10^{44}\) erg s\(^{-1}\), respectively. Total cavity power of \(7.90 \times 10^{44}\) erg s\(^{-1}\) corresponds to a net enthalpy content of \({\sim }6.20\times 10^{59}\) erg. Here, uncertainties involved in the estimation of cavity powers depend on the errors in the measurement of physical sizes of the cavities, which was done by fitting ellipses to them by visual inspection, and also on the quality of data. As a result, we anticipate greater uncertainties, up to about 20%, in the enthalpy estimation (McNamara & Nulsen 2007; Gitti et al. 2010; Kadam et al. 2019).

Fig. 8
figure 8

Profile of the cooling time of ICM in the core of RXCJ0352.9\(+\)1941. The horizontal dashed line corresponds to the cooling time of 7.7 Gyr.

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4.2 Cooling vs heating of the ICM

Without central heating, ICM in the cluster’s core must cool radiatively, depositing a large fraction of cool gas at the core. From the spectral analysis discussed above, we obtain a profile of ICM cooling time as a function of projected distance using Sarazin (1988):

$$\begin{aligned} t_\mathrm{\textrm{cool}} = 0.8 \times 10^{10} \ \textrm{yr} \left( \frac{n_\textrm{e}}{10^{-3} \ \textrm{cm}^{-3}}\right) ^{-1} \left( \frac{T}{10^{7} \ \textrm{K}}\right) ^{1.6}, \end{aligned}$$
(4)

where \(n_\textrm{e}\) and T represent the electron density and plasma temperature at a projected distance r, the resultant cooling time profile is shown in Figure 8, which yields a cooling time of \(\sim \) \(2.7 \times 10^8\) yr. Assuming classical analogy, we define the ‘cooling radius’ (\(R_\textrm{cool}\)) as the distance where cooling time is \({<}7.7\) Gyr (Hudson et al. 2010) (horizontal dashed line) and is equal to 50.33 arcsec (100 kpc). We compute the bolometric (0.01–100 keV) cooling luminosity within \(R_\textrm{cool}\) as \(L_\textrm{cool} = 1.54^{+0.01}_{-0.01} \times 10^{44}\) erg s\(^{-1}\). A recent study Wang et al. (2023) provided more physically motivated ways to estimate cooling radii, like cool-core condensation radius (\(R_{\textrm{ccc}}\)) and the quenched cooling flow radius (\(R_{\textrm{qcf}}\)). These yielded a tight correlation with the AGN feedback compared to that obtained using the \(R_\textrm{cool}\) value. The estimates for these radii in the present case were found to be \(R_{\textrm{ccc}} = 39.5\) kpc and \(R_{\textrm{qcf}} = 58.1\) kpc, resulting in the bolometric (0.01–100 keV) luminosities equal to \(L_{\textrm{ccc}} = 6.54^{+0.08}_{-0.10} \times 10^{43}\) erg s\(^{-1}\) and \(L_{\textrm{qcf}} = 9.87^{+0.08}_{-0.13} \times 10^{43}\) erg \(\textrm{s}^{-1}\), respectively. The estimates from these radii are found an order of magnitude lower than estimated above using classical cooling radius. Wang et al. (2023) for a sample of cool-core clusters demonstrated that the feeding and feedback processes are linked more tightly when estimated using the \(R_{\textrm{qcf}}\), even compared to \(R_{\textrm{ccc}}\).

We then estimate the mass deposition rate adopting classical cooling radius as:

$$\begin{aligned} \dot{M}_\textrm{cool} = \frac{2 \mu m_\textrm{H} L_\textrm{cool}}{5 \ \textrm{kT}}, \end{aligned}$$
(5)

where \(\mu \) is the molecular weight. This resulted in the mass deposition rate of \(\dot{M}_\textrm{cool}= 238\pm 5.05\) \(M_{\odot }\) yr\(^{-1}\), while that estimated using the quenched cooling flow radius (\(R_{\textrm{qcf}}\)) was found to be equal to \(152\pm 3.23\) \(M_{\odot }\) yr\(^{-1}\). Using the \(H_{\alpha }\) flux luminosity reported by Pulido et al. (2018) the star formation rate in the core of this cluster to be equal to 12.6 \(M_\odot \) yr\(^{-1}\), an order of magnitude lower than even expected from the quenched cooling flow analogy. This discrepancy between the expected and measured values of the cooling mass confirms that the gas in the core of this cluster is not cooling systematically, but is heated instead to prevent further star formation.

Fig. 9
figure 9

Left panel: Balance between the mechanical power (\(P_\textrm{cav}\)) vs X-ray cooling luminosity adopted from Hlavacek-Larrondo et al. (2012). We also add data points from the studies by Rafferty et al. (2006) and Nulsen et al. (2009). To confirm the balance between the two processes for RXCJ0352.9\(+\)1941, we also plot its position estimated using \(R_\textrm{cool}\), \(R_{\textrm{qcf}}\) and \(R_{\textrm{ccc}}\) (respectively, magenta plus, green cross and black dot). The diagonal lines from top to bottom exhibit the equivalence between the two for enthalpy levels at 1pV, 4pV, and 16pV. Right panel: Balance between the cavity power (\(P_\textrm{cav}\)) and 1.4 GHz radio power, adopted from Paggi et al. (2014) for the sample of Cavagnolo et al. (2010). The green dashed line represents the best-fit relation for the sample of giant ellipticals (gEs). RXCJ0352.9\(+\)1941 occupies a position above the best fit of Cavagnolo et al. (2010) .

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Various sources have been considered for the intermittent heating of the ICM. Previous studies on cool-core clusters utilizing high angular resolution X-ray data from the Chandra observatory have shown that the enthalpy injected by the radio-jets emanating from the central AGN is capable enough to prevent the ICM cooling and thus, inhibiting the star formation (Fabian 1994; Peterson & Fabian 2006). Furthermore, to assess a balance in RXCJ0352.9\(+\)1941, we compared the estimates of mechanical power injected by the central AGN using cavities (\(P_\textrm{cav}\)) with the radiative loss of the ICM (\(L_\textrm{cool}\)). A comparison of the estimates of bolometric cooling luminosity (\(L_\textrm{cool}\)) and total cavity power (\(P_\textrm{cav}\)) confirmed that the enthalpy content of the cavities is in excess that required to offset the radiative loss and hence to quench the cooling flow. This was evident from the position occupied by RXCJ0352.9\(+\)1941 in the graph (Figure 9, left panel) between the cavity power (\(P_\textrm{cav}\)) vs X-ray cooling luminosity (\(L_\textrm{cool}\)) adopted from Hlavacek-Larrondo et al. (2013). We plot the position of RXCJ0352.9\(+\)1941 in this graph by using X-ray cooling luminosities estimated using all three methods discussed above. The dashed slanted lines in the plot correspond to \(P_\textrm{cav} = L_\textrm{cool}\) for energy inputs of 1pV, 4pV and 16pV, respectively, from top to bottom. All the three estimates for RXCJ0352.9\(+\)1941 with this confirm that the radio-mode feedback energy delivered by the AGN is enough to compensate for the cooling loss, consistent with those seen in other systems studied by Bîrzan et al. (2004), Rafferty et al. (2006), Nulsen et al. (2009), Best et al. (2006), and at relatively higher redshifts by Hlavacek-Larrondo et al. (2012, 2015). The balance between the two is evident for the systems belonging to clusters and even for giant ellipticals indicates that the atmospheres of cool-core clusters are stabilized by the radio mode feedback.

Combined studies of cool-core clusters in X-ray and radio bands have established that the depressions or cavities in the X-ray surface brightness are carved by radio jets emanating from the central AGN (e.g., Randall et al. 2011; Vantyghem et al. 2014; Snios et al. 2018). Further, such cavities are often found to be filled with radio emission of relativistic plasma. In the present case, we also found that the extended radio emission at 1.4 GHz mapped using GMRT data covers the X-ray cavities. The measured value of flux density \(20.8\pm 2.1\) mJy at 1.4 GHz for RXCJ0352.9\(+\)1941 was used to compute its radio power as Cavagnolo et al. (2010):

$$\begin{aligned} P_{\nu _0}=4 \pi D_\textrm{L}^{2} S_{\nu _0} \nu _{0} (1+z)^{\alpha -1}, \end{aligned}$$
(6)
Fig. 10
figure 10

Left panel: GMRT 1.4 GHz contours (red) at −3, \(3\times \sigma \) increased by \(\sqrt{2}\) times till \(48\times \sigma \) overlaid on Chandra X-ray emission map (black contours) at 1–\(9\times 2\) counts. Right panel: Central 35 arcsec region of the \(\beta \)-model subtracted residual map overlaid with 1.4 GHz GMRT radio contours at \(2,8,32,128\times \sigma \). The radio image rms noise is \(\sigma =0.05\) mJy beam\(^{-1}\), resolution \(=\) 2.6 arcsec \(\times \) 2.0 arcsec and position angle \(=\) 71.8\(^{\circ }\).

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where \(D_\textrm{L}\), \(S_{\nu _0}\), and \(\alpha \), respectively, represent the luminosity distance, the flux density at frequency \(\nu _0\), and the radio spectral index (\(S_{\nu } \sim \nu ^{-\alpha }\)). Assuming \(\alpha = - 0.8\) (typical for radio galaxies; Condon 1992) 1.4 GHz radio power was equal to \(7.4\pm 0.8\times 10^{39}\) erg s\(^{-1}\). This was then used to check the balance with that of the cavity power \(P_\textrm{cav}\) as studied by Cavagnolo et al. (2010) (Figure 9, right panel). RXCJ0352.9\(+\)1941 (magenta plus) occupies a position much above the best-fit relation of Cavagnolo et al. (2010), implying that the radio source hosted by this cluster is capable enough to deliver sufficient energy and hence to carve the X-ray cavities and to quench the cooling flow. This is in agreement with the results of several other studies Baldi et al. (2009), Gitti et al. (2010), O’Sullivan et al. (2011), Vagshette et al. (2016, 2017), Pandge et al. (2019) and Pasini et al. (2021).

4.3 Radio jets and cavity association

A combined study employing data in X-ray and radio bands on a large sample of cooling flow clusters has established a convincing association of the radio source with the core of such clusters (Dunn & Fabian 2006). RXCJ0352.9\(+\)1941 is also reported to host a radio-loud AGN (Green et al. 2016) that exhibits multiple jets and extended diffuse radio emission like a lobe, as we report. Our 1.4 GHz GMRT radio study also confirms the association of a strong radio core with the optical (BCG) and X-ray peak of the central AGN (Figures 10, left panel). The diffuse radio emission also reveals the presence of two pairs of jet-like features depicting AGN outflows of non-thermal particles in the form of diffuse jets. The inner pair of jets (‘pj’ and ‘pj\(^{\prime }\)’) coincides with the NW and SE cavities (Figure 10, Right panel), thereby providing an evidence of pushing aside the plasma to carve them. The longest secondary jet, ‘sj’, is extended up to 20 arcsec (40 kpc) in the northeast direction, while ‘sj\('\)’ does not provide clear evidence except a couple of isolated sources in the southwest. The diffuse radio-emitting clouds and/or lobes of non-thermal particles were roughly found to occupy regions of low X-ray emission (Figure 10, right panel).

The radio morphology also exhibits a misalignment between the inner pair of lobes (pj’s) and the extended diffuse emission (sj’s). Unlike in typical bent-tailed galaxies (Sebastia et al. 2017; Gendron-Marsolais et al. 2020; Lal 2020), the bending seen in this cluster is not smooth. The sharp bend and the absence of the counter-lobe make it difficult to confirm this as a bent-tailed radio galaxy. A strong argument favoring a bent-jet scenario is the alignment of the base of ‘sj’ with the termination of the ‘pj’ jet and not with the core. This morphology is quite similar to that of the bent-jet radio galaxy in group NGC 1550 (Kolokythas et al. 2020). However, the bending angle in RXCJ0352.9\(+\)1941 is much larger than in NGC 1550, and unlike in NGC 1550, it does not coincide with the cold fronts evident in this system.

Another viable proposition is that RXCJ0352.9\(+\)1941 hosts an X-shaped radio galaxy (Lal et al. 2019; Bruno et al. 2019; Garofalo et al. 2020). The possible mechanisms responsible for the origin of X-shaped radio morphology include precession of jets (Parma et al. 1985), sudden spin flip of jets due to binary black hole merger (Dennett-Thorpe et al. 2002), or diverted back-flow of the ISM/ICM along the minor axis of the host (Leahy & Williams 1984). The morphological features evident in the present case, such as the absence of hot-spot in the secondary jet (‘sj’), significant long length of ‘sj’ relative to primary lobes, and its orientation along the major axis of the BCG, all collectively point towards the spin-flip scenario of its formation (Gopal-Krishna et al. 2012). However, high-resolution, deep multi-frequency radio data on this source are called for before arriving at any proper conclusion regarding the origin of such an intricate radio morphology.

4.4 Cold front and sloshing scenario

As discussed in Sections 3.2 and 3.3.1 the surface brightness analysis revealed a discontinuity in its profile at about 31 arcsec (\(\sim \)62 kpc) with a density jump of \(1.37\pm 0.05\). Temperature on the inner (\(2.01\pm 0.19\) keV) and outer (\(3.45\pm 0.50\) keV) side of the discontinuity reveals a jump of \(1.44\pm 0.53\) keV, while pressure maintaining continuity across this discontinuity point towards its association with a cold front like that seen in several other clusters, e.g., Toothbrush cluster (Botteon et al. 2020), Abell 401, RXC J0528.9−3927 and Abell 1914 (Botteon et al. 2018), 3C 320 (Vagshette et al. 2019), Abell 2626 (Kadam et al. 2019), RXJ2014.8−2430 (Walker et al. 2014), Abell 496 (Roediger et al. 2012).

It is believed that cold fronts in cool-core clusters are formed by sloshing of the cluster core, likely triggered by off-axis minor mergers or the passage of small substructures causing the offset in ICM from hydrostatic equilibrium. Such an offset causes the gas in the potential well to oscillate, resulting in the formation of cold fronts around core of the cluster (see, Ascasibar & Markevitch 2006; Roediger et al. 2011). ICM in the environment of RXCJ0352.9\(+\)1941 appears highly dynamic, implying that the cold front might have formed due to an off-axis minor merger. The evidence supporting this was provided by detecting two extended spiral-like features on the north and south part of cluster emission and are consistent with the findings of Paterno-Mahler et al. (2013).

Sloshing of gas may affect the distribution of relativistic electrons in the cluster due to sloshing-generated turbulence. This may increase radio emission via the synchrotron mechanism (Clarke et al. 2004; van Weeren et al. 2019). Therefore, we speculate that the origin of extended diffuse radio emission surrounding the BCG in RXCJ0352.9\(+\)1941 may also be due to sloshing, at least the possibility cannot be fully ruled out. Furthermore, Ferrari (2005), Koyama et al. (2008) and Rawle et al. (2014) have proposed that an off-axis minor merger may deposit a significant amount of gas in the core of the cluster resulting in an enhanced star formation. In the present case, the reported star formation of 12.6 \(M_{\odot }\) yr\(^{-1}\), higher than that witnessed in other cool core clusters 0.1 to 5 \(M_{\odot }\) yr\(^{-1}\) (O’Dea et al. 2008; McDonald et al. 2011), probably point such a merger.

5 Conclusions

We conducted a comprehensive analysis of 30 ks Chandra data and 46.8 ks (13 h) 1.4 GHz GMRT radio data on the cluster RXCJ0352.9\(+\)1941 with an objective to investigate AGN activities at its core. We also explore the evidence of AGN feedback and its energy budget in each outburst it injects into the ICM. Our important findings from the study are summarized as follows:

  • This study confirmed a pair of X-ray cavities at projected distances of 10.30 kpc and 20.80 kpc, respectively, on the NW and SE of the X-ray peak and was carried out employing various image processing techniques. Total mechanical power stored in the cavities was estimated to be \(\sim \) \(7.90\times 10^{44}\) erg s\(^{-1}\), while the enthalpy \(\sim \) \(6.20\times 10^{59}\) erg, much higher than required for quenching of the cooling flow in its core.

  • Spectral analysis of the plasma distributed in this cluster yielded bolometric (0.01–100 keV) X-ray luminosity from within the cooling radius (\(\sim \)100 kpc) equal to \(L_\textrm{cool} = 1.54^{+0.01}_{-0.01} \times 10^{44}\) erg s\(^{-1}\) requiring a mass deposition of \(238\pm 5.05\) \(M_\odot \) yr\(^{-1}\). This happens to be an order of magnitude higher than the quantum detected in the form of star formation of 12.6 \(M_\odot \) yr\(^{-1}\), implying that the gas in the core is heated instead by an intermittent source like AGN outburst.

  • Analysis of the GMRT L band (1.4 GHz) data revealed a bright radio source at the core with multiple jet-like emission characteristics. The observed X-shaped morphology of diffuse radio emission is a composite of an orthogonal extended external one-sided jet and an inner pair of jets along the X-ray cavities. The 1.4 GHz radio power \(P_{1.4\ \textrm{GHz}} = 7.4 \pm 0.8 \times 10^{39}\) erg s\(^{-1}\) is found to correlate strongly with the mechanical power quantified from the cavity analysis. The clear association of inner jets with the X-ray cavities and the balance between the radio power and enthalpy content of cavities confirms the intermittent heating of the ICM by radio outbursts of central AGN.

  • The hard X-ray emission from the central 2 arcsec with a luminosity \(\sim \) \(9.66\times 10^{42}\) erg s\(^{-1}\) and a power-law photon index \((\Gamma ) = 0.72\pm 0.12\) suggests its association with AGN.

  • The X-ray surface brightness evidenced two non-uniform, extended spiral emissions structures on either side of the core, pointing towards gas sloshing due to a minor merger. This could result in a surface brightness edge on the southwest due to a cold front at \(\sim \)31 arcsec (62 kpc) with a temperature jump of 1.44 keV.