A&A 585, A3 (2016) AstronomyDOI: 10.1051/0004-6361/201526833 
&
× cESO 2015 
Astrophysics 

Hot gas and magnetic arms of NGC 6946: Indications for reconnection heating? 
M. Wezgowiec1,2,M. Ehle3, and R. Beck4 
1 Astronomisches Institut der Ruhr-Universität Bochum, Universitätsstrasse 150, 44780 Bochum, Germany e-mail: markmet@oa.uj.edu.pl 2 Obserwatorium Astronomiczne Uniwersytetu Jagiello´
nskiego, ul. Orla 171, 30-244 Kraków, Poland 3 ESA-ESAC, XMM-Newton Science Operations Centre, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 4 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 
Received 25 June 2015 / Accepted 15 October 2015 

ABSTRACT 
Context. The grand-design face-on spiral galaxy NGC 6946 is remarkable because of its high star formation activity, the massive northern spiral arm, and the magnetic arms, which are observed in polarized radio synchrotron emission and are located between the optical arms and possibly are magnetic reconnection regions. Aims. We used electron densities and temperatures in star-forming (active) and less active regions and compared them to fndings from the analysis of the radio data to study the energy budget of NGC 6946. The hot gas above the magnetic arms between the optical arms might suggest gas heating by reconnection. We also study the population of point sources in NGC 6946, including the origin of the puzzling ultra-luminous emission complex MF16. Methods. X-ray observations of NGC 6946 performed with XMM-Newton were used to study the emission from X-ray point sources and diffuse hot gas, including the magnetic arms and the halo. Spectral ftting of the diffuseX-rayemission allowedus toderive temperatures of the hot gas. With assumptions about the emission volume, this allowed us to estimate gas densities, masses, and cooling times. Results. To explain the X-ray emission from the spiral arms of NGC 6946 two-temperature plasma models are needed to account for the disk and halo emission. The interarm regions show only one thermal component. We observe that the temperature of the hot gas in and above the magnetic arm regions increases slightly when compared to the average temperatures in the areas in and above the spiral arms. For the southwestern part of the disk, which is depolarized in the radio range by Faraday rotation, we fnd more efficient mixing of disk and halo gas. Conclusions. We propose magnetic reconnection in the magnetic arm regions of NGC 6946 as the possible cause of the additional heating of the gas and ordering of the magnetic felds. In the southwestern part of the galactic disk we observed indications of a possible faster outfow of the hot gas. A very hot gas within the MF 16 nebula possibly suggests shock heating by a supernova explosion. 
Key words. galaxies: individual: NGC 6946 – galaxies: ISM – galaxies: spiral – galaxies: magnetic felds 
1. Introduction Table 1. Basic astronomical properties of NGC 6946. 
NGC 6946 (see Table 1) is a Scd spiral galaxy seen face-on, 
Morphological type SABc 

which is listed in Arp’s atlas of peculiar galaxies because of its 
Inclination 18◦ 

massive northern spiral arm. Its large optical diameter and low 
Diameter D25 11.5 inclination make NGC 6946 one of the most prominent grand
RA2000 20h34m53s design spiral galaxies in the sky. It is known to host a bright +60◦09 13 
Dec2000 starburst nucleus (see e.g. Telesco & Harper 1980). Detections Distancea 7Mpc of CO radio emission lines (Nieten et al. 1999; Walsh et al. Notes. All data except for the distance are taken from the HYPERLEDA 
2002) gave further evidence for the high star-forming activity 
database – http://leda.univ-lyon1.fr <BR>–see Paturel (2003). 
of NGC 6946 (especially in the northern spiral arm), proved that 
(a) Taken from Israel (1980). 
molecular clouds containing warm and dense gas are distributed throughout the inner disk, and showed that the total molecular gas mass is exceptionally high for a spiral galaxy. The distribu-1.1. Previous radio continuum findings tions of the emission from NGC 6946 in various spectral ranges 
NGC 6946 has been thoroughly studied in the radio regime in were analysed with wavelet functions (see Frick et al. 2000). 
total and polarized emission (Beck 1991; Ehle & Beck 1993). Radio polarization observations at 18 cm and 20 cm wavelengths Based on observations obtained with XMM-Newton,an ESA sci-revealed excess Faraday rotation and strong depolarization in the ence mission with instruments and contributions directly funded by SW quadrant of NGC 6946 that is probably due to a large-scale ESA Member States and NASA. magnetic feld along the line of sight, oriented approximately 
Article published by EDP Sciences A3, page 1 of 20 
perpendicular to the disk plane (Beck 1991). Analysis of polar-ization data at four frequencies also suggested strong vertical felds extending far above the disk (Beck 2007). Such feld lines should enable an outfow of hot gas into a halo. As the SW quad-rant of NGC 6946 is a region of relatively low star-formation ac-tivity, this phenomenon resembles a coronal hole on the Sun. 
The average energy density of the warm ionized medium in the interstellar medium (ISM) of the inner disk of NGC 6946 was found to be lower by a factor of about 10 than the energy densities of the magnetic feld and that of the cosmic rays, re-sulting in the conclusion that the magnetic feld dominates ther-mal processes in the disk and halos of galaxies (Beck 2004). A signifcant fraction of the diffuse ISM must be unstable, giving rise to gas outfows. 
Radio polarization data at λ6 cm led to the discovery of a new phenomenon: highly aligned magnetic felds that are con-centrated in two main spiral features, located almost precisely between the optical spiral arms of NGC 6946 (Beck & Hoernes 1996, their Fig. 1). No enhanced densities of molecular, neutral, or warm ionized gas have been detected at the positions of these magnetic arms. However, radio observations revealed signifcant Faraday rotation in these regions so that some ionized gas must be present. Frick et al. (2000) analysed the magnetic and optical spiral arms in NGC 6946 using 1D wavelet transformations and found that each magnetic arm is similar to the preceding optical arm and hence can be regarded as a phase-shifted image. 
Rudimentary magnetic arms were also found in other spiral galaxies (Beck 2015), but NGC 6946 still is the most prominent example. 
The magnetic arms contradict density-wave models, which predict enhanced ordered magnetic felds at the inner edges of the arms. Several mechanisms were proposed to explain the magnetic arms. For example, the continuous injection and ampli-fcation of turbulent felds by supernova shock fronts may suppress the mean-feld dynamo in the material arms (Moss et al. 2013, 2015). Alternatively, the introduction of a relaxation time of the magnetic response in the dynamo equation may lead to a phase shift between the material and magnetic spiral arms (Chamandy et al. 2013a,b). The mean-feld dynamo in the ma-terial arms might also be suppressed by outfows driven by star formation (Chamandy et al. 2015). 
We propose here that the strongly polarized radio emission from the magnetic arms may also suggest the existence of re-connection regions where cosmic rays are accelerated. The gas heated by the same process should be detectable in the X-ray do-main (Lesch & Bender 1990; Hanasz & Lesch 2003). By com-paring the properties of the hot gas in the magnetic and spiral arms, we may be able to trace a possible additional heating of the gas that would be caused by the reconnection processes. 
1.2. Earlier X-ray observations 
Despite the rather high NH-value of about 2 × 1021 cm−2 (see Table 2), NGC 6946 was detected by ROSAT’s All Sky sur-vey with a count rate of 0.1 cts s−1. Analysing the 36 ks ROSAT PSPC pointed observation, Schlegel (1994a,b,c)apart from SN 1980K additionally reported emission from nine point-like X-ray sources and diffuse emission from NGC 6946. The brightest source (identifed at that time with a very luminous supernova remnant MF16) has a count rate of 0.07 cts s−1 corre-
−2 

sponding to a fux of 8.3×10−13ergcms−1 in the energy range 0.5−2 keV, three sources are fainter by about a factor of 10, and the rest (fainter by a factor of 40) are at the detection threshold. 
Table 2. Characteristics of the XMM-Newton X-ray observations of NGC 6946. 
Obs ID  0200670301  
0500730101  
0500730201  
0691570101  
a column density NH  1.84  
MOS flter  medium  
MOS obs. mode  FF  
pn flter  medium  
pn obs. mode  FF  
Total/clean pn time [ks]  13.1/8.3  
28.4/20.2  
33.3/29.7  
114.3/98.2  


Notes. (a) Column density in [1021 cm−2] weighted average value after LAB Survey of Galactic H i Kalberla et al. (2005). 
Holt et al. (2003) studied discrete X-ray sources in NGC 6946 using a 60 ks Chandra ACIS observation and found the source population dominated by high-mass X-ray binaries. 
−1 

Their survey was complete down to approximately 1037 erg s. However, in contrast to previous results, the ultra-luminous MF16 complex was found to be defcient in line emission ex-pected from an interaction with a dense surrounding medium. Its spectrum lacks pronounced spectral lines and can be ft with a variety of models that are all associated with unusually high luminosities, leaving the origin of the MF16 related X-ray emission unknown. Schlegel et al. (2003) used the same Chandra observations and the luminosity function derived by Holt et al. (2003) to distinguish point sources from the diffuse emission. These authors estimated that as much as 10% of the total soft X-ray emission could be due to a hot diffuse component. 
We checked the Chandra archive and found additional ACIS-S pointings: one on-axis pointing aiming at SN2002HH (30 ks, IAU Circ. 8024 and Roberts & Colbert 2003), and three (30 ks each) off-axis pointings centred on SN2004et. The com-bination of these Chandra observations was used by severeal authors (Soria & Perna 2008; Fridriksson et al. 2008; Kajava & Poutanen 2009; Liu 2011) to investigate individual sources 
(e.g. supernovae, ultra-luminous sources) in NGC 6946 and their spectral and temporal variability. Recent observations (20 ks, PI Kochanek) were also aimed at studying point-source popu-lations, which is beyond the scope of this paper. 
1.3. Immediate objectives 
This paper focuses on a detailed analysis of the extended emission from the hot gas of NGC 6946 with the use of the data ac-quired by the XMM-Newton X-ray telescope (Jansen et al. 2001). The parameters of the hot gas acquired from the spectral analysis of selected regions of the galaxy are compared with the properties of the radio emission, especially with its polarized component that traces the structure of the magnetic feld of the galaxy. 
In the following section (Sect. 2) details of the data reduction and analysis are presented. Section 3 presents the distribution of the X-ray emission from both diffuse gas and point-source pop-ulations, and we also describe the spectra we obtained. In Sect. 4 we thoroughly discuss the results, including correlations and comparisons with the polarized radio emission from NGC 6946. We also provide new insight into the nature of the ultra-luminous source MF16. We conclude in Sect. 5. 
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M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 


2. Observations and data reduction 
NGC 6946 has been observed 11 times between 2003 and 2006 with the XMM-Newton telescope (Jansen et al. 2001), but the observations always suffered from heavy high faring radia-tion. The only observation that yielded any clean data was made on 13 June 2004 (ObsID 0200670301). Consequently, the galaxy was observed again, on 2 and 8 November 2007 (ObsIDs 0500730201 and 0500730101, respectively, see Table 2). The data were still affected by high faring radiation, but this time it was possible to obtain many good-quality data. The effect of frequent faring radiation on the observations was caused by vis-ibility constraints that required NGC 6946 to be observed at the end of an XMM-Newton revolution. In recent years the orbit has evolved and NGC 6946 can be much better observed. Since early 2012 it has become possible to observe this galaxy for almost a full orbit (144 ks). The most recent observations, performed between 21 and 23 of December 2012 and aimed at the ultra-luminous source NGC 6946 X-1 (ObsID 0691570101), provided a long exposure that was relatively free of high faring radiation; this resulted in 98 ks of good data. 
The data were processed using the SAS 13.0.0 package (Gabriel et al. 2004) with standard reduction procedures. Following the routine of tasks epchain and emchain, event lists for two EPIC-MOS cameras (Turner et al. 2001)and the EPIC-pn camera (Strüder et al. 2001) were obtained. Next, the event lists were carefully fltered for periods of intense radiation of high-energy background by creating light curves of high-energy emission. These light curves were used to produce good time interval (GTI) tables, which mark times of low count rates of high-energy emission. Such tables (time ranges) were then used to remove the remaining data when high count rates were ob-served. The resulting lists were checked for the residual existence of soft proton fare contamination, which could infuence the faint extended emission. To do that, we used a script1 that performs calculations developed by Molendi et al. (2004). We found that only the shortest observation (ObsID 0200670301) is contaminated very slightly by soft proton radiation. To ensure the best-quality data (crucial to analyse diffuse emission), we only used events with FLAG = 0 and PATTERN ≤ 4 (EPIC-pn) or FLAG = 0 and PATTERN ≤ 12 (EPIC-MOS) in the following data processing. 
The fltered event lists were used to produce images, background images, exposure maps (without vignetting correction), masked for an acceptable detector area using the images script2, modifed by the authors to allow adaptive smoothing. All images and maps were produced (with exposure correction) in four en-ergy bands of 0.2−1keV,1−2keV, 2−4.5 keV, and 4.5−12 keV. The images were then combined into fnal EPIC images and adaptively smoothed with a maximum smoothing scale of 30 FWHM. The rms values were obtained by averaging the emission over a large source-free area in the fnal map. 
Another set of images was also constructed after excluding all point sources found within the D25 diameter of NGC 6946 from the event lists (see below for details on point source exclusion). This was done with the help of a routine used to create re-flled blank sky background maps − ghostholes_ind3.In this way we obtained a map of diffuse emission where all regions of 
1 http://xmm2.esac.esa.int/external/xmm_sw_cal/ <BR>background/epic_scripts.shtml#flare <BR>2 http://xmm.esac.esa.int/external/xmm_science/ <BR>gallery/utils/images.shtml <BR>3 ftp://xmm.esac.esa.int/pub/ccf/constituents/extras/ <BR>background/epic/blank_sky/scripts <BR>
excluded point sources are flled with emission close to extracted regions by sampling adjacent events and randomising spatial coordinates4. Although this method is used to handle background maps, we obtained good results when we applied it to real source data. Section 3.1.1 presents images of soft (0.2−1keV) and medium (1−2 keV) emission, together with a corresponding hardness ratio map, defned as 
med − soft 

HR = , 
med + soft 

for images with and without detected point sources. 
Next, the spectral analysis was performed. To create spectra we only used the event list from the EPIC-pn camera because it offers the highest sensitivity in the soft energy band. Only the emission above 0.3 keV was analysed because the internal noise of the pn camera is too high below this limit5. Although this is not crucial when combined with MOS cameras to produce images, it is important to exclude the softest emission below 
0.3 keV to obtain reliable good-quality spectra. 
Unsmoothed images for all bands were used to search for point sources with the standard SAS edetect_chain procedure. Regions found to include a possible point source were marked. The area was individually chosen for each source to ensure that we excluded all pixels brighter than the surrounding background. These areas were then used to construct spectral regions for which spectra were acquired. 
The non-default way of excluding the detected point sources helped to keep more diffuse emission in the fnal spectra. However, expecting some contribution from the PSF wings, we added a power-law component to our model fts to account for any residual emission. A power-law component was also needed to account for unresolved point sources. The background spectra were obtained using blank sky event lists (see Carter & Read 2007). These blank sky event lists were fltered using the same procedures as for the source event lists. For each spectrum we produced response matrices and effective area fles. For the lat-ter, detector maps needed for extended emission analysis were also created. The spectra were binned, which resulted in a better signal-to-noise ratio. To obtain a reasonable number of bins at the same time, we chose to have 25 total counts per energy bin. The spectra were ftted using XSPEC 11 (Arnaud 1996). 
Since observations 0500730201 and 0500730101 have identical pointings and position angles, we merged the cleaned event lists using the SAS task merge. The spectra extracted from this merged lists give the same model-ftting results as separate spectra ftted simultaneously, but the errors are better con-strained, therefore we used the former spectra in our fnal analysis. It was not possible to also merge-in the shortest observation (ObsID 0200670301) because it has different parameters (pointing and position angle), and simultaneous ftting with the larger data set showed that both spectra are systematically offset. This resulted in a poorer model ft. We assume that this might arise because the observation was signifcantly affected by high far-ing radiation and because the fltered “clean” data still show residual contamination that might infuence the spectral ftting. Although we used this observation for image production, we therefore excluded the pn data from our spectral analysis. For the same inconsistency reasons (different pointing and position angle), we used the longest observation 0691570101 separately 
4 http://xmm2.esac.esa.int/external/xmm_sw_cal/ <BR>background/blank_sky.shtml#BGsoft <BR>5 http://xmm.esac.esa.int/external/xmm_user_support/ <BR>documentation/uhb <BR>
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NGC 6946 XMM-Newton EPIC 0.2-1 keV on H-alpha  NGC 6946 XMM-Newton "ghosted" EPIC 0.2-1 keV on H-alpha  
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06 06 
04 04 20 35 30 15 00 34 45 30 15 20 35 30 15 00 34 45 30 15 RIGHT ASCENSION (J2000) RIGHT ASCENSION (J2000) 
Fig. <BR>1. <BR>Left: map of soft X-ray emission from NGC 6946 in the 0.2−1 keV band overlaid onto an Hα image. The contours are 3, 5, 8, 16, 25, 40, 60, 80, 100, 200, 500, and 1000 × rms. The map is adaptively smoothed with the largest scale of 30. Right: same map, but with point sources excluded from the galactic disk (see text for details). 
when performing the spectral analysis. This approach resulted in two corresponding spectra for each of the studied regions. Each pair of spectra was merged (as well as their corresponding background spectra) using the SAS task epicspeccombine. Although for multiple spectra a most commonly advised routine is a simultaneous ft rather than a ft to a combined spectrum, we note that for spectra with a very different sensitivity (certainly in our case), a combination of spectra leads to a much better handle on the background and consequently a better ft. This is because background subtraction only takes place for the merged spectrum after the source and background spectra are combined (contrary to a simultaneous ft, where each spectrum is background subtracted before the ft). 
Forthe overlays wealsousedthe XMM-Newton Optical Monitor data acquired during the same observations and pro-duced an image in the UVM2 flter using the standard SAS om-chain procedure. 

3. Results 
3.1. Distribution of the X-ray emission 
3.1.1. Diffuse emission 
NGC 6946 shows soft extended X-ray emission corresponding to the entire star-forming disk (Fig. 1), with the brightest emis<BR>sion closely following the star-forming regions. Although the southern part of the star-forming disk is less pronounced than the northern one, no asymmetries of the emission from the hot gas are visible. In contrast, the X-ray emission seems to extend farther out beyond star-forming regions in the southern part of the galaxy. An area of diffuse emission around the galactic centre forms a structure resembling a very small bar that crosses the central core and is aligned with the Hα emission. 
The hot gas disk visible in the 1−2 keV energy band (Fig. 2) is extended in a similar way as the emission in the softer en-ergy band (Fig. 1). This may suggest large amounts of very hot gas in the galactic disk and/or halo. To further investigate the contribution from the hottest gas to the X-ray emission from NGC 6946, we produced a hardness ratio map using both dis-tributions (Fig. 3). 
As mentioned before, the two distribution are similar on average because the values in most parts of the HR map are close to 
0. Nevertheless, north-east and south-west of the centre, distinct areas of softer emission are clearly visible. This corresponds well to the orientation of the bright star-forming regions visi-ble in the Hα map (Fig. 1). However, the softest emission is produced in the south-western part of the disk, where the pro-duction of young massive stars is diminished, as seen in the UV map (Fig. 2). 

3.1.2. Point sources 
Figure 4 shows all detected point sources within the D25 disk of NGC 6946. For all sources we performed a spectral analysis. For weak sources the hardness ratios (HRs) were derived (see Table 3). We used the same energy bands as in Pietsch et al. (2004): (0.2−0.5) keV, (0.5−1.0)keV, (1.0−2.0) keV, (2.0−4.5)keV, and (4.5−12) keV as bands 1 to 5. Consequently, the hardness ratios are calculated as HRi = Bi+1 − Bi/Bi+1 + Bi for i = 1to4,where Bi is the count rate in band i,as defned above. For sources with more than 500 net counts in the total en-ergy band (0.2−12 keV), spectra were extracted and ftted with models (see Sect. 3.2.1). 
The left panel of Fig. 4 suggests that some of the sources might not originate from within the galaxy and are instead more distant background objects. Moreover, the centre of the most extended region of source 26 does not seem to coincide with the visible Hα clump, but more precise astrometry of the Chandra observation associated this source with the galaxy (e.g. Kajava & Poutanen 2009). This source is the brightest point source – the ultra-luminous complex MF16 that is assumed to be a supernova remnant (e.g. Matonick & Fesen 1997). It is not a pure point source, as it is considerably larger than the point spread function of the XMM-Newton EPIC cameras (of 12). 
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M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 
NGC 6946 XMM-Newton EPIC 1-2 keV on UV 
NGC 6946 XMM-Newton EPIC 1-2 keV on UV 
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04 20 35 30 15 00 34 45 30 15 20 35 30 15 00 34 45 30 15 RIGHT ASCENSION (J2000) RIGHT ASCENSION (J2000) 
Fig. <BR>2. <BR>Left: map of medium X-ray emission from NGC 6946 in the 1−2 keV band overlaid onto the XMM-Newton Optical Monitor UVM2 flter image. The contours are 3, 5, 8, 16, 25, 40, 60, 80, 100, 200, 300, 500, and 1000 × rms. The map is adaptively smoothed with the largest scale of 
30. Right: same map, but with point sources excluded from the galactic disk (see text for details). 
NGC 6946 XMM-Newton EPIC HR "ghosted" map 1-2 keV and 0.2-1 keV 
NGC 6946 XMM-Newton EPIC HR map between 1-2 keV and 0.2-1 keV 
-0.4 -0.2 -0.0 0.2 0.4 
-0.4 -0.2 -0.0 0.2 0.4 

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04  20 35 30  15  00 34 45 RIGHT ASCENSION (J2000)  30  15  20 35 30  15  00 34 45 RIGHT ASCENSION (J2000)  30  15  

Fig. <BR>3. <BR>Maps of the hardness ratio between medium and soft X-ray emission from NGC 6946 (Figs. 2 and 1). The map is truncated at the 3σ level of the 1−2keV map. Left: map with point sources. Right: map without point sources. 
Another interesting source is source 17, overlapping in Fig. 4 with sources 16 and 20. This source was not visible in previous observations (where sources 16 and 20 were detected), but only in the most recent sensitive observations. 


3.2. Spectral analysis of the X-ray emission 
For spectra of the hot gas we used a model that attributed one or two thermal plasmas and/or a contribution from unresolved point-like sources. Thermal plasma is represented in this work by a mekal model, which is a model of an emission spectrum from hot diffuse gas based on the model calculations of Mewe and Kaastra (Mewe et al. 1985; Kaastra 1992). In all models we fxed the metallicity to solar. This was determined by a test spectral ftting of the spectra, which showed that in a wide range of metallicities (0.1−1.5 solar), no signifcant change in gas temperatures or power-law photon indices could be observed. Slight deviations of these parameters were still within the er-rors provided by the models that used solar metallicity. This 
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Fig. <BR>4. <BR>Left: all point-like sources detected in NGC 6946 (see text for a detailed description) overlaid on an Hα image. Right: the same regions as in the left panel overlaid on the map of soft X-ray emission in the 0.2−1keV band as showninFig. 1. 
suggests that all differences that are found in gas temperatures when ftting spectra do not result from a possible combined ef-fect of abundance gradients and enforcing solar metallicities in the models. It also shows that an additional power-law component in the models of diffuse emission does account for emission from unresolved point-like sources and is not introduced to mimic variable gas abundance because excluding the power-law component from the model and again varying metallicities resulted in unphysical values of the parameters. Consequently, the quality of the model fts remained very low (with reduced χ2 > 2). 
A contribution from unresolved point-like sources is ftted with a simple power law. For some models an additional component to account for the internal absorption needed to be used. For all models we also used a fxed foreground (galactic) absorption. Tables 4 and 8 present an overview of the various spectral mod-els, including the obtained parameters. The errors provided for the model parameters are always 1σ errors. The derived X-ray fuxes and luminosities are shown in Tables 5 and 9. 
The same model components were used for the spectral analysis of the brightest point sources (see Sect. 3.1.2). Sincewedid not aim to perform a variability analysis of point sources, we used all data that were suitable for spectral analysis (for the se-lection and merging of separate data sets, see Sect. 2), similarly as for regions of diffuse emission. 
The regions of the diffuse X-ray emission from which the spectra were extracted are presented in Fig. 9. Extraction ar-eas for the brightest point-sources are the same as found by the source-detection analysis (cf. Fig. 4). All plots of the modelled spectra together with the ftted models are presented in Figs. 11 and 12. 
3.2.1. Brightest sources 
For almost all sources (except for source 27) for which spec-tral ftting was performed, we also used the thermal plasma component (see Table 4) to account for diffuse emission pro-jected onto each of the sources. The amount of this emission was often signifcant as a result of the sensitive observations of a gas-rich galaxy with a relatively large point spread function of the EPIC-pn camera that did not allow clearly separating the studied sources. Many of the spectra also required an additional model component to account for the high internal absorption. 
For one source (source 5) a model with a power-law com-ponent did not give good results. The spectrum was ftted best when using two thermal components. It is possible that it is sim-ply a hot gas clump that was classifed by the source detection routine to be a point source. Alternatively, the lowest count number of all ftted spectra might also be the reason for difficulties in fnding a proper ft. The hot component ftted in this model reaches values of almost 2 keV, which is fairly unexpected for the hot gas in the galactic disk. 
For source 17, which was undetected in earlier observations, a complex model had to be ftted. Its power-law component is poorly constrained, however. The two sources near this position that were detected previously, sources 16 and 20, were not de-tected in the recent sensitive observation because the brightness of the diffuse emission was higher throughout, and also because the bright source 17 has wings. For consistency of the results, however, we used all observations to extract spectra for all three sources. Nevertheless, the complexity of the model for source 17 might be caused by admixtures from the two adjacent sources. 
The spectrum of the core region, source 19, where the densest and the hottest gas might be expected, could be ft-ted equally well with either one or two thermal components. We present both model fts. The model with two components yielded 0.32+0.02 keV and 0.70+0.07 keV, while a single tempera
−0.03 −0.06 

ture component showed a temperature of 0.62 ± 0.04 keV. These values and the derived fuxes for this region (see Table 5) suggest that most of the emission originates from the hotter component. The main difference between both model fts, however, is a signifcant variation of the internal absorption (see Table 4). 
By ftting a model (consisting of one power-law and two thermal components) to the spectrum of MF16 (source 26), we obtained a temperature of 1.04 ± 0.03 keV for the hot com-ponent. Still, most of the fux from MF16 originates from the power-law component that is associated with the central source. To further investigate the spectrum of this source, we followed 
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Table 3. Countrates and hardness ratios for the resolved point-like sources in NGC 6946
ID α2000 δ 2000 RB1 B2 B3 B4 B5 Ct HR1 HR2 HR3 HR4 
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) 

1 20 h34m21s . 4 +60 ◦ 10 15. 217 5 55 17 34 29 1400.83 −0.53 0.33 −0.08 2 20 h34m24s . 9 +60 ◦ 10 35. 6 15 7 87 102 87 86 369 0.85 0.08 −0.08 −0.01 3 20 h 34 m 25s . 9 +60 ◦ 09 07. 0 19 52 349 577 322 68 1368 0.74 0.25 −0.28 −0.65 4 20 h34m26s . 6 +60 ◦ 11 13. 913 22 17 90048 −0.13 −0.31 −1n/a 5 20 h 34 m 34s . 4 +60 ◦ 10 31. 2 16 18 325 262 45 2 652 0.9 −0.11 −0.71 −0.91 6 20 h 34 m 36s . 5 +60 ◦ 09 30. 5 21 160 723 520 79 42 1524 0.64 −0.16 −0.74 −0.31 7 20 h34m37s . 8 +60 ◦ 04 33. 1 20 13 78 163 108 65 427 0.71 0.35 −0.2 −0.25 8 20 h34m40s . 1 +60 ◦ 08 23. 314 01111026528306 1 −0.04 −0.22 −0.4 9 20 h34m44s . 8 +60 ◦ 07 18. 0 15 31 192 94 19 19 355 0.72 −0.34 −0.66 0 10 20h34m46s . 6 +60 ◦ 13 25. 115 71 52 62 69 69 323 −0.15 0.09 0.05 0 11 20 h 34 m 48s . 0 +60 ◦ 09 32. 2 16 97 583 690 252 80 1702 0.71 0.08 −0.46 −0.52 12 20 h 34 m 48s . 8 +60 ◦ 08 10. 1 17 42 312 441 203 79 1077 0.76 0.17 −0.37 −0.44 13 20h34m49s . 0 +60 ◦ 12 17. 0 18 6 96 190 101 47 440 0.89 0.33 −0.31 −0.36 14 20 h 34 m 49s . 1 +60 ◦ 05 53. 8 19 106 599 194 21 9 929 0.7 −0.51 −0.8 −0.39 15 20h34m49s . 4 +60 ◦ 13 41. 911 0 21 24 30 22 97 10.07 0.11 −0.15 16 20 h 34 m 50s . 4 +60 ◦ 10 17. 0 18 79 608 470 177 70 1404 0.77 −0.13 −0.45 −0.43 17 20 h 34 m 51s . 4 +60 ◦ 10 43. 7 17 123 871 1468 827 201 3490 0.75 0.26 −0.28 −0.61 18 20h34m51s . 8 +60 ◦ 12 48. 611 2 31 45 7 7 92 0.88 0.18 −0.73 0 19 20 h 34 m 52s . 4 +60 ◦ 09 10. 6 23 269 2545 4542 2061 499 9916 0.81 0.28 −0.38 −0.61 20 20 h 34 m 53s . 5 +60 ◦ 10 54. 8 16 66 411 465 233 59 1234 0.72 0.06 −0.33 −0.6 21 20 h 34 m 56s . 7 +60 ◦ 08 32. 6 20 84 651 809 529 279 2352 0.77 0.11 −0.21 −0.31 22 20h34m57s . 1 +60 ◦ 05 32. 6 17 6 68 82 18 38 212 0.84 0.09 −0.64 0.36 23 20 h 34 m 57s . 8 +60 ◦ 09 48. 0 14 33 446 1004 475 58 2016 0.86 0.38 −0.36 −0.78 24 20 h 35 m 00s . 2 +60 ◦ 09 08. 0 24 812 4413 3982 688 99 9994 0.69 −0.05 −0.71 −0.75 25 20h35m00s . 7 +60 ◦ 12 50. 815 0 34 5331 7125 10.22 −0.26 −0.63 26 20 h 35 m 00s . 8 +60 ◦ 11 29. 9 38 3684 16674 17157 5547 1588 44650 0.64 0.01 −0.51 −0.55 27 20 h 35 m 01s . 2 +60 ◦ 10 09. 4 18 87 614 1017 638 263 2619 0.75 0.25 −0.23 −0.42 28 20h35m05s . 4 +60 ◦ 06 21. 4 16 7 50 160 115 63 395 0.75 0.52 −0.16 −0.29 29 20h35m11s . 5 +60 ◦ 08 57. 8 15 33 194 133 13 2 375 0.71 −0.19 −0.82 −0.73 30 20h35m12s . 7 +60 ◦ 07 31. 416 0 55 8353 9200 1 0.2 −0.22 −0.71 31 20h35m14s . 0 +60 ◦ 05 21. 0 16 15 43 74 55 34 221 0.49 0.26 −0.15 −0.24 32 20 h 35 m 18s . 7 +60 ◦ 10 55. 5 18 32 183 767 445 114 1541 0.7 0.61 −0.27 −0.59 33 20h35m25s . 5 +60 ◦ 09 54. 318 9 221 79 7 2 3180.92 −0.47 −0.84 −0.6 34 20h35m28s . 1 +60 ◦ 09 20. 514 3 221 79 7 0 3100.97 −0.47 −0.84 −1 35 20h35m32s . 4 +60 ◦ 10 17. 9 19 18 68 50 48 11 195 0.57 −0.15 −0.02 −0.63 
M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 
A3, page 7 of 20 
Notes. (1) Number as in Fig. 4; (2), (3) equatorial coordinates; (4) extraction radius in arcsec; (5)−(9) net counts in relevant energy bands (see Sect. 3.1.2), (10) net counts in the total energy band;(11)−(14) hardness ratios (see Sect. 3.1.2). Sources for which spectra weref tted with models (see Sect. 3.2) are listed in boldface. 
residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV −0.01 0 0.010.020.03 0 0.02 0.04 0 5×10−3 0 5×10−3 0.01 0.015 0.02 −0.01 0 0.01 0 0.01 0.02 0.03 0.04 −5×10−3 0 5×10−3 0.010 5×10−3 0.01 0.015 0.02 

Source 3 Source 5 
residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV 
0 0.02 0.04 0.06 −0.01 0 0.01 0 0.01 0.02 0.03 0.04 0 0.01 0.02 0 0.01 0.02 0.03 0.04 −5×10−3 0 5×10−30 0.01 
−0.01 0 0.01 0.02 0.010.015 0.02 
0.512 5 0.51 2 

channel energy (keV) channel energy (keV) Source 6 Source 11 
0.5 1 2 0.512 channel energy (keV) channel energy (keV) 
Source 12 Source 14 
0.5 110 5 
2 
0.5 1 

channel energy (keV) channel energy (keV) Source 16 Source 17 
0.51 2 0.512 5 

channel energy (keV) channel energy (keV) 
Fig. <BR>5. <BR>Model fts to the spectra of selected sources in NGC 6946. See text and Tables 4 and 5. 
A3, page 8 of 20 M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 Table 4. Model-ft parameters for the point sources studied in NGC 6946. 
ID  Model  Internal  kT1  kT2  Photon  χ2 red  Net  
type  nHa  [keV]  [keV]  Index  counts  
3 5  wabs(mekal+wabs*power law) wabs(mekal+mekal)  4.19+2.07 −1.76 –  0.23+0.04 −0.05 0.54 ± 0.09  – 1.93+0.65 −0.32  2.62 ± 0.23 –  0.94 0.80  1368 652  
6  wabs(mekal+wabs*power law)  1.86+0.47 −0.44  0.60+0.11 −0.35  –  3.91+0.61 −0.41  1.04  1524  
11  wabs(mekal+wabs*power law)  1.78+1.66 −0.54  0.38+0.16 −0.08  –  2.48+0.48 −0.21  0.99  1702  
12  wabs(mekal+power law)  –  0.58+0.21 −0.22  –  1.78 ± 0.12  0.91  1077  
14  wabs(mekal+power law)  –  0.46+0.06 −0.08  –  3.12+0.56 −0.91  1.12  929  
16  wabs(mekal+power law)  –  0.38+0.21 −0.06  –  2.03+0.15 −0.13  1.15  1404  
17  wabs(mekal+mekal+wabs*power law)  5.29+2.05 −1.33  0.18 ± 0.02  0.66 ± 0.06  2.31+0.83 −1.04  0.91  3490  
19  wabs(mekal+wabs(mekal+power law))  6.87+1.02 −1.21  0.32+0.02 −0.03  0.70+0.07 −0.06  2.55+0.07 −0.03  1.02  9916  
19b  wabs(mekal+wabs*power law)  2.89+0.31 −0.33  0.62 ± 0.04  –  2.36+0.03 −0.07  1.03  9916  
20  wabs(mekal+power law)  –  0.62+0.08 −0.12  –  1.65+0.12 −0.11  0.90  1234  
21  wabs(mekal+power law)  –  0.45+0.08 −0.06  –  1.52+0.08 −0.07  1.12  2352  
23  wabs(mekal+wabs*power law)  3.29+0.81 −1.05  0.30+0.21 −0.07  –  2.52+0.22 −0.20  1.10  2016  
24  wabs(mekal+wabs*power law)  2.16+0.17 −0.21  0.78 ± 0.05  –  3.80 ± 0.15  1.23  9994  
26  wabs(mekal+mekal+power law)  –  0.40+0.09 −0.03  1.04 ± 0.03  2.26 ± 0.03  1.19  44650  
26c  wabs(mekal+mekal+power law+diskbb)  –  0.66 ± 0.06  1.34+0.32 −0.22  1.98 ± 0.08  1.11  44650  
27  wabs*power law  –  –  –  1.68 ± 0.05  1.05  2619  
32  wabs(mekal+wabs*power law)  8.83+2.15 −1.70  0.25+0.06 −0.05  –  2.82+0.26 −0.17  0.80  1541  

Notes. (a) Column density in [1021 cm−2]. (b) Single temperature model for the thermal component. (c) Model with an additional multicolour disk model component of Tin = 0.26+0.02 keV. ID 19 is the core central source in NGC 6946 and ID 26 is MF16. 
−0.01 

Kajava & Poutanen (2009) and added a multicolour disk component to our model. We obtained a similar value for the tempera-ture of the inner disk. 

3.2.2. Regions of diffuse emission 
To analyse emission of the hot gas from NGC 6946, we used Hα and UV images to choose areas that correspond to the star-forming regions. The radio morphology of the galaxy was also taken into account because the most prominent polarized features were found between the gaseous spiral arms of NGC 6946 (see Fig. 10). All selected regions are presented in Fig. 9.A brief description of all regions is presented in Table 6.For trans-parency, region letters are used throughout this paper. In the pro-cess of extracting the spectra, the emission from point sources (Fig. 4) was excluded. 
To investigate the temperature of the hot gas in selected re-gions of NGC 6946, we ftted a single thermal plasma model, adding a power-law component to account for undetected point sources and/or residual emission from excluded sources. Only regions C and F did not require this additional power-law com-ponent. This could simply be caused by a lower number of net counts in their spectra, resulting in a low signal-to-noise ratio, hence lower accuracy of the ftting, so that the basic models are equally good in ftting the data. On the other hand, both spectra show very little emission above 1 keV, which suggests that the harder emission from point sources contributes hardly anything. 
In Table 7 we present the results of single thermal plasma model ftting. For regions of the spiral galactic arms (regions A, E, G, and H), very steep photon indices of the power-law component are visible, which is unexpected for typical galactic X-ray point sources. This might be due to enhanced emission in the soft-to-medium energy band (around and above 1 keV), however, which can also suggest that a second thermal component is necessary to account for the signifcant emission from the hot gas in the galactic disk. To check this possibility, we ftted a model consisting of two thermal components for the ar-eas of the spiral arms and kept the previously introduced power-law component. Since both parameters and residuals of the new fts were much more physical, that is, showed values in ex-pected ranges, we used them as the fnal fts for the subsequent analysis. 
To ensure that a single thermal plasma model is the best-ft model for the remaining regions (central areas and interarm regions), we also ftted a model with two thermal components to their corresponding spectra. In all cases we obtained significantly fatter (lower) photon indices of the power-law component, which suggests that some of the harder emission from the unresolved point sources was ftted with the new second ther-mal component. Furthermore, most of the ftted parameters were poorly constrained. For some of them it was impossible to get any constraints. The fnal models for all regions are presented in Table 8. 
For regions of the spiral arms for which a model with two thermal components was used, we assumed that the cooler com-ponent (∼0.3 keV) of the hot gas is associated with the galactic halo and the hotter component (∼0.7 keV) with the emission from the disk, as is observed in edge-on galaxies (e.g. Tüllmann et al. 2006). 
A3, page 9 of 20 
residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV 
0 0.01 0.02 0.03 0 0.02 0.04 −0.1 0 0.1 0 0.2 0.4 0.6 0.8 −5×10−3 0 5×10−30.01 0 0.01 0.02 0.03 −5×10−3 0 5×10−3 0.010 0.01 0.02 

Source 20 Source 21 
residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV −5×10−3 0 5×10−3 0 5×10−3 0.01 0.015 0.02 −0.1 0 0.1 0.20 0.2 0.4 0.6 0.8 −0.05 0 0.05 0 0.1 0.2 −0.01 0 0.01 0.020 0.01 0.02 0.03 0.04 
0.51 2 0.512 5 

channel energy (keV) channel energy (keV) Source 23 Source 24 
0.51 2 0.51 2 

channel energy (keV) channel energy (keV) 
Source 26 
Region 26: model with a multicolour disk model component 

0.51 2 0.51 2 channel energy (keV) channel energy (keV) 
Source 27 Source 32 
0.5 110 5 
2 
0.5 110 5 
2 
channel energy (keV) channel energy (keV) 

Fig. <BR>6. <BR>Model fts to the spectra of selected sources in NGC 6946. See text and Tables 4 and 5. 
A3, page 10 of 20 
M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 
Source 19 single temperature model Source 19 
residuals normalized counts/sec/keV 
−0.05 0 0.05 0 0.05 0.1 0.15 

residuals normalized counts/sec/keV 
0 0.05 0 0.05 0.1 0.15 


0.51 2 5 0.512 5 channel energy (keV) channel energy (keV) 
Fig. <BR>7. <BR>Model fts to the spectra of the nuclear region of NGC 6946. See text and Tables 4 and 5. 
Source 26 
residuals normalized counts/sec/keV 
−0.1 0 0.1 0 0.2 0.4 0.6 0.8 
−0.1 0 0.1 0.2 0 0.2 0.4 0.6 0.8 
Region 26: model with a multicolour disk model component 

residuals normalized counts/sec/keV 

0.51 2 channel energy (keV) 

Fig. <BR>8. <BR>Model fts to the spectra of MF16. See text and Tables 4 and 5. 
For the remaining regions, that is, for the central areas and the interarm regions, we assumed that the single thermal component can be described as a mixture of gas components from the disk and the halo above. The parameters of these com-ponents seem to be similar to the level, which does not allow clearly separating them at a given sensitivity level. For the in-terarm regions this can be easily explained by the lack of star-forming regions in the disk, which causes the gas to be relatively uniform throughout the entire volume. Nevertheless, we cannot use this argument for the central regions of the galaxy, where the disk emission is certainly signifcant. A reasonable explanation for this case is a high star-forming activity of NGC 6946 and the consequent internal absorption that is highest in the central densest part of the galactic disk. This absorption may cause some of the disk emission from the central regions I and J to re-main hidden, and the rest, together with the halo gas, mimics a homogenous medium. 
Region B shows almost no Hα or UV emission, while region J includes the central parts of the galaxy. Both regions differ signifcantly in the value of the ftted temperature of the hot gas. It is much hotter (0.60+0.06 keV) for the quiet region 
−0.08 

B than for region J with its clear galactic-disk (nuclear) emission (0.42+0.09 keV). The remaining single thermal component 
−0.05 

model fts show that the temperature of the hot gas is between 
0.5 keV and 0.55 keV. Halo components of the model fts to the regions of spiral arms show a very constant temperature 

0.51 2 channel energy (keV) 

of around 0.28 keV. For the disk components, however, differences are observed, as the south-western and western part of the disk (spiral arms A and H) have a signifcantly lower temperature than the eastern and north-eastern part (spiral arms E and G). 
For all regions except for region H (western spiral arm) most of the X-ray fux is produced by the power-law component that is attributed to unresolved and/or residual emission from point sources. For the exceptional region H we note, however, that the value of the power-law fux is only poorly constrained. Therefore, its value might be much higher, which would lead to a higher contribution to the total fux. A high contribution from the power-law components of the fts might arise because NGC 6946 is a starburst galaxy with a large population of X-ray point sources (Fig. 4). The method of source extraction used in this paper, described in Sect. 2, might certainly cause this ef-fect. However, as argued before, this ensured that as little as possible of the diffuse emission has been lost by point-source extraction. 
For the regions of the spiral arms, more fux comes from the halo components according to the fts, which agrees with a physical picture where halo emission is produced in a much larger volume density of the underlying star formation. These fractions are equal only for the western spiral arm (region H); we discuss this in Sect. 4.2.1 in more detail. 
A3, page 11 of 20 

Table 5. Total (0.3−12 keV) unabsorbed fuxes in 10−14erg cm−2s−1 for modelled point sources in NGC 6946 along with luminosities of their power-law components in 1039 erg s−1. 
ID Mekal cold Mekal hot Power law Total Luminosity 
3 1.5+0.6 – 18.8+6.3 20.3+6.8 1.10+0.37 
−0.8 −4.3 −5.1 −0.25 
5 1.0+0.1 1.1+0.3 – 2.1 ± 0.4 – 
−0.2 −0.2 

6 2.0+0.7 – 41.1+31.3 43.1+32.0 2.41+1.84 
−1.1 −14.0 −15.2 −0.82 
11 0.8+0.9 – 9.7+4.9 10.5+5.8 0.57+0.29 
−0.4 −2.5 −2.9 −0.15 
12 0.3 ± 0.2 – 5.3+1.3 5.6+1.5 0.31+0.08 
−1.2 −1.4 −0.07 

14 2.0+0.8 – 1.3+1.0 3.3+1.1 0.08+0.06 
−0.4 −0.6 −0.7 −0.04 
16 1.2+0.5 – 4.3+1.0 5.5+1.6 0.25+0.06 
−0.4 −0.8 −1.3 −0.05 
17 1.6+0.6 1.6 ± 0.6 25.7+5.2 28.9+6.3 1.51+0.30 
−0.5 −5.8 −6.9 −0.34 
19 4.9+0.6 26.0+15.6 69.6+6.5 100.5+22.8 4.08+0.38 
−0.8 −11.2 −2.9 −14.9 −0.17 
19a 3.6 ± 0.6 – 58.6+5.7 62.2+6.3 3.44+0.33 
−2.4 −3.0 −0.14 

20 0.8 ± 0.2 – 5.6+1.6 6.4+1.7 0.33+0.09 
−1.4 −1.5 −0.08 

21 0.9 ± 0.3 – 11.4+2.1 12.4+2.3 0.67+0.12 
−1.9 −2.2 −0.11 

23 0.6+0.7 – 17.7+5.3 18.3+5.9 1.04+0.31 
−0.4 −3.3 −3.8 −0.19 
24 4.5 ± 0.9 – 108.0+16.7 112.6+17.6 6.33+0.98 
−14.9 −15.9 −0.87 

26 10.5+2.5 14.5+1.7 128.3+4.2 153.3+8.4 7.52+0.25 
−2.0 −1.6 −4.4 −8.0 −0.26 26b 10.2 ± 2.4 9.4+2.3 104.1+14.4 156.2+32.1 8.03+2.05 
−1.4 −16.9 −21.2 −1.76 
27– –14.8+1.4 14.8+1.4 0.87 ± 0.08 
−1.3 −1.3 

32 0.7 ± 0.3 – 36.3+9.3 37.0+9.6 2.13+0.55 
−6.0 −6.2 −0.35 

Notes. (a) Single temperature model for the thermal component. (b) Model with an additional multicolour disk model component with a fux of 32.9+21.4 erg cm−2s−1. ID 19 is the core central source in NGC 6946 and ID 26 is MF16. 
−12.8 × 10−14 


Fig. <BR>9. <BR>Regions of diffuse X-ray emission from NGC 6946 (see text for a detailed description) overlaid on the same maps as in Fig. 4. 
4. Discussion sources we ftted models to the acquired spectra (see Sect. 3.2.1). As mentioned above, all sources except for source 27 required 



4.1. Point sources 
an additional thermal component in the model. This was most likely due to the characteristics of the observations with the Of the 35 point sources found in the galactic disk of NGC 6946, XMM-Newton telescope, that is, a relatively low resolution with for 19 of them we were able to calculate only the hardness a high sensitivity to diffuse X-ray emission. As a result, all ratios. All values are presented in Table 3. For the remaining 
A3, page 12 of 20 
M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 
NGC6946  6cm Polarized Intensity + B-Vectors (VLA+Effelsberg) + H-Alpha 

DECLINATION (J2000) 
60 14 
13 
12 
11 
10 
09 
08 
07 
06 
05 

04 20 35 30 15 00 34 45 30 15 RIGHT ASCENSION (J2000) 

Fig. <BR>10. <BR>Map of radio-polarized intensity at 4.85 GHz (λ 6cm) of NGC 6946 (from Beck 2007). The red lines show the orientation of the magnetic felds. 
Table 6. Regions in NGC 6946 used for the spectral analysis. 
Region Region letter description 
A south-western arm 
B north-western interarm 
C south-western interarm 
D central region w/o UV emission 
E south-eastern arm 
F eastern interarm 
G northeastern arm 
H western arms 
I south-eastern interarm 
J central region with UV emission 

spectra of the studied point sources included signifcant information from the diffuse gas present across the entire disk of NGC 6946. 
For several sources, an additional component to account for internal absorption was needed to obtain a good ft (see Table 4). For three sources, 19, 23, and 32, this was crucial. For source 19, which is the core region of NGC 6946 and therefore not just a point source, this additional absorption is easy to explain be-cause we observe the densest parts of the galaxy. The two other sources, however, are located in areas relatively free of star for-mation (see Fig. 4, left). Furthermore, none of the extended re-gions used for the spectral analysis of the diffuse emission com-ing from the hot gas needed an additional internal absorption component to be described by the model. Therefore, the argument of (relatively) low-resolution observations of a gas-and dust-rich galaxy cannot be used here. Instead, for each source that required an internal absorption component in the model, we 
Table 7. Parameters of single plasma model-fts to the diffuse emission regions studied in NGC 6946. 
Region kT Photon Reduced [keV] index χ2 
A0.53+0.05 2.55+0.26 1.21 
−0.08 −0.17 
B0.60+0.06 1.84 ± 0.22 1.13 
−0.08 
C0.55+0.10 –1.15 
−0.11 
D0.49+0.07 1.78+0.13 0.99 
−0.14 −0.08 
E0.53+0.04 2.31+0.20 1.17 
−0.12 −0.23 


F0.53 ± 0.06 – 1.05 
G0.50+0.02 2.54+0.05 1.35 
−0.03 −0.11 
H0.53+0.08 2.68+0.45 1.24 
−0.03 −0.40 
I0.50+0.14 1.86+0.29 1.07 
−0.13 −0.25 
J0.42+0.09 1.69+0.19 1.01 
−0.05 −0.16 

propose that it is an X-ray binary (or an intermediate-mass black hole, IMBH) surrounded by a dust torus. 
To calculate luminosities of the spectrally analysed point sources, we only used the fuxes of the power-law component to exclude the contribution from the galactic hot gas in the mod-elled spectrum (Table 5). Half of the sources show luminosities higher than 1039 erg s−1. This value is the most widely used ob-servational defnition of an ultra-luminous source (ULX); it is often associated with an accreting IMBH that forms in the core collapse of young dense stellar clusters (e.g. Miller & Hamilton 2002). Since the abundance of ULXs is often linked to recent star formation activity (e.g. Berghea et al. 2013), a signifcant number of ULXs in NGC 6946 agrees well with the vivid star formation of this galaxy. 
One of these sources is the nebula MF 16 (region 26) men-tioned above. Although some of its thermal emission (from both model components) can be associated with the galactic hot gas, as mentioned above, a signifcant contribution from the hotter component needs a different explanation. That the gas tempera-ture exceeds 1 keV (Table 4), which is much higher than the tem<BR>perature of the disk gas, may provide further evidence that MF16 might be indeed a supernova remnant, as previously claimed by Matonick & Fesen (1997), and the very high temperature of the hot gas may result from shock heating of the medium sur-rounding the explosion region. This contradicts the fndings of Berghea & Dudik (2012), who claimed that no signs of shock heating are present. 


4.2. Extended emission 
4.2.1. Parameters of the hot gas 
From our spectral model fts we were able to derive more param-eters of the hot gas, including electron densities ne, masses M, thermal energies th, and cooling times τ. To perform our cal-culations we used the model of thermal cooling and ionization equilibrium of Nulsen et al. (1984), where LX = 1.11 · Λ(T) n2 V η, η is an unknown flling factor and Λ(T) is a cool-
e 3 

ing coefficient of the order of 10−22ergcms−1 for temperatures of a few millions K (Raymond et al. 1976). However, the main difficulty in calculating the physical parameters of the hot gas component are the assumptions about the emitting volume V. 
A3, page 13 of 20 
residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV −0.05 0 0.05 0 0.1 0.2 −0.02 0 0.02 0 0.02 0.04 0.06 0.08 −0.02 0 0.02 0 0.01 0.02 0.03 0.04 0 0.05 0 0.05 0.1 0.15 

Region A Region B 
residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV residuals normalized counts/sec/keV −0.05 0 0.05 0.1 0 0.05 0.1 0.15 0.2 −0.02 0 0.02 0 0.02 0.04 −0.01 0 0.01 0.02 0 0.02 0.04 −0.04−0.02 0 0.020.04 0 0.05 0.1 
0.51 2 
0.5 1 

channel energy (keV) channel energy (keV) Region C Region D 
0.51 2 0.512 channel energy (keV) channel energy (keV) 
Region E Region F 
0.51 2 0.5 1 

channel energy (keV) channel energy (keV) Region G Region H 
0.5 1 2 0.5 channel energy (keV) Fig. <BR>11. <BR>Model fts to the regions of diffuse X-ray emission in NGC 6946. See Tables 8 and 9.  1 channel energy (keV)  2  
A3, page 14 of 20  

M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 Table 8. Final model-ft parameters for the regions studied in NGC 6946. 
Region  Model  kT1  kT2  Photon  χ2 red  Net  
type  [keV]  [keV]  index  counts  
A  wabs(mekal+mekal+power law)  0.28+0.03 −0.04  0.73+0.07 −0.06  1.82+0.36 −0.44  0.96  3512  
B  wabs(mekal+power law)  0.60+0.06 −0.08  –  1.84 ± 0.22  1.13  2516  
C  wabs*mekal  0.55+0.10 −0.11  –  –  1.15  385  
D  wabs(mekal+power law)  0.49+0.07 −0.14  –  1.78+0.13 −0.08  0.99  1581  
E  wabs(mekal+mekal+power law)  0.30+0.05 −0.03  0.80+0.09 −0.14  1.72+0.26 −0.21  0.99  2552  
F  wabs*mekal  0.53 ± 0.06  –  –  1.05  896  
G  wabs(mekal+mekal+power law)  0.27 ± 0.02  0.78 ± 0.06  1.93+0.17 −0.19  1.03  8179  
H  wabs(mekal+mekal+power law)  0.28+0.04 −0.03  0.68+0.07 −0.05  1.59+0.70 −0.88  1.09  5008  
I  wabs(mekal+power law)  0.50+0.14 −0.13  –  1.86+0.29 −0.25  1.07  1211  
J  wabs(mekal+power law)  0.42+0.09 −0.05  –  1.69+0.19 −0.16  1.01  2349  

Notes. (a) Column density in [1021 cm−2]. 
Region I Region J 

channel energy (keV) channel energy (keV) 
It seems straightforward to assume that we only see soft X-ray emission from the visible side of the disk (and therefore the halo), with all emission from the other side being absorbed by the neutral hydrogen in the galactic disk. For the visible part of the halo emission, we assumed a cylindrical volume above the disk of NGC 6946, extending out to half of the D25 diameter of the galaxy (10 kpc). In this geometry, the halo around NGC 6946 would be roughly spherical. This approach seems to be justifed for a starbust galaxy that has signifcantly extended halos of the X-ray emission. For the disk emission we assumed a disk thickness of 1 kpc. For the interarm regions, for which a single ther-mal model was ftted, we used volumes of 10 kpc times the area of a region, as the model describes the mixed emission from both the disk and the halo (see Sect. 3.2.2). 
Tables 10 and 11 present the derived parameters of the hot gas in the areas of diffuse emission in NGC 6946. 
To verify the obtained values, a comparison with earlier Chandra observations of NGC 6946 by Schlegel et al. (2003) would be an important step. Because of the low sensitivity to diffuse emission of these observations, the analysis was unfortunately made only for the entire galactic disk and no detailed study is available. Still, their temperatures of 0.25 ± 0.03 keV and 0.70 ± 0.10 keV for two thermal components agree very well with our values for the halo and the disk gas temperatures, respectively. The electron density of ∼0.012 (× η−0.5)cm−3 de-rived by Schlegel et al. (2003) for the 1 kpc thick disk also matches our results well if we consider a ten times larger vol-ume than used for our calculations. A similar study of six other nearby face-on late-type spiral galaxies was reported by Owen & Warwick (2009), who obtained temperatures of two thermal model fts of 0.2−0.3 keV and 0.6−0.7 keV and the derived elec-tron densities of the gas of the order of a few 10−3(×η−0.5)cm−3, depending on the level of the star-forming activity. 

4.2.2. Hot gas components 
As mentioned before, for the regions of the spiral arms we needed a two-temperature model to account for the emission from the hot gas residing in both galactic disk and the surround-ing halo. Although the temperatures of the hot gas are almost identical for the halo components and similar for the disk com-ponents (where two pairs could be distinguished − A with H and E with G − see Table 8), the derived parameters show signifcant differences (see Table 11). As expected, for the north-eastern spi<BR>ral arm with the brightest Hα and UV emission, marked as region G, we obtained the highest values of number density and energy density of all spiral arms. 
A3, page 15 of 20 

A&A 585, A3 (2016) Table 9. Total (0.3−12 keV) unabsorbed fuxes in 10−14 erg cm−2s−1 for modelled regions in NGC 6946. 
Region Mekal cold Mekal hot Power law Total 
A  3.5+0.8 (0.32) −0.9  2.5+0.8 (0.23) −0.6  4.8+5.1 (0.45) −2.0  10.8+6.7 −3.5  
B  2.4+0.3 (0.22) −0.5  –  8.5+4.0 (0.78) −2.5  10.9+4.4 −2.9  
C  1.1+0.1 (1.00) −0.2  –  –  1.1+0.1 −0.2  
D  1.4+0.2 (0.25) −0.3  –  4.2+1.0 (0.75) −1.1  5.6+1.2 −1.4  
E  2.6±0.9 (0.26)  1.6+0.7 (0.16) −0.6  5.7+3.5 (0.58) −2.2  9.8+5.0 −3.74  
F  2.1+0.1 (1.00) −0.2  –  –  2.1+0.1 −0.2  
G  9.3+1.5 (0.31) −1.4  5.2+1.0 (0.18) −1.3  15.3+5.4 (0.51) −3.3  29.7+7.8 −6.0  
H  6.6+1.9 (0.43) −1.7  6.4+1.5 (0.42) −1.8  2.3+12.8 (0.15) −1.9  15.4+16.0 −5.5  
I  1.2 ± 0.2 (0.30)  –  2.8+1.7 (0.70) −1.1  4.0+1.8 −1.3  
J  2.0 ± 0.5 (0.21)  –  7.5+2.6 (0.79) −1.8  9.5+3.1 −2.3  

Notes. Values in parentheses are fractions of the total fux for a given component. Table 10. Derived parameters of the hot gas in the interarm and central regions of NGC 6946. 
(Mhalo (Ehalo ( halo (τhaloη0.5)a 
Region (nhaloη−0.5)a gas η0.5)a η0.5)a η−0.5)a 
th th 
[10−3 cm−3] [106 M ] [1054 erg] [10−12 erg cm−3] [Myr] 
B  0.84 ± 0.07  5.09+0.37 −0.47  8.74+1.58 −1.87  1.22+0.22 −0.26  1969+98 −13  
C  0.72+0.07 −0.06  2.66+0.26 −0.24  4.20+1.24 −1.14  0.96+0.28 −0.26  2063+388 −277  
D  2.03+0.15 −0.12  1.22+0.09 −0.07  1.71+0.39 −0.56  2.40+0.54 −0.79  662+48 −96  
F  1.22 ± 0.06  3.08+0.15 −0.16  4.67+0.79 −0.74  1.56+0.26 −0.25  1202+139 −84  
I  1.22+0.11 −0.12  1.86+0.16 −0.18  2.66+1.05 −0.88  1.47+0.58 −0.49  1107+325 −146  
J  2.63+0.22 −0.28  1.48+0.12 −0.16  1.78+0.56 −0.38  2.66+0.84 −0.57  480+25 −24  

Notes. (a) η is the volume flling factor. The columns are the region name, electron number density, total gas mass, total thermal energy, thermal energy density, and cooling time. 

4.2.3. Magnetic fields in NGC 6946 
To analyse the magnetic feld parameters we used the same re-gions as for the spectral analysis. For each region both total in-tensity and polarized intensity fuxes at a radio wavelength of 
6.2 cm with a beam of 15 were obtained. Then, using the en-ergy equipartition formula provided by Beck & Krause (2005), we calculated the strengths of both the total and ordered mag-netic felds. The calculations were made assuming a synchrotron spectral index of 1.0, an inclination of the galactic disk of 30◦ , and a proton-to-electron ratio of 100. For the emitting volume a disk of 1 kpc thickness was assumed. The main uncertainties are introduced by the last two parameters. They may vary by a factor of 2. With the assumed spectral index this amounts to an error of ∼30% for the strength of the magnetic feld and ∼60% for its energy density. We note here, however, that such errors are systematic, which means that we may in fact expect the relative uncertainties between the points to be smaller. Table 12 summa-rizes our results and also provides values for the energy densities of the magnetic feld. 
Apart from the central regions of the galaxy (regions D and J), the strength of the total magnetic feld is roughly con-stant across the disk. A slight increase can be observed in the most prominent spiral arms (regions A and G). Consequently, these regions show higher energy densities of the magnetic feld, with the maximum near the galactic core. The strengths of the ordered magnetic feld are also similar in all parts of the disk, with higher values in the areas of the magnetic arms and the central region of the galaxy. As suggested by Fig. 10, the areas of the magnetic arms show a much higher degree of polarization than the other regions. 

4.2.4. Hot gas and magnetic fields of spiral and magnetic arms 
In addition to the grand-design structure of its gaseous spiral arms, NGC 6946 presents a distinct spiral structure of the magnetic felds which resembles magnetic arms that are phaseshifted with regard to the gaseous ones. These magnetic arms coincide well with the interarm regions. Since the spiral arm and interarm regions vary signifcantly in terms of the ISM structure, we investigated the emission from the hot gas in both areas to ob-tain more clues about the interplay of the magnetic feld and the hot plasma. Because a model with two thermal components was used to analyse the emission from the spiral arms (accounting for the disk and halo components), to compare it with the emission from the hot gas in and above the interarm (magnetic arm) areas, we needed to calculate averages of the values obtained from the two-temperature fts. 
A3, page 16 of 20 M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 Table 11. Derived parameters of the hot gas in and above the spiral arm regions of NGC 6946. 
(Mdisk (Edisk ( disk (τhaloη0.5)a 
Region (ndiskη−0.5)a gas η0.5)a η0.5)a η−0.5)a 
th th 
[10−3 cm−3] [106 M ] [1054 erg] [10−12 erg cm−3] [Myr] 
Adisk  4.13+0.52 −0.40  1.14+0.15 −0.11  2.39+0.56 −0.41  7.25+1.69 −1.24  517+47 −34  
Ahalo  1.69+0.15 −0.19  4.68+0.42 −0.54  3.75+0.78 −0.91  1.14+0.24 −0.28  579+12 −10  
Edisk  2.92+0.47 −0.49  1.05+0.17 −0.18  2.41+0.70 −0.76  5.62+1.63 −1.77  815+79 −83  
Ehalo  1.26+0.16 −0.24  4.53+0.56 −0.87  3.89+1.21 −1.06  0.91+0.28 −0.25  809+90 −22  
Gdisk  4.63+0.31 −0.55  2.15+0.14 −0.26  4.79+0.72 −0.90  8.70+1.30 −1.62  498+42 −18  
Ghalo  2.15 ± 0.01  9.96 ± 0.07  7.70+0.63 −0.62  1.40 ± 0.11  448+37 −31  
Hdisk  3.65+0.37 −0.49  3.19+0.32 −0.42  6.21+1.33 −1.22  5.95+1.28 −1.17  524+63 −8  
Hhalo  1.31+0.14 −0.16  11.44+1.22 −1.43  9.18+1.34 −2.01  0.88+0.13 −0.19  752+39 −83  

Notes. (a) η is the volume flling factor. The columns are the region name, electron number density, total gas mass, total thermal energy, thermal energy density, and cooling time. 
Table 12. Properties of the magnetic felds in NGC 6946. 
Region S synch psynch Btot B Bord [mJy/beam] [%] [μG] [10−12 erg cm−3] [μG] 
A  0.67  7.7  17.2 ± 5.2  11.8 ± 7.1  4.9 ± 1.5  
B  0.36  22.6  14.4 ± 4.3  8.3 ± 5.0  7.2 ± 2.2  
C  0.31  26.3  13.8 ± 4.1  7.6 ± 4.6  7.4 ± 2.2  
D  1.74  9.3  21.8 ± 6.5  18.9 ± 11.3  6.8 ± 2.0  
E  0.42  12.7  15.2 ± 4.6  9.1 ± 5.5  5.6 ± 1.7  
F  0.39  16.5  14.8 ± 4.4  8.8 ± 5.3  6.2 ± 1.9  
G  0.54  6.5  16.3 ± 4.9  10.6 ± 6.4  4.2 ± 1.3  
H  0.39  10.8  14.9 ± 4.5  8.9 ± 5.3  5.0 ± 1.5  
I  0.35  20.5  14.3 ± 4.3  8.2 ± 4.9  6.8 ± 2.0  
J  1.40  14.6  20.4 ± 6.1  16.6 ± 10.0  8.1 ± 2.4  

Notes. The columns are the region name, non-thermal radio fux, degree of polarization, total magnetic feld strength, magnetic feld energy, and ordered magnetic feld strength. 
We added gas masses and thermal energies for the appropriate regions. Next, we calculated number and energy densities, taking into account the volumes assumed for the disk and halo component emission (the area of a given region times 1 or 10 kpc, respectively). Our results are presented in Table 13.We compared the averaged values of number and energy densities for all spiral arm regions with respective values for the inter-arm regions. We also calculated the ratios of the thermal energy densities to number densities, hence obtaining an average energy per particle, which is independent of the unknown volume-flling factor (Ep = /n). 
We present our results in Table 14. The interarm regions show higher values of an energy per particle than for the spiral arm regions. This is consistent with the single-temperature fts (Fig. 7), which show slightly higher temperatures for the regions of the magnetic arms. This means that there may be an additional effect that provides thermal energy to the in-terarm regions. Since this additional heating might also be due to magnetic reconnection, we analysed the magnetic feld properties of the areas of the spiral arms and the interarm regions. 

4.2.5. Heating of the gas by magnetic reconnection? 
Because for the interarm regions we have the information about the hot gas coming from both the disk and the above halo (onetemperature ft to the spectra), a direct comparison of the energy densities of disk hot gas and magnetic felds is possible for the regions of the spiral arms alone. Nevertheless, since we are in-terested in the global energy budget of the galaxy, we need in-formation about both thermal and magnetic energy densities for the disk and the halo. Although halo magnetic felds surely ex-ist (as observed in edge-on spiral galaxies), we do not have any direct information on their structure and strength in the case of NGC 6946. The observed radio emission is, however, an inte-gration along the line of sight, that is, we see contributions from both the galaxy disk and halo. Since the majority of the cosmic rays originates in the underlying disk, an assumption for the emitting volume (the disk) seems to be justifed. As the vertical scale height of the halo magnetic felds of ∼6−7 kpc (e.g. Beck 2015) is similar to the assumed size of the hot gas halo (10 kpc), we do not expect a signifcant change of the magnetic energy density in the halo, especially when an uncertainty of its 
A3, page 17 of 20 

A&A 585, A3 (2016) Table 13. Averaged parameters of the hot gas in and above the spiral arm regions of NGC 6946. 
Region (n η−0.5)a (Mgasη0.5)a (Ethη0.5)a ( thη−0.5)a [10−3cm−3] [106 M ] [1054 erg] [10−12 erg cm−3] 
A  1.91+0.19 −0.21  5.82+0.57 −0.66  6.14+1.34 −1.32  1.70+0.37 −0.38  
E  1.41+0.18 −0.27  5.58+0.72 −1.05  6.30+1.91 −1.82  1.34+0.40 −0.39  
G  2.38+0.03 −0.06  12.11+0.21 −0.33  12.49+1.35 −1.51  2.06+0.22 −0.25  
H  1.52+0.16 −0.19  14.63+1.54 −1.85  15.39+2.65 −3.22  1.35+0.23 −0.29  

Notes. (a) η is the volume flling factor. The columns are the region name, electron number density, total gas mass, total thermal energy, and thermal energy density. 
Table 14. Thermal energy per particle and energy densities of the magnetic feld for regions of the spiral and magnetic arms of NGC 6946. 
Spiral arm  Ep  B  Magnetic arm  Ep  B  
A  0.89+0.10 −0.11  11.8 ± 7.1  B  1.45+0.14 −0.15  8.3 ± 5.0  
E  0.95+0.14 −0.12  9.1 ± 5.5  C  1.33+0.23 −0.27  7.6 ± 4.6  
G  0.87+0.08 −0.09  10.6 ± 6.4  F  1.28+0.15 −0.16  8.8 ± 5.3  
H  0.88+0.06 −0.08  8.9 ± 5.3  I  1.20+0.34 −0.31  8.2 ± 4.9  

Notes. Ep − energy per particle in 10−9 erg; B − magnetic energy density in 10−12 erg cm−3. 
calculation (60%) is considered. It is therefore justifed to com-pare the obtained magnetic energy densities with those of the hot 18 gas in and above the interarm regions. 
Still, for all areas of the disk of NGC 6946 we see much 

higher energy densities of the magnetic felds than those of the 
disk component of the hot gas (Tables 11 and 12). Interestingly, for the region of the most prominent spiral arm (region G), con-ditions closest to equilibrium are observed, with the energy den-sity of the magnetic feld only 22% higher than that of the hot gas in the galactic disk. For the remaining spiral arms this difference is as high as 50−63%. If we compare the magnetic feld energy 
densities to those of the halo (Tables 10 and 11)or averaged values for the hot gas in and above the spiral arms (disk+halo, Table 13), a distinct dominance of magnetic felds by a factor of a few is visible. This suggests that only in the areas of high star-forming activity it is possible that the thermal energy density of the gas is similar to that of the local magnetic felds. 
To investigate the interplay between the thermal gas and the magnetic felds in greater detail, we compared the averaged (i.e. from both disk and halo components) thermal energies per par-ticle with the magnetic feld energy densities for the spiral and magnetic arms. We calculated the average values for the gaseous spiral arms and the magnetic arms, which resulted in an energy density of the magnetic feld of about 10.1 × 10−12 erg cm−3 for 
−3 

the spiral arms and 8.2 × 10−12 erg cmfor the interarm re-gions and for energies per particle of 0.90 × 10−9 erg and 1.32 × 10−9 erg, respectively. Our results are presented in Table 14.An anti-correlation between the magnetic feld strength (and its en-ergy) and the thermal energy of the gas is visible (Fig. 13); with a slight decrease of the energy density of the magnetic feld (by 23%), the energy per particle increases signifcantly (by 68%). 
A possible explanation is that in regions that simultaneously show higher thermal energies of the gas and lower en-ergies of the magnetic felds, some of the energy of the mag-netic feld might have been converted into thermal energy by 
-12-3 
ε  [10  erg cm ] 
B
14 
10 

6 
2 
-9
EP [10 erg] 

Fig. <BR>13. <BR>Relation between energy per particle (EP) and energy density of the magnetic feld ( B) in the spiral and the magnetic arms of NGC 6946. Open symbols with dashed error bars present each spiral arm (left side of the plot) and magnetic arm (right side of the plot). Filled symbols with solid error bars present average values of the respective data points. 
magnetic reconnection. Fast reconnection should be possible in most astrophysical plasmas (Hanasz & Lesch 2003), with a heating rate proportional to the Alfvén speed (Lesch & Bender 1990; Lazarian et al. 2015). As the gas density in the interarm regions is lower while the total magnetic feld is almost as strong as in the spiral arms, the Alfvén speed is higher, and hence the heating rate is higher in interarm regions. Indeed, we do observe such an additional heating of the gas in the magnetic arm regions (see Tables 7 and 8). 
In general, such a slight increase in temperature in the inter-arm regions could be easily explained by longer cooling times that are due to the lower density of the gas. However, if we 
A3, page 18 of 20 
M. Wezgowiec et al.: Hot gas and magnetic arms of NGC 6946 
0,8 
0,6 
0,4 
0,2 
-9
EP [10 erg] 

Fig. <BR>14. <BR>Relation between energy per particle (EP) and regularity (Bord/Btot) of the magnetic feld in the spiral and the magnetic arms of NGC 6946. Symbols are the same as used in Fig. 13. 
compare interarm regions B and C with F and I, we note that in magnetic arms B and C higher temperatures, lower number and energy densities than in magnetic arms F and I were ob-tained. Surprisingly, the difference in cooling times reaches al-most a factor of 2. Still, for all four interarm regions practically the same magnetic feld strengths and energy densities were ob-served. The difference is visible, however, when ordered felds are considered – in both regions B and C we see a much higher regularity of the feld (i.e. the ratio of the strengths of ordered and total magnetic feld). This trend is visible in all magnetic arms when compared to the spiral arms – the regularity of the magnetic feld increases with the energy per particle (Fig. 14). 
The above fndings allow constructing a picture of both tur-bulence and reconnection acting in a galactic disk. Although in the spiral arms reconnection effects are expected to be more ef-fcient (stronger feld tangling), their action might be difficult to see because both the heating and feld (dis)ordering is dom-inated by turbulence. In the interarm regions, however, where the magnetic feld is highly ordered, reconnection heating may dominate turbulence heating, and the increase in temperature due to reconnection heating might be noticeable. This is what we observe, especially in the magnetic arms B and C, which have slightly higher temperatures than most star-forming spiral arms. Although reconnection is a very local process, acting at distances of a few pc or less, if it is equally efficient throughout the entire magnetic arm, it might contribute to the feld ordering, an effect that would last longer because of the weaker turbulence. Again, this high feld ordering is most distinctly seen in magnetic arms B and C. 
The region of the western spiral arm (region H) is interesting. While for the other spiral arm regions we observe a significant contribution from the halo component (see Table 9), re<BR>gion H shows almost equal contributions from the halo and disk components. Furthermore, the difference of temperatures of the two components is the lowest in this region, owing mainly to the lowest temperature of all spiral arm disk components. This may suggest that for the western spiral arm mixing of the disk and the halo gas is the most efficient. Since the southern part of region H is in the area of strong Faraday depolarization, as reported by Beck (1991, 2007), this might be a piece of evidence for vertical magnetic felds and enhanced outfow speed in this area of the galactic disk. In particular the region of the south-western spiral 


B /B 
ord tot 
arm (region A), which also contributes to the depolarization area, shows a similar trend for the interplay of the halo and disk gas components, although at a lower level. 


5. Summary and conclusions 
The detailed analysis of the X-ray emission from the hot gas in NGC 6946, together with earlier radio continuum studies, can be summarized as follows: 
− A spectral analysis of the point sources revealed a signif-cant number of ULXs, which agrees with the enhanced star formation of the galaxy. 
− The galaxy presents signifcant emission from the hot gas across its entire star-forming disk. Intensity enhancements are found in the regions of the spiral arms, also in the harder energy band. A signifcant amount of the very soft emission is found in the region of high Faraday depolarization. 
− The radio-polarized emission structure is refected in the spectral properties of the hot gas − areas of magnetic arms visible in the interarm regions are well described with a single thermal plasma model, which shows that the temperature of the hot gas is slightly higher than in the spiral arm regions. 
− An increase in temperature of the hot gas in the magnetic arm regions could be described as additional heating due to magnetic reconnection. 
− A possible conversion of magnetic feld energy into thermal energy of the hot gas in the interarm regions is suggested by the lower energy density and strength of the magnetic feld and the higher thermal energy per particle, when compared to the areas of the spiral arms. 
− In the conditions of low turbulence in the magnetic arm re-gions, reconnection, acting mostly on tangled felds, might also contribute to the feld ordering, as suggested by both the highest temperatures of the hot gas and the highest degree of polarization in magnetic arms B and C. 
− We found signatures of a very hot gas in the area of the ultra-luminous source MF 16, which may suggest shock heating of the gas by a supernova explosion. 
Acknowledgements. We thank Wolfgang Pietsch and Stefania Carpano for their collaboration on the original XMM-Newton observing proposals that form the base of this paper. Special thanks go to Harald Lesch and Alex Lazarian, who improved our understanding of the reconnection theory. We also thank Stefanie Komossa for useful comments on an earlier version of the paper, and the anonymous referee for a helpful report. 

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