New radio continuum study of the large magellanic
cloud supernova remnant N49

Maddie Ghavam, Miroslav D Filipović, Rami Alsaberi, Luke Barnes, Evan J

Crawford, Frank Haberl, Patrick Kavanagh, Pierre Maggi, Jeffrey Payne,
Gavin Rowell, et al.

► To cite this version:

Maddie Ghavam, Miroslav D Filipović, Rami Alsaberi, Luke Barnes, Evan J Crawford, et al. New radio continuum study of the large magellanic cloud supernova remnant N49. Publications of the Astronomical Society of Australia, 2024, 41, pp.e089. 10.1017/pasa.2024.73. insu-04848171

HAL Id: insu-04848171

https://insu.hal.science/insu-04848171v1

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Research Article

# New radio continuum study of the large magellanic cloud supernova remnant N49

Maddie Ghavam¹, Miroslav D. Filipović¹, Rami Alsaberi¹, Luke Barnes¹, Evan J. Crawford¹, Frank Haberl², Patrick Kavanagh³, Pierre Maggi⁴, Jeffrey Payne¹, Gavin Rowell¹,⁵, Sano Hidetoshi⁶, Manami Sasaki⁷, Neda Rajabpour¹, Nicholas Tothill¹ and Dejan Urošević⁸

¹Western Sydney University, Penrith, NSW, Australia, ²Max-Planck-Institut für extraterrestrische Physik, Garching, Germany, ³School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, Ireland, ⁴Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, Strasbourg, France, ⁵School of Physical Sciences, The University of Adelaide, Adelaide, Australia, ⁶Faculty of Engineering, Gifu University, Gifu, Japan, ⁷Dr. Karl Remeis Observatory, Erlangen Centre for Astroparticle Physics, Friedrich-Alexander University Erlangen-Nürnberg, Bamberg, Germany and ⁸Department of Astronomy, Faculty of Mathematics, University of Belgrade, Belgrade, Serbia

## Abstract

We present new Australia Telescope Compact Array (ATCA) radio observations towards N 49, one of the brightest extragalactic supernova remnants (SNRs) located in the Large Magellanic Cloud (LMC). Our new and archival ATCA radio observations were analysed along with *Chandra* X-ray data. These observations show a prominent ‘bullet’ shaped feature beyond the southwestern boundary of the SNR. Both X-ray morphology and radio polarisation analysis support a physical connection of this feature to the SNR. The ‘bullet’ feature’s apparent velocity is estimated at ~1 300 km s⁻¹, based on its distance (~10 pc) from the remnant’s geometric centre and estimated age (~7 600 yr). we estimated the radio spectral index, α = −0.55 ± 0.03 which is typical of middle-age SNRs. Polarisation maps created for N 49 show low to moderate levels of mean fractional polarisation estimated at 7±1% and 10±1% for 5.5 and 9 GHz, respectively. These values are noticeably larger than found in previous studies. Moreover, the mean value for the Faraday rotation of SNR N 49 from combining CABB data is 212±65 rad m⁻² and the maximum value of RM is 591±103 rad m⁻².

**Keywords:** ISM: supernova remnants; (galaxies:) Magellanic Clouds; radio continuum: ISM; ATCA

(Received 10 April 2024; revised 4 August 2024; accepted 10 August 2024)

## 1. Introduction

Observations of supernova remnants (SNRs) place important constraints on star and galaxy formation. SNRs evolve to be relatively bright at radio wavelengths as charged particles are ejected and accelerated by shock waves interacting with interstellar medium (ISM). Radio SNRs provide a pathway to explore cosmic magnetic fields and test models of galaxy evolution (Filipovic & Bozzetto 2017; Filipović & Tothill 2021). They are characterised by non-thermal radio continuum emission (Sturner et al. 1997).

The LMC is among the closest face-on galaxies to the Milky Way. Its distance has been reliably measured at ~50 kpc (di Benedetto 2008). It lies away from the Galactic Plane where extinction is minimal, making the LMC an excellent research laboratory for investigating objects such as SNRs.

In the past decades, hundreds of radio sources have been catalogued in the LMC via radio, X-ray, optical, and IR surveys. Most are classified as either H ii regions, Planetary Nebulae (PNe) or SNRs, appearing at different evolutionary stages (Filipovic et al.

1998b; Bozzetto et al. 2017; Leverenz et al. 2017; Maggi et al. 2016; Leverenz et al. 2016; Bozzetto et al. 2015; Lakićević et al. 2015; Filipović et al. 2009).

N 49 (LHA 120-N 49; DEM L190 or MCSNR J0526–6605) was the first extragalactic SNR discovered, over half a century ago (Mathewson & Healey 1963). It is one of the brightest extragalactic radio SNRs. It is located near the northern boundary of the LMC; centred on RA (J2000) = 05h26m00.1s and Dec (J2000) = −66°05′00.4″ (Bozzetto et al. 2017) and has a diameter of ~18 pc (di Benedetto 2008; Pietrzyński et al. 2019). The Sedov (1959) age of this young to mid-age LMC SNR is estimated to be about 7 600 yr, with explosion energy of $E_0 \sim 1.2 \times 10^{51}$ erg (Leahy 2017).

The morphology of N 49 is somewhat unusual for an SNR. Earlier observations show an asymmetric shell; the east southeastern side of the SNR is several times brighter than the rest of the object (Vancura et al. 1992b; Williams, Chu, & Gruendl 2006; Dickel & Milne 1998). The most likely explanation for this asymmetry is that the blast wave is expanding into a higher density Inter Cloud Medium (ICM), causing the shocked material to appear bright in X-ray, UV, and optical wavelengths (Vancura et al. 1992b) see Fig. 1.

N 49 is an ideal object for scientific studies because it is bright across multiple wavelength windows including X-ray (Park et al. 2003), ultraviolet (UV) (Vancura et al. 1992b), optical (Vancura et al. 1992a), infrared (Williams et al. 2006), and radio (Dickel & Milne 1998). Despite having a large amount of data, several key

**Corresponding author:** Maddie Ghavam, Email: 18534030@student.westernsydney.edu.au.

**Cite this article:** Ghavam M, Filipović MD, Alsaberi R, Barnes L, Crawford EJ, Haberl F, Kavanagh P, Maggi P, Payne J, Rowell G, Hidetoshi S, Sasaki M, Rajabpour N, Tothill N and Urošević D. (2024) New radio continuum study of the large magellanic cloud supernova remnant N49. *Publications of the Astronomical Society of Australia* **41**, e089, 1–12.
https://doi.org/10.1017/pasa.2024.73
<figure><img src="image_2.png" /><figcaption>**Figure 1.** Combined RGB map of N 49 where Red is radio (5.5 GHz ATCA), Green is optical (HST) and Blue is X-ray (Chandra).</figcaption></figure>

features remain poorly studied. Additionally, their interpretation remains controversial, including a 'bullet' feature in the south-west side of the SNR and a Soft Gamma Repeater (SGR) in the north.

Studies using CO data, provide evidence that N 49 is interacting with a nearby cloud located to the southeast with a tracer of cold molecular hydrogen gas (Yamane 2018; Sano et al. 2023). High-excitation optical iron emission lines indicate substantial dust grain destruction occurring in this region (Dopita et al. 2016). Cluster searches in γ-ray images reveal high energy photons originating from hadronic processesª through interactions with dense H ii regions (Campana et al. 2022).

Chandra observations show metal-rich ejecta at both the centre and periphery of N 49 (Park et al. 2003, 2012). Beyond the southwestern boundary and towards the eastern boundary are two metal-rich 'bullet' features (also known in the literature as shrapnel or knots) detected in earlier radio and X-ray studies (Dickel & Milne 1998). The southwestern bullet is an extended feature with a head (~4'' in radius or 23 pc at 50 kpc) and a tail that connects to the main SNR shell (Fig. 4). Spectral analysis of the head region indicates Silicon (Si) and Sulphur (S) enhancement most likely caused by multiple evolutionary phases. The enhanced Si lines in the eastern boundary suggest another ejecta-rich region (Park et al. 2012). In general, earlier morphological studies based on radio data (e.g. Dickel&Milne 1998) show similarity to later X-ray studies (Park et al. 2003).

There has been controversy regarding N 49's thermonuclear versus core-collapse origin. Park et al. (2012) argued that the observed Si/S ratio in the ejecta suggests a thermonuclear (type

Ia) origin. Other results seem to imply a core-collapse origin. For example, the recombining plasma (RP) state of N 49 determined from Suzaku observations appears consistent with a core-collapse model from a massive star (Uchida, Koyama, & Yamaguchi 2015). In this scenario, shocks travelled through a dense circumstellar medium created by a massive progenitor. The high radio brightness of N 49 also suggests a core-collapse origin, since the radio luminosity of a thermonuclear SNR is somewhat less (Bozzetto et al. 2017, their fig. 16).

X-ray observations show that the point source SGR 0526−66 (PSR B0525−66) is located in the middle of the northern part of N 49. This particular SGR is only one of two known magnetars in the LMC (Park et al. 2004; Badenes et al. 2009; Imbrogno et al. 2023) The position of this SGR is RA (J2000) = 05h26m00.7s and Dec (J2000) = −66°04′35.0″ and its age has been estimated to ~1 900 yr (Park et al. 2012; Vink&Kuiper 2006). The close proximity of SGR 0526−66 would normally be sufficient evidence to classify N 49 as a core-collapse SNR (Badenes et al. 2009). However, stars more massive than 21.5 M☉ are very scarce near N 49, implying that either SGR 0526−66 came from a progenitor with a mass below 30 M☉ (Hill et al. 1995) or that the magnetar is merely a chance projection along the line of sight. Support for the latter is found in Dickel et al. (1995). They note the location and spectral indices of the X-ray hot spots of N 49 and SGR 0526−66 are probably not related. Further, Gaensler et al. (2001) suse radio observations of N 49 and SGR 0526−66 to conclude that existing claims of associations between the two are implausible.

Motivated by previous studies and a desire to understand N 49's features, we obtained new ATCA radio observations at 2.1, 5.5, and 9 GHz to create higher resolution and more sensitive

<footnote>ªProcesses involving particles made up of quarks and subject to the strong force.</footnote>
<table><caption>**Table 1.** Details of ATCA Observations of SNR N 49 used in this study. Source 1934–638 was used as a primary (bandpass and flux density) calibrator in all observations.</caption><thead><tr><th>Observing</th><th>Project</th><th>Frequency</th><th>Array</th><th>Integration Time</th><th>Bandwidth</th><th>Phase</th><th>Reference</th></tr><tr><th>Date</th><th>Code</th><th>(GHz)</th><th>Config.</th><th>(minutes)</th><th>(MHz)</th><th></th><th></th></tr></thead><tbody><tr><td>1992 Apr 23</td><td>C177</td><td>2.4</td><td>6C</td><td>523.3</td><td>128</td><td>0407–658</td><td>Dickel et al. (1995)</td></tr><tr><td>1992 Jun 5</td><td>C177</td><td>2.4</td><td>1.5D</td><td>401.1</td><td>128</td><td>0407–658</td><td>Dickel et al. (1995)</td></tr><tr><td>1992 Jun 17</td><td>C177</td><td>2.4</td><td>1.5B</td><td>347</td><td>128</td><td>0407–658</td><td>Dickel et al. (1995)</td></tr><tr><td>1993 Jul 19</td><td>C177</td><td>4.5,6</td><td>6C</td><td>361.2</td><td>128</td><td>0454–810</td><td>Dickel & Milne (1998)</td></tr><tr><td>1993 Aug 27</td><td>C177</td><td>4.79, 8.64</td><td>1.5B</td><td>528.2</td><td>128</td><td>0454–810</td><td>Dickel & Milne (1998)</td></tr><tr><td>1993 Oct 12</td><td>C177</td><td>4.79, 8.64</td><td>1.5D</td><td>700.5</td><td>128</td><td>0454–810</td><td>Dickel & Milne (1998)</td></tr><tr><td>1994 Oct 20</td><td>C177</td><td>4.79, 8.64</td><td>750C</td><td>719.2</td><td>128</td><td>0454–810</td><td>Dickel & Milne (1998)</td></tr><tr><td>1994 Nov 26</td><td>C177</td><td>4.79, 8.64</td><td>375</td><td>607.7</td><td>128</td><td>0454–810</td><td>Dickel & Milne (1998)</td></tr><tr><td>1996 Jul 5</td><td>C520</td><td>4.8, 8.64</td><td>6C</td><td>483.0</td><td>128</td><td>0515–674</td><td>Fender et al. (1998)</td></tr><tr><td>1996 Jul 7</td><td>C520</td><td>4.8, 8.64</td><td>6C</td><td>106</td><td>128</td><td>0515–674</td><td>Fender et al. (1998)</td></tr><tr><td>2019 Nov 30</td><td>C3275</td><td>2.1, 5.5, 9</td><td>1.5C</td><td>21.6</td><td>2048</td><td>0530–727</td><td>This work</td></tr><tr><td>2020 Jan 2</td><td>CX454</td><td>5.5, 9</td><td>1.5C</td><td>201</td><td>2048</td><td>0530–727</td><td>This work</td></tr><tr><td>2020 Feb 10</td><td>CX459</td><td>5.5, 9</td><td>6A</td><td>198</td><td>2048</td><td>0530–727</td><td>This work</td></tr><tr><td>2020 Feb 23</td><td>C3292</td><td>2.1, 5.5, 9</td><td>EW367</td><td>150</td><td>2048</td><td>0530–727</td><td>This work</td></tr></tbody></table>

images. We also use this data to construct polarisation maps to understand its magnetic fields better. Data and reduction techniques are presented in Section 2, results in Section 3, and a discussion in Section 4. Finally, conclusions and future prospects are presented in Section 5.

## 2. Observational data and reductions

### 2.1. Radio data

Our new ATCA observations of N 49 were performed in 30 November 2019, 2 January, 10 February 2020, and 23 February 2020 (project codes C3275, CX454, CX459, and C3292). These observations utilised a frequency switching mode (between 2 100 MHz and 5 500/9 000 MHz) in 6A, 1.5C, and EW367 configurations. Observations were carried out in ‘snap-shot’ mode, with 1-h integrations over a 12-h period minimum, using the Compact Array Broadband Backend (CABB) (2 048 MHz bandwidth) centred at wavelengths of 3/6 cm$^b$ and 13 cm ($v=2$ 100 MHz).

Our data reductions also used available ATCA archival observations from the Australia Telescope National Facility (ATNF) online archive.$^c$ Two different data sets were combined for analysis. The first was before the CABB upgrade from project C177 (pre-CABB; 1990s, with 128-MHz bandwidth) and included observations at Intermediate frequencies (IFS) 2.4, 4.5, 4.79, 6, and 8.64 GHz (Dickel et al. 1995; Dickel & Milne 1998). As the remnant is so evolved combining data from 25 yr will not introduce errors. The second data set, C520 (pre-CABB), includes observations at IFS 4.79 and 8.64 GHz (Fender, Southwell, & Tzioumis 1998). Each 128 MHz-wide frequency band was correlated in 33 separate channels of equal width. Details of these observations are listed in Table 1.

<table><caption>**Table 2.** Details of CABB and pre-CABB radio continuum N 49 images created and used in this study.</caption><thead><tr><th>Frequency<br>(GHz)</th><th>Beam size<br>(arcsec)</th><th>RMS<br>(mJy beam<sup>-1</sup>)</th><th>S<sub>v</sub><br>(Jy)</th><th>Note</th></tr></thead><tbody><tr><td>2.1</td><td>4" × 4"</td><td>0.128</td><td>1.09</td><td>CABB</td></tr><tr><td>2.4</td><td>8.9" × 6.6"</td><td>0.100</td><td>0.930</td><td>pre-CABB</td></tr><tr><td>4.79</td><td>5" × 5"</td><td>0.067</td><td>0.838</td><td>pre-CABB</td></tr><tr><td>5.5</td><td>5" × 5"</td><td>0.055</td><td>1.02</td><td>CABB</td></tr><tr><td>8.64</td><td>5" × 5"</td><td>0.042</td><td>0.651</td><td>pre-CABB</td></tr><tr><td>9.0</td><td>4" × 4"</td><td>0.064</td><td>0.30</td><td>CABB</td></tr></tbody></table>

Data reduction and imaging were performed using the MIRIAD$^d$ (Sault, Teuben, & Wright 1995), KARMA$^e$ (Gooch 1995), and DS9$^f$ (Joye & Mandel 2003) packages. We measured N 49 flux densities (Table 2) as described in Hurley-Walker et al. (2019, Section 2.4) and Filipović et al. (2022), Bozzetto et al. (2023).

To obtain the 5.5 and 9 GHz frequency images, four sets (‘12-h days’) of observational data (projects C3275, CX454, CX459, and C3292) were combined. In all cases, 1934–638 was used as the standard bandpass and flux density calibrator while the phase calibrator was 0530–727. Automated task PGFLAG was used to flag errors in the data; tasks BLFLAG and UVFLAG were used for minor manual flagging. A robust weighting of 0.5 created the best radio images at 5.5 and 9 GHz.

Likewise, to create the 2.1 GHz image, two observational sets (days) of data were combined from projects C3275 and C3292. Two array configurations were available: 1.5C and 6A. Imaging processing was similar to that used above for the 5.5 and 9 GHz images. Fig. 2 shows total intensity images at 2.1, 5.5, and 9 GHz, respectively.

<footnote>$^b$ $v=4$ 500–6 500 and 8 000–10 000 MHz; centred at 5500 and 9000 MHz, respectively</footnote>

<footnote>$^c$ https://atoa.atnf.csiro.au.</footnote>

<footnote>$^d$ http://www.atnf.csiro.au/computing/software/miriad/.</footnote>

<footnote>$^e$ http://www.atnf.csiro.au/computing/software/karma/.</footnote>

<footnote>$^f$ https://sites.google.com/cfa.harvard.edu/saoimageds9.</footnote>
<figure><img src="image_3.png" /><figcaption>**Figure 2.** CABB radio continuum images of SNR N 49. 5.5 GHz contour levels overlaid on each of the 3 images are 1, 2, 3, 4, and 5 mJy beam⁻¹. **Left:** 2.1 GHz image with a resolution (beam size) of 4" × 4" **Middle:** 5.5 GHz image with a resolution (beam size) of 5" × 5" **Right:** 9 GHz image with a resolution (beam size) of 4" × 4". White circles in the lower left corner scale the synthesised beam.</figcaption></figure>

<figure><img src="image_4.png" /><figcaption>**Figure 3.** Pre-CABB update radio continuum images of SNR N 49. 4.79 GHz contour levels overlaid on each of the 3 images are 0.85, 1.5, 2.5, 3.5, and 4.5 mJy beam⁻¹. **Left:** 2.4 GHz image with a resolution (beam size) of 8.9" × 6.6". **Middle:** 4.79 GHz image with a resolution (beam size) of 5" × 5". **Right:** 8.64 GHz image with a resolution (beam size) of 5" × 5". White circles in the lower left corner scale the synthesised beam.</figcaption></figure>

To compare new CABB data with pre-CABB upgrade observations, three sets of pre-CABB data (project C177) were combined to obtain a 2.4 GHz frequency image of N 49. Array configurations at this frequency included 1.5B, 1.5D, and 6C. Again, a robust weighting of 0.5 created the best radio images. The MIRIAD task SELFCAL was also applied to perform self-calibration of the visibility data (Briggs 1995). Phase SELFCAL was performed 3 times which improved image resolution compared to the previous work of Dickel et al. (1995).

To obtain 4.79 and 8.64 GHz images, data from projects C177 and C520 utilising configurations 1.5B, 1.5D, 6C, 750C, and 375 were all combined for their respective frequencies. A robust weighting of -0.5 was used for 4.79 GHz and 0.5 for 8.64 GHz image reduction. The resolution of both 4.79 and 8.64 GHz images were smoothed to 5" × 5" using the MIRIAD task INVERT. Tasks PMOSMEM and RESTOR created the resulting convolved mosaic images. Integrated N 49 flux densities at 4.79 and 8.64 GHz are 0.838 ± 0.1 Jy and 0.651 ± 0.1 Jy, respectively. Most of the uncertainties reported are systematic due to calibration and statistical fluctuations.

Fig. 3 shows the total intensity of pre-CABB images at 2.4, 4.79, and 8.64 GHz. Details of the images used in this study are listed in Table 2.

### 2.1.1. Polarimetry

SNR polarimetry can provide details on the intensity of the polarised emission, polarisation degree, and magnetic field orientation. Moreover, SNRs magnetic fields play a significant role in the cosmic ray acceleration mechanism (Reynoso, Velázquez, & Cichowolski 2018) By combining radio with X-ray data, the strength of the actual magnetic field can be determined (Dubner 2011).

Polarisation maps can be created from full Stokes parameters, including I, Q, U, and V data that describe multiple wave components (Robishaw & Heiles 2018 and Burke & Graham-Smith 1997).

Formally, the linear polarisation state of a radio wave as an observable quantity can be described as

$$P = Q + iU = pIe^{2i\chi} \qquad (1)$$

where I is the flux density of the radio emission (in units of Jy beam⁻¹), p the linear fractional polarisation, and χ the observed position angle of the radio wave given by:

$$\chi = \frac{1}{2} \tan^{-1} \left( \frac{U}{Q} \right). \qquad (2)$$
<figure><img src="image_5.png" /><figcaption>Figure 4. An X-ray three-colour image of N 49 that shows our new Radio data superimposed as contours. Red represents the energy band 0.5–1.2 keV (soft), green corresponds to the energy band 1.2–2.0 keV (Medium) and blue represents the energy band 2.0–7.0 keV (hard). This X-ray image is overlaid with 5.5 GHz radio contours at 0.25, 1.4, 2.6, 3.8, and 5 mJy beam⁻¹. The distance between SNR centre to the ‘bullet’ feature is used to estimate the upper and lower angular displacement values as explained in Table 3.</figcaption></figure>

Our polarised intensity maps produced by the vector combination of the Stokes Q and U maps were statistically corrected for bias using the MIRIAD task IMPOL. The mean fractional polarisation has been evaluated in two ways: (1) by dividing the polarised intensity map by the total intensity map, determined as a mean ratio, and (2) by dividing the integrated polarised intensity of the source by the integrated total intensity.IMPOL was used to calculate the Stokes I, Q, and U parameters, from which were derived the polarised emission, position angle, and resultant uncertainty maps (Equations 1 and 2).

Whenever an electromagnetic wave passes through magnetised plasma or magneto-ionic material, the polarisation angle of the wave is rotated from its intrinsic value ($\chi_0$), due to the different phase velocities of the two opposite-hand polarisation modes. This effect is known as Faraday rotation. For an astronomical radio source, the total observed Faraday rotation along the line of sight can be estimated from the variation of the position angle with respect to the observing wavelength, $\Delta\chi/\Delta\chi_{obs}^2$. This quantity is known as rotation measure (RM).

The measured change in position angle of radiation, $\Delta\chi$, for an electromagnetic wave arriving at an observer, assuming a single magnetic field with only one source along the line of sight and no internal Faraday rotation or beam depolarisation is defined as:

$$ \Delta\chi = \chi_{\text{obs}} - \chi_0 = RM\lambda_{\text{obs}}^2, \quad (3) $$

where $\chi_{obs}$ and $\chi_0$ (rotation angle of the source) are in radians and the wavelength of the observed radiation, $\lambda_{obs}$, in metres.

Using the assumptions above and the equation for Faraday depth, the RM (rad m⁻²) can be normalised to physical parameters:

$$ RM = 0.81 \int_{0(\text{source})}^{L(\text{observer})} n_e B_{\parallel} dl, \quad (4) $$

where $n_e$ is the number density of thermal electrons (in units of cm⁻³), $B_{\parallel}$ is the magnetic field component in the direction of the line of sight to the source (in µG), and $l$ is the displacement (in pc) between the source and observer. Equation (4) indicates that the RM represents a relation between the observed position angle, $\chi_{obs}$, and the magneto-ionic properties of plasma in radio sources. (Burn 1966).

To determine the RM and the true orientation of the magnetic field (B), observations at two or more frequencies are required. This is to resolve a degeneracy of the unknown number of half cycles of rotations of the position angle between the source and observer; that is, the measurements of the position angles are uncertain by $\pm n\pi$. More details on how to remove this ambiguity and determine an accurate rotation measure by careful selection of observational wavelengths can be found in Clarke (2004). However, one still can argue that the entire source cannot be described by a single RM (O’Sullivan et al. 2012).

The MIRIAD task IMRM fits the position angle image vectors from at least two position angle images up to five different frequencies on a pixel-by-pixel basis. In the same process, the task computes the unrotated angle $\chi_0$. In this study, we used combined images at 5.5 and 9 GHz (CABB images) to obtain a reasonable RM estimate.

There was no reliable evidence of polarisation emission at 2.1 GHz image, most likely, because the depolarisation at these frequencies is caused by Faraday rotation. MIRIAD task UVSPLIT was used to break these wide-band frequencies (2.048 GHz) into two narrower bands, each with a maximum bandwidth of 1 GHz. The cumulative effect of these four smaller frequencies can help identify the overall trend more accurately and reduce the ambiguity in the RM calculation. While using only two broadband frequencies leads to ambiguities due to the periodic nature of the polarisation angle, splitting these into smaller frequencies can help mitigate but not fully resolve these ambiguities. Each additional frequency provides more data points, improving the fit and potentially identifying the correct RM. In all four bands, we only calculated RM when the signal-to-noise ratio was at least 10σ. Furthermore, ~10% error is due to the $n\pi$ ambiguity in measurements of the position angle (Brentjens & de Bruyn 2005) as we use four bands in our RM estimation.

## 2.2. X-Ray data

Park et al. (2012) presented an X-ray study on N 49 using the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. The SNR was observed on 18 July 2009 and 19 September 2009 (ObsIDs 1023, 10806, 10807, and 10808) during AO10. To compare these with our new radio data, we re-processed the original X-ray data using the CIAO v4.9 software package with CALDB v4.7.6 (Fruscione et al. 2006). The merge-obs<fnref n="8" /> and chandra-repro<fnref n="9" /> scripts (Fruscione et al. 2006) were used to create the combined energy-filtered and exposure-corrected images. The total effective exposure time after data reduction is ~108 ksec which matches the effective exposure time of the original reduced image stated in Park et al. (2012). The reduced three-colour (RGB) X-ray image of the soft (0.5–1.2 keV), medium (1.2–2.0 keV), and hard (2.0–7.0 keV) energy bands is presented in Fig. 4.

<footnote n="8">⁸http://cxc.harvard.edu/ciao/ahelp/mergeobs.html.</footnote>

<footnote n="9">⁹http://cxc.harvard.edu/ciao/ahelp/chandra_repro.html.</footnote>
## 2.3. Optical data

Optical HST images (Hα, [S ii], and [O iii]) were downloaded from the Mikulski Archive for Space Telescopes.<fnref n="1" /> All information regarding these HST observations and their data reduction are given in Bilikova et al. (2007). These data have been used to create our optical images in this study.

# 3. Results and analysis

## 3.1. Morphology

Fig. 4 shows the three-colour *Chandra* ACIS image of N 49 where complex and asymmetric X-ray emission features are evident. It is evident from the RGB image that the softest X-rays are significantly inside the SNR. The outer boundary of the N 49 shell exhibits extensive regions of green and blue, which are notably harder. In most cases, the outer shock tends to be harder compared to the reverse shock within the ejected material (Leahy, Ranasinghe, & Gelowitz 2020). Two metal-rich ejecta as suggested by Park et al. (2012) have been detected: one towards the southwest and another, less obvious one (not studied here) towards the east to northeast. The western (to southwestern) half of N 49 is dominated by hard X-rays, which indicates the blast wave is expanding into low-density ISM. Our radio data also suggest this. Uchida et al. (2015) noted that the X-ray images of N 49 show an irregular morphology that is brightest inside the radio shell, as is a typical characteristic of a mixed morphology SNR. Also, optical images suggest an outflow pointing up to the north direction, which could be indicative of some asymmetry in the progenitor SN event.

In Fig. 4, Using a method by<fnref n="1" /> Collischon et al. (2021),s we estimated the geometrical centre of the N 49 radio image as RA (J2000) = 05h25m59.2s and Dec (J2000) = -66°04'59.6". We note there is a soft gamma repeater, SGR 0526-66, positioned at RA (J2000) = 05h26m00.9s and Dec (J2000) = -66°04'31.6".

The hard X-ray knot in the southwestern part of N 49, beyond the remnant's shock boundary has been called the 'bullet' and is located at RA (J2000) = 05h25m52.4s and Dec (J2000) = -66°05'14.7". This feature has emission lines that dominate the knot's X-ray spectrum which can be modelled by a metal-rich hot thermal plasma (Park et al. 2003). Based on this result, it appears it was created by ejected fragments from the SN explosion that produced N 49. Additionally, there is evidence of a weak trail behind the head of the bullet (Park et al. 2003).

Park et al. (2003) notes strong Si enhancement in the eastern region of the remnant corresponding to an internal cloud (area of a low density region between clouds of interstellar material within N 49) which resembles the spectral properties of the head of the 'bullet'. This region may be a candidate ejecta feature (positioned at RA (J2000) = 05h25m52.2s and Dec (J2000) = -66°05'16.7"), probably isolated from the complex emission due to shocked dense clumpy clouds (Park et al. 2003).

### 3.1.1. The 'Bullet's' Muzzle (kinetic) energy

N 49 exhibits features rarely seen in SNRs of similar age and type. Most prominent is the X-ray ejecta 'bullet' (Fig. 4) extending beyond the remnant's shell in the southwest. This feature has predominantly hard emission (2.0-7.0 keV), as shown in blue.

<table><caption>**Table 3.** N 49 kick velocity estimate. Upper and lower angular displacement values were estimated using the SNR centre as an upper limit, and the 'midpoint' as the lower limit (see Fig. 4). We assume a distance to the LMC of 50 kpc to calculate the physical displacement and an SNR age of 7 600 yr to calculate the kick velocity.</caption><thead><tr><th>Object</th><th>Measured angle<br>(degree)</th><th>Displacement<br>(parsec)</th><th>Kick velocity<br>(km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>Bullet</td><td>75<sup>+0.97</sup><sub>-0.97</sub></td><td>10.4<sup>+0.53</sup><sub>-0.53</sub></td><td>1 300<sup>+66.4</sup><sub>-66.4</sub></td></tr></tbody></table>

Outer shell-like X-ray features in N 49 are largely coincident with radio shell contours as seen in Fig. 4, most likely indicating regions of blast wave shock. In fact, hard X-ray emission is reasonably correlated with radio and appears to peak towards the southeast edge.

The average velocity of the 'bullet' has been estimated at ~1 300 km s⁻<fnref n="1" />, assuming its distance to the SNR centre of ~10 pc and remnant age of 7 600 yr (Leahy 2017). The 'bullet' displacement and the measured angle indicate how far and in which direction the SNR's centre might have shifted over time. In this case, we note the SN explosion centre of N 49 inferred from the projection of the southwest 'bullet' trail is shifted the geometrical centre by ~10.4 pc, and forming an angle of ~75° with the initial centre.

The high temperature and large ionisation timescale of this bright X-ray knot support its origin as a high-speed (bow-shock) ejecta. As the SNR encounters regions of varying density in the ISM, these interactions contribute to the asymmetrical shape that leads to a bow shock. After the SNR expands and interacts with the surrounding ISM, influenced by factors such as relative motion and ISM density variations, a bow shock can eventually develop.

In an SNR with a density gradient in the surrounding ISM, the centre of the remnant is positioned towards the high-density emission. This occurs because the shock wave decelerates more in the denser region, leading to an asymmetrical expansion and accumulation of material on the high-density side. The side facing the denser medium appears more compressed, while the side facing the lower-density medium is more extended, all resulting in the different geometric and mass centres of the SNR (Janka et al. 2012).

To constrain the knot's precise origin is difficult since the original supernova (SN) might neither be in the geometrical centre (although still possible) nor at the 'midpoint'. Bearing this in mind, we estimate a somewhat crude 'bullet' kinetic energy, $E_K$, assuming a pre-shock density, as measured by Park et al. (2012), of 2 cm⁻³ with an increase by a factor of 4 assumed for the post-shock region. We estimate the 'bullet' volume using our *Chandra* image, assuming an ellipsoid with semi-minor and semi-major axes of 3" and 5", respectively. Combined with the velocity estimates listed in Table 3, this gives a possible $E_K$ range of 0.3–5×10⁴⁹ erg, or a fraction to a few per cent of the total SN energy. Our mass estimate is likely an upper limit assuming a filling fraction less than 1 or a non-uniform density profile (i.e. not a monolithic 'bullet'). The kinetic energy uncertainty budget is dominated by the poorly constrained velocity as it enters the calculation squared. Although large, our crude $E_K$ is similar to that estimated for the jet of Cas A (Willingale et al. 2003; Orlando et al. 2016). On the other hand, this is more than measured for 'shrapnel' from the Vela SNR (García et al. 2017).

<footnote n="1">¹https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.</footnote>

<footnote n="1">¹https://github.com/ccollischon/banana.</footnote>
<figure><img src="image_6.png" /><figcaption>**Figure 5.** The polarisation map of N 49 at 5.5 GHz (left column) and at 9 GHz (right column) where respective fractional polarisation vectors shown on the top images are overlaid on corresponding intensity ATCA images. The blue circles in the lower left corner represent a synthesised beam of 5'' × 5'' and 4'' × 4'', for 5.5 and 9 GHz, respectively. The blue line below the circles represents 100% polarisation. The bar on the right side represents the greyscale intensity gradients for the ATCA images in Jy beam⁻¹. Polarisation intensity maps at 5.5 GHz (bottom left) and at 9 GHz (bottom right) are shown in the bottom images with radio intensity contour lines overlaid; radio contours are 0.05, 1, 2, 4, and 6 mJy beam⁻¹ for 5.5 and 9 GHz, respectively.</figcaption></figure>

<figure><img src="image_7.png" /><figcaption>**Figure 6.** Fractional polarisation vectors overlaid on their corresponding ATCA intensity images. The image on the left is at 4.79 GHz (pre-CABB), large green ellipse in these images indicates an enhanced polarisation region around the proposed 'bullet ejecta' or bow-shock PWN. The image on the right is at 8.64 GHz (pre-CABB). The blue circle in the lower left corner of this image represents the synthesised beam width of 5'' × 5'' and the blue line below, a fractional polarisation vector of 100%.</figcaption></figure>
<figure><img src="image_8.png" /><figcaption>**Figure 7.** The rotation measure map (left) of N 49 overlaid on 5.5 GHz image. The pink boxes represent RM values estimated from the position angles associated with linear polarisation. The maximum value of RM is ~591 rad m⁻². The blue ellipse in the lower left corner represents the synthesised beam width of 5′ × 5′. The image on the right shows magnetic field vectors overlaying the 5.5 GHz radio image.</figcaption></figure>

What alternative scenario could explain the ‘bullet’? Its morphology could suggest a bow-shock Pulsar Wind Nebulae (PWN) origin. The main difference would be that a bow-shock PWN would not be expected to have such strong Si and S lines, as seen in the X-ray spectrum (Park et al. 2012). While a PWN origin is unlikely, one way to distinguish such a scenario is through high-resolution and high-sensitivity radio observations that measure the change in the spectral index within this region. Specifically, a more flat spectral index (−0.3α0) would favour a PWN origin, while a steeper index (α − 0.5) would point towards a SN explosion origin. In Fig. 8 we can see some flattening of the spectral index (−0.45α − 0.35), compared to the rest of the remnant. But, this spectral index range falls into the ‘grey’ area where neither scenario can be favoured.

Several galactic SNRs are characterised by knot-like ejecta, and such clumps have been observed in both major types of SNe. Examples include the Tycho SNR as type Ia (Yamaguchi et al. 2017), and Cas A, G292.0+1.8, Puppis A and big-Vela as core-collapse (García et al. 2017). These Galactic SNRs exhibit a large range of ages – from a few hundred to tens of thousands of years old. Knots from ejecta have been detected beyond the main shock in big-Vela (DeLaney et al. 2010) and Tycho (Yamaguchi et al. 2017). Also, supersonic speeds in either bow-shock PWN or ‘bullets’ are not unusual, as is documented in several studies (Kargaltsev et al. 2017, see their table 1). X-ray morphology and radio polarisation indicate a strong physical connection of this feature to the SNR similar to many known Galactic SNR such as Vela and Cas A.

**3.2. Polarisation and Faraday rotation**

Polarisation fraction and Faraday rotation provide powerful trac-
ers of magnetic field orientation and strength.

In Fig. 5 we show fractional polarisation vectors and polari-
sation intensity maps at 5.5 and 9 GHz. Fractional polarisation
vectors for pre-CABB update images at 4.79 and 8.64 GHz are
shown in Fig. 6. We did not detect reliable polarisation emis-
sions at 2.1 and 2.4 GHz. This is likely a result of depolarisation

induced by Faraday rotation, which is prominent at these frequen-
cies. Fig. 7. (left) illustrates the Faraday rotation of N 49 which
is determined from the position angles from the CABB data set
as described above. The mean value for the Faraday rotation of
SNR N 49 is 212 ± 65 rad m⁻² and the maximum value of RM
is 591±103 rad m⁻². This RM value is suggestive of a denser
medium (as RM is linear with nₑ) as also evidenced by bright-
ness in both radio and X-rays. The resulting magnetic field map
shown in Fig. 7 (right) is a relative zero-level image obtained in
the same way as for U and Q stokes. The magnetic field is stronger
on the western side and coincides with the enhanced total intensity
emission.

We estimate a mean fractional polarisation at 5.5 GHz of 7±1% with a maximum of 82±10% (in the west). The mean fractional polarisation at 9 GHz is 10±1% with a maximum of 85±13%. Pre-CABB data has significantly better uv coverage because 10 days of data were combined using different arrays. At 4.79 GHz we estimate a mean fractional polarisation of 8±3% with a maximum of 33%. The mean fractional polarisation at 8.64 GHz is even higher at 10±1% with a maximum of 47%. This is somewhat higher than a previous study of N 49 by Dickel & Milne (1998) who found a mean fractional polarisation across the remnant of 2.5% at 4.79 GHz and 4.8% at 8.64 GHz. This polarisation structure suggests a highly organised magnetic field strongly aligned with the ‘bullet’ feature and its trail (see Fig. 7).

We use the equipartition formulae<sup>k</sup> (Arbutina et al. 2012; Arbutina et al. 2013; Urošević, Pavlović, & Arbutina 2018) to estimate the magnetic field strength for N 49. The average equipartition field over the whole shell of N 49 is ~90 µG with an estimated minimum energy<sup>l</sup> of E<sub>min</sub>=1.7×10<sup>48</sup> erg, assuming a power-law distribution for electrons, denoted in the model by ‘kappa’, κ, equal to zero.

<footnote>k<http://poincare.matf.bg.ac.rs/arbo/eqp/.</footnote>

<footnote n="1">¹We use the following N 49 values: θ=0.625', κ = 0, S<sub>1</sub> GHz=1.835 Jy and f = 0.25; for κ ≠ 0 we estimate the average equipartition field of 231 µG with an estimated minimum energy of E<sub>min</sub>=1.1×10<sup>50</sup> erg which is probably an overestimate because the physical background gives better equipartition arguments for κ = 0 (Urošević et al. 2018).</footnote>
<figure><img src="image_9.png" /><figcaption>**Figure 8.** Radio continuum spectrum of N 49 using MWA, ASKAP, and ATCA data (Table 4). The black solid line shows a linear least squares fit in logarithmic space, giving a spectral index of $\alpha = -0.55 \pm 0.03$. The relative errors (assumed to be 10%) are shown as vertical bars.</figcaption></figure>

Although N 49 is most likely a middle-aged SNR, the equipment assumption is not ideal for the determination of the magnetic field strength (perhaps only valid as an order of magnitude estimate, as used in Urošević et al. 2018). In any case, the estimated value of ~90 µG can be explained by the magnetic field amplification at the strong shocks in relatively young to middle-aged and highly luminous SNRs.

### 3.3. N 49 spectral index

Radio SNRs often follow a power-law spectrum in which the spectral index, $\alpha$, is steep as defined by $S_v \propto v^\alpha$; where $S_v$ represents flux density at $v$ frequency. To accurately measure the spectral index of N 49, we combined our observations with integrated flux density measurements across a wide range of frequencies obtained from the Murchison Widefield Array (MWA; 84–200 MHz; For et al. 2018), Molonglo, Parkes, and ATCA (408–14 700 MHz) radio telescopes, as shown in Table 4.

In Fig. 8, we plot integrated flux densities vs. frequency. Relative errors, assumed to be 10%, are used as error bars on the logarithmic plot. The resulting radio spectral index, $\alpha = -0.55 \pm 0.03$, is typical of middle-age SNRs (Filipovic et al. 1998a; Urošević 2014; Bozzetto et al. 2017).

SNR N 49 has an apparent diameter of 75", which at the LMC distance of 50 kpc corresponds to 18.2 pc. We estimate its flux density at 1 GHz to be $S_{1GHz} = 1.82 \pm 0.04$ Jy, the surface brightness to be $1.75 \times 10^{-19} \text{ W m}^{-2} \text{ Hz}^{-1} \text{ sr}^{-1}$, and the total radio luminosity (10 MHz–100 GHz) $9.22 \times 10^{27} \text{ W}$. The position of N 49 within the surface brightness to diameter ($\Sigma-D$) diagram ($\Sigma=1.8 \times 10^{-19} \text{ W m}^{-2} \text{ Hz}^{-1} \text{ sr}^{-1}$, D=18.2 pc) by Pavlović et al. (2018) suggests that this remnant is in its earlytomid Sedov phase (Urošević 2020, 2022). This is consistent with an explosion energy of $2 \times 10^{51} \text{ erg}$ evolving in an environment having a density of ~0.02 cm$^{-3}$. Such a low-density environment, however, is not consistent with our estimate of the remnant's RM. This is because a low-density medium would not provide enough electrons to produce significant Faraday rotation. Therefore, for an SNR with a high RM, the surrounding environment must have a relatively higher electron

<table><caption>**Table 4.** Flux density measurements of SNR N 49 at multiple radio frequencies. † indicates that we used images from For et al. (2018) to measure N 49 flux densities.</caption><thead><tr><th>ν<br>(MHz)</th><th>Flux density<br>S<sub>v</sub> (Jy)</th><th>Telescope</th><th>Reference</th></tr></thead><tbody><tr><td>173†</td><td>5.34</td><td>MWA</td><td>This work</td></tr><tr><td>181†</td><td>5.02</td><td>MWA</td><td>This work</td></tr><tr><td>189†</td><td>4.79</td><td>MWA</td><td>This work</td></tr><tr><td>196†</td><td>4.78</td><td>MWA</td><td>This work</td></tr><tr><td>200†</td><td>4.72</td><td>MWA</td><td>This work</td></tr><tr><td>204†</td><td>4.37</td><td>MWA</td><td>This work</td></tr><tr><td>212†</td><td>4.22</td><td>MWA</td><td>This work</td></tr><tr><td>220†</td><td>4.56</td><td>MWA</td><td>This work</td></tr><tr><td>227†</td><td>4.45</td><td>MWA</td><td>This work</td></tr><tr><td>408</td><td>2.95</td><td>Molonglo</td><td>Bozzetto et al. (2017)</td></tr><tr><td>843</td><td>2.01</td><td>MOST</td><td>Bozzetto et al. (2017)</td></tr><tr><td>888</td><td>1.27</td><td>ASKAP</td><td>Pennock et al. (2021)</td></tr><tr><td>1 377</td><td>1.33</td><td>ATCA</td><td>Bozzetto et al. (2017)</td></tr><tr><td>1 420</td><td>1.19</td><td>ATCA</td><td>Bozzetto et al. (2017)</td></tr><tr><td>2 100</td><td>1.09</td><td>ATCA</td><td>This work</td></tr><tr><td>2 378</td><td>0.960</td><td>ATCA</td><td>Bozzetto et al. (2017)</td></tr><tr><td>2 400</td><td>0.930</td><td>ATCA</td><td>This work</td></tr><tr><td>2 450</td><td>1.890</td><td>ATCA</td><td>Bozzetto et al. (2017)</td></tr><tr><td>2 700</td><td>1.16</td><td>ATCA</td><td>Bozzetto et al. (2017)</td></tr><tr><td>4 790</td><td>0.838</td><td>ATCA</td><td>This work</td></tr><tr><td>4 750</td><td>1.01</td><td>Parkes</td><td>Bozzetto et al. (2017)</td></tr><tr><td>4 790</td><td>0.730</td><td>Parkes</td><td>Bozzetto et al. (2017)</td></tr><tr><td>4 800</td><td>0.644</td><td>ATCA</td><td>Bozzetto et al. (2017)</td></tr><tr><td>5 500</td><td>1.02</td><td>ATCA</td><td>This work</td></tr><tr><td>8 550</td><td>0.619</td><td>Parkes</td><td>Bozzetto et al. (2017)</td></tr><tr><td>8 640</td><td>0.651</td><td>ATCA</td><td>This work</td></tr><tr><td>8 640</td><td>0.423</td><td>ATCA</td><td>Bozzetto et al. (2017)</td></tr><tr><td>8 800</td><td>0.800</td><td>Parkes</td><td>Bozzetto et al. (2017)</td></tr><tr><td>9 000</td><td>0.30</td><td>ATCA</td><td>This work</td></tr><tr><td>14 700</td><td>0.58</td><td>Parkes</td><td>Bozzetto et al. (2017)</td></tr></tbody></table>

density, suggesting interaction with denser regions of the ISM. This denser medium would contribute to the higher electron density required to explain the observed RM values, however, RM also depends on the strength of the magnetic field along the line of sight ($B_{||}$) where a stronger magnetic field could, in principle, increase the RM.

## 4. Discussion

### 4.1. N 49 emission features

N 49 is one of the brightest optical SNR in the LMC. While its semi-circled distinctive filamentary crescent opens to the northwest and emits very faint emission, a bright emission ridge can be seen in the east and southeast as shown in Fig. 9. Such filamentary structures in optical images indicate that optical filaments observed at distances of 5–10 pc may not be directly associated
<figure><img src="image_10.png" /><figcaption>**Figure 9.** The HST optical image of N 49 as described in Bilikova et al. (2007) (RGB = Hα (red), [S ii] (green), and [O iii] (blue) overlaid with 5.5 GHz radio contours (0.25, 1.4, 2.6,3,8,5 and 5 mJy beam⁻¹).</figcaption></figure>

with the material that was initially surrounding the progenitor star but rather with the more general ISM that the shockwave has encountered and interacted with as it expanded. Massive progenitor stars usually clear most of their surrounding material during their lifetimes, due to their powerful stellar winds (Bilikova et al. 2007).

N 49 is located within a high column density Hi ridge between two kpc-scale super-giant shells, LMC4 and LMC5 (Meaburn 1980). These are thought to have formed from multiple generations of stellar feedback (Fujii et al. 2021). Multi-wavelength observations show clear evidence of interaction between the remnant and dense clumpy interstellar clouds on the eastern side (Vancura et al. 1992a). This interaction leads to bright emission in radio, optical, infrared, ultraviolet, and X-ray bands (Park et al. 2003; Bilikova et al. 2007). The radio morphology of N 49 is generally consistent with trends seen at optical and X-ray wavelengths.

In the optical image, a line of brilliant filaments is seen as a ridge that runs south-east from the SNR. We have overlaid 5.5 GHz radio contours on the optical image (Fig. 9) to show the association between the optical and radio continuum emissions. We re-emphasise that N 49 lacks bright filaments in its western part; this may be due to a cooler low-density environment of dust and gas.

The emission line ratio of singularly ionised sulphur to hydrogen-alpha ([S ii]/Hα > 0.4) is primarily used in optical extragalactic searches for SNR, as expected for shock-heated regions (Mathewson & Clarke 1973; D'Odorico, Perinotto & Benvenuti 1980; Matonick & Fesen 1997; Blair & Long 1997). As it can be seen in Fig. 10, [S ii]/Hα ratios of 0.45–1.1 have been measured for

this SNR using HST images. The bullet feature shows only weak patches of Hα emission on the west side of the remnant.

N 49's X-ray/radio boundary of diffuse emission extends to the south and east along its circumference (Fig. 4). A diffuse emission component also appears to be embedded in the outermost emission patches which follow the X-ray/radio boundary. X-ray and radio data confirm the cavity's presence in the remnant and asymmetric expansion of the gas has been observed in this region. This is associated with irregular density distributions of materials surrounding the explosion (Campana et al. 2022).

## 4.2. Comparison with other similar SNRs

Studies of SNRs, including N 49, are essential because they provide unique constraints on the properties of these systems (Gaensler et al. 2003). We compare N 49 with several well-studied SNRs and PWNe in the Small & Large Magellanic Clouds (MCs) and the Milky Way Galaxy. For example, both MCSNR J0540–693 and MCSNR J0453–6829 in the LMC have PWNe; the former hosting a 50 ms pulsar (Gotthelf & Wang 2000), while the latter has an estimated spectral index α = −0.39 ± 0.03, consistent with non-thermal radio shell emission (Haberl et al. 2012). N 206 (B 0532–71.0) is an SNR in the LMC suggested to be in the middle to late stage of its evolution (Klinger et al. 2002) with a small X-ray and radio continuum knot at the outer tip. This feature's elongated morphology and the surrounding wedge-shaped X-ray enhancement suggest a possible bow-shock PWN structure, with a spectral index over the remnant of −0.33. This value is fairly flat for an SNR; spectral indices for PWNe tend to be greater than −0.4, as
<figure><img src="image_11.png" /><figcaption>**Figure 10.** The [S ii]/Hα ratio map indicates the bright filaments and extent of emission.</figcaption></figure>

compared to a typical shell SNR that tends to be between −0.8 and −0.3. An X-ray study of N 206 suggests this SNR-PWN system is generated by an eastward moving pulsar (Williams et al. 2005).

We observe a much wider range of PWNe and SNR in our Galaxy. For example, IC 443 is a mixed-morphology<sup>m</sup> Galactic SNR is notable for its interaction with surrounding molecular clouds. The PWN is detected in the southern edge of the SNR and is suggested to be associated; it was produced around 30 000 yr ago in a core-collapse SN event (Olbert et al. 2001). Observational characteristics of this PWN show a flat spectrum radio emission (α= −0.1 to −0.3), a steep X-ray spectrum (α<sub>x</sub>= 1.0–1.5) and a high degree of linear polarisation (>5%). The tail of the nebula does not point towards the geometric centre of the SNR (Olbert et al. 2001). The pulsar B 1951+32A is associated with a bullet-shaped PWN having a bow-shocked morphology, seen in radio and X-ray as moving with a supersonic velocity. This pulsar is associated with the strongly polarised (~15–30%) non-thermal Galactic radio SNR CTB 80 (Castelletti et al. 2003). The radio spectral index of this SNR has been estimated to be α = −0.36 ± 0.02 (Castelletti & Dubner 2005; Downes 1970).

N 49 contrasts with IC 443, N 206 (MCSNR J0531–7100) and CTB 80 which show similarities in radio spectral index, radio emission, and morphology. N49s typical SNR radio spectral index (α = −0.54 ± 0.02) and its high radio polarisation in the southwestern part suggests a knot scenario is more probable than a PWN explanation.

**5. Conclusions and future studies**

We present new radio continuum intensity and polarisation images of the well-known LMC SNR N 49. A high fractional polarisation region is found around the area where the proposed ‘bullet’ ejecta is positioned with moderate levels of mean fractional polarisation at 5.5 and 9 GHz of 7±1% and 10±1%, respectively,

throughout the remnant as a whole. In the vicinity of the so-called ‘bullet’ knot, these polarisation values are noticeably larger than found in previous studies.

The mean value for the Faraday rotation of SNR N 49 from combining CABB data is 212±65 rad m⁻² and the maximum value of RM is 591±103 rad m⁻². The strong RM near the southwest of the SNR might correspond with strong hard X-rays positioned to the southeast.

Together with *Chandra* X-ray observations, our analyses of new and archival (pre-CABB; 1990s) ATCA observations has allowed further study of prominent features of the ‘bullet’ found beyond the southwestern boundary. This presumed ejecta knot is possibly interacting with a molecular cloud, causing increased brightness in this region while no polarisation can be seen in the cloud proper. Thermal soft X-ray emissions may barely be seen within this region in the three-colour image of N 49 (Fig. 4).

We note the explosion centre of N 49, based on the knot's trail projection is offseted from the geometrical centre of the SNR (~44'' or ~10.4 pc). The next generation's high dynamic range and resolution radio observations of N 49 are essential for establishing the connection and nature of the knot's polarisation, magnetic field, and Faraday rotation.

**Acknowledgment.** The ATCA is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by Australian Commonwealth Scientific and Industrial Research Organisation (CSIRO). This paper includes archived data obtained through the Australia Telescope Online Archive (http://atoa.atnf.csiro.au). We used the *KARMA* and *MIRIAD* software packages developed by the ATNF. MDF and GR acknowledge ARC funding through grant DP200100784. D.U. acknowledges the Ministry of Education, Science and Technological Development of the Republic of Serbia through contract No. 451-03-68/2022-14/200104, and for the support through the joint project of the Serbian Academy of Sciences and Arts and Bulgarian Academy of Sciences on the detection of extragalactic SNR and H ii regions. We thank Jane Kaczmarek for her suggestions and support. We thank an anonymous referee for comments and suggestions that greatly improved our paper.

<footnote><sup>m</sup>Known as thermal composite SNR, these appear as a regular radio shell-type remnant with centrally peaked thermal X-ray emission.</footnote>
**Data availability.** We used archival data from the Australia Telescope Compact Array (ATCA), which was accessed through the online archives of the Australia Telescope National Facility (ATNF)ª. The X-ray imaging results were derived from the Chandra Data Archive (CDA) dataº. Additionally, optical HST images (Hα, [S ii], and [O iii]) were downloaded from the Mikulski Archive for Space Telescopes (MAST)P

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