G189.6+03.3: The first complete X-ray view provided by SRG/eROSITA

Camilloni, Francesco; Becker, Werner

doi:10.1051/0004-6361/202347300

Cited by 3 publications

(1 citation statement)

References 70 publications

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“…The supernova remnants IC443 and G189.6+03.3 (cf. Camilloni & Becker 2023) are visible in the upper right corner. Photons to produce the image were colour-coded according to their energy (red for energies 0.2-0.4 keV, green for 0.4-0.6 keV, blue for 0.6-1.2 keV).…”

Section: Data Reductionmentioning

confidence: 99%

Searching for X-ray counterparts of degree-wide TeV halos around middle-aged pulsars with SRG/eROSITA

Khokhriakova,

Becker,

Ponti

et al. 2024

A&A

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Extended gamma-ray TeV emission (TeV halos) has been detected around middle-aged pulsars. A proposed model to explain these TeV halos is that electrons from a degree-wide pulsar wind nebula (PWN) get up-scattered by cosmic microwave background photons through inverse Compton processes. However, no X-ray degree-wide faint diffuse PWNe have been found around these middle-aged pulsars in previous X-ray observations. We performed a search for degree-wide PWNe around Geminga, PSR B0656+14, B0540+23, J0633+0632, and J0631+1036 using data from the first four consecutive Spectrum Roentgen Gamma/eROSITA all-sky surveys. In order to better understand the mechanisms underlying the formation of TeV halos, we investigated the magnetic field strength within an area of 1 degree in radius centred on those pulsars. To achieve our goals, we selected a list of suitable candidate pulsars in the eROSITA-DE part of the sky and applied data reduction techniques to process the eROSITA data. We then performed a spatial analysis of the regions around selected pulsars. We do not detect any degree-wide diffuse emission driven by rotation-powered pulsars around Geminga, PSR B0656+14, B0540+23, J0633+0632, or J0631+1036. Indeed, close inspection of the data shows that the pulsars of interest are all embedded in diffuse emission from supernova remnants such as the Monogem Ring or the Rosetta Nebula, while PSR B0540+23 is located sim 2.5 degrees away from the Crab pulsar, which is exceptionally bright, causing its X-ray emission to spread over a significant area up to the position of PSR B0540+23 and therefore strongly diminishes our capacity to search for degree-wide bright diffuse X-ray emission. Despite the non-detection of any degree-wide PWN surrounding the analysed pulsars, we set flux upper limits to provide useful information on magnetic field strength and its spatial distribution around those pulsars, providing additional constraints on the proposed theory for the formation of TeV halos around pulsars.

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Section: Data Reductionmentioning

confidence: 99%

Searching for X-ray counterparts of degree-wide TeV halos around middle-aged pulsars with SRG/eROSITA

Khokhriakova,

Becker,

Ponti

et al. 2024

A&A

Self Cite

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A new understanding of the Gemini-Monoceros X-ray enhancement from discoveries with eROSITA

Knies,

Sasaki,

Becker

et al. 2024

A&A

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Aims. The Gemini-Monoceros X-ray enhancement is a rich field for studying diffuse X-ray emission and supernova remnants (SNRs). Most SNRs in this part of the sky are notoriously difficult to observe due to their large extent. With the launch of the extended ROentgen Survey with an Imaging Telescope Array (eROSITA) on board the Spektrum-Röntgen-Gamma platform in 2019, we are now able to fully study those objects for the first time with CCD resolution. Many of the SNRs in the vicinity are suspected to be very old remnants, which are severely understudied in X-rays due to numerous observational challenges. In addition, the identification of new faint large SNRs might help to solve the long-standing discrepancy between the observed and expected number of Galactic SNRs. Methods. We performed a detailed X-ray spectral analysis of the entire Gemini-Monoceros X-ray enhancement and a detailed background analysis of the vicinity, which allowed us to model the background with a high precision inside the X-ray enhancement. We also made use of multiwavelength data to better understand the morphology and to constrain the distances to the different sources. Based on the spectral analysis, we estimated the properties of the sources and calculated a grid of model SNRs to determine the individual SNR properties. Results. Most of the diffuse plasma of the Monogem Ring SNR is well described by a single nonequilibrium ionization (NEI) component with an average temperature of kT = 0.14 ± 0.03 keV. We obtain an age of ≈1.2 × 105 yr – consistent with PSR B0656+14 – for the Monogem Ring and an explosion energy typical for a core-collapse (CC) supernova (SN). In the southeast, we found evidence for a significant temperature enhancement and a second plasma component. Our findings show that a scenario of two SNRs at ≈300 pc is likely, with the new candidate having an age of ≈50 000 yr. We were also able to improve on previous results for the Monoceros Loop and PKS 0646+06 SNRs by disentangling the foreground diffuse emission of the Monogem Ring SNR. We obtained significantly higher temperatures than previous studies, and for PKS 0646+06 a much lower estimated age of the SNR. We also found a new SNR candidate G190.4+12.5 which most likely is located at D > 1.5 kpc, expanding into a low density medium at a high distance from the Galactic plane, with an estimated age of 40 000–60 000 yr.

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Optical and H i observations of IC 443 and G189.6 + 3.3 in a complex environment

Bakış,

Paylı,

Aktekin

et al. 2024

Monthly Notices of the Royal Astronomical Society

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The supernova remnant (SNR) IC 443 is one of the best-studied Galactic SNRs at many wavelengths. It is interacting with a very complex environment, including the SNR G189.6 + 3.3 and H ii regions. In this paper, we report on observations of IC 443 and G189.6 + 3.3 using 1.5- and 1-m telescopes to better understand the nature of these SNRs in the optical band. We obtain H$\alpha$ images showing both filamentary and diffuse structures, and long-slit spectra from many locations, with Balmer and forbidden lines detected for IC 443 and G189.6 + 3.3. The [S ii]/ H$\alpha$ ratios confirm the SNR nature of G189.6 + 3.3. The ranges of our estimated electron density and pre-shock cloud density clearly indicate the complex structure surrounding IC 443 and G189.6 + 3.3. We also investigate the archival H i data and newly find some shell-like distributions of H i that are possibly associated with G189.6 $+$ 3.3.

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G189.6+03.3: The first complete X-ray view provided by SRG/eROSITA

Cited by 3 publications

References 70 publications

Searching for X-ray counterparts of degree-wide TeV halos around middle-aged pulsars with SRG/eROSITA

Searching for X-ray counterparts of degree-wide TeV halos around middle-aged pulsars with SRG/eROSITA

A new understanding of the Gemini-Monoceros X-ray enhancement from discoveries with eROSITA

Optical and H i observations of IC 443 and G189.6 + 3.3 in a complex environment

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