A complete radio study of SNR G15.4+0.1 from new GMRT observations

Supán, L.; Castelletti, G.; Joshi, B. C.; Surnis, Mayuresh; Supanitsky, D.

doi:10.1051/0004-6361/201425284

Cited by 7 publications

(6 citation statements)

References 39 publications

(48 reference statements)

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“…G15.4+0.1 was first identified as a faint SNR during the Galactic plane survey by the Very Large Array (VLA) at 330 MHz (Brogan et al 2006). Subsequent observation of the radio shell was reported with a diameter of nearly 15′ (Castelletti et al 2013), and the global spectral index is 0.62 ± 0.03 from 330 to 4800 MHz (Supan et al 2015;Su et al 2017). In other energy bands, H. E. S. S. Collaboration et al (2014) detected the point-like TeV γ-ray source HESS J1818-154, which is spatially consistent with the SNR.…”

Section: Introductionmentioning

confidence: 99%

“…In other energy bands, H. E. S. S. Collaboration et al (2014) detected the point-like TeV γ-ray source HESS J1818-154, which is spatially consistent with the SNR. A molecular gas complex is likely associated with the SNR at a distance of 4.8 kpc (Supan et al 2015). An age of 8200 yr is obtained with a dynamical evolution model for the SNR (Chevalier 1974).…”

Section: Introductionmentioning

confidence: 99%

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Advanced γ-Ray Emission Studies of G15.4+0.1 with Fermi-LAT: Evidence of Escaping Cosmic Rays Interacting with Surrounding Molecular Clouds

Xin

Liu

et al. 2023

ApJ

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We present an analysis of γ-ray emission in the direction of supernova remnant (SNR) G15.4+0.1 with 13 yr Fermi Large Area Telescope data. There are three point-like GeV sources in this region: one is spatially coincident with the TeV source HESS J1818-154 and is interpreted as the counterpart of HESS J1818-154. Its γ-ray spectrum can be well fitted by a single power law with an index of 2.3. The other two sources with log-parabola spectra are spatially coincident with dense regions of surrounding molecular clouds revealed by CO observations. Their γ-ray emission originates from hadronic π 0 decay due to inelastic collisions between nuclei in the clouds and cosmic rays accelerated in and escaping from SNR G15.4+0.1. The total energy of the escaping protons is about 1048 erg, assuming a point-like instantaneous injection. However, the inferred diffusion coefficients are lower than the typical Galactic value.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Advanced γ-Ray Emission Studies of G15.4+0.1 with Fermi-LAT: Evidence of Escaping Cosmic Rays Interacting with Surrounding Molecular Clouds

Xin

Liu

et al. 2023

ApJ

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“…Deep, high resolution images obtained with the SKA are therefore likely to (a) discover faint emission from the SNRs and (b) increase the number of pulsar-PWN associations. Coupled with simultaneous sensitive time resolution searches with the SKA, these can be very useful in constraining evolution and dynamics of such objects (Castelletti et al 2011;Castelletti et al 2013;Supan et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Neutron Star Physics in the Square Kilometre Array Era: An Indian Perspective

Konar¹,

Bagchi²,

Bandyopadhyay³

et al. 2016

J Astrophys Astron

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It is an exceptionally opportune time for Astrophysics when a number of next-generation mega-instruments are poised to observe the universe across the entire electromagnetic spectrum with unprecedented data quality. The Square Kilometre Array (SKA) is undoubtedly one of the major components of this scenario. In particular, the SKA is expected to discover tens of thousands of new neutron stars giving a major fillip to a wide range of scientific investigations. India has a sizeable community of scientists working on different aspects of neutron star physics with immediate access to both the uGMRT (an SKA pathfinder) and the recently launched X-ray observatory Astrosat. The current interests of the community largely centre around studies of -a) the generation of neutron stars and the SNe connection, b) the neutron star population and evolutionary pathways, c) the evolution of neutron stars in binaries and the magnetic fields, d) the neutron star equation of state, e) the radio pulsar emission mechanism, and, f) the radio pulsars as probes of gravitational physics. Most of these studies are the main goals of the SKA first phase, which is likely to be operational in the next four years. This article summarises the science goals of the Indian neutron star community in the SKA era, with significant focus on coordinated efforts among the SKA and other existing/upcoming instruments.

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“…Overall, we note that the spectral components do not appear to be correlated with features in total intensity, in the sense that the brighter regions are not those with flatter spectrum as is expected under the first-order particle acceleration mechanism. A simi-lar spectral behaviour has been found in the shell-class Galactic SNRs G39.2−0.3, G41.1−0.3 (Anderson & Rudnick 1993), and G15.4+0.1 (Supan et al 2015), for which it was proposed that different mechanisms are responsible for the spectral and brightness variations observed across these sources.…”

Section: The Radio Continuum Emission: Morphology and Spectrummentioning

confidence: 88%

G51.04+0.07 and its environment: Identification of a new Galactic supernova remnant at low radio frequencies

Supán

Castelletti

Peters

et al. 2018

A&A

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We have identified a new supernova remnant (SNR), G51.04+0.07, using observations at 74 MHz from the Very Large Array Low-Frequency Sky Survey Redux. Earlier, higher frequency radio continuum, recombination line, and infrared data had correctly inferred the presence of nonthermal radio emission within a larger, complex environment including ionised nebulae and active star formation. However, our observations have allowed us to redefine at least one SNR as a relatively small source (7 ′ .5×3 ′ in size) located at the southern periphery of the originally defined SNR candidate G51.21+0.11. The integrated flux density of G51.04+0.07 at 74 MHz is 6.1±0.8 Jy, while its radio continuum spectrum has a slope α=−0.52±0.05 (S ν ∝ ν α ), typical of a shell-type remnant. We also measured spatial variations in the spectral index between 74 and 1400 MHz across the source, ranging from a steeper spectrum (α=−0.50±0.04) coincident with the brightest emission to a flatter component (α=−0.30±0.07) in the surrounding fainter region. To probe the interstellar medium into which the redefined SNR is likely evolving, we have analysed the surrounding atomic and molecular gas using the 21 cm neutral hydrogen (HI) and 13 CO (J=1−0) emissions. We found that G51.04+0.07 is confined within an elongated HI cavity and that its radio emission is consistent with the remains of a stellar explosion that occurred ∼6300 yr ago at a distance of 7.7±2.3 kpc. Kinematic data suggest that the newly discovered SNR lies in front of HII regions in the complex, consistent with the lack of a turnover in the low frequency continuum spectrum. The CO observations revealed molecular material that traces the central and northern parts of G51.04+0.07. The interaction between the cloud and the radio source is not conclusive and motivates further study. The relatively low flux density (∼1.5 Jy at 1400 MHz) of G51.04+0.07 is consistent with this and many similar SNRs lying hidden along complex lines of sight towards inner Galactic emission complexes. It would also not be surprising if the larger complex studied here hosted additional SNRs.

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A complete radio study of SNR G15.4+0.1 from new GMRT observations

Cited by 7 publications

References 39 publications

Advanced γ-Ray Emission Studies of G15.4+0.1 with Fermi-LAT: Evidence of Escaping Cosmic Rays Interacting with Surrounding Molecular Clouds

Advanced γ-Ray Emission Studies of G15.4+0.1 with Fermi-LAT: Evidence of Escaping Cosmic Rays Interacting with Surrounding Molecular Clouds

Neutron Star Physics in the Square Kilometre Array Era: An Indian Perspective

G51.04+0.07 and its environment: Identification of a new Galactic supernova remnant at low radio frequencies

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