Volume 576, April 2015
|Number of page(s)||11|
|Section||Interstellar and circumstellar matter|
|Published online||02 April 2015|
A complete radio study of SNR G15.4+0.1 from new GMRT observations
Instituto de Astronomía y Física del Espacio (IAFE CONICET-UBA),
CC 67, Suc. 28,
2 National Centre for Radio Astrophysics (NCRA-TIFR), Post Bag No 3, Ganeshkhind, 411007 Pune , India
Received: 5 November 2014
Accepted: 16 January 2015
Aims. The supernova remnant (SNR) G15.4+0.1 is considered to be the possible counterpart of the γ-ray source HESS J1818−154. With the goal of getting a complete view of this remnant and understanding the nature of the γ-ray flux, we conducted a detailed radio study that includes the search for pulsations and a model of the broadband emission for the SNR G15.4+0.1/HESS J1818−154 system.
Methods. Low-frequency imaging at 624 MHz and pulsar observations at 624 and 1404 MHz towards G15.4+0.1 were carried out with the Giant Metrewave Radio Telescope (GMRT). We correlated the new radio data with observations of the source at X-ray and infrared wavelengths from XMM-Newton and Herschel observatories, respectively. To characterize the neutral hydrogen (HI) medium towards G15.4+0.1, we used data from the Southern Galactic Plane Survey. We modelled the spectral energy distribution (SED) using both hadronic and leptonic scenarios.
Results. From the combination of the new GMRT observations with existing data, we derived a continuum spectral index α = −0.62 ± 0.03 for the whole remnant. The local synchrotron spectra of G15.4+0.1, calculated from the combination of the GMRT data with 330 MHz observations from the Very Large Array, tends to be flatter in the central part of the remnant, accompanying the region where the blast wave is impinging molecular gas. No spectral index trace was found indicating the radio counterpart to the pulsar wind nebula proposed from X-ray observations. In addition, the search for radio pulsations yielded negative results. Emission at far-infrared wavelengths is observed in the region where the SNR shock is interacting with dense molecular clumps. We also identified HI features forming a shell that wraps most of the outer border of G15.4+0.1. Characteristic parameters were estimated for the shocked HI gas. We found that either a purely hadronic or leptonic model is compatible with the broadband emission known so far.
Key words: ISM: individual objects: SNR G15.4+0.1 / ISM: supernova remnants / radio continuum: ISM / gamma rays: ISM
© ESO, 2015
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