4 research outputs found
Updated radio Σ−D relation for galactic supernova remnants
We present the updated empirical radio surface-brightness-to-diameter (Σ − D)
relation for supernova remnants (SNRs) in our Galaxy. Our original
calibration sample of Galactic SNRs with independently determined distances
(Pavlović et al. 2013, hereafter Paper I) is reconsidered and updated with
data which became available in the past two years. The orthogonal fitting
procedure and probability-density-function-based (PDF) method are applied to
the calibration sample in the logΣ − logD plane. Non-standard orthogonal
regression keeps the Σ−D and D−Σ relations invariant within estimated
uncertainties. Our previous Monte Carlo simulations verified that the slopes
of the empirical Σ−D relation should be determined by using the orthogonal
regression, because of its good performances for data sets with severe
scatter. The updated calibration sample contains 65 shell SNRs. 6 new
Galactic SNRs are added to the sample from Paper I, one is omitted and
distances are changed for 10 SNRs. The slope derived is here slightly steeper
(β ≈ 5.2) than the Σ−D slope in Paper I (β ≈ 4.8). The PDF method relies on
data points density maps which can provide more reliable calibrations that
preserve more information contained in the calibration sample. We estimate
distances to five new faint Galactic SNRs discovered for the first time by
Canadian Galactic Plane Survey, and obtained distances of 2.3, 4.0, 1.3, 2.9
and 4.7 kiloparsecs for G108.5+11.0, G128.5+2.6, G149.5+3.2, G150.8+3.8 and
G160.1−1.1, respectively. The updated empirical relation is used to estimate
distances of 160 shell Galactic SNRs and new results change their distance
scales up to 15 per cent, compared to the results from Paper I. The PDF
calculation can provide even few times higher or lower values in comparison
with the orthogonal fit, as it uses a totally different approach. However, on
average, this difference is 32, 24 and 18 per cent for mode, median and mean
distances. [Projekat Ministarstva nauke Republike Srbije, br. 176005:
Emission nebulae: structure and evolution’. B.V. also acknowledges financial
support through the Project i br. 176021: Visible and invisible matter in
nearby galaxies: theory and observations
Optical observations of the nearby galaxy IC342 with narrow band [SII] and Hα filters. I
We present observations of a portion of the nearby spiral galaxy IC342 using
narrow band [SII] and Hα filters. These observations were carried out in
November 2011 with the 2m RCC telescope at Rozhen National Astronomical
Observatory in Bulgaria. In this paper we report coordinates, diameters, Hα
and [SII] fluxes for 203 HII regions detected in two fields of view in IC342
galaxy. The number of detected HII regions is 5 times higher than previously
known in these two parts of the galaxy. [Projekat Ministarstva nauke
Republike Srbije, br. 176005: Emission nebulae: structure and evolution
Searching for an interstellar medium association for HESS J1534-571
The Galactic supernova remnant HESSJ1534−571 (also known as G323.7 − 1.0) has a shell-like morphology in TeV gamma-ray emission and is a key object in the study of cosmic ray origin. Little is known about its distance and local environment. We examine Mopra 12CO/13CO(1–0) data, Australian Telescope Compact Array HI, and Parkes HI data towards HESSJ1534−571. We trace molecular clouds in at least five velocity ranges, including clumpy interstellar medium structures near a dip in HI emission at a kinematic velocity consistent with the Scutum–Crux arm at ∼3.5 kpc. This feature may be a cavity blown-out by the progenitor star, a scenario that suggests HESSJ1534−571 resulted from a core-collapse event. By employing parametrizations fitted to a sample of supernova remnants of known distance, we find that the radio continuum brightness of HESSJ1534−571 is consistent with the ∼3.5 kpc kinematic distance of the Scutum–Crux arm HI dip. Modelling of the supernova evolution suggests a ∼8–24 kyr age for HESSJ1534−571 at this distance.Nigel I. Maxted, C. Braiding, G. F. Wong, G. P. Rowell ... Gavin P. Rowell ... Fabien Voisin ... et al