The MOST supernova remnant catalogue (MSC)

Whiteoak, J. B.; Green, A. J.

doi:10.1051/aas:1996202

Cited by 293 publications

(473 citation statements)

References 53 publications

Supporting

Mentioning

441

Contrasting

Unclassified

Order By: Relevance

“…In this respect, the disk radius of 0°.18±0°. 01 obtained by Li et al (2017) using Fermi-LAT data for CTB 37A is in better agreement with the radio extension of the shell reported by Whiteoak & Green (1996).…”

Section: Source Confusionsupporting

confidence: 87%

Search for Extended Sources in the Galactic Plane Using Six Years of Fermi-Large Area Telescope Pass 8 Data above 10 GeV

Ackermann

Ajello

Baldini

et al. 2017

ApJ

View full text Add to dashboard Cite

The spatial extension of a γ-ray source is an essential ingredient to determine its spectral properties, as well as its potential multiwavelength counterpart. The capability to spatially resolve γ-ray sources is greatly improved by the newly delivered Fermi-Large Area Telescope (LAT) Pass 8 event-level analysis, which provides a greater acceptance and an improved point-spread function, two crucial factors for the detection of extended sources. Here, we present a complete search for extended sources located within 7°from the Galactic plane, using 6 yr of Fermi-LAT data above 10 GeV. We find 46 extended sources and provide their morphological and spectral characteristics. This constitutes the first catalog of hard Fermi-LAT extended sources, named the Fermi Galactic Extended Source Catalog, which allows a thorough study of the properties of the Galactic plane in the sub-TeV domain.

show abstract

Section: Source Confusionsupporting

confidence: 87%

Search for Extended Sources in the Galactic Plane Using Six Years of Fermi-Large Area Telescope Pass 8 Data above 10 GeV

Ackermann

Ajello

Baldini

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…The bright "" knee ÏÏ in the southwest corner of the remnant exhibits striking variations in the hardness ratio, with the soft vertical arm and the progressively harder horizontal arm as one moves away (to the west) from the "" knee ÏÏ bend. The 0.843 GHz radio contours shown in Figures 2 and 3, from the Molonglo Observatory Synthesis Telescope (MOST) catalog (Whiteoak & Green 1996), demonstrate that the X-ray hardness is positively correlated with the radio/X-ray brightness ratio.…”

Section: Rcw 86 and Its X-ray Spectrummentioning

confidence: 93%

“…The Sedov model parameters are very similar in all three regions : shock temperatures in the range from 1.0 to 1.4 keV, low (\0.2 keV) postshock electron temperatures, and ionization timescales in the range from 1.4 ] 1011 to 1.8 ] 1011 cm~3 s. For the nonthermal srcut models, we obtain break frequencies of 7.5 ] 1016, 8.2 ] 1016, and 2 ] 1017 Hz for the hard, medium-hard, and soft regions, respectively, and radio spectral frequencies in the range FIG. 2.ÈGIS image of the southwest knee of RCW 86, overlaid with 0.843 GHz radio contours (based on MOST radio data ; Whiteoak & Green 1996). The X-ray and radio emission peaks nearly overlap, but radio emission is much stronger in the horizontal arm to the west of the knee bend than in the vertical arm to the north.…”

Section: Rcw 86 and Its X-ray Spectrummentioning

confidence: 99%

Thermal and Nonthermal X‐Ray Emission in Supernova Remnant RCW 86

Borkowski

Rho

Reynolds

et al. 2001

ApJ

View full text Add to dashboard Cite

Supernova remnants may exhibit both thermal and nonthermal X-ray emission. Such remnants can be distinguished by the weakness of their X-ray lines because of the presence of a strong nonthermal X-ray continuum. RCW 86 is a remnant with weak lines, resulting in low and peculiar abundances when thermal models alone are used to interpret its X-ray spectrum. This indicates the presence of a strong nonthermal synchrotron continuum. We analyze ASCA X-ray spectra of RCW 86 with the help of both nonequilibrium ionization thermal models and nonthermal synchrotron models. A two-temperature thermal model and a simple nonthermal model with an exponential cuto † (plus interstellar absorption) give reasonable results. We obtain a blast-wave velocity of 800 km s~1, a shock ionization age of 1 ] 1011È3 ] 1011 cm~3 s, and the break in nonthermal spectra at 2 ] 1016È4 ] 1016 Hz. The strength of the nonthermal continuum correlates well with the radio brightness in the bright southwest section of the remnant. This is convincing evidence for X-ray synchrotron emission in RCW 86.

show abstract

“…Mitra et al 2003, and references therein). We used the SNR catalogue produced from observations at 843 MHz with the Molonglo Observatory Synthesis Telescope by Whiteoak & Green (1996), and its updates, to identify targets for which the RM estimate is likely to be biased. Since not all sources rejected by Haverkorn et al (2008) were identified in this way, we also inspected the 2.4 GHz Stokes I maps from Parkes (Duncan et al 1995b), to ensure consistency with Haverkorn et al…”

Section: Rm Corruption By Supernova Remnantsmentioning

confidence: 99%

The large-scale magnetic field in the fourth Galactic quadrant

Nota¹,

Katgert²

2010

A&A

View full text Add to dashboard Cite

Aims. We have re-examined the published rotation measures (RMs) of extragalactic point sources and pulsars with |b| < 3 • to study the magnetic field in the fourth Galactic quadrant. Methods. We reduced the influence of structure in electron density as much as possible by excluding objects for which Hα-data indicate large fluctuations in n e somewhere along the line of sight. We also excluded objects for which the RM may have been significantly "corrupted" by an intervening supernova remnant. We modeled RM(l), the longitude dependence of RM of the unaffected extragalactic sources and pulsars. We assumed several geometries for the large-scale field. All but one of those are based on logarithmic spiral arms (with various pitch angles and widths), while one has circular symmetry. We also made different assumptions about the large-scale n e -distribution. Results. The data suggest the following generic behaviour of the large-scale field in the 4th Galactic quadrant. The field is most likely organized along logarithmic spiral arms and shows two significant reversals: from the Norma arm (CCW field) to the Norma-Crux interarm region (CW field), and from the Norma-Crux interarm region to the Crux arm (CCW field). The present data do not constrain the field in and beyond the Crux-Carina interarm region. Although the models give a good description of the global character of RM(l), individual RM-estimates deviate by typically 15 times their measurement errors. We argue that these large deviations are most likely due to the "small-scale" field that dominates on scales of up to several hundred pc. Conclusions. The picture that emerges is thus of a field that has significant structure on smaller scales, but for which the average values in arms and interarm regions are nevertheless well-defined. In addition, this smaller-amplitude large-scale field appears to reverse at each arm-interarm boundary that we can study with the present data. We briefly discuss the link between these results and theoretical predictions.

show abstract

The MOST supernova remnant catalogue (MSC)

Cited by 293 publications

References 53 publications

Search for Extended Sources in the Galactic Plane Using Six Years of Fermi-Large Area Telescope Pass 8 Data above 10 GeV

Search for Extended Sources in the Galactic Plane Using Six Years of Fermi-Large Area Telescope Pass 8 Data above 10 GeV

Thermal and Nonthermal X‐Ray Emission in Supernova Remnant RCW 86

The large-scale magnetic field in the fourth Galactic quadrant

Contact Info

Product

Resources

About