The Parkes-MIT-NRAO (PMN) Surveys. VIII. Source Catalog for the Zenith Survey (-37.0 degrees &lt; delta &lt; -29.0 degrees )

Wright, A. E.; Griffith, Mark R.; Hunt, Andrew J.; Troup, E. R.; Burke, B. F.; Ekers, R. D.

doi:10.1086/192272

Cited by 104 publications

(88 citation statements)

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“…The spectral indices (F ∝ ν α ) range from flat (α ∼ 0) to steep (α ∼ -1). The total 6cm flux in Table 2 is given both for our images and for the single-dish observations by Wright et al (1994Wright et al ( , 1996. The difference between these indicates the amount of diffuse emission which is missing from our images.…”

Section: Resultsmentioning

confidence: 99%

Star formation in southern Seyfert galaxies

Forbes¹,

Norris²

1998

Monthly Notices RAS

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We have produced radio maps, using the ATCA, of the central regions of six southern Seyfert 2 galaxies (NGC 1365, 4945, 6221, 6810, 7582, and Circinus) with circumnuclear star formation, to estimate the relative contribution of star formation activity compared to activity from the active galactic nucleus (AGN). The radio morphologies range from extended diffuse structures to compact nuclear emission, with no evidence, even in the relatively compact sources, for synchrotron self-absorption. In each case the radio to far-infrared (FIR) ratio has a value consistent with star formation, and in all but one case the radio to [FeII] ratio is also consistent with star formation. We derive supernova rates and conclude that, despite the presence of a Seyfert nucleus in these galaxies, the radio, FIR, and [FeII] line emission are dominated by processes associated with the circumnuclear star formation (i.e. supernova remnants and H II regions) rather than with the AGN.

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Section: Resultsmentioning

confidence: 99%

Star formation in southern Seyfert galaxies

Forbes¹,

Norris²

1998

Monthly Notices RAS

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“…13−15 but with constants R 0 = 8.4 kpc and Θ 0 = 254 km s −1 for kinematic distances. Wright et al (1994Wright et al ( , 1996Griffith et al (1994Griffith et al ( , 1995; xrm+08: Xu et al (2008); zzr+08: Zhang et al (2008). Table A.2.…”

Section: Appendix A: Tracer Data For Spiral Structurementioning

confidence: 99%

The spiral structure of our Milky Way Galaxy

Hou

Han

Shi

2009

A&A

162

223

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Context. The spiral structure of our Milky Way Galaxy is not yet known. HII regions and giant molecular clouds are the most prominent spiral tracers. Models with 2−4 arms have been proposed to outline the structure of our Galaxy. Aims. Recently, new data of spiral tracers covering a larger region of the Galactic disk have been published. We wish to outline the spiral structure of the Milky way using all tracer data. Methods. We collected the spiral tracer data of our Milky Way from the literature, namely, HII regions and giant molecular clouds (GMCs). With weighting factors based on the excitation parameters of HII regions or the masses of GMCs, we fitted the distribution of these tracers with models of two, three, four spiral-arms or polynomial spiral arms. The distances of tracers, if not available from stellar or direct measurements, were estimated kinetically from the standard rotation curve of Brand & Blitz (1993, A&A, 275, 67) with R 0 = 8.5 kpc, and Θ 0 = 220 km s −1 or the newly fitted rotation curves with R 0 = 8.0 kpc and Θ 0 = 220 km s −1 or R 0 = 8.4 kpc and Θ 0 = 254 km s −1 . Results. We found that the two-arm logarithmic model cannot fit the data in many regions. The three-and the four-arm logarithmic models are able to connect most tracers. However, at least two observed tangential directions cannot be matched by the three-or four-arm model. We composed a polynomial spiral arm model, which can not only fit the tracer distribution but also match observed tangential directions. Using new rotation curves with R 0 = 8.0 kpc and Θ 0 = 220 km s −1 and R 0 = 8.4 kpc and Θ 0 = 254 km s −1 for the estimation of kinematic distances, we found that the distribution of HII regions and GMCs can fit the models well, although the results do not change significantly compared to the parameters with the standard R 0 and Θ 0 .

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“…The NVSS catalog does not provide information about spectral index, so we checked these 2704 sources against the CATS database, which nowadays contains one of the most complete collections of radio catalogs, and found the sources that had been observed under other campaigns at different frequency bands. If a source was not found in any other catalog, for example, was absent from the GB6 catalog, with flux limit 18 mJy, and the PMN catalog (Wright et al 1996), with flux limit 40-70 mJy at 5 GHz, this indicates with high probability that the spectral index is significantly less than À0.5. In total, this initial list had 302 sources.…”

Section: Source Selectionmentioning

confidence: 99%

The Third VLBA Calibrator Survey: VCS3

Petrov¹,

Kovalev²,

Fomalont³

et al. 2005

154

168

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We present the third extension to the Very Long Baseline Array (VLBI ) Calibrator Survey, containing 360 new sources not previously observed with very long baseline interferometry (VLBI). The survey, based on three 24 hour VLBA observing sessions, fills the areas on the sky above declination À45 where the calibrator density is less than one source within a 4 radius disk at any given direction. The positions were derived from astrometric analysis of the group delays determined at 2.3 and 8.6 GHz frequency bands using the CALC/SOLVE software package. The VCS3 catalog of source positions, plots of correlated flux density versus length of projected baseline, and contour plots and FITS files of naturally weighted CLEAN images, as well as calibrated visibility function files, are available electronically from the Goddard Geodetic VLBI Group.

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The Parkes-MIT-NRAO (PMN) Surveys. VIII. Source Catalog for the Zenith Survey (-37.0 degrees < delta < -29.0 degrees )

Cited by 104 publications

References 0 publications

Star formation in southern Seyfert galaxies

Star formation in southern Seyfert galaxies

The spiral structure of our Milky Way Galaxy

The Third VLBA Calibrator Survey: VCS3

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