The Parkes-MIT-NRAO (PMN) surveys. I - The 4850 MHz surveys and data reduction

Griffith, Mark R.; Wright, A. E.

doi:10.1086/116545

Cited by 274 publications

(225 citation statements)

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“…Several of these can be identified with IRAS or MSX point-sources, some of which are marked in Fig. A.1. The brightest compact Herschel source in this area can be identified with the giant H II region PMN J1056-6005, which was detected in the Parkes-MIT-NRAO 4850 MHz survey (Griffith & Wright 1993), and seems to be identical to the H II region GAL 289.06-00.36 listed in Caswell & Haynes (1987). Cersosimo et al (2009) detected emission in the H166α radio recombination line from this region and determined a distance of D = 7.1 ±0.3 kpc.…”

Section: Appendix A: Cloud Complexes At the Edges Of The Herschel Mapsmentioning

confidence: 61%

Herschelfar-infrared observations of the Carina Nebula complex

Roccatagliata

Preibisch

Ratzka

et al. 2013

A&A

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Context. The star formation process in large clusters/associations can be strongly influenced by the feedback from high-mass stars. Whether the resulting net effect of the feedback is predominantly negative (cloud dispersal) or positive (triggering of star formation due to cloud compression) is still an open question. Aims. The Carina Nebula complex (CNC) represents one of the most massive star-forming regions in our Galaxy. We use our Herschel far-infrared observations to study the properties of the clouds over the entire area of the CNC (with a diameter of ≈3.2 • , which corresponds to ≈125 pc at a distance of 2.3 kpc). The good angular resolution (10 −36 ) of the Herschel maps corresponds to physical scales of 0.1-0.4 pc, and allows us to analyze the small-scale (i.e., clump-size) structures of the clouds. Methods. The full extent of the CNC was mapped with PACS and SPIRE in the 70, 160, 250, 350, and 500 μm bands. We determined temperatures and column densities at each point in these maps by modeling the observed far-infrared spectral energy distributions. We also derived a map showing the strength of the UV radiation field. We investigated the relation between the cloud properties and the spatial distribution of the high-mass stars and computed total cloud masses for different density thresholds. Results. Our Herschel maps resolve for the first time the small-scale structure of the dense clouds over the entire spatial extent of the CNC. Several particularly interesting regions, including the prominent pillars south of η Car, are analyzed in detail. We compare the cloud masses derived from the Herschel data with previous mass estimates based on sub-mm and molecular line data. Our maps also reveal a peculiar wave-like pattern in the northern part of the Carina Nebula. Finally, we characterize two prominent cloud complexes at the periphery of our Herschel maps, which are probably molecular clouds in the Galactic background. Conclusions. We find that the density and temperature structure of the clouds in most parts of the CNC is dominated by the strong feedback from the numerous massive stars, and not by random turbulence. Comparing the cloud mass and the star formation rate derived for the CNC with other Galactic star-forming regions suggests that the CNC is forming stars in a particularly efficient way. We suggest this to be a consequence of triggered star formation by radiative cloud compression.

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Section: Appendix A: Cloud Complexes At the Edges Of The Herschel Mapsmentioning

confidence: 61%

Herschelfar-infrared observations of the Carina Nebula complex

Roccatagliata

Preibisch

Ratzka

et al. 2013

A&A

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“…North of the celestial equator, we used the 6 and 20 cm Green Bank survey catalogs GB6 and NORTH20CM (Gregory et al 1996;White & Becker 1992), while south of the equator we used the 6 cm Parkes-MIT-NRAO catalog PMN (Griffith & Wright 1993). For objects south of the celestial equator, where a survey at a frequency different from the one of the PMN (6 cm) was missing when we started this project (the NVSS; Condon et al [1998], now available, reaches in any case only ¼ À40 ), we conducted a snapshot survey with the Australia Telescope Compact Array (ATCA) at 3.6 and 6 cm.…”

Section: Candidate Selectionmentioning

confidence: 99%

The Deep X‐Ray Radio Blazar Survey. III. Radio Number Counts, Evolutionary Properties, and Luminosity Function of Blazars

Padovani

Giommi

Landt

et al. 2007

ApJ

113

174

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Our knowledge of the blazar surface densities and luminosity functions, which are fundamental parameters, relies still on samples at relatively high flux limits. As a result, our understanding of this rare class of active galactic nuclei is mostly based on relatively bright and intrinsically luminous sources. We present the radio number counts, evolutionary properties, and luminosity functions of the faintest blazar sample with basically complete ($95%) identifications. Based on the Deep X-Ray Radio Blazar Survey (DXRBS), it includes 129 flat-spectrum radio quasars (FSRQs) and 24 BL Lac objects down to a 5 GHz flux and power $50 mJy and $10 24 W Hz À1 , respectively, an order of magnitude improvement as compared to previously published (radio-selected) blazar samples. DXRBS FSRQs are seen to evolve strongly, up to redshift %1.5, above which high-power sources show a decline in their comoving space density. DXRBS BL Lac objects, on the other hand, do not evolve. High-energy and low-energy peaked BL Lac objects (HBLs and LBLs, respectively) share the same lack of cosmological evolution, which is at variance with some previous results. The observed luminosity functions are in good agreement with the predictions of unified schemes, with FSRQs getting close to their expected minimum power. Despite the fact that the large majority of our blazars are FSRQs, BL Lac objects are intrinsically $50 times more numerous. Finally, the relative numbers of HBLs and LBLs in the radio and X-ray bands are different from those predicted by the so-called blazar sequence and support a scenario in which HBLs represent a small minority (%10%) of all BL Lac objects.

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“…A sample of 178 radio-excess objects was selected in Paper I by cross-correlating the Parkes-MIT-NRAO 5 GHz catalog (Griffith & Wright 1993;Griffith et al 1994Griffith et al , 1995Wright et al 1994Wright et al , 1996 with the 60 m IRAS Faint Source Catalog ( FSC) ( Moshir et al 1992). The radio-excess objects have log ½S (60 m)=S (4:8 GHz) < 1:80 and thus lie above the well-known FIR /radio correlation for radio-quiet objects (typically log ½S (60 m)=S (4:8 GHz) $ 2:3).…”

Section: Observationsmentioning

confidence: 99%

Radio-ExcessIRASGalaxies. II. Host Galaxies

2004

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This is the second of a series of papers studying a sample of radio-excess IRAS galaxies. These galaxies have radio emission in excess of that expected due to star formation, but largely fall between the traditional categories of radio-loud and radio-quiet active galaxies. R-band images of the hosts of far-infrared ( FIR)-luminous radioexcess galaxies are presented and analyzed. The hosts of the FIR-luminous radio-excess galaxies are luminous galaxies, on average 0.8 mag brighter than M Ã R . Their optical luminosities and morphologies are similar to comparison samples of radio-loud compact steep-spectrum and gigahertz peaked-spectrum sources and extended radio galaxies. We find a similar fraction of galaxies in our sample ($70%) with companions or distorted morphologies as in radio-loud comparison samples. This is consistent with radio activity being associated with tidal interaction. The majority (65%) of the FIR-luminous radio-excess galaxies have radio source sizes that are smaller than the optical host by more than an order of magnitude. These compact radio sources may be young precursors to classical radio galaxies or a different population of radio sources, possibly confined by the host interstellar medium. The host galaxy types were determined by analysis of the surface brightness distributions. The elliptical hosts have effective surface brightnesses and radii consistent with known ellipticals but inconsistent with a population of brightest cluster galaxies. Thus, it is unlikely these objects are the precursors of FR I radio galaxies. The disk hosts have smaller sizes and low radio excesses. However, they have a range of radio source sizes, which is not expected if they are radio-''loud'' Seyfert galaxies.

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The Parkes-MIT-NRAO (PMN) surveys. I - The 4850 MHz surveys and data reduction

Cited by 274 publications

References 0 publications

Herschelfar-infrared observations of the Carina Nebula complex

Herschelfar-infrared observations of the Carina Nebula complex

The Deep X‐Ray Radio Blazar Survey. III. Radio Number Counts, Evolutionary Properties, and Luminosity Function of Blazars

Radio-ExcessIRASGalaxies. II. Host Galaxies

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