The RMS survey

Urquhart, J. S.; Busfield, A. L.; Hoare, M. G.; Lumsden, S. L.; Clarke, A. J.; Moore, T. J. T.; Mottram, J. C.; Oudmaijer, R. D.

doi:10.1051/0004-6361:20065837

Cited by 105 publications

(187 citation statements)

References 18 publications

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“…Using our unbiased sample of 391 compact and UCHII regions we estimate the Galactic scale height of massive stars to be 0.6 • . This is in line with the values derived from the UCHII regions identified from the ATCA observations (Urquhart et al 2007a) and by Reed (2000) from the distribution of nearby OB stars.…”

Section: Discussionsupporting

confidence: 90%

“…The radio continuum data presented here complement the observations of the southern hemisphere sample of RMS sources presented in Urquhart et al (2007a). The full data set now includes 6 cm observations for ∼1800 MYSO candidates, and together with archival data provides radio continuum data for the entire RMS catalogue.…”

Section: Discussionmentioning

confidence: 80%

“…In a recent paper (Urquhart et al 2007a, hereafter Paper I) we presented the results of a set of high resolution radio observations towards 826 RMS sources located in the southern hemisphere (i.e., 230 • < l < 350 • ). These observations were made at 4.8 and 8.6 GHz with the Australia Telescope Compact Array (ATCA) 2 and had a 4σ sensitivity of ∼1 mJy and spatial resolution of ∼2 .…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

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The RMS survey

Urquhart

Hoare²,

Purcell

et al. 2009

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Context. The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, well-selected sample of massive young stellar objects (MYSOs). We have identified ∼2000 MYSO candidates located throughout the Galaxy by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. The aim of these follow-up observations is to identify other objects with similar colours such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe) and distinguish between genuine MYSOs and nearby low-mass YSOs. Aims. To identify the populations of UCHII regions and PNe within the sample and examine their Galactic distribution. Methods. We have conducted high resolution radio continuum observations at 6 cm towards 659 MYSO candidates in the northern hemisphere (10 • < l < 250 • ) using the Very Large Array (VLA). These observations have a spatial resolution of ∼1-2 and typical image rms noise values of ∼0.22 mJy -sensitive enough to detect a HII region powered by B0.5 star at the far side of the Galaxy. In addition to these targeted observations we present archival data towards a further 315 RMS sources extracted from a previous VLA survey of the inner Galaxy.Results. We present the results of radio continuum observations made towards 974 MYSO candidates, 272 (∼27% of the observed sample) of which are found to be associated with radio emission above a 4σ detection limit (∼1 mJy). Using results from other parts of our multi-wavelength survey we separate these RMS-radio associations into two distinct types of objects, classifying 51 as PNe and a further 208 as either compact or UC HII regions. Including all HII regions and PNe identified either from the literature or from the multi-wavelength data these numbers increase to 391 and 79, respectively. Using this well selected sample of HII regions we estimate their Galactic scale height to be 0.6 • . In addition to the RMS-radio associations we are able to set upper limits on the radio emission of ≤1 mJy for the 702 non-detections, which is below the level expected if they had already begun to ionise their surroundings. Conclusions. Using radio continuum and archival data we have identified 79 PNe and 391 HII regions within the northern RMS catalogue. We estimate the total fraction of contamination by PNe in the RMS sample is of order 10%. The sample of HII regions is probably the best representation to date of the Galactic population of HII regions as a whole.

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Section: Discussionsupporting

confidence: 90%

Section: Discussionmentioning

confidence: 80%

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

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The RMS survey

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Purcell

et al. 2009

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“…Therefore, it might be expected that this object is associated with a Hii region. While this object is a radio non-detection (Urquhart et al 2007), it is possible that a weak Hii region has escaped detection due to the large distance to this object (13 kpc). This could explain the cometary morphology of this source.…”

Section: I: G3396221−001209mentioning

confidence: 99%

Probing the envelopes of massive young stellar objects with diffraction limited mid-infrared imaging

Wheelwright

Wit

Oudmaijer

et al. 2012

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Context. Massive stars form whilst they are still embedded in dense envelopes. As a result, the roles of rotation, mass loss and accretion in massive star formation are not well understood. Aims. This study evaluates the source of the Q-band, λ c = 19.5 μm, emission of massive young stellar objects (MYSOs). This allows us to determine the relative importance of rotation and outflow activity in shaping the circumstellar environments of MYSOs on 1000 AU scales. Methods. We obtained diffraction limited mid-infrared images of a sample of 20 MYSOs using the VLT/VISIR and Subaru/COMICS instruments. For these 8 m class telescopes and the sample selected, the diffraction limit, ∼0.6 , corresponds to approximately 1000 AU. We compare the images and the spectral energy distributions (SEDs) observed to a 2D, axis-symmetric dust radiative transfer model that reproduces VLTI/MIDI observations of the MYSO W33A. We vary the inclination, mass infall rate, and outflow opening angle to simultaneously recreate the behaviour of the sample of MYSOs in the spatial and spectral domains. Results. The mid-IR emission of 70 percent of the MYSOs is spatially resolved. In the majority of cases, the spatial extent of their emission and their SEDs can be reproduced by the W33A model featuring an in-falling, rotating dusty envelope with outflow cavities. There is independent evidence that most of the sources which are not fit by the model are associated with ultracompact H ii regions and are thus more evolved. Conclusions. We find that, in general, the diverse ∼20 μm morphology of MYSOs can be attributed to warm dust in the walls of outflow cavities seen at different inclinations. This implies that the warm dust in the outflow cavity walls dominates the Q-band emission of MYSOs. In turn, this emphasises that outflows are an ubiquitous feature of massive star formation.

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“…These include; ∼1 resolution continuum radio observations to identify regions of ionised emission (Urquhart et al 2007a(Urquhart et al , 2009; ground-based ∼1 resolution mid-IR imaging where Spitzer IRAC (3.6 μm, 4.5 μm, 5.8 μm and 8.0 μm) imaging from the GLIMPSE survey (Benjamin et al 2003;Churchwell et al 2009) is unavailable to identify multiplicity in the ∼18 MSX beam, obtain better astrometry and ensure that the survey does not bias against YSOs near H ii regions (e.g. Mottram et al 2007); 13 CO molecular line observations in order to obtain kinematic distances (Urquhart et al 2007b(Urquhart et al , 2008a; and near-IR spectroscopy (e.g.…”

Section: Introductionmentioning

confidence: 99%

The RMS survey: far-infrared photometry of young massive stars

Mottram

Hoare²,

Lumsden³

et al. 2010

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Context. The Red MSX Source (RMS) survey is a multi-wavelength campaign of follow-up observations of a colour-selected sample of candidate massive young stellar objects (MYSOs) in the galactic plane. This survey is returning the largest well-selected sample of MYSOs to date, while identifying other dust contaminant sources with similar mid-infrared colours including a large number of new ultra-compact (UC) H ii regions.Aims. To measure the far-infrared (IR) flux, which lies near the peak of the spectral energy distribution (SED) of MYSOs and UCH ii regions, so that, together with distance information, the luminosity of these sources can be obtained.Methods. Less than 50% of RMS sources are associated with IRAS point sources with detections at 60 μm and 100 μm, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources. Results. Far-IR fluxes are obtained for a total of 1113 RMS candidates identified as young sources. Of these 734 have flux measurements using IGA 60 μm and 100 μm images and 724 using MIPSGAL 70 μm images, with 345 having measurements in both data sets.

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The RMS survey

Cited by 105 publications

References 18 publications

The RMS survey

The RMS survey

Probing the envelopes of massive young stellar objects with diffraction limited mid-infrared imaging

The RMS survey: far-infrared photometry of young massive stars

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