MAGPIS: A Multi-Array Galactic Plane Imaging Survey

Helfand, D. J.; Becker, R. H.; White, R. L.; Fallon, Adam; Tuttle, Sarah

doi:10.1086/503253

Cited by 312 publications

(403 citation statements)

References 25 publications

(15 reference statements)

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“…We will also correlate our data with existing radio surveys in the centimeter range: the NRAO VLA Sky Survey (NVSS, Condon et al 1998), the Multi-Array Galactic Plane Imaging Survey (MAGPIS, Helfand et al 2006), the Sydney University Molonglo Sky Survey (SUMSS, Mauch et al 2003), and the Co-Ordinated Radio "N" Infrared Survey for High-mass star formation (CORNISH) 1 . It will be of particular interest to compare with surveys of the radio continuum and maser emission that will be possible with the Expanded Very Large Array and the 1 http://www.ast.leeds.ac.uk/Cornish/index.html Australia Telescope Compact Array in the near future (Menten 2007).…”

Section: Ancillary Datamentioning

confidence: 99%

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Schüller¹,

Menten²,

Contreras

et al. 2009

A&A

732

927

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Context. Thanks to its excellent 5100 m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so far. Aims. Our goal is to produce a large-scale, systematic database of massive pre-and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. Only a systematic survey of the Galactic Plane can provide the statistical basis for unbiased studies. A well characterized sample of Galactic star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submillimeter wavelengths also represents a preparatory work for Herschel and ALMA. Methods. The APEX telescope is ideally located to observe the inner Milky Way. The Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer array observing at 870 μm, with a beam size of 19. 2. Taking advantage of its large field of view (11. 4) and excellent sensitivity, we started an unbiased survey of the entire Galactic Plane accessible to APEX, with a typical noise level of 50−70 mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). Results. As a first step, we covered ∼95 deg 2 of the Galactic Plane. These data reveal ∼6000 compact sources brighter than 0.25 Jy, or 63 sources per square degree, as well as extended structures, many of them filamentary. About two thirds of the compact sources have no bright infrared counterpart, and some of them are likely to correspond to the precursors of (high-mass) proto-stars or protoclusters. Other compact sources harbor hot cores, compact H ii regions, or young embedded clusters, thus tracing more evolved stages after massive stars have formed. Assuming a typical distance of 5 kpc, most sources are clumps smaller than 1 pc with masses from a few 10 to a few 100 M . In this first introductory paper, we show preliminary results from these ongoing observations, and discuss the mid-and long-term perspectives of the survey.

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Section: Ancillary Datamentioning

confidence: 99%

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Schüller¹,

Menten²,

Contreras

et al. 2009

A&A

732

927

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“…A comparison of the two catalogs (radio and infrared) allowed the authors to find a sample of 687 radio sources with highly-reliable infrared counterparts. Only 228 of 687 targets were detected in the new MAGPIS at 20 cm (Helfand et al 2006).…”

Section: Sample Selectionmentioning

confidence: 99%

7 mm continuum observations of ultra compact HII regions

Leto

Umana²,

Trigilio³

et al. 2009

A&A

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Aims. Ultra compact HII (UCHII) regions are indicators of high-mass star formation sites and are distributed mainly in the Galactic plane. They exhibit a broad band spectrum with significant emission between near-IR and radio wavelengths. We intend to investigate the possible contribution of the forthcoming ESA Planck mission to the science of UCHII regions by evaluating the possibility of detecting UCHIIs that are bright in the radio regime. Methods. We performed new 7 mm observations of a sample of UCHII regions. The observations were designed to acquire highfrequency radio spectra. For each source in our sample, the free-free radio spectrum has been modeled. Along with far-IR measurements, our spectra allow us to estimate the flux densities of the sources in the millimeter and sub-millimeter bands. We extrapolated and summed the ionized-gas (free-free radio emission) and dust (thermal emission) contributions in the afore mentioned wavelength ranges. The possibility of Planck detecting the selected sources can be assessed by comparing the estimated flux densities to the expected sensitivity in each Planck channel. To obtain a realistic estimation of the noise produced by the Galactic emission, the Planck sky model software package was used. Results. For each target source, from our new 7 mm data and other radio measurements from the literature, important physical parameters such as electron density and their spatial distribution, source geometry and emission measure were derived. We conclude that, in the case of the present sample, located close to the Galactic center, Planck will have a very low detection rate. In contrast, assuming that our sample is representative of the whole UCHII-region population, we derive a very high probability of detecting this kind of source with Planck if located instead close to the anticenter. From the analysis of the ionized-gas properties, we suggest that the selected sample could also be contaminated by other kinds of Galactic objects.

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“…However, new radiocontinuum surveys of the galactic plane (Helfand et al 2006;Brogan et al 2006) have recently identified a host of (candidate) SNR in the inner galaxy and surveys searching for signposts of interaction in the 1720 MHz transition of OH have been conducted by Hewitt & Yusef-Zadeh (2009).…”

Section: Introductionmentioning

confidence: 99%

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

Liszt

2009

A&A

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Results. Although broad CO lines characteristic of shocked gas were not seen in this kinematically complex region, a bright (14 K), new, marginally-resolved ±9 km s −1 outflow source G5.638+0.233 and a comparably bright rim of CO emission were found at/around the periphery of SNR G5.55+0.12. Most of the periphery of SNR G5.71-0.08 is surrounded by a bright rim of CO emission. CO emission at the 7 km s −1 velocity of a 1720 OH maser spot near SNR G5.70-0.12 is very bright, 19 K, but gas at −21 km s −1 is widespread over the region and CO emission is rather weak toward the OH maser spots at this velocity north of G5.4-1.2. Other very bright CO lines in the region are associated with H II regions, i.e. 27 K toward W28A2 = G5.89-0.39 and 15 K toward an MSX-IR source at l = 5.9 o , b = −0.13 o which is probably the exciting agent of a separate, classical HII region just north of W28A2.

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MAGPIS: A Multi-Array Galactic Plane Imaging Survey

Cited by 312 publications

References 25 publications

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

7 mm continuum observations of ultra compact HII regions

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

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