The JCMT Plane Survey: first complete data release – emission maps and compact source catalogue

Eden, David; Moore, T. J. T.; Plume, R.; Urquhart, J. S.; Thompson, M. A.; Parsons, Harriet; Dempsey, Jessica T.; Rigby, Andrew; Morgan, L. K.; Thomas, H. S.; Berry, D. S.; Buckle, Jane; Brunt, C. M.; Butner, H. M.; Carretero, D.; Chrysostomou, A.; Currie, Malcolm J.; Devilliers, H. M.; Fich, M.; Gibb, A. G.; Hoare, M. G.; Jenness, Tim; Manser, G.; Mottram, J. C.; Natario, C.; Olguin, Fernando A.; Peretto, N.; Pestalozzi, M.; Polychroni, D.; Redman, R. O.; Salji, C.; Summers, L. J.; Tahani, K.; Traficante, A.; Difrancesco, J.; Evans, A.; Fuller, G. A.; Johnstone, Doug; Joncas, G.; Longmore, S.; Martín, P. G.; Richer, J. S.; Weferling, B.; White, G. J.; Zhu, Meiping

doi:10.1093/mnras/stx874

Cited by 51 publications

(68 citation statements)

References 78 publications

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“…The survey was conducted using the Submillimetre Common-User Bolometer Array 2 (SCUBA2; Holland et al 2013) on the James Clerk Maxwell Telescope. The JPS survey has produced a compact source catalogue of ∼8 000 sources (Eden et al 2017) that has a completeness of 95 per cent at 0.04 Jy beam −1 and 0.3 Jy for the peak and integrated fluxes respectively. The JCMT has a dish size of 15 m with an angular resolution (FWHM) of 14.4 arcsec.…”

Section: Jcmt Plane Surveymentioning

confidence: 99%

“…The improved sensitivity of JPS means that although the fluxes for the different components are similar, the difference in the signal to noise ratio is sufficient (i.e., ∆SNR > 3) for source extraction to identify them as individual structures. Eden et al (2017) compared the peak and integrated fluxes between the detected ATLASGAL and JPS sources, and found them to be linearly correlated. They reported a small systematic offset with lower JPS peak flux densities, which was shown by Moore et al (2015) to be due to the smaller beam size of the JCMT.…”

Section: Jcmt Plane Surveymentioning

confidence: 99%

“…In this paper we match the methanol masers reported in the most recent MMB catalogue (265 sources; Breen et al 2015) with dense clumps identified by the ATLASGAL and JPS (JCMT Plane Survey; Moore et al 2015;Eden et al 2017) surveys, to produce the largest and most complete census of the physical environments where high-mass stars are forming across the Milky Way. This particular study will focus on expanding these previous works by taking advantage of the availability of integrated maser fluxes (Breen et al 2015), distances and bolometric luminosities that were not available in the two previous studies conducted (Urquhart et al 2013(Urquhart et al , 2015.…”

Section: Introductionmentioning

confidence: 99%

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ATLASGAL – physical parameters of dust clumps associated with 6.7 GHz methanol masers

Billington

Urquhart

König

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We have constructed the largest sample of dust-associated class II 6.7 GHz methanol masers yet obtained. New measurements from the the Methanol MultiBeam (MMB) Survey were combined with the 870 µm APEX Telescope Large Area Survey of the Galaxy (AT-LASGAL) and the 850 µm JCMT Plane Survey (JPS). Together with two previous studies we have now identified the host clumps for 958 methanol masers across the Galactic Plane, covering approximately 99 per cent of the MMB catalogue and increasing the known sample of dust-associated masers by over 30 per cent. We investigate correlations between the physical properties of the clumps and masers using distances and luminosities drawn from the literature. Clumps hosting methanol masers are significantly more compact and have higher volume densities than the general population of clumps. We determine a minimum volume density threshold of n(H 2 )≥ 10 4 cm −3 for the efficient formation of intermediate-and highmass stars. We find 6.7 GHz methanol masers are associated with a distinct part of the evolutionary process (L bol /M fwhm ratios of between 10 0.6 and 10 2.2 ) and have well defined turning on and termination points. We estimate the lower limit for the mass of embedded objects to be ≥ 6 M and the statistical lifetime of the methanol maser stage to be ∼ 3.3×10 4 yrs. This suggests that methanol masers are indeed reliable tracers of high mass star formation, and indicates that the evolutionary period traced by this marker is relatively rapid.

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Section: Jcmt Plane Surveymentioning

confidence: 99%

Section: Jcmt Plane Surveymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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ATLASGAL – physical parameters of dust clumps associated with 6.7 GHz methanol masers

Billington

Urquhart

König

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The average smoothed pixel-to-pixel noise is 7.19 mJy beam −1 . The JPS 850 µm compact-source catalogue identified by Eden et al (2017) using the Fellwalker algorithm (Berry 2015) is also adopted in this study.…”

Section: Ir To Sub-millimetre Continuum Datamentioning

confidence: 99%

Star formation in IRDC G31.97+0.07

Zhou

Zhu

Yuan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We utilize multiple-waveband continuum and molecular-line data of CO isotopes, to study the dynamical structure and physical properties of the IRDC G31.97+0.07. We derive the dust temperature and H 2 column density maps of the whole structure by SED fitting. The total mass is about 2.5 × 10 5 M for the whole filamentary structure and about 7.8×10 4 M for the IRDC. Column density PDFs produced from the column density map are generally in the power-law form suggesting that this part is mainly gravity-dominant. The flatter slope of the PDF of the IRDC implies that it might be compressed by an adjacent, larger H II region. There are 27 clumps identified from the 850 µm continuum located in this filamentary structure. Based on the average spacing of the fragments in the IRDC, we estimate the age of the IRDC. The age is about 6.4 Myr assuming inclination angle i = 30 • . For 18 clumps with relatively strong CO and 13 CO (3-2) emission, we study their line profiles and stabilities. We find 5 clumps with blue profiles which indicate gas infall motion and 2 clumps with red profiles which indicate outflows or expansion. Only one clump has α vir > 2, suggesting that most clumps are gravitationally bound and tend to collapse. In the Mass-R eq diagram, 23 of 27 clumps are above the threshold for high-mass star formation, suggesting that this region can be a good place for studying high-mass star-forming.

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“…FellWalker is less dependent on specific parameter settings than CLUMPFIND (Berry et al 2007). The source extraction process with FellWalker in the SCOPE survey is the same as that used by the JCMT Plane Survey, and details can be found in Moore et al (2015) and Eden et al (2017). A mask constructed above a threshold of 3σ (i.e., three times the pixel-topixel noise) in the S/N map is applied to the intensity map as input for the task CUPID:EXTRACTCLUMPS, which extracts the peak and integrated flux density values of the clumps.…”

Section: Dense Clumpsmentioning

confidence: 99%

The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17

Liu

Kim

Juvela

et al. 2018

ApJS

Self Cite

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The low dust temperatures (<14 K) of Planck Galactic cold clumps (PGCCs) make them ideal targets to probe the initial conditions and very early phase of star formation. "TOP-SCOPE" is a joint survey program targeting ∼2000 PGCCs in J=1-0 transitions of CO isotopologues and ∼1000 PGCCs in 850 μm continuum emission. The objective of the "TOP-SCOPE" survey and the joint surveys (SMT 10 m, KVN 21 m, and NRO 45 m) is to statistically study the initial conditions occurring during star formation and the evolution of molecular clouds, across a wide range of environments. The observations, data analysis, and example science cases for these surveys are introduced with an exemplar source, PGCC G26.53+0.17 (G26), which is a filamentary infrared dark cloud (IRDC). The total mass, length, and mean line mass (M/L) of the G26 filament are ∼6200 M ☉ , ∼12 pc, and ∼500 M ☉ pc −1 , respectively. Ten massive clumps, including eight starless ones, are found along the filament. The most massive clump as a whole may still be in global collapse, while its denser part seems to be undergoing expansion owing to outflow feedback. The fragmentation in the G26 filament from cloud scale to clump scale is in agreement with gravitational fragmentation of an isothermal, nonmagnetized, and turbulent supported cylinder. A bimodal behavior in dust emissivity spectral index (β) distribution is found in G26, suggesting grain growth along the filament. The G26 filament may be formed owing to large-scale compression flows evidenced by the temperature and velocity gradients across its natal cloud.

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The JCMT Plane Survey: first complete data release – emission maps and compact source catalogue

Cited by 51 publications

References 78 publications

ATLASGAL – physical parameters of dust clumps associated with 6.7 GHz methanol masers

ATLASGAL – physical parameters of dust clumps associated with 6.7 GHz methanol masers

Star formation in IRDC G31.97+0.07

The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17

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