ATLASGAL – properties of a complete sample of Galactic clumps★

Urquhart, J. S.; König, C.; Giannetti, A.; Leurini, S.; Moore, T. J. T.; Eden, David; Pillai, T.; Thompson, M. A.; Braiding, Catherine; Burton, M. G.; Csengeri, T.; Dempsey, Jessica T.; Figura, C.; Froebrich, D.; Menten, K. M.; Schüller, F.; Smith, Michael D.; Wyrowski, F.

doi:10.1093/mnras/stx2258

Cited by 300 publications

(686 citation statements)

References 140 publications

(219 reference statements)

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“…most massive, most luminous, etc) sources may host a methanol maser as all sources fall above the thresholds on each property to host a methanol maser. Notably, we find that sources down to a threshold of ∼ 0.08 g cm −2 are capable of hosting a methanol maser and therefore a massive protostar, comparable to the threshold of approximately 0.05 g cm −2 for massive star formation found by Urquhart et al (2018). As 6.7 GHz methanol masers exclusively trace high-mass protostars, this suggests that this all sources above this threshold on mass surface density may form high-mass stars.…”

Section: Physical Interpretationsupporting

confidence: 67%

The evolutionary status of protostellar clumps hosting class II methanol masers

Jones

Fuller

Breen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The Methanol MultiBeam survey (MMB) provides the most complete sample of Galactic massive young stellar objects (MYSOs) hosting 6.7 GHz class II methanol masers. We characterise the properties of these maser sources using dust emission detected by the Herschel Infrared Galactic Plane Survey (Hi-GAL) to assess their evolutionary state. Associating 731 (73%) of MMB sources with compact emission at four Hi-GAL wavelengths, we derive clump properties and define the requirements of a MYSO to host a 6.7 GHz maser. The median far-infrared (FIR) mass and luminosity are 630 M and 2500 L for sources on the near side of Galactic centre and 3200 M and 10000 L for more distant sources. The median luminosity-to-mass ratio is similar for both at ∼4.2 L / M . We identify an apparent minimum 70 µm luminosity required to sustain a methanol maser of a given luminosity (with L 70 ∝ L 6.7 0.6 ). The maser host clumps have higher mass and higher FIR luminosities than the general Galactic population of protostellar MYSOs. Using principal component analysis, we find 896 protostellar clumps satisfy the requirements to host a methanol maser but lack a detection in the MMB. Finding a 70 µm flux density deficiency in these objects, we favour the scenario in which these objects are evolved beyond the age where a luminous 6.7 GHz maser can be sustained. Finally, segregation by association with secondary maser species identifies evolutionary differences within the population of 6.7GHz sources.

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Section: Physical Interpretationsupporting

confidence: 67%

The evolutionary status of protostellar clumps hosting class II methanol masers

Jones

Fuller

Breen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Similar amplitudes have been determined also from observations by Reid et al (2014) and from simulations by Ramón-Fox & Bonnell (2018). These uncertainties on RVs introduce errors on the estimated distances that can be as large as ∼ 1 kpc (Roman-Duval et al 2009;Urquhart et al 2018;Ramón-Fox & Bonnell 2018).…”

Section: Uncertainties On Kinematic Distancessupporting

confidence: 76%

The Hi-GAL catalogue of dusty filamentary structures in the Galactic plane

Schisano

Molinari

Elia

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The recent data collected by Herschel have confirmed that interstellar structures with filamentary shape are ubiquitously present in the Milky Way. Filaments are thought to be formed by several physical mechanisms acting from the large Galactic scales down to the sub-pc fractions of molecular clouds, and they might represent a possible link between star formation and the large-scale structure of the Galaxy. In order to study this potential link, a statistically significant sample of filaments spread throughout the Galaxy is required. In this work we present the first catalogue of 32, 059 candidate filaments automatically identified in the Hi-GAL survey of the entire Galactic Plane. For these objects we determined morphological (length, l a , and geometrical shape) and physical (average column density, N H 2 , and average temperature, T) properties. We identified filaments with a wide range of properties: 2 ≤ l a ≤ 100 , 10 20 ≤ N H 2 ≤ 10 23 cm −2 and 10 ≤ T ≤ 35 K. We discuss their association with the Hi-GAL compact sources, finding that the most tenuous (and stable) structures do not host any major condensation and we also assign a distance to ∼ 18, 400 filaments for which we determine mass, physical size, stability conditions and Galactic distribution. When compared to the spiral arms structure, we find no significant difference between the physical properties of on-arm and inter-arm filaments. We compared our sample with previous studies, finding that our Hi-GAL filament catalogue represents a significant extension in terms of Galactic coverage and sensitivity. This catalogue represents an unique and important tool for future studies devoted to understanding the filament life-cycle.

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“…3 (2015). The four spiral and local arms are shown by different colors and their positions are taken from Urquhart et al (2018) and its references Taylor & Cordes (1993) and Bronfman et al (2000). Most of the errors of v lsr are less than 2 km s −1 and the associated error bars are smaller than the point size in (a).…”

Section: Kinematic Uncertaintymentioning

confidence: 99%

“…The fraction is calculated by the number ratio of HMSCs to massive ATLASGAL clumps in each distance range, as shown in the numbers in figure. The sample of ATLASGAL clumps is taken from the catalog in Csengeri et al (2014) and the clump distance is taken from Urquhart et al (2018). ATLASGAL clumps with a 870 µm peak intensity higher than 0.5 Jy beam −1 are extracted to be in line with the column density criterion for massive star formation in Sect.…”

Section: Difference In Propertiesmentioning

confidence: 99%

H II regions and high-mass starless clump candidates

Zhang

Zavagno

Yuan

et al. 2020

A&A

Self Cite

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Context. The role of ionization feedback on high-mass (> 8 M ) star formation is still highly debated. Questions remain concerning the presence of nearby H ii regions changes the properties of early high-mass star formation and whether H ii regions promote or inhibit the formation of high-mass stars. Aims. To characterize the role of H ii regions on the formation of high-mass stars, we study the properties of a sample of candidates high-mass starless clumps (HMSCs), of which about 90% have masses larger than 100 M . These high-mass objects probably represent the earliest stages of high-mass star formation; we search if (and how) their properties are modified by the presence of an H ii region. Methods. We took advantage of the recently published catalog of HMSC candidates. By cross matching the HMSCs and H ii regions, we classified HMSCs into three categories: 1) The HMSCs associated with H ii regions both in the position in the projected plane of the sky and in velocity; 2) HMSCs associated in the plane of the sky, but not in velocity; and 3) HMSCs far away from any H ii regions in the projected sky plane. We carried out comparisons between associated and nonassociated HMSCs based on statistical analyses of multiwavelength data from infrared to radio. Results. We show that there are systematic differences of the properties of HMSCs in different environments. Statistical analyses suggest that HMSCs associated with H ii regions are warmer, more luminous, more centrally-peaked and turbulent. We also clearly show, for the first time, that the ratio of bolometric luminosity to envelope mass of HMSCs (L/M) could not be a reliable evolutionary probe for early massive star formation due to the external heating effects of the H ii regions. Conclusions. We show HMSCs associated with H ii regions present statistically significant differences from HMSCs far away from H ii regions, especially for dust temperature and L/M. More centrally peaked and turbulent properties of HMSCs associated with H ii regions may promote the formation of high-mass stars by limiting fragmentation. High-resolution interferometric surveys toward HMSCs are crucial to reveal how H ii regions impact the star formation process inside HMSCs.

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ATLASGAL – properties of a complete sample of Galactic clumps★

Cited by 300 publications

References 140 publications

The evolutionary status of protostellar clumps hosting class II methanol masers

The evolutionary status of protostellar clumps hosting class II methanol masers

The Hi-GAL catalogue of dusty filamentary structures in the Galactic plane

H II regions and high-mass starless clump candidates

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ATLASGAL – properties of a complete sample of Galactic clumps★

Cited by 300 publications

References 140 publications

The evolutionary status of protostellar clumps hosting class II methanol masers

The evolutionary status of protostellar clumps hosting class II methanol masers

The Hi-GAL catalogue of dusty filamentary structures in the Galactic plane

H II regions and high-mass starless clump candidates

Contact Info

Product

Resources

About

H II regions and high-mass starless clump candidates