Spectrophotometric distances to Galactic H ii regions

Moisés, A. P.; Damineli, A.; Figuerêdo, E.; Blum, Robert; Conti, Peter S.; Barbosa, C. L.

doi:10.1111/j.1365-2966.2010.17713.x

Cited by 79 publications

(106 citation statements)

References 95 publications

(297 reference statements)

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“…This is supported by statistical studies; for instance, Battersby et al (2011) show that tracers of star formation are more likely associated with higher dust temperatures, while König et al (2016) show an increase in dust temperature with evolutionary stage by fitting the spectral energy distribution of ATLASGAL clumps over a range of evolutionary stages. Hence, a temperature correction is neces- Sanna et al (2014) (g) Moisés et al (2011) ( †) We revised the spectrophotometric distance of 1.81 kpc by Moisés et al (2011). (h) Wu et al (2014) (i) Wu et al (2012) (j) Reid et al (2014) (k) Dutra et al (2003) (l) Straw et al (1987) (m) Xu et al (2011) (n) Sanna et al (2009) (o) Leurini et al (2011) (p) Kurayama et al (2011) (q) Russeil (2003) (r) Motogi et al (2011) (s) López et al (2011) ( ‡) Peretto et al (2013) adopts 3.25 kpc.…”

Section: Temperature Estimatesmentioning

confidence: 99%

“…We collected distance estimates from the literature using primarily maser parallax measurements (see Reid et al 2014 for an overview) or spectrophotometric distance estimates (e.g. Russeil 2003;Moisés et al 2011) for the known GMCs. For the remaining unassociated sources we used the high-density tracer NH 3 to determine kinematic distances from Wienen et al (2012Wienen et al ( , 2015.…”

Section: Distances and Association With Massive Molecular Complexesmentioning

confidence: 99%

See 1 more Smart Citation

The ATLASGAL survey: The sample of young massive cluster progenitors

Csengeri

Bontemps

Wyrowski

et al. 2017

A&A

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Context. The progenitors of high-mass stars and clusters are still challenging to recognise. Only unbiased surveys, sensitive to compact regions of high dust column density, can unambiguously reveal such a small population of particularly massive and cold clumps. Aims. Here we use the ATLASGAL survey to identify a sample of candidate progenitors of massive clusters in the inner Galaxy. Methods. We characterise a flux limited sample of compact sources selected from the ATLASGAL survey. Sensitive mid-infrared data at 21−24 µm from the WISE and MIPSGAL surveys were explored to search for embedded objects, and complementary spectroscopic data were used to investigate their stability and their star formation activity. Results. We identify an unbiased sample of infrared-quiet massive clumps in the Galaxy that potentially represent the earliest stages of massive cluster formation. An important fraction of this sample consists of sources that have not been studied in detail before. We first find that clumps hosting more evolved embedded objects and infrared-quiet clumps exhibit similar physical properties in terms of mass and size, suggesting that the sources are not only capable of forming high-mass stars, but likely also follow a single evolutionary track leading to the formation of massive clusters. The majority of the clumps are likely not in virial-equilibrium, suggesting collapse on the clump scale. Conclusions. We identify the precursors of the most massive clusters in the Galaxy within our completeness limit, and argue that these objects are undergoing large-scale collapse. This is in line with the low number of infrared-quiet massive clumps and earlier findings that star formation, in particular for high-mass objects is a fast, dynamic process. We propose a scenario in which massive clumps start to fragment and collapse before their final mass is accumulated indicating that strong self-gravity and global collapse is needed to build up rich clusters and the most massive stars.

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Section: Temperature Estimatesmentioning

confidence: 99%

Section: Distances and Association With Massive Molecular Complexesmentioning

confidence: 99%

The ATLASGAL survey: The sample of young massive cluster progenitors

Csengeri

Bontemps

Wyrowski

et al. 2017

A&A

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“…Pinheiro et al (2010) identified the ionizing stars in nine HII regions, and derived their photometric distances. Moisés et al (2011) used the nearinfrared color images to study the stellar content of 35 HII regions, and estimated their spectrophotometric distances. Russeil et al (2012) analyzed the data of OB stars in two star forming complexes (see , NGC 6334 and NGC 6357, and revised their photometric distances.…”

Section: Hii Regionsmentioning

confidence: 99%

“…The kinematic distance ambiguity for many HII regions, GMCs, and 6.7 GHz methanol masers has been solved (e.g., Roman-Duval et Lépine et al 2011;Anderson et al 2012;Urquhart et al 2012;Jones & Dickey 2012), which enables us to estimate their kinematic distances. In addition, the more reliable trigonometric or photometric distances of a number of HII regions or masers have been measured (e.g., Rygl et al 2010;Sato et al 2010a; Moisés et al 2011;Xu et al 2011Xu et al , 2013Russeil et al 2012;Zhang et al 2014;Foster & Brunt 2014). The available spiral tracers have almost doubled as compared to those listed in Hou et al (2009).…”

Section: Introductionmentioning

confidence: 99%

The observed spiral structure of the Milky Way

Hou

Han

2014

A&A

227

233

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Context. The spiral structure of the Milky Way is not yet well determined. The keys to understanding this structure are to increase the number of reliable spiral tracers and to determine their distances as accurately as possible. HII regions, giant molecular clouds (GMCs), and 6.7 GHz methanol masers are closely related to high mass star formation, and hence they are excellent spiral tracers. The distances for many of them have been determined in the literature with trigonometric, photometric, and/or kinematic methods. Aims. We update the catalogs of Galactic HII regions, GMCs, and 6.7 GHz methanol masers, and then outline the spiral structure of the Milky Way. Methods. We collected data for more than 2500 known HII regions, 1300 GMCs, and 900 6.7 GHz methanol masers. If the photometric or trigonometric distance was not yet available, we determined the kinematic distance using a Galaxy rotation curve with the current IAU standard, R 0 = 8.5 kpc and Θ 0 = 220 km s −1 , and the most recent updated values of R 0 = 8.3 kpc and Θ 0 = 239 km s −1 , after velocities of tracers are modified with the adopted solar motions. With the weight factors based on the excitation parameters of HII regions or the masses of GMCs, we get the distributions of these spiral tracers.Results. The distribution of tracers shows at least four segments of arms in the first Galactic quadrant, and three segments in the fourth quadrant. The Perseus Arm and the Local Arm are also delineated by many bright HII regions. The arm segments traced by massive star forming regions and GMCs are able to match the HI arms in the outer Galaxy. We found that the models of three-arm and four-arm logarithmic spirals are able to connect most spiral tracers. A model of polynomial-logarithmic spirals is also proposed, which not only delineates the tracer distribution, but also matches the observed tangential directions.

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“…Kinematic distances have been determined for 17 of these masers by Green & McClure-Griffiths (2011) 2 , spectrophotometric distances have been determined for 2 masers by Moisés et al (2011) and maser parallax distances are available for another 2 sources (MMB196.454-01.677 and MMB232.620+00.996; Honma et al 2007 andReid et al 2009b, respectively). Combined with the sources associated with complexes, these two steps provide distances for 38 of the 77 methanol masers of interest for this study.…”

Section: Literature Distancesmentioning

confidence: 99%

The almost ubiquitous association of 6.7-GHz methanol masers with dust★

Urquhart

Moore

Menten

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We report the results of 870-µmcontinuum observations, using the Large APEX Bolometer Camera (LABOCA), towards 77 class-II, 6.7-GHz methanol masers identified by the Methanol Multibeam (MMB) survey to map the thermal emission from cool dust towards these objects. These data complement a study of 630 methanol masers associated with compact dense clumps identified from the ATLASGAL survey. Compact dust emission is detected towards 70 sources, which implies a dust-association rate of 99 per cent for the full MMB catalogue. Evaluation of the derived dust and maser properties leads us to conclude that the combined sample represents a single population tracing the same phenomenon. We find median clump masses of a few 10 3 M ⊙ and that all but a handful of sources satisfy the mass-size criterion required for massive star formation. This study provides the strongest evidence of the almost ubiquitous association of methanol masers with massive, star-forming clumps. The fraction of methanol-maser associated clumps is a factor of ∼2 lower in the outer Galaxy than the inner Galaxy, possibly a result of the lower metallicity environment of the former. We find no difference in the clump-mass and maser-luminosity distributions of the inner and outer Galaxy. The maser-pumping and clump-formation mechanisms are therefore likely to be relatively invariant to Galactic location. Finally, we use the ratio of maser luminosity and clump mass to investigate the hypothesis that the maser luminosity is a good indicator of the evolutionary stage of the embedded source, however, we find no evidence to support this.

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Spectrophotometric distances to Galactic H ii regions

Cited by 79 publications

References 95 publications

The ATLASGAL survey: The sample of young massive cluster progenitors

The ATLASGAL survey: The sample of young massive cluster progenitors

The observed spiral structure of the Milky Way

The almost ubiquitous association of 6.7-GHz methanol masers with dust★

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