ATLASGAL – evolutionary trends in high-mass star formation

Urquhart, J. S.; Wells, M. R. A.; Pillai, T.; Leurini, S.; Giannetti, A.; Moore, T. J. T.; Thompson, M. A.; Figura, C.; Colombo, D.; Yang, A. Y.; Koenig, C.; Wyrowski, F.; Menten, K. M.; Rigby, A. J.; Eden, David; Ragan, S. E.

doi:10.1093/mnras/stab3511

Cited by 43 publications

(53 citation statements)

References 120 publications

(102 reference statements)

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“…In contrast, the cIIM masers at 6.7 GHz appear in the later phase of the evolution. It is also in agreement with the recent study of Urquhart et al (2022), which shows that outflow activity is the earliest indication that star formation has begun. Water and cIM masers may reside in shock waves of the outflows from the protostars (Kaufman & Neufeld 1996;Voronkov et al 2006).…”

Section: The Evolution Trends Of Different Maser Speciessupporting

confidence: 93%

“…The physical properties (distance, dust temperature, luminosity, mass, and gas column density) of approximately 8000 dense clumps have been determined (Urquhart et al 2018). The latest release of ATLASGAL CSC is available in Urquhart et al (2022). Comparison of the water maser samples with the ATLASGAL CSC dense clumps provides a straightforward and convenient way of investigating the physical conditions in which these masers arise.…”

Section: The Maser Sample Infrared and Submillimeter Clump Catalogsmentioning

confidence: 99%

“…The sample of OH and CH 3 OH masers at 6.7 and 12 GHz is close to the sample used by Billington et al (2020), complemented by additional detections stored in the maser database (Ladeyschikov et al 2019) in 16 papers (e.g., Caswell et al 1995;Caswell 1996;Beuther et al 2002;Bartkiewicz et al 2009;Caswell 2009;Cyganowski et al 2009). In this section, we used the latest version of ATLASGAL CSC (Urquhart et al 2022).…”

Section: The Evolution Trends Of Different Maser Speciesmentioning

confidence: 99%

“…Both catalogs were used for analyzing sources associated with water masers. Interestingly, among the 814 water maser sources in SFRs, 80% are associated with submillimeter sources from the ATLASGAL complete compact source catalog (Contreras et al 2013;Urquhart et al 2014Urquhart et al , 2018Urquhart et al , 2022 (hereafter ATLASGAL CSC) and 85% are associated with infrared sources from the Hi-GAL compact source catalog II (Elia et al 2021) (hereafter Hi-GAL CSC). Based on the ATLASGAL physical parameters catalog, we perform a search of water maser sources toward ATLASGAL clumps to explore the detection rates toward sources with a high probability of maser detection based on the generalized linear model (hereafter GLM) of maser presence.…”

Section: Introductionmentioning

confidence: 99%

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Water Masers as an Early Tracer of Star Formation

Ladeyschikov¹,

Gong

Соболев³

et al. 2022

ApJS

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We present a study of the correlation between 22 GHz water maser emission and far-infrared/submillimeter (IR/sub-mm) sources. The generalized linear model (GLM) is used to predict H2O maser detection in a particular source with defined physical parameters. We checked the GLM predictions by observing a sample of selected sources with the Effelsberg 100 m telescope. In total, 359 sources were observed. H2O masers were detected in 124 sources, with 56 new detections. We found 22 sources with a significant flux variability. Using the GLM analysis, we estimate that 2392 ± 339 star formation regions (SFRs) in the Galaxy may harbor H2O masers detectable by single-dish observations at the noise level of ∼0.05 Jy. Analyzing the luminosity-to-mass ratio (L/M) of the ATLASGAL and Hi-GAL clumps associated with different maser species, we find that 22 GHz water masers have significantly lower values of L/M in comparison to 6.7 GHz class II methanol and 1665 MHz OH masers. This implies that 22 GHz water masers may appear prior to 6.7 GHz methanol and OH masers in the evolutionary sequence of SFRs. From the analysis of physical offsets between host clumps and maser interferometric positions, we found no significant difference between the H2O and class II methanol maser offsets against the host clump position. We conclude that the tight association between water masers and IR/sub-mm sources may provide insight into the pumping conditions of these masers and the evolutionary stages of their onset.

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Section: The Evolution Trends Of Different Maser Speciessupporting

confidence: 93%

Section: The Maser Sample Infrared and Submillimeter Clump Catalogsmentioning

confidence: 99%

Section: The Evolution Trends Of Different Maser Speciesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Water Masers as an Early Tracer of Star Formation

Ladeyschikov¹,

Gong

Соболев³

et al. 2022

ApJS

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“…The definitions of the evolutionary stages of HMSFRs, including physical and chemical classifications, are still not clear (Hoq et al 2013;Miettinen 2014;Gerner et al 2014;Urquhart et al 2014b;Zhang et al 2016;König et al 2017;Urquhart et al 2019Urquhart et al , 2022. Based on the physical properties of the clumps, the sequence of a HMSFR is usually divided into four evolutionary stages: quiescent, high-mass protostellar object (protostellar), massive young stellar object (YSO), and Hii region (see Urquhart et al 2019, 2022, andreferences therein).…”

Section: Evolution Of Hc 3 Nmentioning

confidence: 99%

Cyanopolyyne line survey towards high-mass star-forming regions with TMRT

Wang,

Zhang,

Yan

et al. 2022

Preprint

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Context. Cyanopolyynes (HC 2n+1 N, n = 1,2,3), which are the linear carbon chain molecules, are precursors for the prebiotic synthesis of simple amino acids. They are important for understanding prebiotic chemistry and may be good tracers of the star formation sequence. Aims. We aim to search for cyanopolyynes in high-mass star-forming regions (HMSFRs) at possibly different evolutionary stages, investigate the evolution of HC 3 N and its relation with shock tracers, and detect the existence of HC 5 N and HC 7 N in HMSFRs with a formed protostar. Methods. We carried out a cyanopolyyne line survey towards a large sample of HMSFRs using the Shanghai Tian Ma 65m Radio Telescope (TMRT). Our sample consisted of 123 targets taken from the TMRT C band line survey. It included three kinds of sources, namely those with detection of the 6.7 GHz CH 3 OH maser alone, with detection of the radio recombination line (RRL) alone, and with detection of both (hereafter referred to as Maser-only, RRL-only, and Maser-RRL sources, respectively). For our sample with detection of cyanopolyynes, their column densities were derived using the rotational temperature measured from the NH 3 lines. We constructed and fitted the far-infrared (FIR) spectral energy distributions (SED; obtained from the Herschel FIR data and the Atacama Pathfinder Experiment data at 870 µm) of our HC 3 N sources. Moreover, by analysing the relation between HC 3 N and other shock tracers, we also investigate whether HC 3 N is a good tracer of shocks. Results. We detected HC 3 N in 38 sources, HC 5 N in 11 sources, and HC 7 N in G24.790+0.084, with the highest detection rate being found for Maser-RRL sources and a very low detection rate found for RRL-only sources. The mean column density of HC 3 N was found to be (1.75±0.42)×10 13 , (2.84±0.47)×10 13 , and (0.82±0.15)×10 13 cm −2 for Maser-only, Maser-RRL, and RRL-only sources, respectively. Based on a fit of the FIR SED, we derive their dust temperatures, H 2 column densities, and abundances of cyanopolyynes relative to H 2 . The mean relative abundance of HC 3 N was found to be (1.22±0.52)×10 −10 for Maser-only, (5.40±1.45)×10 −10 for Maser-RRL, and (1.65±1.50)×10 −10 for RRL-only sources, respectively. Conclusions. The detection rate, the column density, and the relative abundance of HC 3 N increase from Maser-only to Maser-RRL sources and decrease from Maser-RRL to RRL-only sources. This trend is consistent with the proposed evolutionary trend of HC 3 N under the assumption that our Maser-only, Maser-RRL, and RRL-only sources correspond to massive young stellar objects, ultracompact Hii regions, and normal classical Hii regions, respectively. Our detections enlarge the sample of HC 3 N in HMSFRs and support the idea that unsaturated complex organic molecules can exist in HMSFRs with a formed protostar. Furthermore, a statistical analysis of the integrated line intensity and column density of HC 3 N and shock-tracing molecules (SiO, H 2 CO) enabled us to find positive correlations between them. This suggests th...

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Evolutionary Trends in Star Formation

Urquhart

2022

Proc. IAU

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Over the past 20 years, the Galactic plane has been surveyed at high resolution at wavelengths from 1 micron through to 20 cm. The combination of these surveys has produced large samples of deeply embedded young stars located across the Galactic disc. These continuum surveys are complemented by spectral line surveys of thermal, radio recombination, and molecular maser (OH, H2O, CH3OH) lines. The identified sources cover the whole range of evolutionary stages in the star formation process, allowing the physical properties of these stages to be measured. This information has been used to calculate the star formation efficiency and star formation rate of the Milky Way and to evaluate the impact of environment and location within the disc. This review provides an overview of some of the most significant studies in recent years and discusses how the evolutionary sequence has been used to investigate the correlation of other star formation tracers and maser associations.

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ATLASGAL – evolutionary trends in high-mass star formation

Cited by 43 publications

References 120 publications

Water Masers as an Early Tracer of Star Formation

Water Masers as an Early Tracer of Star Formation

Cyanopolyyne line survey towards high-mass star-forming regions with TMRT

Evolutionary Trends in Star Formation

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