A Survey of the SO
 J
 
 K
 
  = 1
 0
 –0
 1
 Transition toward Massive Star‐forming Regions

Mateen, Mala; Höfner, P.; Araya, E. D.

doi:10.1086/508423

Cited by 7 publications

(6 citation statements)

References 55 publications

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“…The FIR luminosities of our sources, taken from Wood & Churchwell (1989); Kurtz et al (1994); Beuther et al (2002b); Mateen et al (2006); Walsh et al (1997) are the IR fluxes from IRAS converted into total luminosities for the sources at the distances listed in those papers. The FIR luminosity can be taken as a tracer of the total luminosity of the source if the distance is known (Wood & Churchwell 1989).…”

Section: Resultsmentioning

confidence: 99%

Looking for outflow and infall signatures in high-mass star-forming regions

Klaassen

Testi

Beuther

2012

A&A

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Context. Many physical parameters change with time in star-forming regions. Here we attempt to correlate changes in the infall and outflow motions in high-mass star-forming regions with evolutionary stage using JCMT observations. Aims. From a sample of 45 high-mass star-forming regions in three phases of evolution, we investigate the presence of established infall and outflow tracers to determine whether there are any trends attributable to the age of the source. Methods. We obtained JCMT observations of HCO + /H 13 CO + J = 4−3 to trace large-scale infall, and SiO J = 8−7 to trace recent outflow activity. We compared the infall and outflow detections to the evolutionary stage of the host source (high-mass protostellar objects, hypercompact HII regions, and ultracompact HII regions). Results. We find a surprising lack of SiO detections in the middle stage (hypercompact HII regions), which may be an observational bias. When SiO is detected, we find that the integrated intensity of the line increases with evolutionary stage. The integrated intensity of SiO varies with the full width at half maximum of the H 13 CO + . All of the sources with infall signatures onto ultracompact HII regions have corresponding outflow signatures as well.

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Section: Resultsmentioning

confidence: 99%

Looking for outflow and infall signatures in high-mass star-forming regions

Klaassen

Testi

Beuther

2012

A&A

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“…The probe of massive star-forming clumps, SO J k = 1 0 − 0 1 (i.e. 30 GHz) emission, has also been detected in both regions (Mateen, Hofner, & Araya 2006).…”

Section: Introductionmentioning

confidence: 88%

Infrared study of the star-forming region associated with the UC HII regions G45.07+0.13 and G45.12+0.13

Azatyan

Nikoghosyan

Harutyunian

et al. 2022

Publ. Astron. Soc. Aust.

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Ultra-compact H ii (UC HII) regions are an important phase in the formation and early evolution of massive stars and a key component of the interstellar medium (ISM). The main objectives of this work are to study the young stellar population associated with the G45.07+0.13 and G45.12+0.13 UC HII regions, as well as the ISM in which they are embedded. We determined the distribution of the hydrogen column density (N( $\mathrm{H}_2$ )) and dust temperature ( $T_d$ ) in the molecular cloud using Modified blackbody fitting on Herschel images obtained in four bands: 160, 250, 350, and $500\,\unicode{x03BC}\mathrm{m}$ . We used near-, mid-, and far-infrared photometric data to identify and classify the young stellar objects (YSOs). Their main parameters were determined by the radiation transfer models. We also constructed a colour-magnitude diagram and K luminosity functions (KLFs) to compare the parameters of stellar objects with the results of the radiative transfer models. We found that N( $\mathrm{H}_2$ ) varies from ${\sim}3.0 \times 10^{23}$ to $5.5 \times 10^{23}\,\mathrm{cm}^{-2}$ within the G45.07+0.13 and G45.12+0.13 regions, respectively. The maximum $T_d$ value is 35 K in G45.12+0.13 and 42 K in G45.07+0.13. $T_d$ then drops significantly from the centre to the periphery, reaching about 18–20 K at distances of ${\sim}2.6$ and ${\sim}3.7\,\mathrm{pc}$ from InfraRed Astronomical Satellite (IRAS) 19110+1045 (G45.07+0.13) and IRAS 19111+1048 (G45.12+0.13), respectively. The gas plus dust mass value included in G45.12+0.13 is ${\sim}3.4 \times 10^5\,\mathrm{M}_\odot$ and ${\sim}1.7 \times 10^5\,\mathrm{M}_\odot$ in G45.07+0.13. The UC HII regions are connected through a cold ( $T_d = 19\,\mathrm{K}$ ) bridge. The radial surface density distribution of the identified 518 YSOs exhibits dense clusters in the vicinity of both IRAS sources. The parameters of YSOs in the IRAS clusters (124 objects) and 394 non-cluster objects surrounding them show some differences. About 75% of the YSOs belonging to the IRAS clusters have an evolutionary age greater than $10^6$ yr. Their slope $\alpha$ of the KLF agrees well with a Salpeter-type initial mass function (IMF) ( $\gamma = 1.35$ ) for a high mass range (O–F stars, $\beta \sim 2$ ) at 1 Myr. The non-cluster objects are uniformly distributed in the molecular cloud, 80% of which are located to the right of the 0.1 Myr isochrone. The slope $\alpha$ of the KLF of non-cluster objects is $0.55\,\pm\,0.09$ , corresponding better to a Salpeter-type IMF for low-mass objects (G–M stars, $\beta \sim 1$ ). Our results show that two dense stellar clusters are embedded in these two physically connected UC HII regions. The clusters include several high- and intermediate-mass zero-age main sequence stellar objects. Based on the small age spread of the stellar objects, we suggest that the clusters originate from a single triggering shock. The extended emission observed in both UC HII regions is likely due to the stellar clusters.

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“…All sources are within 10 • of the Galactic center and have not been studied in detail previously. CN138 is near IRAS source 18073-2046, which has been studied by Mateen, Hofner & Araya (2006) in SO J=1-0, Scoville et al (1987) in radio recombination lines, Walsh et al (1997) in methanol masers and Slysh et al (1999) in methanol masers. However, IRAS 18073-2046 appears to be coincident with CN139 in the bubble catalog, a large, complex bubble.…”

Section: Datamentioning

confidence: 99%

Ir Dust Bubbles. Ii. Probing the Detailed Structure and Young Massive Stellar Populations of Galactic H Ii Regions

Watson¹,

Corn²,

Churchwell³

et al. 2009

ApJ

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We present an analysis of late-O/early-B-powered, parsec-sized bubbles and associated star-formation using 2MASS, GLIMPSE, MIPSGAL and MAGPIS surveys. Three bubbles were selected from the Churchwell et al. (2007) catalog. We confirm that the structure identified in Watson et al. (2008) holds in less energetic bubbles, i.e. a PDR, identified by 8 µm emission due to PAHs surrounds hot dust, identified by 24 µm emission and ionized gas, identified by 20 cm continuum. We estimate the dynamical age of two bubbles by comparing bubble sizes to numerical models of Hosokawa & Inutsuka (2006). We also identify and analyze candidate young stellar objects (YSOs) using SED fitting and identify sites of possible triggered star-formation. Lastly, we identify likely ionizing sources for two sources based on SED fitting.

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A Survey of the SO J _K = 1 ₀ –0 ₁ Transition toward Massive Star‐forming Regions

Cited by 7 publications

References 55 publications

Looking for outflow and infall signatures in high-mass star-forming regions

Looking for outflow and infall signatures in high-mass star-forming regions

Infrared study of the star-forming region associated with the UC HII regions G45.07+0.13 and G45.12+0.13

Ir Dust Bubbles. Ii. Probing the Detailed Structure and Young Massive Stellar Populations of Galactic H Ii Regions

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A Survey of the SO J K = 1 0 –0 1 Transition toward Massive Star‐forming Regions

Cited by 7 publications

References 55 publications

Looking for outflow and infall signatures in high-mass star-forming regions

Looking for outflow and infall signatures in high-mass star-forming regions

Infrared study of the star-forming region associated with the UC HII regions G45.07+0.13 and G45.12+0.13

Ir Dust Bubbles. Ii. Probing the Detailed Structure and Young Massive Stellar Populations of Galactic H Ii Regions

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Product

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A Survey of the SO J _K = 1 ₀ –0 ₁ Transition toward Massive Star‐forming Regions