Characterizing the radio continuum nature of sources in the massive star-forming region W75N (B)

Rodríguez-Kamenetzky, Adriana; Carrasco-González, Carlos; Torrelles, J. M.; Vlemmings, Wouter; Rodrı́guez, Luis F.; Surcis, G.; Gómez, José F.; Cantó, J.; Goddi, C.; Kim, J S; Kim, S W; Añez-López, N.; Curiel, S.; Langevelde, H. J. van

doi:10.1093/mnras/staa1742

Cited by 11 publications

(23 citation statements)

References 39 publications

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“…Shepherd 2001;Minh et al 2010). Three radio continuum sources were also detected towards MM1 (VLA1, VLA2 and VLA3), which have been identified as ultra-compact HII (UC HII) regions or thermal jets (Hunter et al 1994;Torrelles et al 1997;Shepherd et al 2003;Carrasco-González et al 2010;Rodríguez-Kamenetzky et al 2020). Shepherd et al (2004) found that the VLA sources drive high-velocity molecular outflows traced by SiO (2−1 and 1−0) emission.…”

Section: Introductionmentioning

confidence: 99%

Protostellar Interferometric Line Survey of the Cygnus X region (PILS-Cygnus)

Walt

Kristensen

Jørgensen

et al. 2021

A&A

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Context. Complex organic molecules (COMs) are commonly detected in and near star-forming regions. However, the dominant process in the release of these COMs from the icy grains – where they predominately form – to the gas phase is still an open question. Aims. We investigate the origin of COM emission in a high-mass protostellar source, CygX-N30 MM1, through high-angular-resolution interferometric observations over a continuous broad frequency range. Methods. We used 32 GHz Submillimeter Array observations with continuous frequency coverage from 329 to 361 GHz at an angular resolution of ~1″ to do a line survey and obtain a chemical inventory of the source. The line emission in the frequency range was used to determine column densities and excitation temperatures for the COMs. We also mapped out the intensity distribution of the different species. Results. We identified approximately 400 lines that can be attributed to 29 different molecular species and their isotopologues. We find that the molecular peak emission is along a linear gradient, and coincides with the axis of red- and blueshifted H2CO and CS emission. Chemical differentiation is detected along this gradient, with the O-bearing molecular species peaking towards one component of the system and the N- and S-bearing species peaking towards the other. The chemical gradient is offset from but parallel to the axis through the two continuum sources. The inferred column densities and excitation temperatures are compared to other sources where COMs are abundant. Only one deuterated molecule is detected, HDO, while an upper limit for CH2DOH is derived, leading to a D/H ratio of <0.1%. Conclusions. We conclude that the origin of the observed COM emission is probably a combination of the young stellar sources along with accretion of infalling material onto a disc-like structure surrounding a young protostar and located close to one of the continuum sources. This disc and protostar are associated with the O-bearing molecular species, while the S- and N-bearing species on the other hand are associated with the other continuum core, which is probably a protostar that is slightly more evolved than the other component of the system. The low D/H ratio likely reflects a pre-stellar phase where the COMs formed on the ices at warm temperatures (~30 K), where the deuterium fractionation would have been inefficient. The observations and results presented here demonstrate the importance of good frequency coverage and high angular resolution when disentangling the origin of COM emission.

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Section: Introductionmentioning

confidence: 99%

Protostellar Interferometric Line Survey of the Cygnus X region (PILS-Cygnus)

Walt

Kristensen

Jørgensen

et al. 2021

A&A

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“…G345.49+1.47 is part of a small group of HMYSOs toward which active disk accretion has been proposed while simultaneously exciting an Hii region. Other like sources are G35.20−0.74N and recently W75N (B) VLA1 (Rodríguez-Kamenetzky et al 2020). G345.49+1.47 was also part of the sources studied by Cesaroni et al (2017) at 0.…”

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confidence: 84%

A photoionized accretion disk around a young high-mass star

Guzmán,

Sanhueza,

Zapata

et al. 2020

Preprint

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We present high spatial resolution (52 au) observations of the high-mass young stellar object (HMYSO) G345.4938+01.4677 made using the Atacama Large Millimeter/submillimeter Array (ALMA). This O-type HMYSO is located at 2.38 kpc and it is associated with a luminosity of 1.5 × 10 5 L . We detect circumstellar emission from the H38β hydrogen recombination line showing a compact structure rotating perpendicularly to the previously detected radio jet. We interpret this emission as tracing a photo-ionized accretion disk around the HMYSO. While this disk-like structure seems currently too small to sustain continued accretion, the data present direct observational evidence of how disks can effectively survive the photo-ionization feedback from young high-mass stars. We also report the detection of a low-mass young stellar object in the vicinity of the HMYSO and suggest that it forms a high-mass and low-mass star binary system. INTRODUCTION.In the recent years, and with the advent of new observational instruments such as the Atacama Large Millimeter/sub-millimeter Array (ALMA), evidence have been gathering pointing toward most high-mass stars acquiring their mass through disk accretion (Tan et al. 2014). It is becoming apparent that the principal characteristic which allows accretion to proceed onto most young high-mass young stellar objects (HMYSOs) -despite the venerable theoretical problems of radiation and ionization feedback (Wolfire & Cassinelli 1987;Kahn 1974;Larson & Starrfield 1971) -is that this accretion occurs through a disk (Kuiper et al. 2010;Yorke & Sonnhalter 2002;Nakano 1989).The signposts of disk accretion toward embedded HMYSOs are mainly of two kinds: highly collimated (aperture ≤ 5 • ) fast jets with velocities comparable to the escape speed of the compact object, and compact (sub-1000 au) circumstellar disks. Slower, less collimated outflows can be produced by other processes like ionization feedback (Peters et al. 2012), magnetic braking (Hennebelle et al. 2011, and mergers of smaller stars (Bally & Zinnecker 2005). Rotating structures ∼3000 au or bigger (Beltrán & de Wit 2016) are too large to link them necessarily with disk accretion onto a central, compact HMYSO, and may even be transient non-equilibrium structures (so-called toroids, Cesaroni et al. 2006).

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“…The radio sources are unresolved in the map. Also, 1112-r4 and r5 are likely to be one radio HH-object (Rodríguez-Kamenetzky et al 2020).…”

Section: Radio Flux Densitymentioning

confidence: 99%

“…Only nine sources meet the criteria of UC-or HC-H II regions in at least one map. Two of them are the most luminous radio sources in MDC 1112, whose natures have been long under debate (Torrelles et al 1997;Shepherd 2001;Carrasco-González et al 2010b;Rodríguez-Kamenetzky et al 2020). Source 675-r1 reaches the criteria only on the Q-band A-configuration map, which only picks up the most compact components.…”

Section: H II Regionsmentioning

confidence: 99%

“…This conclusion was questioned by Shepherd (2001) and Carrasco-González et al (2010b), who claimed that 1112-r1 was insufficient to power the large-scale outflow (Hunter et al 1994) and the main powering source should be 1112-r3. The most recent works by Carrasco-González et al (2010b and Rodríguez-Kamenetzky et al (2020) concluded that 1112-r1 was an UC H II region, 1112-r2 a thermal, ionized wind, and 1112-r3 a thermal jet. They also concluded that 1112-r4, r5, and r6 were all Herbig-Haro (HH) objects with r4 and r5 together as a bright radio HH object and r6 as an obscured one.…”

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confidence: 99%

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Surveys of Clumps, Cores, and Condensations in the Cygnus X: II. Radio Properties of the Massive Dense Cores

Wang,

Qiu,

Cao

et al. 2021

Preprint

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We have carried out a high-sensitivity and high-resolution radio continuum study towards a sample of 47 massive dense cores (MDCs) in the Cygnus X star-forming complex using the Karl G. Jansky Very Large Array, aiming to detect and characterize the radio emission associated with star-forming activities down to ∼0.01 pc scales. We have detected 64 radio sources within or closely around the full widths at half-maximum (FWHMs) of the MDCs, of which 37 are reported for the first time. The majority of the detected radio sources are associated with dust condensations embedded within the MDCs, and they are mostly weak and compact. We are able to build spectral energy distributions for 8 sources. Two of them indicate non-thermal emission and the other six indicate thermal free-free emission. We have determined that most of the radio sources are ionized jets or winds originating from massive young stellar objects, whereas only a few sources are likely to be ultra-compact H II regions. Further quantitative analyses indicate that the radio luminosity of the detected radio sources increases along the evolution path of the MDCs.

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Characterizing the radio continuum nature of sources in the massive star-forming region W75N (B)

Cited by 11 publications

References 39 publications

Protostellar Interferometric Line Survey of the Cygnus X region (PILS-Cygnus)

Protostellar Interferometric Line Survey of the Cygnus X region (PILS-Cygnus)

A photoionized accretion disk around a young high-mass star

Surveys of Clumps, Cores, and Condensations in the Cygnus X: II. Radio Properties of the Massive Dense Cores

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