Connecting Galactic and extragalactic outflows: From the Cygnus-X cluster to active galaxies

Skretas, I. M.; Kristensen, L. E.

doi:10.1051/0004-6361/202141944

Cited by 9 publications

(6 citation statements)

References 44 publications

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“…mass, density and temperature structure) appear to be similar to both low-and high-mass protostars in general, when scaled with luminosity (Pitts et al 2022). Second, the outflows from these sources also appear similar to low-and highmass sources, again when scaled with the luminosity (Skretas & Kristensen 2022). These two results suggest that the PILS-Cygnus sources are not special when it comes to envelope structure as well as accretion and ejection processes.…”

Section: Introductionmentioning

confidence: 68%

“…The molecular outflows may impact the observed emission, either through excitation (some molecules will more readily be excited in the dense and warm gas in outflows) or chemistry (sputtering and gas-phase reactions may lead to abundances of some molecules increasing dramatically). The sources all show outflow activity as traced by CO 3-2 emission (Skretas & Kristensen 2022). The directions and extent of the outflows are shown in the continuum maps with red and blue arrows, for easy comparison with the observed molecular emission described below.…”

Section: Continuum Emissionmentioning

confidence: 96%

“…Furthermore, a number of sources show SiO 8-7 emission, another shock and outflow tracer. The SiO emission tends to be more compact, and less extended than the CO emission (≲ a few arcsec, Skretas & Kristensen 2022).…”

Section: Continuum Emissionmentioning

confidence: 99%

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

Walt¹,

Kristensen²,

Calcutt³

et al. 2023

A&A

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Context. Molecular lines are commonly detected towards protostellar sources. However, to get a better understanding of the chemistry of these sources we need unbiased molecular surveys over a wide frequency range for as many sources as possible to shed light on the origin of this chemistry, particularly any influence from the external environment. Aims. We present results from the PILS-Cygnus survey of ten intermediate-to high-mass protostellar sources in the nearby Cygnus-X complex, through high angular resolution interferometric observations over a wide frequency range. Methods. Using the Submillimeter Array (SMA), a spectral line survey of ten sources was performed in the frequency range 329-361 GHz, with an angular resolution of ∼1 ′′ . 5, or ∼2000 AU at a source distance of 1.3 kpc from the Sun. Spectral modelling was performed to identify molecular emission and determine column densities and excitation temperatures for each source. Emission maps were made to study the morphology of emission. Finally, emission properties were compared across the sample. Results. We detect CH 3 OH towards nine of the ten sources, with CH 3 OCH 3 and CH 3 OCHO towards three sources. We further detect CH 3 CN towards four sources. Towards five sources the chemistry is spatially differentiated, meaning that different species peak at different positions and are offset from the peak continuum emission. Low levels of deuteration are detected towards four sources in HDO emission, whereas deuterated complex organic molecule emission is detected towards one source (CH 2 DOH towards N63). The chemical properties of each source do not correlate with their position in the Cygnus-X complex, nor do the distance or direction to the nearest OB associations. However, the five sources located in the DR21 filament do appear to show less line emission compared to the five sources outside the filament. Conclusions. This work shows how important wide frequency coverage observations are combined with high angular resolution observations for studying the protostellar environment. Furthermore, based on the ten sources observed here, the external environment appears to only play a minor role in setting the chemical environment on these small scales (< 2000 AU).

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Section: Introductionmentioning

confidence: 68%

Section: Continuum Emissionmentioning

confidence: 96%

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

Walt¹,

Kristensen²,

Calcutt³

et al. 2023

A&A

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“…An alternative is to probe this population with outflow emission. Studies show that there is a proportionality between this emission and protostellar envelope mass (e.g., Bontemps et al 1996;Skretas & Kristensen 2022). Kristensen & Bergin (2015) utilized this link to construct the cluster-in-a-box model 1 , simulating methanol emission from low-mass outflows in embedded star-forming clusters.…”

Section: Cluster-in-a-box Modelmentioning

confidence: 99%

Water emission tracing active star formation from the Milky Way to high-$z$ galaxies

Dutkowska¹,

Kristensen²

2022

Preprint

Self Cite

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Context. The question of how most stars in the Universe form remains open. While star formation predominantly takes place in young massive clusters, the current framework focuses on isolated star formation. This poses a problem when trying to constrain the initial stellar mass and the core mass functions, both in the local and distant Universe. Aims. One way to access the bulk of protostellar activity within star-forming clusters is to trace signposts of active star formation with emission from molecular outflows. These outflows are bright, e.g., in water emission, which is observable throughout cosmological times, providing a direct observational link between nearby and distant galaxies. We propose to utilize the in-depth knowledge of local star formation as seen with molecular tracers, such as water, to explore the nature of star formation in the Universe. Methods. We present a large-scale statistical galactic model of emission from galactic active star-forming regions. Our model is built on observations of well-resolved nearby clusters. By simulating emission from molecular outflows, which is known to scale with mass, we create a proxy that can be used to predict the emission from clustered star formation at galactic scales. In particular, the para-H 2 O 2 02 − 1 11 line is well-suited for this purpose, as it is among one of the brightest transitions observed toward Galactic star-forming regions and is now routinely observed toward distant galaxies. Results. We evaluated the impact of the most important global-star formation parameters (i.e., initial stellar mass function, molecular cloud mass distribution, star formation efficiency, and free-fall time efficiency) on simulation results. We observe that for emission from the para-H 2 O 2 02 − 1 11 line, the initial mass function and molecular cloud mass distribution have a negligible impact on the emission, both locally and globally, whereas the opposite holds for star-formation efficiency and free-fall time efficiency. Moreover, this water transition proves to be a low-contrast tracer of star formation, with I ν ∝ M env . Conclusions. The fine-tuning of the model and adaptation to morphologies of distant galaxies should result in realistic predictions of observed molecular emission and make the galaxy-in-a-box model a tool to analyze and better understand star formation throughout cosmological times.

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“…An alternative is to probe this population with outflow emission. Studies show that there is a proportionality between this emission and protostellar envelope mass (e.g., Bontemps et al 1996;Skretas & Kristensen 2022). Kristensen & Bergin (2015) used this link to construct the cluster-in-a-box model 1 , simulating methanol emission from low-mass outflows in embedded star-forming clusters.…”

Section: Cluster-in-a-box Modelmentioning

confidence: 99%

Water emission tracing active star formation from the Milky Way to high-z galaxies

Dutkowska¹,

Kristensen²

2022

A&A

Self Cite

View full text Add to dashboard Cite

Context. The question of how most stars in the Universe form remains open. While star formation predominantly takes place in young massive clusters, the current framework focuses on isolated star formation. This poses a problem when trying to constrain the initial stellar mass and the core mass functions, both in the local and distant Universe. Aims. One way to access the bulk of protostellar activity within star-forming clusters is to trace signposts of active star formation with emission from molecular outflows. These outflows are bright (e.g., in water emission), which is observable throughout cosmological times, providing a direct observational link between nearby and distant galaxies. We propose to utilize the in-depth knowledge of local star formation as seen with molecular tracers, such as water, to explore the nature of star formation in the Universe. Methods. We present a large-scale statistical galactic model of emission from galactic active star-forming regions. Our model is built on observations of well-resolved nearby clusters. By simulating emission from molecular outflows, which is known to scale with mass, we create a proxy that can be used to predict the emission from clustered star formation on galactic scales. In particular, the para-H 2 O 2 02 − 1 11 line is well suited for this purpose as it is one of the brightest transitions observed toward Galactic star-forming regions and is now routinely observed toward distant galaxies. Results. We evaluated the impact of the most important global star formation parameters (i.e., initial stellar mass function, molecular cloud mass distribution, star formation efficiency, and free-fall time efficiency) on simulation results. We observe that for emission from the para-H 2 O 2 02 − 1 11 line, the initial mass function and molecular cloud mass distribution have a negligible impact on the emission, both locally and globally, whereas the opposite holds for star formation efficiency and free-fall time efficiency. Moreover, this water transition proves to be a low-contrast tracer of star formation, with I ν ∝ M env . Conclusions. The fine-tuning of the model and adaptation to morphologies of distant galaxies should result in realistic predictions of observed molecular emission and make the galaxy-in-a-box model a tool for analyzing and better understanding star formation throughout cosmological times.

show abstract

Connecting Galactic and extragalactic outflows: From the Cygnus-X cluster to active galaxies

Cited by 9 publications

References 44 publications

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

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

Water emission tracing active star formation from the Milky Way to high-$z$ galaxies

Water emission tracing active star formation from the Milky Way to high-z galaxies

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