Detection of two power-law tails in the probability distribution functions of massive GMCs

We report the novel detection of complex high column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC 6334), obtained from dust emission observed with Herschel. The low column density range can be fitted with a lognormal dist...

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Vydáno v:Monthly notices of the Royal Astronomical Society Ročník 453; číslo 1; s. L41 - L45
Hlavní autoři: Schneider, N., Bontemps, S., Girichidis, P., Rayner, T., Motte, F., André, Ph, Russeil, D., Abergel, A., Anderson, L., Arzoumanian, D., Benedettini, M., Csengeri, T., Didelon, P., Francesco, J. Di, Griffin, M., Hill, T., Klessen, R. S., Ossenkopf, V., Pezzuto, S., Rivera-Ingraham, A., Spinoglio, L., Tremblin, P., Zavagno, A.
Médium: Journal Article
Jazyk:angličtina
Vydáno: Oxford University Press 11.10.2015
Oxford University Press (OUP): Policy P - Oxford Open Option A
Témata:
Astrophysics
Cosmology and Extra-Galactic Astrophysics
Sciences of the Universe
ISM: clouds
dust, extinction
dust extinction
ISSN:1745-3925, 0035-8711, 1745-3933, 1365-2966
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Abstract We report the novel detection of complex high column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC 6334), obtained from dust emission observed with Herschel. The low column density range can be fitted with a lognormal distribution. A first power-law tail starts above an extinction (A V) of ∼6–14. It has a slope of α = 1.3–2 for the ρ ∝ r −α profile for an equivalent density distribution (spherical or cylindrical geometry), and is thus consistent with free-fall gravitational collapse. Above A V ∼40, 60, and 140, we detect an excess that can be fitted by a flatter power-law tail with α > 2. It correlates with the central regions of the cloud (ridges/hubs) of size ∼1 pc and densities above 104 cm−3. This excess may be caused by physical processes that slow down collapse and reduce the flow of mass towards higher densities. Possible are: (1) rotation, which introduces an angular momentum barrier, (2) increasing optical depth and weaker cooling, (3) magnetic fields, (4) geometrical effects, and (5) protostellar feedback. The excess/second power-law tail is closely linked to high-mass star-formation though it does not imply a universal column density threshold for the formation of (high-mass) stars.
AbstractList We report the novel detection of complex high column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC 6334), obtained from dust emission observed with Herschel. The low column density range can be fitted with a lognormal distribution. A first power-law tail starts above an extinction (AV) of ∼6–14. It has a slope of α = 1.3–2 for the ρ ∝ r−α profile for an equivalent density distribution (spherical or cylindrical geometry), and is thus consistent with free-fall gravitational collapse. Above AV ∼40, 60, and 140, we detect an excess that can be fitted by a flatter power-law tail with α > 2. It correlates with the central regions of the cloud (ridges/hubs) of size ∼1 pc and densities above 104 cm−3. This excess may be caused by physical processes that slow down collapse and reduce the flow of mass towards higher densities. Possible are: (1) rotation, which introduces an angular momentum barrier, (2) increasing optical depth and weaker cooling, (3) magnetic fields, (4) geometrical effects, and (5) protostellar feedback. The excess/second power-law tail is closely linked to high-mass star-formation though it does not imply a universal column density threshold for the formation of (high-mass) stars.
We report the novel detection of complex high column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC 6334), obtained from dust emission observed with Herschel. The low column density range can be fitted with a lognormal distribution. A first power-law tail starts above an extinction (A V) of ∼6–14. It has a slope of α = 1.3–2 for the ρ ∝ r −α profile for an equivalent density distribution (spherical or cylindrical geometry), and is thus consistent with free-fall gravitational collapse. Above A V ∼40, 60, and 140, we detect an excess that can be fitted by a flatter power-law tail with α > 2. It correlates with the central regions of the cloud (ridges/hubs) of size ∼1 pc and densities above 104 cm−3. This excess may be caused by physical processes that slow down collapse and reduce the flow of mass towards higher densities. Possible are: (1) rotation, which introduces an angular momentum barrier, (2) increasing optical depth and weaker cooling, (3) magnetic fields, (4) geometrical effects, and (5) protostellar feedback. The excess/second power-law tail is closely linked to high-mass star-formation though it does not imply a universal column density threshold for the formation of (high-mass) stars.
We report the novel detection of complex high-column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC6334), obtained from dust emission observed with Herschel. The low column density range can be fit with a lognormal distribution. A first power-law tail starts above an extinction (A$_v$) of ~6-14. It has a slope of $\alpha$ = 1.3$-$2 for the $\rho$ $\alpha$ $r^{-\alpha}$ profile for an equivalent density distribution (spherical or cylindrical geometry), and is thus consistent with free-fall gravitational collapse. Above A$_v$~40, 60, and 140, we detect an excess that can be fitted by a flatter power law tail with $\alpha$ > 2. It correlates with the central regions of the cloud (ridges/hubs) of size ~1 pc and densities above 10$^4$ cm$^{-3}$. This excess may be caused by physical processes that slow down collapse and reduce the flow of mass towards higher densities. Possible are: 1. rotation, which introduces an angular momentum barrier, 2. increasing optical depth and weaker cooling, 3. magnetic fields, 4. geometrical effects, and 5. protostellar feedback. The excess/second power-law tail is closely linked to high-mass star-formation though it does not imply a universal column density threshold for the formation of (high-mass) stars.
Author Bontemps, S.
Francesco, J. Di
Ossenkopf, V.
Tremblin, P.
Klessen, R. S.
Girichidis, P.
Zavagno, A.
Didelon, P.
Anderson, L.
Arzoumanian, D.
Rivera-Ingraham, A.
Griffin, M.
Schneider, N.
Benedettini, M.
Csengeri, T.
Pezzuto, S.
Abergel, A.
André, Ph
Rayner, T.
Hill, T.
Russeil, D.
Spinoglio, L.
Motte, F.
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Issue 1
Keywords ISM: clouds
dust, extinction
dust extinction
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Snippet We report the novel detection of complex high column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions...
We report the novel detection of complex high-column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions...
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SubjectTerms Astrophysics
Cosmology and Extra-Galactic Astrophysics
Sciences of the Universe
Title Detection of two power-law tails in the probability distribution functions of massive GMCs
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