Herschel infrared views show prestellar cores originate in the fragmentation of complex filamentary networks of cold dust, Alexander Men’shchikov: Rich Murray 2010.06.06

[Rich Murray]

Herschel infrared views show prestellar cores originate in the fragmentation
of complex filamentary networks of cold dust, Alexander Men’shchikov: Rich
Murray 2010.06.06
rmforall.blogspot.com/2010_06_01_archive.htm
Sunday, June 6, 2010
<http://groups.yahoo.com/group/AstroDeep/52>
_______________________________________________


<http://herschel.esac.esa.int/FirstResultsSymposium.shtml>

Herschel First Results Symposium
(aka ESLAB 2010)
ESTEC, Noordwijk, 4-7 May 2010

The first major scientific symposium presenting Herschel
scientific results took place on 4-7 May 2010.
More than 400 astronomers came to ESTEC, Noordwijk,
to share in the excitement.

This meeting was the ESLAB 2010 symposium;
ESLAB is an annual meeting organised by the
Research and Scientific Support Department (RSSD)
which in 2010 was fully dedicated to Herschel and its first
science results.

Tuesday 4 May 2010
Plenary session 3 -- Session chair: Albrecht Poglitsch

<http://herschel.esac.esa.int/FirstResultsSymposium/presentations/P31_MenshchikovA-FilamentsAquilaPolaris.pdf>

Alexander Men’shchikov talk and slide show:
67 slides as 25.45 mb pdf, 4 May 2010

Filamentary Structures and Compact Objects in the
Aquila and Polaris Clouds observed by Herschel --
Alexander Men'shchikov
[ Service d'Astrophysique, CEA Saclay FRANCE
Laboratoire AIM, CEA/DSM--CNRS--
Universit´e Paris Diderot,
IRFU/Service d’Astrophysique, C.E. Saclay,
Orme des Merisiers,
91191 Gif-sur-Yvette, France ]

slide #63 Conclusions
• Fascinating filamentary structures are everywhere -- as deep
as we can see with the sensitivity of our instruments
• All extracted objects (starless cores, prestellar cores,
embedded protostars) are physically related to the filaments
• The observations suggest that, in general, prestellar cores
originate in the fragmentation of complex filamentary networks
• To unravel the roles and relative importance of gravity,
turbulence, and magnetic fields, we need to obtain additional
kinematic information

Filaments in the Polaris cloud are 10-15 deg K
and ~ 0.5 deg long = few parsecs

#38 3.3 deg full field views at ~37 sec resolution

#44 1.2 deg sub-field views at ~40 sec resolution -- high
contrast filaments and objects

#45 naive visual detection of matching of filaments and objects

#46 starless cores by "getsources" software

#59 [paraphrase] Theoretical MHD models of shocks in
supersonic turbulent motions in weakly magnetized clouds
evolve complex sheets, filaments, and cores
with torodial or helical magnetic fields.

<http://arxiv4.library.cornell.edu/abs/1005.3115>
7p pdf 39 authors

Filamentary structures and compact objects in the Aquila
and Polaris clouds observed by Herschel

A. Men'shchikov, Ph. André, P. Didelon, V. Könyves,
N. Schneider, F. Motte, S. Bontemps, D. Arzoumanian,
M. Attard, A. Abergel, J.-P. Baluteau, J.-Ph. Bernard,
L. Cambrésy, P. Cox, J. Di Francesco, A. M. di Giorgio,
M. Griffin, P. Hargrave, M. Huang, J. Kirk, J. Z. Li,
P. Martin, V. Minier, M.-A. Miville-Deschênes,
S. Molinari, G. Olofsson, S. Pezzuto, H. Roussel,
D. Russeil, P. Saraceno, M. Sauvage, B. Sibthorpe,
L. Spinoglio, L. Testi, D. Ward-Thompson, G. White,
C. D. Wilson, A. Woodcraft, A. Zavagno
(Submitted on 18 May 2010)

Our PACS and SPIRE images of the Aquila Rift and part of
the Polaris Flare regions, taken during the science
demonstration phase of Herschel discovered fascinating,
omnipresent filamentary structures that appear to be
physically related to compact cores.

We briefly describe a new multi-scale, multi-wavelength
source extraction method used to detect objects and
measure their parameters in our Herschel images.

All of the extracted starless cores
(541 in Aquila and 302 in Polaris) appear to form in the
long and very narrow filaments.

With its combination of the far-IR resolution and sensitivity,
Herschel directly reveals the filaments in which the
dense cores are embedded; the filaments are resolved and
have deconvolved widths of 35 arcsec in Aquila and
59 arcsec in Polaris (9000 AU in both regions).

Our first results of observations with Herschel enable us to
suggest that in general dense cores may originate in a process
of fragmentation of complex networks of long, thin filaments,
likely formed as a result of an interplay between gravity,
interstellar turbulence, and magnetic fields.

To unravel the roles of the processes, one has to obtain
additional kinematic and polarization information;
these follow-up observations are planned.

Comments: 7 pages, 2 figures.
Accepted for publication in Astronomy and Astrophysics,
Herschel Special Issue.
Subjects: Galaxy Astrophysics (astro-ph.GA)
Cite as: arXiv:1005.3115v1 [astro-ph.GA]
Submission history
From: Alexander Menshchikov [view email]
[v1] Tue, 18 May 2010 07:40:54 GMT (3331kb)

"Filaments are seen in numerous astronomical images and the
filamentary structure of molecular clouds has been known for
some time (e.g. Schneider & Elmegreen 1979; Goldsmith et al.
2008).

However, Herschel with its combination of the far-IR
resolution and sensitivity directly reveals the filaments in
which the cores are forming.

Our first observations demonstrate the fascinating,
omnipresent filamentary density structure of the cold
ISM and its extraordinarily intimate physical relationship with
the objects that form within the filaments.

They enable us to suggest that in general dense cores may
originate in a process of fragmentation of long, thin filaments,
presumably formed as a result of an interplay between gravity,
interstellar turbulence, and magnetic fields
(see also discussion in Andr´e et al. 2010).

To unravel the role and relative importance of these
processes, one needs additional kinematic and polarization
information (cf. Matthews et al. 2001);
these follow-up observations are planned."


can find filaments similar to Herschel views connecting early
galaxies in HUDF, using high gamma and color saturation:
Rich Murray 2010.06.06

notable bright blue tiny sources on darker 3D fractal web in
HUDF VLT ESO 28 images from 506 galaxies, z about 6,
RJ Bouwens, GD Illingworth, JP Blakeslee, M Franx
2008.02.04 draft 36 page: Rich Murray 2008.08.17
rmforall.blogspot.com/2008_08_01_archive.htm
Sunday, August 17, 2008
<http://groups.yahoo.com/group/AstroDeep/26>
<http://groups.yahoo.com/group/rmforall/86>

<www.flickr.com/photos/rmforall/1363979470/in/photostream>

Click on All Sizes button and select Original to see highest
resolution image.


<www.spacetelescope.org/images/html/zoomable/heic0611a.html>

Zoomable -- The boxes are 3 arcsec wide, 100x100 pixels,
with 0.03 arc-second per pixel.
They are in order of apparent brightness, from 1 to 28.

<www.spacetelescope.org/images/html/heic0611a.html>

Probing the distant Universe for young galaxies

This Hubble Space Telescope image shows 28 of the
brightest of 506 young galaxies that existed when the
universe was less than 1 billion years old.

The galaxies were uncovered in a study of two of the most
distant surveys of the cosmos,
the Hubble Ultra Deep Field (HUDF), completed in 2004,
and the Great Observatories Origins Deep Survey
(GOODS), made in 2003.

Just a few years ago, astronomers had not spotted any
galaxies that existed significantly less than 1 billion years
after the Big Bang.

The galaxies spied in the HUDF and GOODS surveys are
blue galaxies brimming with star birth.

The large image at left shows the Hubble Ultra Deep Field,
taken by the Hubble telescope.

The numbers next to the small blue boxes correspond to
close-up views of 28 of the newly found galaxies at right.
[ arranged by apparent brightness from 1 to 28 ]

The galaxies in the postage-stamp size images appear red
because of their tremendous distance from Earth.
The blue light from their young stars took nearly 13 billion
years to arrive at Earth.
During the journey, the blue light was shifted to red light due
to the expansion of space.

Credit: NASA, ESA, R. Bouwens and G. Illingworth
(University of California, Santa Cruz, USA).....
[ more ]
_______________________________________________


Rich Murray, MA
Boston University Graduate School 1967 psychology,
BS MIT 1964, history and physics,
1943 Otowi Road, Santa Fe, New Mexico 87505
505-501-2298 <[hidden email]>

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