Le travail présenté ici concerne les articles IV et V et n’a pas été effectué en lien direct avec la thèse mais participe à la possible ouverture vers un modèle en émission. Il a suscité une réflexion et une participation1 pour obtenir des données Spitzer correspondant à certains des cœurs présentés ici (Paladini et al. 2012). Ces deux articles concernent l’émissivité des poussières au travers de leur opacité et le lien entre la bande J et la bande à 250 µm (Juvela et al. 2015, Juvela et al., sous presse) dont les premières pages sont inclues ici.
Le programme Herschel Galactic Cold Cores permet l’étude des pous-sières vues en émission dans 116 champs classés comme des structures froides par rapport à leur environnement à l’aide des observations Planck. Alors que la partie infrarouge proche (bande J) est censée être relativement insensible à la nature des poussières, l’émission dans le submillimétrique dépend de leur évolution. On recherche une augmentation de l’émission submillimétrique telle qu’elle a pu être déduite par Stepnik et al. (2003) avec les observa-tions PRONAOS. En effet, les températures atteintes dans les cœurs ne peuvent pas être expliquées par des simples effets d’écrantage du rayonne-ment. L’opacité à 250 µm (τ250) a été obtenue par ajustement de la SED en fixant β à 2. Cette valeur de l’opacité a vocation à être comparée à l’estima-tion de la profondeur optique dans la bande J à partir des données 2MASS. Les corrélations entre τJ et τ250 ont été calculées à une résolution de 180 arcsec dans l’article IV.
τJ sert ici de référence entre zone diffuse et zone dense et on observe une claire déviation de τ250 avec τJ au delà de τJ ∼ 4. On constate une valeur médiane pour C proche de 0 dans l’article IV et la claire déviation mise en évidence par une valeur très positive de C est également proposée dans l’article IV pour L183 comme pour L134. Notre modélisation incluant des agrégats est donc en accord avec les résultats de l’article IV. La corrélation entre τJ et τ250pour les milieux moins denses peut également être utile pour obtenir la structure externe du nuage.
L’article V présente les températures de couleur et l’indice spectral dans une étude globale des 116 champs du programme. Il en résulte une claire anti–corrélation semblable à celle présentée pour les 90 sources du HCS (Figure 5.2). Cette étude est réalisée par l’ajustement de SED, tout comme l’article III, il n’est donc pas étonnant qu’elle révèle ce comportement. De plus cette évolution de T et β peut être interprétée comme vraie en utilisant des propriétés de poussières constantes. En effet, l’anti–corrélation entre 1. La classification des cœurs et le lien avec les températures et β sont par exemple présentés dans la Figure 5.2.
Figure G.1 – Illustration de τ250 en fonction de τJ pour L183. L’ajustement pro-posé est celui donné par l’article IV avec τ250 = A + B×τJ + C×τ2
J. Le coefficient C nous montre l’écart à la proportionnalité entre τJ et τ250 et indique que les pro-priétés des poussières varient entre ces deux bandes.
Figure G.2 – Opacité en bande J et limite de corrélation τJ∼4 tracée par le contour blanc.
T et β est constatée pour des propriétés moyennes constantes alors que β lui-même diminue quand les poussières s’agglomèrent et qu’en parallèle T diminue vers les zones les plus denses pour un nuage donné.
Les indices spectraux que l’article V infère sont plus faibles lorsque l’on s’approche du plan Galactique mais aucune dépendance avec la longitude Galactique n’a pu être relevée. Tout comme Malinen et al. (2011), une claire différence entre cœur préstellaire et cœur avec protoétoiles peut être mise en évidence.
Galactic cold cores V. Dust opacity
? ?? ???M. Juvela1, I. Ristorcelli2,3, D.J. Marshall4, J. Montillaud1,5, V.-M. Pelkonen1,6, N. Ysard7, P. McGehee8, R. Paladini8, L. Pagani9, J. Malinen1, A. Rivera-Ingraham2, C. Lef`evre9, L.V. T´oth10, L.A. Montier2,3, J.-P. Bernard2,3, P. Martin11
1 Department of Physics, P.O.Box 64, FI-00014, University of Helsinki, Finland, mika.juvela@helsinki.fi 2 Universit´e de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
3 CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
4 Laboratoire AIM, IRFU/Service dAstrophysique - CEA/DSM - CNRS - Universit Paris Diderot, B¢t. 709, CEA-Saclay, F-91191, Gif-sur-Yvette Cedex, France
5 Institut UTINAM, CNRS UMR 6213, OSU THETA, Universit´e de Franche-Comt´e, 41 bis avenue de l’Observatoire, 25000 Besanc¸on, France
6 Finnish Centre for Astronomy with ESO (FINCA), University of Turku, V¨ais¨al¨antie 20, FI-21500 Piikki¨o, Finland 7 IAS, Universit´e Paris-Sud, 91405 Orsay cedex, France
8 IPAC, Caltech, Pasadena, USA
9 LERMA, CNRS UMR8112, Observatoire de Paris, 61 avenue de l’observatoire 75014 Paris, France
10 Lor´and E¨otv¨os University, Department of Astronomy, P´azm´any P.s. 1/a, H-1117 Budapest, Hungary (OTKA K62304) 11 CITA, University of Toronto, 60 St. George St., Toronto, ON M5S 3H8, Canada
Received September 15, 1996; accepted March 16, 1997
ABSTRACT
Context. The project Galactic Cold Cores has carried out Herschel photometric observations of interstellar clouds where the Planck
satellite survey has located cold and compact clumps. The sources represent different stages of cloud evolution from starless clumps to protostellar cores and are located in different Galactic environments.
Aims. We examine this sample of 116 Herschel fields to estimate the submillimetre dust opacity and to search for variations that might be attributed to the evolutionary stage of the sources or to environmental factors, including the location within the Galaxy.
Methods. The submillimetre dust opacity was derived from Herschel data, and near-infrared observations of the reddening of back-ground stars are converted into near-infrared optical depth. We investigated the systematic errors affecting these parameters and used modelling to correct for the expected biases. The ratio of 250 µm and J band opacities is correlated with the Galactic location and the star formation activity. We searched for local variations in the ratio τ(250µm)/τ(J) using the correlation plots and opacity ratio
maps.
Results. We find a median ratio of τ(250µm)/τ(J) = (1.6 ± 0.2) ⇥ 10−3, which is more than three times the mean value reported for the diffuse medium. Assuming an opacity spectral index β = 1.8 instead of β = 2.0, the value would be lower by ⇠ 30%. No
significant systematic variation is detected with Galactocentric distance or with Galactic height. Examination of the ⌧(250µm)/⌧(J)
maps reveals six fields with clear indications of a local increase of submillimetre opacity of up to ⌧(250µm)/⌧(J) ⇠ 4 ⇥ 10−3towards the densest clumps. These are all nearby fields with spatially resolved clumps of high column density.
Conclusions.We interpret the increase in the far-infrared opacity as a sign of grain growth in the densest and coldest regions of interstellar clouds.
Key words. ISM: clouds – Infrared: ISM – Submillimeter: ISM – dust, extinction – Stars: formation – Stars: protostars
1. Introduction
The all-sky survey of the Planck satellite (Tauber et al. 2010) has enabled a new approach to studying the earliest stages of star formation. The sub-millimetre measurements, with high sensi-tivity and an angular resolution down to ⇠ 4.50, have enabled
? Planck (http://www.esa.int/Planck) is a project of the European Space Agency – ESA – with instruments provided by two scientific consortia funded by ESA member states (in particular the lead coun-tries: France and Italy) with contributions from NASA (USA), and tele-scope reflectors provided in a collaboration between ESA and a scien-tific Consortium led and funded by Denmark.
?? Herschelis an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with im-portant participation from NASA.
??? Tables 1 and E.1 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/
detecting and classifying of a large number of cold and compact Galactic sources. These probably represent different phases in the evolution of dense interstellar clouds that leads to the for-mation of stars. Careful analysis of the Planck data has led to a list of more than 10000 objects that form the Cold Clump Catalogue of Planck Objects (C3PO, see Planck Collaboration XXIII 2011). At Planck resolution, it is not possible to resolve gravitationally bound cores even in the nearest molecular clouds. The low colour temperature of most of the sources (T < 14 K) strongly suggests that the Planck clumps must have high col-umn densities, possibly at scales not resolved by Planck, and they probably contain even dense cores. A significant fraction of the clumps may be transient structures produced by turbulent flows, however.
Within the Herschel Open Time Key Programme Galactic
Cold Cores, we have carried out dust continuum emission ob-servations of 116 fields that were selected based on Planck
de-1
Galactic cold cores VII. Dust opacity spectral index
? ??M. Juvela1, K. Demyk2, 3, Y. Doi5, A. Hughes3, 2, 8, C. Lefèvre7, D.J. Marshall9, C. Meny2, 3, J. Montillaud4, L. Pagani7, D. Paradis2, 3, I. Ristorcelli2, 3, J. Malinen1, L.A. Montier2, 3, R. Paladini8, V.-M. Pelkonen1, A. Rivera-Ingraham2, 10,
1 Department of Physics, P.O.Box 64, FI-00014, University of Helsinki, Finland, mika.juvela@helsinki.fi 2 Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
3 CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
4 Institut UTINAM, CNRS UMR 6213, OSU THETA, Université de Franche-Comté, 41 bis avenue de l’Observatoire, 25000 Be-sançon, France
5 The University of Tokyo, Komaba 3-8-1, Meguro, Tokyo, 153-8902, Japan 6 IPAC, Caltech, Pasadena, USA
7 LERMA, CNRS UMR8112, Observatoire de Paris, 61 avenue de l’observatoire 75014 Paris, France 8 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
9 Laboratoire AIM, IRFU/Service d’Astrophysique - CEA/DSM - CNRS - Université Paris Diderot, Bât. 709, CEA-Saclay, F-91191, Gif-sur-Yvette Cedex, France
10 European Space Astronomy Centre (ESA-ESAC), PO Box 78, 28691, Villanueva de la Cañada, Madrid, Spain Received September 15, 1996; accepted March 16, 1997
ABSTRACT
Context.The Galactic Cold Cores project has carried out Herschel photometric observations of 116 fields where the Planck survey has found signs of cold dust emission. The fields contain sources in different environments and different phases of star formation. Previous studies have revealed variations in their dust submillimetre opacity.
Aims.The aim is to measure the value of dust opacity spectral index and to understand its variations spatially and with respect to other parameters such as temperature, column density, and Galactic location.
Methods. The dust opacity spectral index β and the dust colour temperature T are derived using Herschel and Planck data. The relation between β and T is examined for the whole sample and inside individual fields.
Results.Based on IRAS and Planck data, the fields are characterised by a median colour temperature of 16.1 K and a median opacity spectral index of β = 1.84. The values are not correlated with Galactic longitude. We observe a clear T –β anti-correlation. In Herschel observations, constrained at lower resolution by Planck data, the variations follow the column density structure and βFIRcan rise to ⇠2.2 in individual clumps. The highest values are found in starless clumps. The Planck 217 GHz band shows a systematic excess that is not restricted to cold clumps and is thus consistent with a general flattening of the dust emission spectrum at millimetre wavelengths. When fitted separately below and above 700 µm, the median spectral index values are βFIR⇠1.91 and β(mm) ⇠ 1.66.
Conclusions.The spectral index changes as a function of column density and wavelength. The comparison of different data sets and the examination of possible error sources show that our results are robust. However, β variations are partly masked by temperature gradients and the changes of the intrinsic grain properties may be even larger.
Key words. ISM: clouds – Infrared: ISM – Submillimetre: ISM – dust, extinction – Stars: formation – Stars: protostars
1. Introduction
The all-sky survey of the Planck satellite (Tauber et al. 2010) en-abled the identification of cold interstellar dust clouds at Galac-tic scale. The high sensitivity and an angular resolution of better than 50allowed the detection and classification of a large number of cold and compact sources that, based on the low temperature alone, are likely to be associated with prestellar phases of the star formation process. Analysis of Planck data led to the cre-ation of the Cold Clump Catalogue of Planck Objects (C3PO,
? Planck (http://www.esa.int/Planck) is a project of the European Space Agency – ESA – with instruments provided by two scientific con-sortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific con-sortium led and funded by Denmark.
?? Herschelis an ESA space observatory with science instruments pro-vided by European-led Principal Investigator consortia and with impor-tant participation from NASA.
see Planck Collaboration XXIII 2011), with more than 10000 sources. The low colour temperatures (mostly T <⇠ 14 K) indi-cate that the fields have high column density structures that are only partially resolved by the ⇠ 50Planck beam. Many of the clumps are likely to contain gravitationally bound cores.
The Herschel Open Time Key Programme Galactic Cold
Corescarried out dust continuum emission observations of 116 fields selected based on the Planck C3PO catalogue. The fields were mapped with Herschel PACS and SPIRE instruments (Pil-bratt et al. 2010; Poglitsch et al. 2010; Griffin et al. 2010) at wavelengths of 100–500 µm. Herschel makes it possible to study the Planck clumps and their internal structure in detail (Juvela et al. 2012; Montillaud et al. 2015, submitted; Rivera-Ingraham et al. 2015, submitted). The mapped fields are typically ⇠ 400
in size, enabling investigation of dust properties at larger scales and, in particular, the comparison of dust properties between the dense and cold regions and their lower density environment. First results have been presented in Planck Collaboration XXIII (2011); Planck Collaboration XXII (2011) and in Juvela et al.
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