Herschel-SPIRE observations of the Polaris flare : structure of the diffuse interstellar medium at the sub-parsec scale

M. -A. Miville-Deschênes; P. G. Martin; A. Abergel; J. -P. Bernard; F. Boulanger; G. Lagache; L. D. Anderson; P. André; H. Arab; J. -P. Baluteau; K. Blagrave; S. Bontemps; M. Cohen; M. Compiegne; P. Cox; E. Dartois; G. Davis; R. Emery; T. Fulton; C. Gry; E. Habart; M. Huang; C. Joblin; S. C. Jones; J. Kirk; T. Lim; S. Madden; G. Makiwa; A. Menshchikov; S. Molinari; H. Moseley; F. Motte; D. A. Naylor; K. Okumura; D. Pinheiro Gocalvez; E. Polehampton; J. A. Rodón; D. Russei; P. Saraceno; N. Schneider; S. Sidher; L. Spencer; B. Swinyard; D. Ward-Thompson; G. J. White; A. Zavagno

hal-00523050, version 1

Herschel-SPIRE observations of the Polaris flare : structure of the diffuse interstellar medium at the sub-parsec scale

M. -A. Miville-Deschênes ¹, P. G. Martin ², A. Abergel ³, J. -P. Bernard, F. Boulanger ³, G. Lagache ³, L. D. Anderson ⁴, P. André ⁵, H. Arab, J. -P. Baluteau ⁴, K. Blagrave, S. Bontemps ^{6, 7, 8, 9}, M. Cohen, M. Compiegne, P. Cox, E. Dartois ³, G. Davis ¹⁰, R. Emery, T. Fulton, C. Gry ⁴, E. Habart ³, M. Huang ¹¹, C. Joblin ¹², S. C. Jones, J. Kirk ¹³, T. Lim ¹⁴, S. Madden ¹⁵, G. Makiwa, A. Menshchikov, S. Molinari ¹⁶, H. Moseley, F. Motte ^17, 18, D. A. Naylor, K. Okumura, D. Pinheiro Gocalvez, E. Polehampton, J. A. Rodón, D. Russei, P. Saraceno ¹⁶, N. Schneider ¹⁹, S. Sidher, L. Spencer, B. Swinyard, D. Ward-Thompson ²⁰, G. J. White ²¹, A. Zavagno ^4, 22

Astronomy and Astrophysics 518 (2010) L104

Résumé : We present a power spectrum analysis of the Herschel-SPIRE observations of the Polaris flare, a high Galactic latitude cirrus cloud midway between the diffuse and molecular phases. The SPIRE images of the Polaris flare reveal for the first time the structure of the diffuse interstellar medium down to 0.01 parsec over a 10 square degrees region. These exceptional observations highlight the highly filamentary and clumpy structure of the interstellar medium even in diffuse regions of the map. The power spectrum analysis shows that the structure of the interstellar medium is well described by a single power law with an exponent of -2.7 +- 0.1 at all scales from 30" to 8 degrees. That the power spectrum slope of the dust emission is constant down to the SPIRE angular resolution is an indication that the inertial range of turbulence extends down to the 0.01 pc scale. The power spectrum analysis also allows the identification of a Poissonian component at sub-arcminute scales in agreement with predictions of the cosmic infrared background level at SPIRE wavelengths. Finally, the comparison of the SPIRE and IRAS 100 micron data of the Polaris flare clearly assesses the capability of SPIRE in maping diffuse emission over large areas.

1 : Institut d'Astrophysique Spatiale
Aucune
2 : Laboratoire des Lois de Comportement du Combustible (LLCC)
CEA : DEN/DEC/SESC/LLCC
3 : Institut d'astrophysique spatiale (IAS)
CNRS : UMR8617 – INSU – Université Paris XI - Paris Sud
4 : Laboratoire d'Astrophysique de Marseille (LAM)
CNRS : UMR6110 – INSU – Université de Provence - Aix-Marseille I
5 : Laboratoire d'Informatique de Nantes Atlantique (LINA)
CNRS : UMR6241 – Université de Nantes – École Nationale Supérieure des Mines - Nantes
6 : Laboratoire d'Astrophysique de Bordeaux (LAB)
CNRS : UMR5804 – INSU – Université Sciences et Technologies - Bordeaux I
7 : Observatoire aquitain des sciences de l'univers (OASU)
CNRS : UMS2567 – INSU – Université Sciences et Technologies - Bordeaux I
8 : Université Sciences et Technologies - Bordeaux 1
Université Sciences et Technologies - Bordeaux I
9 : Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB)
CNRS : UMR5804 – INSU – Université Sciences et Technologies - Bordeaux I
10 : Department of Ecology & Evolutionary Biology
Princeton University
11 : National Astronomical Observatories
Chinese Academy of Sciences
12 : Centre d'étude spatiale des rayonnements (CESR)
CNRS : UMR5187 – Observatoire Midi-Pyrénées – INSU – Université Paul Sabatier [UPS] - Toulouse III
13 : School of Physis & Astronomy
Cardiff University
14 : Laboratoire de Probabilités et Modèles Aléatoires (LPMA)
CNRS : UMR7599 – Université Pierre et Marie Curie [UPMC] - Paris VI – Université Paris VII - Paris Diderot
15 : Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA)
CEA : DSM/DAPNIA
16 : Interplanetary Space Physics Institute (IFSI) (IFSI-INAF)
Interplanetary Space Physics Institute
17 : Laboratoire AIM (AIM)
CEA – Université Paris VII - Paris Diderot
18 : Institut de Recherches sur les lois Fondamentales de l'Univers (ex DAPNIA) (IRFU)
CEA : DSM/IRFU
19 : Astrophysique Interactions Multi-échelles (AIM)
CNRS : UMR7158 – INSU – Université Paris VII - Paris Diderot – CEA : DSM/IRFU
20 : School of Physics & Astronomy
Cardiff University
21 : Engineering Department
University of Cambridge
22 : Observatoire Astronomique de Marseille Provence (OAMP)
INSU – Université de Provence - Aix-Marseille I – CNRS : UMR6110

hal-00523050, version 1
http://hal.archives-ouvertes.fr/hal-00523050
oai:hal.archives-ouvertes.fr:hal-00523050
Contributeur : Marie-Paule Pomies <>
Soumis le : Lundi 4 Octobre 2010, 12:18:28
Dernière modification le : Jeudi 7 Octobre 2010, 10:47:33

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arXiv : 1005.2746

Code Bibliographique ADS : 2010A&A...518L.104M

DOI : 10.1051/0004-6361/201014678

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%% hal-00523050, version 1
%% http://hal.archives-ouvertes.fr/hal-00523050
@article{mivilledeschenes:hal-00523050,
    hal_id = {hal-00523050},
    url = {http://hal.archives-ouvertes.fr/hal-00523050},
    title = {{Herschel-SPIRE observations of the Polaris flare : structure of the diffuse interstellar medium at the sub-parsec scale}},
    author = {Miville-Desch{\^e}nes, M. -A. and Martin, P. G. and Abergel, A. and Bernard, J. -P. and Boulanger, F. and Lagache, G. and Anderson, L. D. and Andr{\'e}, P. and Arab, H. and Baluteau, J. -P. and Blagrave, K. and Bontemps, S. and Cohen, M. and Compiegne, M. and Cox, P. and Dartois, E. and Davis, G. and Emery, R. and Fulton, T. and Gry, C. and Habart, E. and Huang, M. and Joblin, C. and Jones, S. C. and Kirk, J. and Lim, T. and Madden, S. and Makiwa, G. and Menshchikov, A. and Molinari, S. and Moseley, H. and Motte, F. and Naylor, D. A. and Okumura, K. and Gocalvez, D. Pinheiro and Polehampton, E. and Rod{\'o}n, J. A. and Russei, D. and Saraceno, P. and Schneider, N. and Sidher, S. and Spencer, L. and Swinyard, B. and Ward-Thompson, D. and White, G. J. and Zavagno, A.},
    abstract = {{We present a power spectrum analysis of the Herschel-SPIRE observations of the Polaris flare, a high Galactic latitude cirrus cloud midway between the diffuse and molecular phases. The SPIRE images of the Polaris flare reveal for the first time the structure of the diffuse interstellar medium down to 0.01 parsec over a 10 square degrees region. These exceptional observations highlight the highly filamentary and clumpy structure of the interstellar medium even in diffuse regions of the map. The power spectrum analysis shows that the structure of the interstellar medium is well described by a single power law with an exponent of -2.7 +- 0.1 at all scales from 30" to 8 degrees. That the power spectrum slope of the dust emission is constant down to the SPIRE angular resolution is an indication that the inertial range of turbulence extends down to the 0.01 pc scale. The power spectrum analysis also allows the identification of a Poissonian component at sub-arcminute scales in agreement with predictions of the cosmic infrared background level at SPIRE wavelengths. Finally, the comparison of the SPIRE and IRAS 100 micron data of the Polaris flare clearly assesses the capability of SPIRE in maping diffuse emission over large areas.}},
    language = {Anglais},
    affiliation = {Institut d'Astrophysique Spatiale , Laboratoire des Lois de Comportement du Combustible - LLCC , Institut d'astrophysique spatiale - IAS , Laboratoire d'Astrophysique de Marseille - LAM , Laboratoire d'Informatique de Nantes Atlantique - LINA , Laboratoire d'Astrophysique de Bordeaux - LAB , Observatoire aquitain des sciences de l'univers - OASU , Universit{\'e} Sciences et Technologies - Bordeaux 1 , Laboratoire d'astrodynamique, d'astrophysique et d'a{\'e}ronomie de bordeaux - L3AB , Department of Ecology \& Evolutionary Biology , National Astronomical Observatories , Centre d'{\'e}tude spatiale des rayonnements - CESR , School of Physis \& Astronomy , Laboratoire de Probabilit{\'e}s et Mod{\`e}les Al{\'e}atoires - LPMA , D{\'e}partement d'Astrophysique, de physique des Particules, de physique Nucl{\'e}aire et de l'Instrumentation Associ{\'e}e - DAPNIA , Interplanetary Space Physics Institute (IFSI) - IFSI-INAF , Laboratoire AIM - AIM , Institut de Recherches sur les lois Fondamentales de l'Univers (ex DAPNIA) - IRFU , Astrophysique Interactions Multi-{\'e}chelles - AIM , School of Physics \& Astronomy , Engineering Department , Observatoire Astronomique de Marseille Provence - OAMP},
    pages = {L104},
    journal = {Astronomy and Astrophysics},
    volume = {518},
    audience = {internationale },
    doi = {10.1051/0004-6361/201014678 },
    year = {2010},
}

%F hal-00523050, version 1
%0 Journal Article
%U http://hal.archives-ouvertes.fr/hal-00523050
%2 SDU:ASTR:SR;PHYS:ASTR:SR
%T Herschel-SPIRE observations of the Polaris flare : structure of the diffuse interstellar medium at the sub-parsec scale
%A Miville-Deschênes, M. -A.
%A Martin, P. G.
%A Abergel, A.
%A Bernard, J. -P.
%A Boulanger, F.
%A Lagache, G.
%A Anderson, L. D.
%A André, P.
%A Arab, H.
%A Baluteau, J. -P.
%A Blagrave, K.
%A Bontemps, S.
%A Cohen, M.
%A Compiegne, M.
%A Cox, P.
%A Dartois, E.
%A Davis, G.
%A Emery, R.
%A Fulton, T.
%A Gry, C.
%A Habart, E.
%A Huang, M.
%A Joblin, C.
%A Jones, S. C.
%A Kirk, J.
%A Lim, T.
%A Madden, S.
%A Makiwa, G.
%A Menshchikov, A.
%A Molinari, S.
%A Moseley, H.
%A Motte, F.
%A Naylor, D. A.
%A Okumura, K.
%A Gocalvez, D. Pinheiro
%A Polehampton, E.
%A Rodón, J. A.
%A Russei, D.
%A Saraceno, P.
%A Schneider, N.
%A Sidher, S.
%A Spencer, L.
%A Swinyard, B.
%A Ward-Thompson, D.
%A White, G. J.
%A Zavagno, A.
%+ Institut d'Astrophysique Spatiale , Laboratoire des Lois de Comportement du Combustible - LLCC , Institut d'astrophysique spatiale - IAS , Laboratoire d'Astrophysique de Marseille - LAM , Laboratoire d'Informatique de Nantes Atlantique - LINA , Laboratoire d'Astrophysique de Bordeaux - LAB , Observatoire aquitain des sciences de l'univers - OASU , Université Sciences et Technologies - Bordeaux 1 , Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux - L3AB , Department of Ecology & Evolutionary Biology , National Astronomical Observatories , Centre d'étude spatiale des rayonnements - CESR , School of Physis & Astronomy , Laboratoire de Probabilités et Modèles Aléatoires - LPMA , Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée - DAPNIA , Interplanetary Space Physics Institute (IFSI) - IFSI-INAF , Laboratoire AIM - AIM , Institut de Recherches sur les lois Fondamentales de l'Univers (ex DAPNIA) - IRFU , Astrophysique Interactions Multi-échelles - AIM , School of Physics & Astronomy , Engineering Department , Observatoire Astronomique de Marseille Provence - OAMP
%X We present a power spectrum analysis of the Herschel-SPIRE observations of the Polaris flare, a high Galactic latitude cirrus cloud midway between the diffuse and molecular phases. The SPIRE images of the Polaris flare reveal for the first time the structure of the diffuse interstellar medium down to 0.01 parsec over a 10 square degrees region. These exceptional observations highlight the highly filamentary and clumpy structure of the interstellar medium even in diffuse regions of the map. The power spectrum analysis shows that the structure of the interstellar medium is well described by a single power law with an exponent of -2.7 +- 0.1 at all scales from 30" to 8 degrees. That the power spectrum slope of the dust emission is constant down to the SPIRE angular resolution is an indication that the inertial range of turbulence extends down to the 0.01 pc scale. The power spectrum analysis also allows the identification of a Poissonian component at sub-arcminute scales in agreement with predictions of the cosmic infrared background level at SPIRE wavelengths. Finally, the comparison of the SPIRE and IRAS 100 micron data of the Polaris flare clearly assesses the capability of SPIRE in maping diffuse emission over large areas.
%G Anglais
%2 2010
%R 10.1051/0004-6361/201014678
%J Astronomy and Astrophysics
%2 internationale
%8 2010-00-00
%V 518
%P L104

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<author><persName><forename>M.</forename><surname>Cohen</surname></persName></author>
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<author><persName><forename>D. A.</forename><surname>Naylor</surname></persName></author>
<author><persName><forename>K.</forename><surname>Okumura</surname></persName></author>
<author><persName><forename>D. Pinheiro</forename><surname>Gocalvez</surname></persName></author>
<author><persName><forename>E.</forename><surname>Polehampton</surname></persName></author>
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<orgName type="laboratory">IFSI-INAF</orgName>
<orgName type="team">Interplanetary Space Physics Institute (IFSI)</orgName>
<country>IT</country>
<orgName type="institution">Interplanetary Space Physics Institute</orgName>
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<affiliation>
<orgName type="laboratory">AIM</orgName>
<orgName type="team">Astrophysique Interactions Multi-échelles</orgName>
<country>FR</country>
<orgName type="institution">CNRS : UMR7158</orgName>
<orgName type="institution">INSU</orgName>
<orgName type="institution">Université Paris VII - Paris Diderot</orgName>
<orgName type="institution">CEA : DSM/IRFU</orgName>
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<country>GB</country>
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<country>GB</country>
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<country>FR</country>
<orgName type="institution">CNRS : UMR6110</orgName>
<orgName type="institution">INSU</orgName>
<orgName type="institution">Université de Provence - Aix-Marseille I</orgName>
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<affiliation>
<orgName type="laboratory">OAMP</orgName>
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<country>FR</country>
<orgName type="institution">INSU</orgName>
<orgName type="institution">Université de Provence - Aix-Marseille I</orgName>
<orgName type="institution">CNRS : UMR6110</orgName>
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