Collisional debris as laboratories to study star formation

M. Boquien; P. -A. Duc; Y. Wu; V. Charmandaris; U. Lisenfeld; J. Braine; E. Brinks; J. Iglesias-Páramo; C. K. Xu

hal-00401169, version 1

Collisional debris as laboratories to study star formation

M. Boquien ¹, P. -A. Duc ², Y. Wu ³, V. Charmandaris ⁴, U. Lisenfeld ⁵, J. Braine ^6, 7, 8, E. Brinks ⁹, J. Iglesias-Páramo ¹⁰, C. K. Xu ¹¹

The Astronomical Journal 137, 6 (2009) 4561-4576

Résumé : In this paper we address the question whether star formation is driven by local processes or the large scale environment. To do so, we investigate star formation in collisional debris where the gravitational potential well and velocity gradients are shallower and compare our results with previous work on star formation in non-interacting spiral and dwarf galaxies. We have performed multiwavelength spectroscopic and imaging observations (from the far-ultraviolet to the mid-infrared) of 6 interacting systems, identifying a total of 60 star-forming regions in their collision debris. Our analysis indicates that in these regions a) the emission of the dust is at the expected level for their luminosity and metallicity, b) the usual tracers of star formation rate display the typical trend and scatter found in classical star forming regions, and c) the extinction and metallicity are not the main parameters governing the scatter in the properties of intergalactic star forming regions; age effects and variations in the number of stellar populations, seem to play an important role. Our work suggests that local properties such as column density and dust content, rather than the large scale environment seem to drive star formation. This means that intergalactic star forming regions can be used as a reliable tool to study star formation.

1 : Astrophysique Interactions Multi-échelles (AIM)
CNRS : UMR7158 – INSU – Université Paris VII - Paris Diderot – CEA : DSM/IRFU
2 : Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA)
CEA : DSM/DAPNIA
3 : National Laboratory of Pattern Recognition [Beijing] (NLPR)
Institute of Automation, Chinese Academy of Sciences
4 : Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA)
CNRS : UMR8112 – INSU – Observatoire de Paris – Université Pierre et Marie Curie (UPMC) - Paris VI – Université de Cergy Pontoise – Ecole normale supérieure de Paris - ENS Paris
5 : Departamento Física Teórica y del Cosmos
Universidad de Granada – Instituto de Astrofísica de Andalucía (CSIC)
6 : Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB)
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 : Laboratoire d'Astrophysique de Bordeaux (LAB)
CNRS : UMR5804 – INSU – Université Sciences et Technologies - Bordeaux I
9 : Centre for Astrophysics Research
University of Hertfordshire
10 : Laboratoire d'Astrophysique de Marseille (LAM)
CNRS : UMR6110 – INSU – Université de Provence - Aix-Marseille I
11 : Laboratoire de Mathématiques Raphaël Salem (LMRS)
CNRS : UMR6085 – Université de Rouen

hal-00401169, version 1
http://hal.archives-ouvertes.fr/hal-00401169
oai:hal.archives-ouvertes.fr:hal-00401169
Contributeur : Marie-Paule Pomies <>
Soumis le : Jeudi 2 Juillet 2009, 15:39:42
Dernière modification le : Jeudi 2 Juillet 2009, 15:39:42

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arXiv : 0903.3403

DOI : 10.1088/0004-6256/137/6/4561

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%% hal-00401169, version 1
%% http://hal.archives-ouvertes.fr/hal-00401169
@article{boquien:hal-00401169,
    hal_id = {hal-00401169},
    url = {http://hal.archives-ouvertes.fr/hal-00401169},
    title = {{Collisional debris as laboratories to study star formation}},
    author = {Boquien, M. and Duc, P. -A. and Wu, Y. and Charmandaris, V. and Lisenfeld, U. and Braine, J. and Brinks, E. and Iglesias-P{\'a}ramo, J. and Xu, C. K.},
    abstract = {{In this paper we address the question whether star formation is driven by local processes or the large scale environment. To do so, we investigate star formation in collisional debris where the gravitational potential well and velocity gradients are shallower and compare our results with previous work on star formation in non-interacting spiral and dwarf galaxies. We have performed multiwavelength spectroscopic and imaging observations (from the far-ultraviolet to the mid-infrared) of 6 interacting systems, identifying a total of 60 star-forming regions in their collision debris. Our analysis indicates that in these regions a) the emission of the dust is at the expected level for their luminosity and metallicity, b) the usual tracers of star formation rate display the typical trend and scatter found in classical star forming regions, and c) the extinction and metallicity are not the main parameters governing the scatter in the properties of intergalactic star forming regions; age effects and variations in the number of stellar populations, seem to play an important role. Our work suggests that local properties such as column density and dust content, rather than the large scale environment seem to drive star formation. This means that intergalactic star forming regions can be used as a reliable tool to study star formation.}},
    keywords = {galaxies: dwarf, galaxies: interactions, galaxies: irregular, infrared: galaxies, stars: formation, ultraviolet: galaxies},
    language = {Anglais},
    affiliation = {Astrophysique Interactions Multi-{\'e}chelles - AIM , D{\'e}partement d'Astrophysique, de physique des Particules, de physique Nucl{\'e}aire et de l'Instrumentation Associ{\'e}e - DAPNIA , National Laboratory of Pattern Recognition [Beijing] - NLPR , Laboratoire d'Etude du Rayonnement et de la Mati{\`e}re en Astrophysique - LERMA , Departamento F{\'\i}sica Te{\'o}rica y del Cosmos , Laboratoire d'astrodynamique, d'astrophysique et d'a{\'e}ronomie de bordeaux - L3AB , Observatoire aquitain des sciences de l'univers - OASU , Laboratoire d'Astrophysique de Bordeaux - LAB , Centre for Astrophysics Research , Laboratoire d'Astrophysique de Marseille - LAM , Laboratoire de Math{\'e}matiques Rapha{\"e}l Salem - LMRS},
    pages = {4561-4576},
    journal = {The Astronomical Journal},
    volume = {137},
    number = {6 },
    note = {18 pages, 19 figures },
    audience = {internationale },
    doi = {10.1088/0004-6256/137/6/4561 },
    year = {2009},
}

%F hal-00401169, version 1
%0 Journal Article
%U http://hal.archives-ouvertes.fr/hal-00401169
%2 PHYS:ASTR:CO;SDU:ASTR:EP
%T Collisional debris as laboratories to study star formation
%A Boquien, M.
%A Duc, P. -A.
%A Wu, Y.
%A Charmandaris, V.
%A Lisenfeld, U.
%A Braine, J.
%A Brinks, E.
%A Iglesias-Páramo, J.
%A Xu, C. K.
%+ Astrophysique Interactions Multi-échelles - AIM , Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée - DAPNIA , National Laboratory of Pattern Recognition [Beijing] - NLPR , Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique - LERMA , Departamento Física Teórica y del Cosmos , Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux - L3AB , Observatoire aquitain des sciences de l'univers - OASU , Laboratoire d'Astrophysique de Bordeaux - LAB , Centre for Astrophysics Research , Laboratoire d'Astrophysique de Marseille - LAM , Laboratoire de Mathématiques Raphaël Salem - LMRS
%X In this paper we address the question whether star formation is driven by local processes or the large scale environment. To do so, we investigate star formation in collisional debris where the gravitational potential well and velocity gradients are shallower and compare our results with previous work on star formation in non-interacting spiral and dwarf galaxies. We have performed multiwavelength spectroscopic and imaging observations (from the far-ultraviolet to the mid-infrared) of 6 interacting systems, identifying a total of 60 star-forming regions in their collision debris. Our analysis indicates that in these regions a) the emission of the dust is at the expected level for their luminosity and metallicity, b) the usual tracers of star formation rate display the typical trend and scatter found in classical star forming regions, and c) the extinction and metallicity are not the main parameters governing the scatter in the properties of intergalactic star forming regions; age effects and variations in the number of stellar populations, seem to play an important role. Our work suggests that local properties such as column density and dust content, rather than the large scale environment seem to drive star formation. This means that intergalactic star forming regions can be used as a reliable tool to study star formation.
%G Anglais
%2 2009
%R 10.1088/0004-6256/137/6/4561
%J The Astronomical Journal
%2 internationale
%8 2009-00-00
%V 137
%N 6
%P 4561-4576
%K galaxies: dwarf, galaxies: interactions, galaxies: irregular, infrared: galaxies, stars: formation, ultraviolet: galaxies
%Z 18 pages, 19 figures

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