B. Rocca‐Volmerange

Institut d'Astrophysique de Paris

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Michel Fioc

Institut d'Astrophysique de Paris

B. Guiderdoni

Centre de Recherche Astrophysique de Lyon

A. Lançon

Observatoire astronomique de Strasbourg

P. Tsalmantza

Max Planck Institute for Astronomy

M. Kontizas

National and Kapodistrian University of Athens

C. Soubiran

Laboratoire d'Astrophysique de Bordeaux

I. Bellas-Velidis

National Observatory of Athens

D. Le Borgne

Institut d'Astrophysique de Paris

C. Surace

Laboratoire d’Astrophysique de Marseille

C. De Breuck

European Southern Observatory

Cooperative Institutions

Centre National de la Recherche Scientifique

720

Max Planck Society

550

National Institute for Astrophysics

276

Université Paris Cité

258

University College London

223

Sorbonne Université

188

Observatoire de Paris

177

University of Cambridge

162

University of Copenhagen

161

Max Planck Institute for Astronomy

158

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BLUE STARS IN THE CENTER OF THE S0 GALAXY NGC 5102

Astronomy and Astrophysics (1997)

J. M. Deharveng R. Jędrzejewski P. Crane M. J. Disney B. Rocca‐Volmerange

The S0 galaxy NGC 5102 has been observed with the Faint Object Camera on-board the Hubble Space Telescope. Individual blue stars have been resolved in the central region and measured photometrically through the F175W and F342w lters.Thelimitsofdetectionandcompletenessarenotuniform over the eld observed because the unresolved galaxy light in- creases toward the center. Comparison of integrated light with previous IUE observations and study of the light proles de- termined from the FOC images conrm the blue color gradient inward.TheF175w F342wcolorisfoundtogetbluerfrom1: 00 4 (21pc)to0: 00 4(6pc)butthegradientdoesnotcontinueinthenu- cleus. There is no evidence for a central core. The resolved blue stars are slightly more concentrated toward the center than the integrated light distribution. In the m175 vs. m175 m342 plane the stars are at positions where either young stars or P-AGB stars may be expected. Although neither interpretation is cer- tain, several arguments suggest that the majority of the resolved stars are young and belong to the last generation of a star for- mation episode that ended 15 Myr ago. According to spectral evolution models, the IUE ultraviolet spectrum is best repro- duced if this star formation episode started 500{800 Myr ago.

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Evidence that the z = 3.4 radio galaxy B2 0902+34 may be a protogalaxy

Nature (1993)

Steve Eales Steve Rawlings P. J. Puxley B. Rocca‐Volmerange K. D. Küntz

Protogalaxy

X-shaped radio galaxy

10.1038/363140a0

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Citations (29)

ISO ELAIS 1.4GHz survey (Gruppioni+, 1999)

C. Gruppioni P. Ciliegi M. Rowan-Robinson L. E. Cram A. Hopkins

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Évolution photométrique des galaxies : observables, modèles

Annales de Physique (1981)

B. Rocca‐Volmerange

On montre qu’une analyse des observations photométriques de galaxies (couleurs et luminosités intégrées) à l’aide d’un modèle d’évolution galactique nécessite également la connaissance de paramètres tels que Mgaz, MTOT, métallicité, sous-populations,... l’ensemble des données photo-métriques devant être corrigées (extinction, effet de surfaces émettrices, fond de ciel, lumière zodiacale) de manière cohérente.

10.1051/anphys/198106060167

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CHAPTER XI: INDIVIDUAL MEMBERSHIP

Proceedings of the International Astronomical Union (2007)

M. G. Abadi E. Agüero A. V. Ahumada J. A. Ahumada M. V. Alonso

An abstract is not available for this content so a preview has been provided. As you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Content (measure theory)

10.1017/s1743921308024393

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The ESO-Sculptor survey with ISO

HAL (Le Centre pour la Communication Scientifique Directe) (1999)

B. Rocca‐Volmerange V. de Lapparent C. Surace Elais Consortium

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UV to IR Models of Galaxy Evolution and Cosmology

Springer eBooks (1992)

B. Rocca‐Volmerange

10.1007/978-94-011-2434-8_47

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Spectral synthesis of galaxies: from low to high spectral resolution

sf2a (2002)

D. Le Borgne B. Rocca‐Volmerange A. Lançon Michel Fioc Pierre Ocvirk

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Bursting dwarf galaxies from the far-UV and deep surveys

arXiv (Cornell University) (1997)

Michel Fioc B. Rocca‐Volmerange

The far-ultraviolet (UV) counts and the deep optical spectroscopic surveys have revealed an unexpected number of very blue galaxies (vBG). Using constraints from the UV and optical, we apply the galaxy evolution model PEGASE (Fioc & Rocca-Volmerange 1997, hereafter FRV) to describe this population with a cycling star formation. When added to normally evolving galaxy populations, vBG are able to reproduce UV number counts and color distributions as well as deep optical redshift distributions fairly well. Good agreement is also obtained with optical counts (including the Hubble Deep Field). The number of vBG is only a small fraction of the number of normal galaxies, even at faintest magnitudes. In our modelling, the latter explain the bulk of the excess of faint blue galaxies in an open Universe. The problem of the blue excess remains in a flat Universe without cosmological constant.

Field galaxy

10.48550/arxiv.astro-ph/9709064

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The UV spectrum of WZ SGE at nova maximum.

ESASP (1980)

M. Friedjung B. Rocca‐Volmerange G. Debeve

Nova (rocket)

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