Global properties of `ordinary` early-type galaxies: photometry and spectroscopy of stars and globular clusters in NGC 4494


Autoria(s): FOSTER, Caroline; SPITLER, Lee R.; ROMANOWSKY, Aaron J.; FORBES, Duncan A.; POTA, Vincenzo; BEKKI, Kenji; STRADER, Jay; PROCTOR, Robert N.; ARNOLD, Jacob A.; BRODIE, Jean P.
Contribuinte(s)

UNIVERSIDADE DE SÃO PAULO

Data(s)

19/10/2012

19/10/2012

2011

Resumo

We present a comprehensive analysis of the spatial, kinematic and chemical properties of stars and globular clusters (GCs) in the `ordinary` elliptical galaxy NGC 4494 using data from the Keck and Subaru telescopes. We derive galaxy surface brightness and colour profiles out to large galactocentric radii. We compare the latter to metallicities derived using the near-infrared Calcium Triplet. We obtain stellar kinematics out to similar to 3.5 effective radii. The latter appear flattened or elongated beyond similar to 1.8 effective radii in contrast to the relatively round photometric isophotes. In fact, NGC 4494 may be a flattened galaxy, possibly even an S0, seen at an inclination of similar to 45 degrees. We publish a catalogue of 431 GC candidates brighter than i(0) = 24 based on the photometry, of which 109 are confirmed spectroscopically and 54 have measured spectroscopic metallicities. We also report the discovery of three spectroscopically confirmed ultra-compact dwarfs around NGC 4494 with measured metallicities of -0.4 less than or similar to [Fe/H] less than or similar to -0.3. Based on their properties, we conclude that they are simply bright GCs. The metal-poor GCs are found to be rotating with similar amplitude as the galaxy stars, while the metal-rich GCs show marginal rotation. We supplement our analysis with available literature data and results. Using model predictions of galaxy formation, and a suite of merger simulations, we find that many of the observational properties of NGC 4494 may be explained by formation in a relatively recent gas-rich major merger. Complete studies of individual galaxies incorporating a range of observational avenues and methods such as the one presented here will be an invaluable tool for constraining the fine details of galaxy formation models, especially at large galactocentric radii.

Anglo-Australian Observatory

ARC

NSF[AST-0808099]

NSF[AST-0909237]

NSF[AST-0071048]

W.M. Keck Foundation

National Aeronautics and Space Administration (NASA)

Identificador

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, v.415, n.4, p.3393-3416, 2011

0035-8711

http://producao.usp.br/handle/BDPI/27173

10.1111/j.1365-2966.2011.18965.x

http://dx.doi.org/10.1111/j.1365-2966.2011.18965.x

Idioma(s)

eng

Publicador

WILEY-BLACKWELL

Relação

Monthly Notices of the Royal Astronomical Society

Direitos

restrictedAccess

Copyright WILEY-BLACKWELL

Palavras-Chave #galaxies: abundances #galaxies: haloes #galaxies: individual: NGC 4494 #galaxies: kinematics and dynamics #galaxies: star clusters: general #COMPACT DWARF GALAXIES #SIGHT VELOCITY DISTRIBUTIONS #STELLAR POPULATION SYNTHESIS #INFRARED CALCIUM TRIPLET #SUPERMASSIVE BLACK-HOLES #ELLIPTIC GALAXIES #DARK-MATTER #FORNAX CLUSTER #METALLICITY DISTRIBUTION #INTERACTING GALAXIES #Astronomy & Astrophysics
Tipo

article

original article

publishedVersion