Analytical expressions for the deprojected Sérsic model

Baes, M.; Gentile, Gianfranco

doi:10.1051/0004-6361/201015716

Cited by 44 publications

(53 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The Wilson model is defined by an alternate modified isothermal sphere based on the ad hoc stellar distribution function of Wilson (1975), which has more extended envelope structures than the standard King isothermal sphere (Mclaughlin et al 2008). The Sérsic model has an R 1/n surface density profile, which is used for parameterizing the surface brightness profiles of early-type galaxies and bulges of spiral galaxies (Baes & Gentile 2011). However, Tanvir et al (2012) found that some classical GCs in M31 that exhibit cuspy core profiles are well fitted by the Sérsic model of index n ∼ 2 − 6.…”

Section: Structural Modelsmentioning

confidence: 99%

Ages and structural and dynamical parameters of two globular clusters in the M81 group

Ma¹,

Wang²,

Wu³

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

GC-1 and GC-2 are two globular clusters (GCs) in the remote halo of M81 and M82 in the M81 group discovered by Jang et al. using the Hubble Space Telescope (HST) images. These two GCs were observed as part of the Beijing-Arizona-Taiwan-Connecticut (BATC) Multicolor Sky Survey, using 14 intermediate-band filters covering a wavelength range of 4000-10000 Å. We accurately determine these two clusters' ages and masses by comparing their spectral energy distributions (from 2267 to 20000 Å, comprising photometric data in the near-ultraviolet of the Galaxy Evolution Explorer, 14 BATC intermediate-band, and Two Micron All Sky Survey near-infrared JHK s filters) with theoretical stellar population-synthesis models, resulting in ages of 15.50 ± 3.20 for GC-1 and 15.10 ± 2.70 Gyr for GC-2. The masses of GC-1 and GC-2 obtained here are 1.77 − 2.04 × 10 6 and 5.20 − 7.11 × 10 6 M ⊙ , respectively. In addition, the deep observations with the Advanced Camera for Surveys and Wide Field Camera 3 on the HST are used to provide the surface brightness profiles of GC-1 and GC-2. The structural and dynamical parameters are derived from fitting the profiles to three different models; in particular, the internal velocity dispersions of GC-1 and GC-2 are derived, which can be compared with ones obtained based on spectral observations in the future. For the first time, in this paper, the r h versus M V diagram shows that GC-2 is an ultra-compact dwarf in the M81 group.

show abstract

Section: Structural Modelsmentioning

confidence: 99%

Ages and structural and dynamical parameters of two globular clusters in the M81 group

Ma¹,

Wang²,

Wu³

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The apparent axis ratio of the bulge q b is also a free parameter of the model. The 3D luminosity density corresponding to this intensity distribution on the sky can be expressed using complex special functions (Mazure & Capelato 2002;Baes & Gentile 2011;Baes & Van Hese 2011). To describe the surface brightness distribution of the threedimensional axisymmetric stellar disc, radiative transfer modellers usually use a 3D luminosity density model where the radial and vertical profile of the luminosity density are exponential (the double-exponential disc).…”

Section: Decomposition Of the Irac 36 µM Imagementioning

confidence: 99%

HERschelObservations of Edge-on Spirals (HEROES)

Mosenkov

Allaert

Baes

et al. 2016

A&A

View full text Add to dashboard Cite

We investigate the dust energy balance for the edge-on galaxy IC 2531, one of the seven galaxies in the HEROES sample. We perform a state-of-the-art radiative transfer modelling based, for the first time, on a set of optical and near-infrared galaxy images. We show that by taking into account near-infrared imaging in the modelling significantly improves the constraints on the retrieved parameters of the dust content. We confirm the result from previous studies that including a young stellar population in the modelling is important to explain the observed stellar energy distribution. However, the discrepancy between the observed and modelled thermal emission at far-infrared wavelengths, the so-called dust energy balance problem, is still present: the model underestimates the observed fluxes by a factor of about two. We compare two different dust models, and find that dust parameters, and thus the spectral energy distribution in the infrared domain, are sensitive to the adopted dust model. In general, the THEMIS model reproduces the observed emission in the infrared wavelength domain better than the popular BARE-GR-S model. Our study of IC 2531 is a pilot case for detailed and uniform radiative transfer modelling of the entire HEROES sample, which will shed more light on the strength and origins of the dust energy balance problem.

show abstract

“…For the bulges, we assumed the traditional Sérsic profile (Sersic 1968;Caon et al 1993;Prieto et al 2001;Baes & Gentile 2011),…”

Section: Fitting Functionsmentioning

confidence: 99%

Formation of S0 galaxies through mergers

Querejeta

Eliche‐Moral

Tapia

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Observations reveal a strong structural coupling between bulge and disc in S0 galaxies, which seems difficult to explain if they have formed from supposedly catastrophic events such as major mergers. Aims. We face this question by quantifying the bulge-disc coupling in dissipative simulations of major and minor mergers that result in realistic S0s. Methods. We have studied the dissipative N-body binary merger simulations from the GalMer database that give rise to realistic, relaxed E/S0 and S0 remnants (67 major and 29 minor mergers). We simulate surface brightness profiles of these S0-like remnants in the K band, mimicking typical observational conditions, to perform bulge-disc decompositions analogous to those carried out in real S0s. Additional components have been included when needed. The global bulge-disc structure of these remnants has been compared with real data. Results. The S0-like remnants distribute in the B/T -r e -h d parameter space consistently with real bright S0s, where B/T is the bulgeto-total luminosity ratio, r e is the bulge effective radius, and h d is the disc scalelength. Major mergers can rebuild a bulge-disc coupling in the remnants after having destroyed the structures of the progenitors, whereas minor mergers directly preserve them. Remnants exhibit B/T and r e /h d spanning a wide range of values, and their distribution is consistent with observations. Many remnants have bulge Sérsic indices ranging 1 < n < 2, flat appearance, and contain residual star formation in embedded discs, a result which agrees with the presence of pseudobulges in real S0s. Conclusions. Contrary to the popular view, mergers (and in particular, major events) can result in S0 remnants with realistically coupled bulge-disc structures in less than ∼3 Gyr. The bulge-disc coupling and the presence of pseudobulges in real S0s cannot be used as an argument against the possible major-merger origin of these galaxies.

show abstract

Analytical expressions for the deprojected Sérsic model

Cited by 44 publications

References 41 publications

Ages and structural and dynamical parameters of two globular clusters in the M81 group

Ages and structural and dynamical parameters of two globular clusters in the M81 group

HERschelObservations of Edge-on Spirals (HEROES)

Formation of S0 galaxies through mergers

Contact Info

Product

Resources

About