Photometric scaling relations of lenticular and spiral galaxies

Laurikainen, Eija; Salo, H.; Buta, Ronald J.; Knapen, Johan H.; Comerón, Sébastien

doi:10.1111/j.1365-2966.2010.16521.x

Cited by 202 publications

(417 citation statements)

References 140 publications

(294 reference statements)

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“…A1 and those in Dullo & Graham (2013) show that NGC 507, NGC 4382 and NGC 5813 are coreSérsic lenticular galaxies that are well described by a coreSérsic bulge plus an exponential disc model with very small rms residuals of 0.027 mag arcsec −2 , 0.016 mag arcsec −2 and 0.015 mag arcsec −2 , respectively. Laurikainen et al (2010Laurikainen et al ( , 2011 have also detected a weak nuclear bar in the unsharp mask image of NGC 507. Further, all of our core-Sérsic elliptical galaxies (Table 1), except for NGC 1016, NGC 3706 and NGC 4073, are in common with Hopkins et al (2009b).…”

Section: Multi-component Model Fits For Core-sérsic Galaxiesmentioning

confidence: 99%

See 1 more Smart Citation

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

145

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New surface brightness profiles from 26 early-type galaxies with suspected partially depleted cores have been extracted from the full radial extent of Hubble Space Telescope images. We have carefully quantified the radial stellar distributions of the elliptical galaxies using the core-Sérsic model whereas for the lenticular galaxies a core-Sérsic bulge plus an exponential disc model gives the best representation. We additionally caution about the use of excessive multiple Sérsic functions for decomposing galaxies and compare with past fits in the literature. The structural parameters obtained from our fitted models are in general, in good agreement with our initial study using radially limited (R < ∼ 10 ′′ ) profiles, and are used here to update several "central" as well as "global" galaxy scaling relations. We find near-linear relations between the break radius R b and the spheroid luminosity L such that R b ∝ L 1.13±0.13 , and with the supermassive black hole mass. This is internally consistent with the notion that major, dry mergers add the stellar and black hole mass in equal proportion, i.e., M BH ∝ L. In addition, we observe a linear relation R b ∝ R 0.98±0.15 e for the core-Sérsic elliptical galaxies-where R e is the galaxies' effective half light radii-which is collectively consistent with the approximately-linear, bright-end of the curved L − R e relation. Finally, we measure accurate stellar mass deficits M def that are in general 0.5−4 M BH , and we identify two galaxies (NGC 1399, NGC 5061) that, due to their high M def /M BH ratio, may have experienced oscillatory core-passage by a (gravitational radiation)-kicked black hole. The galaxy scaling relations and stellar mass deficits favor core-Sérsic galaxy formation through a few "dry" major merger events involving supermassive black holes such that M def ∝ M 3.70±0.76 BH , for M BH > ∼ 2 × 10 8 M ⊙ .

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Section: Multi-component Model Fits For Core-sérsic Galaxiesmentioning

confidence: 99%

“…Laurikainen et al (2010Laurikainen et al ( , 2011 fit a 3-component (bulge+bar+disc) model to this galaxy's ∼240 ′′ Ks-band light profile and noted that it has a large disc-like outer envelope and a weak inner bar. However, these (bar and disc) components were not detected in the ∼80 ′′ V -band light profile that we modelled.…”

Section: C1 Ngc 0584mentioning

confidence: 99%

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

145

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“…2, we define as Ellipticals all model galaxies with B/T > 0.7, and split our sample by hierarchy considering separately central and satellite galaxies in the upper and lower rows (only bins containing more that 10 objects are considered). Our choice for the threshold at B/T ∼ 0.7 is motivated by observational studies (Weinzirl et al 2009;Laurikainen et al 2010)) and by consistency with previous studies. We want to stress that our results do not change qualitatively if we assume a different B/T threshold for the definition of Elliptical galaxies (in the range 0.5-0.9).…”

Section: Resultsmentioning

confidence: 99%

On the dependence of galaxy morphologies on galaxy mergers

Fontanot

Macciò

Hirschmann

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The distribution of galaxy morphological types is a key test for models of galaxy formation and evolution, providing strong constraints on the relative contribution of different physical processes responsible for the growth of the spheroidal components. In this paper, we make use of a suite of semi-analytic models to study the efficiency of galaxy mergers in disrupting galaxy discs and building galaxy bulges. In particular, we compare standard prescriptions usually adopted in semi-analytic models, with new prescriptions proposed by Kannan et al., based on results from high-resolution hydrodynamical simulations, and we show that these new implementations reduce the efficiency of bulge formation through mergers. In addition, we compare our model results with a variety of observational measurements of the fraction of spheroid-dominated galaxies as a function of stellar and halo mass, showing that the present uncertainties in the data represent an important limitation to our understanding of spheroid formation. Our results indicate that the main tension between theoretical models and observations does not stem from the survival of purely disc structures (i.e. bulgeless galaxies), rather from the distribution of galaxies of different morphological types, as a function of their stellar mass.

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“…Other photometric relations well documented in the literature include the relation (k) between bulge and disk luminosities (Laurikainen et al 2010), and (f) which relates bulge and total luminosities (Carollo et al 2007). The rotation velocity of the galaxies is usually studied in comparison with integrated photometry, such as given in relation (b), the Tully-Fisher relation, and the sizevelocity relation (m) also studied by Courteau et al (2007).…”

Section: Idmentioning

confidence: 99%

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband

Barbosa

Oliveira

Amram

et al. 2015

Mon. Not. R. Astron. Soc.

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We present R c -band surface photometry for 170 of the 203 galaxies in GHASP, Gassendi H-Alpha survey of SPirals, a sample of late-type galaxies for which high-resolution FabryPerot H maps have previously been obtained. Our data set is constructed by new R c -band observations taken at the Observatoire de Haute-Provence (OHP), supplemented with Sloan Digital Sky Survey (SDSS) archival data, obtained with the purpose of deriving homogeneous photometric profiles and parameters. Our results include R c -band surface brightness profiles for 170 galaxies and ugriz profiles for 108 of these objects. We catalogue several parameters of general interest for further reference, such as total magnitude, effective radius and isophotal parameters -magnitude, position angle, ellipticity and inclination. We also perform a structural decomposition of the surface brightness profiles using a multi-component method in order to separate disks from bulges and bars, and to observe the main scaling relations involving luminosities, sizes and maximum velocities.We determine the R c -band Tully Fisher relation using maximum velocities derived solely from Hα rotation curves for a sample of 80 galaxies, resulting in a slope of −8.1 ± 0.5, zero point of −3.0 ± 1.0 and an estimated intrinsic scatter of 0.28 ± 0.07. We note that, different from the TF-relation in the near-infrared derived for the same sample, no change in the slope of the relation is seen at the low-mass end (for galaxies with V max < 125 km/s). We suggest that this different behaviour of the Tully Fisher relation (with the optical relation being described by a single power-law while the near-infrared by two) may be caused by differences in the stellar mass to light ratio for galaxies with V max < 125 km/s.

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Photometric scaling relations of lenticular and spiral galaxies

Cited by 202 publications

References 140 publications

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

On the dependence of galaxy morphologies on galaxy mergers

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband

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Photometric scaling relations of lenticular and spiral galaxies

Cited by 202 publications

References 140 publications

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

On the dependence of galaxy morphologies on galaxy mergers

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theRcband

Contact Info

Product

Resources

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GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband